[ { "id": "atel_60", "message": "Title: Black Hole Candidate XTE J1859+226 in the Low/Hard State\nAuthors: J. M. Miller, D. W. Fox, D. Pooley, W. H. G. Lewin (MIT)\nDate: 16 Jul 2000; 20:47 UT\nProvenance: Derek W. Fox (derekfox@mit.edu)\nSubjects: Radio, Optical, X-ray, Request for Observations, Black Hole, Transient\nDescription: Recent flaring activity of this source in the optical (Casares et al. 2000, IAUC # 7451 ) has motivated a public RXTE TOO observation on 8 July 2000.\nXTE J1859+226 is a known X-ray nova that reached 1.4 Crab in the RXTE/ASM in October 1999 (Smith 1999, ATEL #47). During that outburst the source exhibited 150 and 187 Hz quasi-periodic oscillations (Cui et al. 2000, ApJ 535, L123) and radio emission (Pooley & Hjellming, IAUC # 7278 ). The source has been undetected in RXTE/ASM dwells since March 2000.\nWe find that the PCA spectrum from 8 July 2000 is consistent with hard power-law emission, with photon index alpha=1.54(10) and total 3-25 keV flux of 1.08(20)e-11 ergs cm^-2 (assumed neutral hydrogen column N_H=5.5e21 cm^-2). This spectrum is consistent with the canonical Low/Hard spectral state of black hole X-ray binary systems.\nObservers may contact the authors (jmm@space.mit.edu) for possible coordination with their ongoing multi-wavelength campaign on this source.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Magnetar", "Active galactic nucleus", "Black hole" ] }, "answerKey": "D" }, { "id": "atel_120", "message": "Title: State Transition of GX 339-4\nAuthors: D. M. Smith, E. Kalemci (Space Sciences Laboratory, U. C. Berkeley), J. A. Tomsick, W. A. Heindl (Center for Astrophysics and Space Science, U. C. San Diego)\nDate: 25 Feb 2003; 02:22 UT\nProvenance: David M. Smith (dsmith@ssl.berkeley.edu)\nSubjects: Radio, X-ray, Gamma Ray, Request for Observations, Black Hole, Transient\nDescription: Referred to by ATel #: 196\nThe black hole candidate GX 339-4, in outburst for nearly a year (ATEL #85) has lately been declining rapidly in luminosity in the soft state and has now started to show signs of a transition to the low/hard state. We have been monitoring this source twice weekly with the Proportional Counter Array (PCA) on the Rossi X-ray Timing Explorer. As of 23 February, 17:30 UT, the power law component of the spectrum now dominates the 3-25 keV count rate. The root-mean-squared variability (beyond Poisson statistics) is low, only 2.4%, yet this is higher than has been seen in the soft state for the last few months. Radio and x-ray observations are particularly encouraged over the course of this week, which should find the source in a truly transitional phase.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Black hole", "Pulsar", "Near-Earth object" ] }, "answerKey": "B" }, { "id": "atel_240", "message": "Title: GX 339-4 detected with INTEGRAL\nAuthors: E. Kuulkers (ESA/ESTEC), A. Bodaghee (ISDC Geneva), L. Foschini (IASF/CNR Bologna), M. Guainazzi (ESA/Vilspa), G. Matt (Universiy of Roma), G. Israel (INAF - OA Roma), F. Nicastro (CfA), T. Oosterbroek (ESA/ESTEC), A. Parmar (ESA/ESTEC), J. Rodriguez (CEA/Saclay & ISDC Geneva), R. Walter (ISDC Geneva)\nDate: 19 Feb 2004; 06:30 UT\nProvenance: Erik Kuulkers (ekuulker@rssd.esa.int)\nSubjects: X-ray, Gamma Ray, Binary, Black Hole, Transient, Variables\nDescription: Referred to by ATel #: 243, 270\nGX 339-4 was in the field of view during an observation of IGR J16318-4848 with INTEGRAL (UT 2004 Feb 18 03:41 - Feb 18 17:29). Further to the increase in activity reported in the optical/radio (ATel #230) and X-rays (ATel #231, #236), we report the detection of GX 339-4 with Jem-X and ISGRI/IBIS onboard INTEGRAL. Between 2004 Feb 18 03:41 - 10:09 (UT) the average observed fluxes were ~37 mCrab, ~46 mCrab, ~24 mCrab, and ~38 mCrab, in, respectively the 3-10 keV, 10-31 keV (Jem-X), 20-60 keV, and 60-200 keV (ISGRI/IBIS) energy bands.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system, Black hole", "Variable star, Black hole", "Circumstellar disk, Black hole", "Minor body, Black hole" ] }, "answerKey": "A" }, { "id": "atel_300", "message": "Title: Radio Monitoring of V4641 with RATAN-600\nAuthors: S. A. Trushkin (SAO RAS)\nDate: 8 Jul 2004; 19:38 UT\nProvenance: Sergei Trushkin (satr@sao.ru)\nSubjects: Radio, Binary, Black Hole\nDescription: Referred to by ATel #: 303\nWe have daily observed V4641 from 9 May up today at 2.3, 4.8, 7.7, 11.2 and 21.7 GHz with RATAN-600 radio telescope. We have reliably detected V4641 June 25, 21:20UT: \n * Freq. mJy err \n * 2.3 160 25 \n * 4.8 250 25 \n * 7.7 270 30 \n * 11.2 285 30 \n\nJuly 03, 20:44UT: \n * Freq. mJy err \n * 2.3 215 25 \n * 4.8 350 30 \n * 7.7 335 30 \n * 11.2 275 30 \n * 21.7 300 35 \n\nand July 04, 20:40UT: \n * Freq. mJy err \n * 2.3 78 15 \n * 4.8 66 10 \n * 7.7 93 20 \n * 11.2 33 10 \n\nSee the graph of the spectra: http://cats.sao.ru/~satr/XB/1819-25/v4641_sp.gif. There are no detectable signals 5,6,7 July ~20:30UT and before 25 June. Thus the detected radio flares decayed during 1-2 days. We will continue observations V4641 to 17 August.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system, Pulsar", "Binary system, Globular cluster", "Binary system, Repeater", "Binary system, Black hole" ] }, "answerKey": "D" }, { "id": "atel_375", "message": "Title: Second-epoch VLA observations of SGR 1806-20\nAuthors: B. M. Gaensler (CfA), C. Kouveliotou (NASA/MSFC, NSSTC), R. Wijers (U. Amsterdam), M. Garrett (JIVE), M. Finger, P. Woods, S. Patel (USRA, NSSTC), M. McLaughlin (Jodrell Bank), R. Fender (U. Southampton), T. Delaney (CfA) report on behalf of a larger team:\nDate: 4 Jan 2005; 15:31 UT\nProvenance: Bryan Gaensler (bgaensler@cfa.harvard.edu)\nSubjects: Radio, Neutron Star, Soft Gamma-ray Repeater, Transient, Variables, Pulsar\nDescription: Referred to by ATel #: 380\nWe observed the soft gamma-ray repeater SGR 1806-20 with the Very Large Array (VLA) in the A-configuration for a second time on January 4, 2005 for one hour (14:15-15:15 UT). We detect the source at the same coordinates as reported by Gaensler et al. (GCN #2929; ATEL #373). Preliminary flux levels, including improved estimates of the fluxes reported in ATEL #373, are as follows (the numbers in parentheses indicate approximate uncertainties in the last significant figures): \n \n \n Frequency Flux (2005 Jan 03.8) Flux (2005 Jan 04.6) \n \n (GHz) (mJy) (mJy) \n \n --------- -------------------- -------------------- \n \n 1.4 172(4) 135(10) \n \n 4.9 80(1) 66(2) \n \n 8.5 53(1) 38(5) \n \nThese results indicate a decay in the flux at a rate of approximately 1.9 mJy/hour at 1.4 GHz. At the same time the spectrum has remained constant. On Jan 3, 2005 the spectral index (in the sense F_nu ~ nu^alpha) was alpha = -0.65+/-0.05, while on Jan 4, 2005 the spectral index was -0.61+/-0.06. \nA reanalysis of the VLA data from 3 Jan 2004 (GCN #2928, GCN #2929; ATEL #373) suggests that the radio source associated with SGR 1806-20 is slightly extended at both 4.9 and 8.5 GHz. Assuming that the underlying geometry is an optically thin, spherical thin shell, data at both frequencies independently suggest a source of approximate diameter 50-100 milliarcseconds. This implies a projected expansion speed of approx (0.3-0.6)c over the 7 days since the initial giant SGR flare (assuming a source distance of 15.1 kpc; Eikenberry, S. et al., ApJ 616, 506, 2004). \nFurther radio observations of this source with the Westerbork Synthesis Radio Telescope (WSRT), the MERLIN VLBI network and the Parkes Radio Observatory are currently underway or are being scheduled, and will be reported as they are analyzed. We will continue monitoring the source with the VLA until it fades below detection level.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Black hole", "Nova", "Variable star" ] }, "answerKey": "A" }, { "id": "atel_425", "message": "Title: Radio holding steady in GRO J1655-40\nAuthors: M. P. Rupen (NRAO/GSFC), A. J. Mioduszewski, V. Dhawan(NRAO)\nDate: 23 Feb 2005; 22:17 UT\nProvenance: Michael P. Rupen (mrupen@nrao.edu)\nSubjects: Radio, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 437, 487\nVery Large Array (VLA) observations of the black hole X-ray binary GRO J1655-40 on Feb. 23rd (MJD 53424.6) show that the radio source seen on Feb. 20th (ATEL #419) has remained roughly constant, with flux densities of 1.53 +/- 0.07 mJy at 4.86 GHz, and 1.45 +/- 0.08 mJy at 8.46 GHz. These data, taken in much better weather conditions, show a fairly flat spectrum (flux density going as frequency to the -0.10 +/- 0.14), suggesting a very small (milliarcsecond or less) source. A Gaussian fit to the 8.46 GHz data yields a more direct upper limit to the size of about 1.1 arcseconds, compared to the 2.6 x 0.6 arcsec full-width-at-half-maxmimum of the beam (major axis oriented 6.1 degrees east of north). Further radio observations are planned. \nThe National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Exoplanet", "Globular cluster, Binary system", "Black hole, Binary system", "Star and stellar system, Binary system" ] }, "answerKey": "C" }, { "id": "atel_500", "message": "Title: Swift XRT Observation of the XTE J1747-274 field\nAuthors: J. A. Kennea, D. N. Burrows (PSU), C. Markwardt (UMD/GSFC), N. Gehrels (GSFC)\nDate: 24 May 2005; 22:25 UT\nProvenance: Jamie A. Kennea (kennea@astro.psu.edu)\nSubjects: X-ray, Transient\nDescription: Referred to by ATel #: 521, 1445, 1459\nStarting on May 23rd 2005, 22:09UT the Swift observatary observed a field centered on the RXTE source RXTE J1747-274 (Markwardt et al., ATEL #498). After ground processing we obtained 1261s of Photon Counting mode data from the Swift XRT. From these data we find a bright point source located at: \n \nRA(J2000): 17:47:17.8 \nDec(J200): -27:20:39 \nWe estimate an uncertainty of 6 arcseconds radius (90% containment). We note that this source is 66 arcseconds away from the INTEGRAL detected transient IGR J17473-2721 (Grebenev et al., ATEL #467) and 7 arcminutes from the RXTE position. This is the only source detected in the XRT field of view and we conclude that the source detected in this field is in fact IGR J17473-2721. \nThe spectrum of this source is highly absorbed, and best fit with a power-law spectrum. The best fit parameters are N_H = (5.2 +/- 0.4) x 10^22 cm^-2 with a photon index of 2.12 +/- 0.16 (errors quoted at 90% confidence). The flux from this source in the 0.5-10 keV range is (8.4 +/- 0.9) x 10^-10 erg/s/cm^2. Assuming a distance of 8.5 kpc and correcting for absorption this gives an X-ray luminosity of approximately 2 x 10^37 erg/s (0.5 - 10 keV). \nIt is noted that this flux is approximately a factor of ten lower than the flux reported from XTE J1747-274 in ATEL #498. Continuing measurements of XTE J1747-274 with RXTE have shown that the source continues to be visible at the flux level seen on May 20th. Therefore we suggest that XTE J1747-274 is in fact outside of the XRT field of view, which is defined as as a box with the corners at the following coordinates: \n \n(1) RA=17:48:21 Dec=-27:21:08 \n(2) RA=17:46:58 Dec=-27:17:04 \n(3) RA=17:46:42 Dec=-27:34:49 \n(4) RA=17:48:06 Dec=-27:38:12", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Quasar", "Black hole, Supernova", "Black hole, Star and stellar system", "Black hole, Neutron star" ] }, "answerKey": "D" }, { "id": "atel_550", "message": "Title: RXTE observations of Swift J1753.5-0127\nAuthors: Ed Morgan (MIT), Jean Swank (NASA/GSFC), Craig Markwardt (Univ. MD and NASA/GSFC), and Neil Gehrels (NASA/GSFC)\nDate: 2 Jul 2005; 19:53 UT\nProvenance: Edward Morgan (ehmorgan@mit.edu)\nSubjects: X-ray, Black Hole\nDescription: Referred to by ATel #: 551, 574\nAnalysis of the ASM data of SWIFT J1753.5-0127 (Atel #546) using the Swift position (Atel #547) show that the outburst began on 2005 June 29, rising to a level of 140 mCrab on July 1. An observation made with the PCA on July 1 at 01:00 UT shows the source at 120 mCrab. The PDS of the PCA observation shows a 0.6 Hz QPO with a shape typically seen in BH Candidates.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Pulsar", "Magnetar", "Repeater" ] }, "answerKey": "A" }, { "id": "atel_650", "message": "Title: A reversal of the X-ray spectral evolution of RX J0720.4-3125 : the blackbody temperature is decreasing\nAuthors: Jacco Vink (Univ. Utrecht), Frank Haberl (MPE), Cor de Vries (SRON), Silvia Zane (MSSL), Roberto Turolla (Univ. Padua), Mariano Mendez (SRON), and Frank Verbunt (Univ. Utrecht)\nDate: 2 Nov 2005; 22:51 UT\nProvenance: Jacco Vink (j.vink@astro.uu.nl)\nSubjects: Neutron Star\nDescription: This telegram is prompted by the latest XMM-Newton observation of the isolated, radio quiet, neutron star RX J0720.4-3125, which shows that the blackbody temperature started decreasing (see Table below). This means that the spectral evolution observed over the last 4 years has reversed. \nMuch like other sources in its class, RX J0720.4-3125 exhibits a blackbody-like spectrum in the soft X-rays. However, since the first Chandra and XMM-Newton observations in 2000, the blackbody temperature underwent rather significant changes, rising from kT~86 eV to kT~95 eV in October 2003 (de Vries et al. 2004, Vink et al. 2004). At the same time, the spectral shape became more complicated exhibiting a significant broad absorption feature (only weakly present in the first observation). Moreover, the strength of the gaussian absorption component (Haberl et al. 2004) increased with time and appears to correlate with the blackbody temperature. The evolution was gradual from 2000 to May 2003, but was more rapid from May 2003 to October 2003. Subsequent observations by XMM-Newton and Chandra did not detect any further evolution from October 2003 to May 2005. The latest XMM-Newton observation (September 23, 2005), however, indicates that the source spectral evolution has reversed. A first hint for a trend reversal was already provided by the previous observation on April 28 2005, but with a lower significance. \nIn order to avoid inter-instrumental calibration issues we only report on the data taken with the XMM-Newton PN instrument in Full Frame Imaging mode with the \"Thin\" filter. \n \nTABLE \n \nObs. Date | kTBB | BB Area | Abs. line Eq. Width \n---|---|---|--- \n| (eV) | (km2 @ 300pc)| (eV) \n13-05-2000 | 86.29±0.10| 23.5 | 5.8 \n06/08-11-2002| 88.39±0.09| 21.8 | 16.6 \n22-05-2004 | 94.96±0.15| 16.9 | 56.8 \n28-04-2005 | 94.56±0.11| 18.5 | 56.0 \n23-09-2005 | 93.38±0.11| 19.2 | 53.2 \nErrors on the temperature indicate 90% confidence ranges. The absorption column, and absorption line energy and width were coupled for all observations, with best-fit values NH = 1.06x1020 cm-2, E = 305 eV and sigma=71 eV, respectively. \nThe cause of the spectral evolution is still unclear. It is unlikely that it is caused by a time-varying accretion rate, because the large proper motion makes accretion from the ISM highly inefficient (Motch et al. 2003). This suggests that the spectral evolution is either connected to the internal evolution of the neutron star, e.g. in the magnetic field strength/topology, or to changes in the viewing geometry of the X-ray emitting region, e.g. if the neutron star precesses. In the latter case a cyclic behavior of the spectral evolution may be expected. \nIn the light of the possible implications for the physical mechanism responsible for the observed changes, the reversal in the temperature evolution is of particular relevance. Note that the temperature evolution since October is modest, but as the rapid change in temperature between May and October 2003 indicates, the spectral evolution may suddenly accelerate on a time scale < 6 month.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Exoplanet", "Minor body", "Repeater" ] }, "answerKey": "A" }, { "id": "atel_725", "message": "Title: Continuing RXTE observations of XTE J1701-462: a new \"Z\" in town?\nAuthors: Jeroen Homan (MIT), Tomaso Belloni (INAF/OAB), Michiel van der Klis, Piergiorgio Casella (U. Amsterdam), Mariano Mendez (SRON), Walter Lewin (MIT), Rob Fender (U. Southampton), Elena Gallo (UCSB), and Neil Gehrels (NASA/GSFC)\nDate: 8 Feb 2006; 12:50 UT\nProvenance: Jeroen Homan (jeroen@space.mit.edu)\nSubjects: X-ray, Binary, Neutron Star, Transient\nDescription: Referred to by ATel #: 748, 777\nSince January 19 the new X-ray transient XTE J1701-462 (ATels #696, #703, #708, #710) has been observed more than 45 times with the Rossi X-ray Timing Explorer (RXTE). Preliminary analysis of the RXTE data suggest the source is a neutron star LMXB and is currently showing behavior typical of the so-called \"Z sources\" (i.e. the brightest, persistent neutron star LMXBs). This would make XTE J1701-462 the first new Z source in nearly 35 years. \nThe prospect of XTE J1701-462 of being a transient Z source opens up interesting possibilities if the source eventually fades away. A major question that can be addressed is whether at lower mass accretion rates Z sources start to behave like atoll sources. Regardless of these future opportunities, XTE J1701-462 already is a unique and interesting source and we strongly urge observers to continue or start monitoring the source at all wavelengths. For those who are interested a detailed description of the RXTE observations is given below. \nFor figures, visit: http://tahti.mit.edu/Z \n\nRXTE/PCA light curves reveal that the source continues to exhibit large count rate changes (by factors of more than two on a time scale of hours). However, occasionally the count rate can be relatively stable for periods of ~1 day. The count rate changes are often accompanied by large changes in the X-ray colors, especially above 8 keV. \nIn a color-color diagram (CCD) these spectral changes result in a multi-branched track that resembles those of some of the neutron star Z sources, in particular that of GX 5-1 (see figure 13 in Jonker et al. 2002, MNRAS, 333, 665). In the plot of our CCD we tentatively identify some of the branches as the horizontal branch (with strong upturn), the normal branch, and the flaring branch (with a dipping branch, as also seen in GX 5-1). Over the course of our observing campaign the overall position of the track has shifted to slightly softer colors. Such shifts are not uncommon in Z sources. These shift are even more apparent in color-intensity diagrams (CIDs). The sharp turn that we identify as the horizontal/normal branch vertex has slowly increased in count rate during the past two and a half weeks, suggesting that the source has increased in brightness by more than 20%. We also note that the flaring branch is inverted - this is particularly clear when plotting count rate vs. soft X-ray color. Such behavior has previously been seen before in the Z source Cygnus X-2. \nThe rapid X-ray variability properties of the source evolve smoothly along the track in the CCD/CID (see link above for example power spectra). At the start of the horizontal branch (upturn) we detect a ~10 Hz QPO that smoothly increases in frequency along the horizontal branch onto the top normal branch where it reaches a maximum of ~55 Hz (see also ATel #703). This QPO is accompanied by band limited noise that also increases in frequency. Both QPO and noise decrease in strength as their frequencies increase. Around the middle of the normal branch we detect a broad feature near 5-6 Hz (see also ATel #703), which is particularly clear in power spectra above 8 keV. The feature disappears near the bottom of the normal branch. On the flaring branch the power spectrum only shows weak red noise (rms variability [0.1-100 Hz] is ~2.5%, compared to 16% on the top of the horizontal branch). \nThe evolution of the timing features along the tracks in the CCD/CID as well as their typical strength and frequency are very similar to those seen in the Z sources. The relatively weak power-law component in the energy spectra further supports the link with the Z sources. Other neutron star signatures, like X-ray bursts, pulsations, or kHz QPOs have not been detected so far.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater", "Near-Earth object", "Neutron star", "Star and stellar system" ] }, "answerKey": "C" }, { "id": "atel_840", "message": "Title: High state of Mkn 421 in the hard X-rays\nAuthors: G. G. Lichti (MPE), A. Neronov, N. Mowlavi (ISDC), M. Ajello, V. Beckmann, C. Boisson, J. Buckley, P. Charlot, W. Collmar, B. Degrange, A. Djannati-Atai, A. Falcone, J. Finley, G. Fossati, G. Henri, K. Katarzynski, D. Kieda, A. Lahteemaki, K. Mannheim, A. Marcowith, M. Punch, A. Saggione, L. Sauge, V. Schoenfelder, A. Sillanpaa, D. Smith, H. Sol, F. Tavecchio, L. Takalo, M. Tornikoski, A. von Kienlin, T. Weekes (Co-Is of the INTEGRAL observation)\nDate: 16 Jun 2006; 20:12 UT\nProvenance: Nami Mowlavi (Nami.Mowlavi@obs.unige.ch)\nSubjects: X-ray, Gamma Ray, AGN\nDescription: Referred to by ATel #: 848, 1449, 2292\nRXTE/ASM data revealed an increased activity in the 3-10 keV energy of the TeV gamma-ray loud blazar Mkn 421. Its intensity began to rise in the middle of April 2006, reached a maximum around mid May and decreased since then. Its intensity began to increase again around 10th of June, 2006. This second increase led to the triggering of a target-of-opportunity observation with INTEGRAL. \n \nThe observation of this blazar by INTEGRAL started on June 14, 2006. The source is detected by both the IBIS/ISGRI imager and the JEM-X X-ray monitor. The flux level during the first two days of observation was ~25 mCrab in both 3-10 keV and 20-40 keV energy bands. From 2006-06-16T07:16 UTC, the fluxes increased to ~50 mCrab within 3 hours in both energy bands, and the source became detected in the 40-80 keV band with a flux of ~25 mCrab. \n \nThe blazar will be monitored continually by INTEGRAL until July 25. Simultaneous observations with other telescopes and instruments are planned with the Metsahovi Radio Observatory at 37 GHz, with the KVA telescope in La Palma, with the VLBA at NRAO, and with SWIFT. MAGIC will also try to observe this source. \n \nFurther follow-up observations of this source at all wavelengths are strongly encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Magnetar", "Exoplanet", "Active galactic nucleus" ] }, "answerKey": "A" }, { "id": "atel_930", "message": "Title: Continuous presence of bipolar jets from Z And during its 2006 outburst\nAuthors: A. Skopal (Astronomical Institute, Slovak Academy of Sciences, Tatranska Lomnica), M. Wolf (Astronomical Institute, Charles University, Prague)\nDate: 3 Nov 2006; 18:18 UT\nProvenance: Augustin Skopal (skopal@ta3.sk)\nSubjects: Optical, Binary, Variables\nDescription: We report on the continuing activity of the symbiotic prototype Z And during its 2006 major outburst that began in 2006 April (cf. ATEL 882). The system still keeps its brightness at a high level (U=9.04, B=9.79, V=9.24, Rc=8.58 as measured on 2006 Oct 26.88 at the Skalnate Pleso Observatory), which is comparable with that from 2006 Aug 15.88 (U=8.87, B=9.43, V=8.94, Stara Lesna Observatory). \nOn 2006 Oct 18.90 we obtained high-resolution spectrum of Z And (R = 13000) at the Ondrejov Observatory, Academy of Sciences of the Czech Republic, using the coude spectrograph of 2-m reflector in the range of 6400 - 6920 A. A strong central H-alpha emission component was accompanied by weak jet emissions located strictly bipolarly at radial velocities |RV| = 1165(+/-11) km/s. The integrated fluxes and FWHM for the violet and the red jet were 4.1(0.5), 2.9(0.5) x 1.0E-12 erg sE-1 cmE-2 and 201(10), 192(11) km/s, respectively. The flux ratio of the violet to the red component was ~ 1.4, whereas on 2006 Aug 30 this ratio was ~ 1. This could be caused by an occultation of the red jet by the giant at its inferior conjunction (orbital phase = 0.016 on 2006 Oct 18.9). Contrary to the spectrum from 2006 Aug 30, absorption component in the HeI 6678 profile was not present. The Raman scattered OVI line at 6830 A was not detectable in the present spectrum. We estimate the full extension of the jet features to about 200 m.a.s. for the distance of 1.5 kpc. Z And thus could be detectable on the radio images, for example.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system", "Repeater", "Stellar evolution", "Pulsar" ] }, "answerKey": "A" }, { "id": "atel_1000", "message": "Title: INTEGRAL observations of GX339-4: preliminary spectral fit results\nAuthors: M. D. Caballero-Garcia (LAEFF/INTA), J. Miller (Univ. of Michigan), E. Kuulkers (ESA/ESAC), M. Diaz Trigo (ESA/ESAC), on behalf of a larger collaboration\nDate: 11 Feb 2007; 09:48 UT\nProvenance: Erik Kuulkers (ekuulker@rssd.esa.int)\nSubjects: Binary, Black Hole, Transient, Variables\nDescription: We present the results of preliminary spectral fits to the first 130 ksec INTEGRAL ToO observation of GX 339-4 (see ATel #980, #986), obtained between 2007, Jan 30, 15:56 and Feb 01, 06:11. We made joint spectral fits to spectra obtained with the JEM-X (5-20 keV) and IBIS/ISGRI (23-300 keV) instruments. \nThe model that best phenomenologically fits the joint spectrum consists of an absorbed multi-color black-body disk plus a powerlaw with a high-energy cut-off at 22 +/- 5 keV and a folding energy of 68 +/- 5 keV. The presence of curvature between 20-30 keV and line-like residuals revealed between 6-8 keV, is likely due to disk reflection. We will explore fits with reflection models in future work. \nThe presence of the radiation coming from the disk is significant, and we find a color temperature of the inner disk of T = 1.5 +/- 0.1 keV. The powerlaw has a photon index of 1.67 +/- 0.07. These parameters are broadly consistent with rising hard states. The implied luminosity of the source in the 5-300 keV band was L = 1.3-1.7 E+38 erg/s, calculated taking into account a distance to the source of 8.5 kpc. \nWe examined the JEM-X and IBIS/ISGRI light curves with a time binning of 1000 sec, in the 3-6, 6-10, 10-15, 15-35, 20-40, 40-60, 60-100, 100-200 keV energy ranges. The source was slowly increasing its brightness since the beginning of the observation in the overall energy range of 3-200 keV. \nPostScript figures of the preliminary spectral fit results, as well as the JEM-X and IBIS/ISGRI light curves, can be found at http://isdc.unige.ch/~kuulkers/GX339-4/.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk, Black hole", "Binary system, Neutron star", "Binary system, Black hole", "Variable star, Black hole" ] }, "answerKey": "C" }, { "id": "atel_1075", "message": "Title: kHz QPOs during the decay of the outburst of IGR J17191-2821\nAuthors: M. Klein-Wolt (University of Amsterdam), R. Wijnands (University of Amsterdam), J. H. Swank (NASA/GSFC), C. B. Markwardt (CRESST/U. Md./NASA/GSFC)\nDate: 16 May 2007; 10:38 UT\nProvenance: Marc Klein-Wolt (klein@science.uva.nl)\nSubjects: X-ray, Neutron Star, Transient\nDescription: Referred to by ATel #: 1096, 4170\nWe continued to monitor the outburst of the transient IGR J17191-2821 (ATels #1021,#1022,#1025,#1065,#1068,#1069,#1070) with RXTE/PCA and Swift/XRT observations. After our last Swift/XRT observation on May 07 (18:30 UTC, ATel #1070) were we detected the source at a level of ~53 mCrab, our pointed RXTE/PCA observations reveal the source has shown a small increase in flux to ~64 mCrab on May 08 (00:21 UTC) and after that a steady decay to about 8 mCrab (May 12, 01:53 UTC). More recent RXTE/PCA bulge scan observations (May12, 23:41 UTC) and the latest observation obtained during our Swift/XRT monitoring campaign (May 13, 23:33 UTC) detect the source at even lower levels of ~5 and ~2 mCrab, respectively. \nIn 12 of our 17 RXTE/PCA observations we detected a kHz QPO in the range between 700 and 900 Hz (detection level at ~9 sigma, single trail in the 2-60 keV energy range). Also, on several occasions when we detected this QPO, we detected an additional kHz QPO at a frequency of ~1030 Hz. Very likely this QPO can be identified with the upper kHz QPO and the one at lower frequencies with the lower kHz QPO. The frequency separation is about 330 Hz and is consistent within 3 sigma with the spin frequency as determined from the oscillations seen during the reported type-I X-ray bursts (ATel # 1068). \nThe behavior of IGR J17191-2821 during its outburst is characteristic for neutron star atoll sources in outburst, and from the combined energy spectral and temporal information we conclude that in the last few days the source has made a transition from the banana to the island state. \nWe thank the Swift Team for scheduling the Swift/XRT observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Minor body", "Neutron star", "Variable star" ] }, "answerKey": "C" }, { "id": "atel_1175", "message": "Title: Swift/XRT observations of the neutron-star X-ray transient SAX J1810.8-2609\nAuthors: N. Degenaar, M. Klein-Wolt and R. Wijnands (University of Amsterdam)\nDate: 9 Aug 2007; 19:38 UT\nProvenance: Rudy Wijnands (rudy@space.mit.edu)\nSubjects: X-ray, Binary, Neutron Star, Transient\nDescription: Referred to by ATel #: 1185, 1227, 1260\nFollowing reports of renewed activity of the neutron-star X-ray transient SAX J1810.8-2609 (GCN 6706 and 6707), we triggered our Swift monitoring program on very-faint X-ray transients when in outburst. As part of this program, SAX J1810.8-2609 is currently observed on a daily basis with Swift using ~1 ksec exposures, starting August 6, 2007. In all our observations so far, the source X-ray spectrum can be fit using an absorbed powerlaw model with a hydrogen column density of Nh~0.5E22 cm2 and a powerlaw index of ~2. The source flux shows a gradual increase from ~4.7E-11 erg/cm2/s on August 6, to ~8.0E-11 erg/cm2/s on August 8 and up to ~1.1E-10 erg/cm2/s on August 9 (2-10 keV unabsorbed fluxes). Assuming a distance to SAX J1810.8-2609 of 5 kpc (inferred from type-I X-ray burst analysis; Natalucci et al., 2000, ApJ 536, 891), the derived fluxes translate into X-ray luminosities of ~1.4E35 erg/s, ~2.4E35 erg/s and ~3.3E35 erg/s, respectively. Swift monitoring observations of SAX J1810.8-2609 are ongoing. \nWe thank the Swift team for a prompt scheduling of our monitoring observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Neutron star", "Minor body", "Interstellar medium" ] }, "answerKey": "B" }, { "id": "atel_1290", "message": "Title: Detection of SN 2006jd in X-Rays with Swift\nAuthors: S. Immler (NASA/CRESST/GSFC), P. J. Brown (PSU), A. V. Filippenko (UC Berkeley), and D. Pooley (U of Wisconsin), on behalf of the Swift satellite team\nDate: 19 Nov 2007; 23:00 UT\nProvenance: Stefan Immler (immler@milkyway.gsfc.nasa.gov)\nSubjects: Optical, Ultra-Violet, X-ray, Supernovae\nDescription: Referred to by ATel #: 1420\nSwift Ultraviolet/Optical Telescope (UVOT) and X-Ray Telescope (XRT) observed the type-IIb SN 2006jd (CBET #673, CBET #679, but reclassified by Filippenko as type-IIn based on recent optical Keck spectra) on 2007-11-16.73 UT. A bright X-ray source is detected in the 2.3 ks XRT observation at the position of the SN, well offset (22 arcsec) from the nucleus of the host galaxy UGC 4179. The XRT net count rate is (6.3+/-2.0)E-03 cts/s, corresponding to an unabsorbed (0.2-10 keV band) X-ray flux of (3.4+/-1.1)E-13 erg/cm/cm/s and a luminosity of (2.5+/-0.8)E41 erg/s for an adopted thermal plasma spectrum with a temperature of kT = 10 keV, a Galactic foreground column density of N_H = 4.5E+20 (Dickey & Lockman, 1990, ARAA 28) and a distance of 79 Mpc (z=0.018556, NED; H_o = 71 km/s/Mpc, Omega_M = 1/3, Omega_L = 2/3). \nThe following approximate UVOT magnitudes were measured in observations beginning at 2007-11-16.73 UT: v = 19.1±0.4 (173 s exposure time), b = 19.3±0.3 (173 s), u = 18.2±0.3 (173 s), uvw1 [181-321nm] = 18.2±0.3 (348 s), uvm2 [166-268 nm] = 18.8±0.3 (465 s), and uvw2 [112-264 nm] = 19.2±0.3 (694 s). The photometry is complicated by the faint SN being superimposed on the galaxy. A background region was chosen to be similar to that near the SN, and the error bars have been increased to account for the uncertainty in the background subtraction. These magnitudes are on the UVOT photometric system (see Poole et al., 2007, MNRAS, accepted [astro-ph/0708.2259]) which in the optical is close to the Johnson UBV system. They have not been corrected for extinction. \nFurther Swift observations are planned.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system", "Accreting object", "Supernova", "Circumstellar disk" ] }, "answerKey": "C" }, { "id": "atel_1400", "message": "Title: Further observations of GRO J1750-27 (AX J1749.1-2639) with INTEGRAL\nAuthors: S. Brandt (DNSC, Denmark), S. Shaw (Southampton, UK/ ISDC, Switzerland), A. Hill (Southampton, UK), P. Kretschmar (ESA/ESAC, Spain), R. Wijnands (UvA, The Netherlands), T. Oosterbroek (ESA/ESTEC, The Netherlands), E. Kuulkers (ESA/ESAC, Spain), V. Beckmann (ISDC, Switzerland), S. Soldi (ISDC, Switzerland), J. Chenevez (DNSC, Denmark), T. J.-L. Courvoisier (ISDC, Switzerland), A. Domingo (LAEFF/INTA, Spain), K. Ebisawa (ISAS, Japan), P. Jonker (SRON, The Netherlands), C. Markwardt (GSFC, USA), A. Paizis (INAF-IASF, Italy), D. Risquez (LAEFF/INTA, Spain), C. Sanchez-Fernandez (ESA/ESAC, Spain)\nDate: 28 Feb 2008; 15:22 UT\nProvenance: Søren Brandt (sb@spacecenter.dk)\nSubjects: X-ray, Gamma Ray, Binary, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 1401, 7096\nThe transient accreting X-ray pulsar GRO J1750-27 (AX J1749.1-2639), which became active end of January 2008 (ATel #1376), has been repeatedly observed by the INTEGRAL Galactic Bulge monitoring program since mid February (ATel #1385) on 11, 20 and 23 Feb. 2008. \nDuring the three observations, totalling about 27 ks, the source has remained bright at a roughly constant level with the following flux averaged over the 3 observations: 186+/-9 mCrab (3-10 keV), 319+/-15 mCrab (10-25 keV), 198+/-2 mCrab (18-40 keV), and 20+/-3 mCrab (40-100 keV). \nWe observe a continuing spin-up with barycentric periods measured with the JEM-X and ISGRI instruments from 4.4547+/-0.0001 s (MJD=54507.7; see also ATel #1385), to 4.4527+/-0.0001 s (MJD=54516.7), and to 4.4518+/-0.0001 s (MJD=54519.7). Applying the orbital parameters of Scott et al. (ApJ 488, 831, 1997) from the 1995 outburst, we estimate the intrinsic spin-up to be 60+/-20 pico-Hz/s, where about 11-15 pHz/s of the error is due to the uncertainties in the 29.817 day orbital period. We note that the spin-up is likely to be higher than the 38 pHz/s observed during the 1995 outburst. \nThe pulse profile clearly shows two broad peaks, while Scott et al. reported a single broad peak in the BATSE data. This may be explained by our broader spectral coverage at lower energies and by better statistics. The peaks differ in their spectral shape: while they are of similar strength below 5 keV, one peak begins to dominate with increasing energy. \nThe pulsed fraction is estimated to about 30% in the ISGRI 18-40 keV band and about 15% in the JEM-X 3-10 keV band. \nThe INTEGRAL Galactic Bulge monitoring program resumes observing the source with 3 day intervals starting on Feb. 29, 2008.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object, Globular cluster", "Binary system, Pulsar", "Accreting object, Pulsar", "Accreting object, Accreting object" ] }, "answerKey": "C" }, { "id": "atel_1470", "message": "Title: Radio Observations of SN 2008be\nAuthors: A. Soderberg (Princeton), P. Chandra (UVA)\nDate: 11 Apr 2008; 17:00 UT\nProvenance: Alicia M. Soderberg (ams@astro.caltech.edu)\nSubjects: Radio, Supernovae\nDescription: We observed the Type IIn SN 2008be (CBET #1303) with the Very Large Array at 8.46 GHz on Apr 8.14 UT. We do not detect a radio source coincident with the optical SN position and place a 3 sigma upper limit on the flux density of 0.12 mJy. We thank the scheduling committee and operators for making these observations possible.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Repeater", "Supernova", "Minor body" ] }, "answerKey": "C" }, { "id": "atel_1560", "message": "Title: Swift detects an outburst of the recurrent supersoft X-ray transient in NGC 300\nAuthors: A. K.H. Kong (NTHU, Taiwan), R. Di Stefano (CfA)\nDate: 5 Jun 2008; 17:40 UT\nProvenance: Albert Kong (akong@cfa.harvard.edu)\nSubjects: X-ray, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 1626\nWe report Swift XRT observations of the supersoft X-ray transient (XMMU J005510.7-373855) in NGC 300 (Kong & Di Stefano 2003). The source was first detected as a supersoft X-ray source (kT ~ 50 eV) in 1992 with ROSAT and disappeared in subsequent X-ray observations. The source was active again in 2000 December and 2001 January and was detected with XMM-Newton with luminosities of 1e38 - 1e39 erg/s. However, the source fell below the detection limit of Chandra HRC-I on 2006 June 1 with a 99% upper limit of 3.5e37 erg/s (0.2-2 keV). NGC 300 was observed with Swift on 2008 May 20 and June 4 for 6 ks and 6.9 ks, respectively. The supersoft X-ray transient was clearly detected with XRT in both observations and all the source photons are from below 0.7 keV. The 0.2-2 keV unabsorbed luminosity is about 2e38 erg/s (d=2Mpc), assuming a blackbody spectrum with kT=60 eV and N_H=1e21 cm^-2 (Kong & Di Stefano 2003).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Quasar", "Star and stellar system, Binary system", "Black hole, Magnetar", "Black hole, Binary system" ] }, "answerKey": "D" }, { "id": "atel_1650", "message": "Title: GLAST LAT detection of a possible new gamma-ray flaring blazar: PKS 1502+106\nAuthors: S. Ciprini (Univ./INFN Perugia) on behalf of the GLAST Large Area Telescope Collaboration\nDate: 8 Aug 2008; 00:02 UT\nProvenance: Stefano Ciprini (stefano.ciprini@pg.infn.it)\nSubjects: Gamma Ray, >GeV, AGN, Quasar\nDescription: Referred to by ATel #: 1661, 1905, 7592, 7801\nThe Large Area Telescope (LAT), one of two instruments on the Gamma-ray Large Area Space Telescope (GLAST) (launched June 11, 2008), which is still in its post-launch commissioning and checkout phase, has been monitoring high flux from a source positionally consistent with the blazar PKS 1502+106 (R.A.:15h04m24.9797s; Dec.:+10d29m39.198s, also known as OR 103 and S3 1502+10) since August 6, 2008. \nPreliminary analysis indicates that the source is in a high state with a gamma-ray flux (E>100MeV) well above pre-defined LAT flaring source reporting threshold of 2x10^-6 photons cm^-2 s^-1. \nThis is a well-known radio source classified as a Flat Spectrum Radio Quasar (FSRQ), observed by several X-ray instruments. This is the first time that it has been reported to have gamma-ray emission. \nPlease note that PKS 1502+106 has two possible redshifts listed in the literature: z=0.56 and 1.83; the former seems preferred (A.E. Wright et al. 1979 ApJ 229,73; B.J. Wilkes 1986, MNRAS, 218, 331). \nBecause GLAST has just started its scientific standard operations, regular gamma-ray monitoring of this source will be pursued. In consideration of the ongoing activity of this source we strongly encourage multiwavelength observations of PKS 1502+106. \nThe GLAST LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Nova", "Active galactic nucleus", "Magnetar" ] }, "answerKey": "C" }, { "id": "atel_1770", "message": "Title: Swift phase-coherent P-Pdot solution for the 1E1547.0-5408 outburst \nAuthors: G. L. Israel (INAF-OA Roma), P. Esposito (INAF-IASF, Milan), N. Rea (U. Amsterdam), H. A. Krimm (CRESST/GSFC/USRA), D. M. Palmer (LANL), N. Gehrels (GSFC), S. Mereghetti, A. Tiengo, F. Senziani (INAF/IASF-Milan), D. Gotz (CEA-Saclay), S. Zane (UCL-MSSL) report on behalf of a larger collaboration\nDate: 8 Oct 2008; 10:28 UT\nProvenance: GianLuca Israel (gianluca@mporzio.astro.it)\nSubjects: X-ray, Neutron Star, Soft Gamma-ray Repeater, Transient, Variables, Pulsar\nDescription: Referred to by ATel #: 1904\nSwift XRT monitored 1E1547.0-5408 in the latest 5 days starting from about 90 seconds since the BAT trigger (Krimm et al. GCN 8311, 8312). During this period observations in the WT mode were carried out for a total exposure time of about 37ks. After having removed bursts and corrected the photon arrival times to the barycenter of the Solar System, the dataset was used to infer a phase-coherent timing solution including both a period and period derivative component. \nAccording to our preliminary analysis the period and period derivative of 1E1547.0-5408 are: P=2.071335(1)s and Pdot=5.7(5) x 10^-11 s/s (1 sigma uncertainties are reported). We note that the period derivative inferred at the time of the previous outburst was 2.318(5)x10^-11 s/s, with a very high second derivative (Camilo et al. 2007, ApJ, 666, L93; Camilo et al. 2008, ApJ, 679, 681). Therefore, our inferred period derivative value is a factor of two larger than the historical one. The above reported period is within 1-sigma from our first measurement (Esposito et al. 2008, ATel #1763) and at about 7-sigma from the recently reported value inferred from RXTE observations (Dib et al. 2008, ATel #1769). \nThe Swift monitoring of 1E1547.0-5408 is still ongoing.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Neutron star", "Black hole", "Stellar evolution" ] }, "answerKey": "B" }, { "id": "atel_1875", "message": "Title: Swift/XRT localisation of XTE J1855-026\nAuthors: P. Romano (INAF-IASF Palermo), S. Mereghetti, L. Sidoli (INAF-IASF Milano), P. A. Evans (UL)\nDate: 15 Dec 2008; 12:20 UT\nProvenance: Pat Romano (romano@ifc.inaf.it)\nSubjects: X-ray, Binary, Transient\nDescription: Referred to by ATel #: 1876\nThe X-ray source XTE J1855-026 was observed by Swift/XRT on 2008-11-19 from 01:18 to 17:33 UT for a total of 9.5 ks onsource. The source was detected with a count rate of CR=(0.51+/-0.01) counts s^-1. Pulsations at P=359.7+/-0.3 s were clearly detected. \nThe spectrum (~3100 counts) was fit in the 0.3-10 keV energy range with an absorbed power-law model yielding a photon index of 1.06(-0.15+0.16) and a column density NH=(4.1+/-0.5)E22 cm^-2, in excess of the Galactic one (0.68E22 cm^-2). The observed (unabsorbed) 2-10 keV flux is 7.5E-11 (9.3e-11) ergs cm^-2 s^-1. \nThe position derived with Swift is RA, Dec(J2000)=283.87685, -2.60516, \nwhich is equivalent to: \nRA (J2000): 18h 55m 30.44s \nDec (J2000): -02d 36' 18.6\" \nwith an uncertainty of 1.9 arcsec (radius, 90% confidence). \nThis position, obtained from the XRT data enhanced by UVOT field astrometry (Goad et al. 2007, A&A, 476, 1401), is 14\" from the original ASCA position (12\" radius error circle, Corbet & Mukai 2002, ApJ 577, 923) and confirms the identification with the optical counterpart proposed by Verrecchia et al (ATel #102). \nWe would like to thank the Swift Team for making these observations possible, in particular N. Gehrels, the duty scientists as well as the science planners.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Repeater", "Neutron star, Black hole", "Variable star, Black hole", "Accreting object, Black hole" ] }, "answerKey": "B" }, { "id": "atel_1950", "message": "Title: An SN-Ia in a very faint dwarf galaxy\nAuthors: A. J. Drake, A. Mahabal, S. G. Djorgovski, M. J. Graham, R. Williams (Caltech); A. D. Myers (UIUC); M. Catelan (PUC); E. C. Beshore, S. M. Larson (LPL); E. Christensen (Gemini Observatory);\nDate: 5 Mar 2009; 01:39 UT\nProvenance: Andrew J. Drake (ajd@cacr.caltech.edu)\nSubjects: Optical, Supernovae, Transient\nDescription: Referred to by ATel #: 2447, 3118\nFurther to Atel#1937, we confirm the discovery of a type Ia supernova with Palomar 200 observations. The CRTS discovery has the following parameters: \n\nCSS090213:030920+160505| Discovery 2009-02-13 UT 03:45:55 | RA 03:09:19.79 | Dec 16:05:05.3 | Type SN Ia \n---|---|---|---|--- \nThe spectrum of CSS090213:030920+160505 (taken on Feb 25th UT) shows this to be an SN-Ia, 12 days past maximum light with redshift z=0.031+/-0.006. \nAs noted in Atel#1937, a nearby 23rd magnitude object is seen in the NOAO deep ecliptic survey (limiting mag 24.2). If this is the host galaxy, at the SN's redshift it would have a mag Mr=-12.6. Alternatively, assuming the supernova was discovered at peak (as suggested by the spectrum), and that its peak is Mr=-19.3, a 23rd magnitude host galaxy would have Mr=-13.1. The two results are thus consistent within the redshift uncertainty. Improved astrometry for the supernova's position shows a clear offset between the SN and the faint NOAO object. Assuming the SN's redshift, the projected separation is ~1.6kpc. This offset is within the extent expected for a low mass dwarf galaxy of the observed brightness. However, a host galaxy below the limits of the NOAO images is also possible. \n\nThis discovery is very similar to SN 2008hp (ATEL#1856) and provides additional evidence for a higher than expected rate of SN in such low-mass galaxies. \nFor finding charts and discovery images please see: http://voeventnet.cacr.caltech.edu/feeds/ATEL/CRTS. \nCurrent candidate and confirmed SNe can be found here.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Supernova", "Exoplanet", "Globular cluster" ] }, "answerKey": "B" }, { "id": "atel_2025", "message": "Title: Detection of Super-Soft X-ray emission in Nova LMC 2009\nAuthors: M F Bode (Liverpool JMU), J P Osborne, K L Page, A P Beardmore (Leicester), J-U Ness (ESA), F M Walter (Stony Brook), M J Darnley (Liverpool JMU), A Evans (Keele), S P S Eyres (Central Lancashire), J Krautter (Heidelberg), T J O'Brien (Manchester), M Orio (INAF-Padova & Wisconsin), G Schwarz (West Chester), S Starrfield (ASU), J Truran (Chicago)\nDate: 20 Apr 2009; 14:57 UT\nProvenance: Michael Bode (mfb@astro.livjm.ac.uk)\nSubjects: Ultra-Violet, X-ray, Nova\nDescription: Referred to by ATel #: 2392, 2423\nWe report Swift satellite X-ray Telescope (XRT) observations of the probable recurrent Nova LMC 2009 (IAUC # 9019 , ATel #1930, #2001). We have detected a highly variable soft X-ray source, initially at a count rate of 0.010 +0.007/-0.005 c/s on day 70.74 after discovery of the outburst (2009 February 5.067 UT, IAUC # 9019 ), which reached 0.042+/-0.009 c/s on day 70.88, then returned to a level of ~0.01 c/s on days 71.55 and 71.94, before climbing to 0.130+/-0.017 c/s on day 73.43. \nThe spectrum from days 70.7 to 70.9 can be approximately modelled with an absorbed black body. With N_H = 1.13e21 cm^-2 in this direction (Kalberla et al. 2005, A&A, 440, 775), kT = 38.8 +10.3/-7.6 eV. The resulting unabsorbed luminosities for d = 48.5 kpc are 2.4e36 erg s^-1 (0.3-10 keV) and 5.3e37 erg s^-1 (bolometric). \nThe nova has been observed with the XRT every few days since mid-February but remained undetected with count rate upper limits (3 sigma) of ~2e-3 c/s over 0.3-10 keV. Although there may have been a marginal detection on day 63 after outburst, we note that the emergence of the Super-Soft Source in this object is at a significantly later time than that in either U Sco (<20 days, Kahabka et al. 1999, A&A 347, L43) or RS Oph (~30 days, Osborne et al., ATel #764) implying that in Nova LMC 2009 the mass loss rate was higher and/or the ejection velocities were lower than in either of these two recurrent novae. \nThe UV brightness, determined from Swift Ultraviolet/Optical Telescope (UVOT) observations, has continued the declining trend, reported in ATel #2001, to around mag(uvw2) = 14 on day 68. Similar variability to the 1.19 day modulation reported in ATEL #2001 appears to be continuing. We note that recent AAVSO photometric timeseries are not so far sufficient to decide between the periods listed there. \nSwift observations are continuing and further ground-based monitoring (both photometry and spectroscopy) is strongly encouraged. We thank the Swift PI, Neil Gehrels, the Swift science team and the Swift mission operations team for their support of these observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova, Variable star", "Nova, Quasar", "Galaxy, Variable star", "Circumstellar disk, Variable star" ] }, "answerKey": "A" }, { "id": "atel_2075", "message": "Title: Swift detection of a flare from IGR J16328-4726. \nAuthors: D. Grupe (PSU), J. Kennea (PSU), P. Evans (U. Leicester), P. Romano (INAF-IASF Palermo), C. Markwardt (CRESST/GSFC/UMD), M. Chester (PSU) \nDate: 10 Jun 2009; 15:31 UT\nProvenance: Jamie A. Kennea (kennea@astro.psu.edu)\nSubjects: X-ray, Transient\nDescription: Referred to by ATel #: 2588\nAt 07:54:27 UT on 2009 June 10, the Swift Burst Alert Telescope (BAT) triggered on a transient source coincident with the INTEGRAL source IGR J16328-4726 (Bird et al., 2007). The BAT on-board calculated location is RA, Dec 248.176, -47.391 which is \n   RA(J2000) = 16h 32m 42s \n   Dec(J2000) = -47d 23' 28\" \nwith an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The peak count rate was ~1273 counts/sec (15-350 keV), at ~183 sec after the trigger. \n \nThe XRT began observing the field of IGR 16328-4726 at 08:00:52.5 UT, 385.3 seconds after the BAT trigger. Using 2754 s of XRT Photon Counting mode data and 6 UVOT images, we find an astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching to the USNO-B1 catalogue): RA, Dec = 248.1579, -47.3951 which is equivalent to: \n   RA (J2000): 16 32 37.88 \n   Dec (J2000): -47 23 42.4 \nwith an uncertainty of 1.7 arcsec (90% confidence). Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, in press, arXiv:0812.3662). The XRT light curve for the first orbit of observations shows that the source brightness is steadily decaying. \n \nThe X-ray spectrum of the first orbit of data can be fit by an absorbed power law model with Gamma = 0.56 +0.75/-0.68 and an absorption column density NH=(8.1 +5.7/-4.9) x 1022 cm-2, which is shows some evidence for absorption in excess of the expected galactic value of 1.54 x 1022 cm-2. \n \nWe note that the high absorption makes the detection of an optical counterpart with UVOT unlikely. Within the XRT error circle we find no USNO-B1 counterparts. We do find one 2MASS counterpart candidate: RA, Dec (J2000)= 16 32 37.91, -47 23 40.9 (J=14.631, H=12.423, K=11.275 mag).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object, Variable star", "Accreting object, Magnetar", "Star and stellar system, Binary system", "Accreting object, Binary system" ] }, "answerKey": "D" }, { "id": "atel_2160", "message": "Title: Fermi LAT detection of increasing gamma-ray activity of blazar PKS 2052-474\nAuthors: C. S. Chang (MPIfR), on behalf of the Fermi Large Area Telescope Collaboration\nDate: 15 Aug 2009; 00:30 UT\nProvenance: Teddy Cheung (ccheung@milkyway.gsfc.nasa.gov)\nSubjects: Gamma Ray, >GeV, Transient\nDescription: Referred to by ATel #: 2162\nThe Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed an increasing gamma-ray flux from a source positionally consistent with PKS 2052-474 (RA=20:56:16.3, DEC=-47:14:47.6, J2000; Ma, C. et al., 1998, AJ, 116,516). Recent optical flaring of this source is reported in ATEL #2158 (Hauser et al.). \nPreliminary analysis indicates that this source has recently brightened. On 9 August 2009 it reached a relatively high state with a gamma-ray flux (E>100MeV) of (8.7 ± 1.6) x 10-7 ph cm-2 s-1 (statistical errors only) for that day. This is a factor of 4 higher than the average level observed in the previous week of all-sky monitoring (29 July - 4 August 2009). The gamma-ray outburst may now be fading, thus we strongly encourage prompt followup observations. \nBecause Fermi operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. For this source the Fermi LAT contact person is C. S. Chang (cschang@mpifr.de). \nThe Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Variable star", "Active galactic nucleus", "Circumstellar disk" ] }, "answerKey": "C" }, { "id": "atel_2225", "message": "Title: SWIFT J1753.5-0127 observed in XMM-Newton slew.\nAuthors: R D Saxton (ESAC), R. Duro (Bamberg), A. Read (Leicester), P. Esquej (Leicester)\nDate: 4 Oct 2009; 10:48 UT\nProvenance: Richard Saxton (richard.saxton@sciops.esa.int)\nSubjects: X-ray, Binary, Black Hole, Transient\nDescription: The X-ray binary, SWIFT J1753.5-0127, discovered in outburst by the Swift BAT in 2005 (Palmer et al. 2005, ATel #546) was observed during an XMM-Newton slew on September 3rd 2009, with a 0.2-10 keV count rate of 118 c/s. Such bright sources suffer from heavy pile-up in the EPIC-pn camera during slews and the real count rate is estimated to be ~250 c/s. \nAfter excluding the inner 10\" of the PSF and using single-pixel events only, to minimise pile-up effects, a spectral fit gives a 0.2-10 keV flux of 9.7+/-1.0E-10 ergs/s/cm^2 and a 2-10 keV flux of 6.6+/-0.9E-10 ergs/s/cm^2. \nThe spectrum requires a power-law plus disk blackbody model for an acceptable fit and the disk temperature can be constrained to 0.34 (+0.17 / -0.09) keV (90% confidence for one free parameter). \nThis is very much in line with X-ray observations performed post-outburst which show that the source remains in the low/hard state while very gradually increasing in brightness (see Miller and Rykoff, Atel #1066). \nThis source was spotted using the XMM-Newton slew data quick analysis tool whose results are available at: http://xmm.esac.esa.int/external/xmm_products/slew_results/web_slew.shtml \nLatest SLEW RESULTS", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Binary system", "Black hole, Accreting object", "Black hole, Black hole", "Stellar evolution, Binary system" ] }, "answerKey": "A" }, { "id": "atel_2300", "message": "Title: Swift and RXTE report the detection of a new galactic transient source Swift J1713.4-4219\nAuthors: H. A. Krimm (CRESST/GSFC/USRA), T. E. Strohmayer (GSFC), J. H. Swank (GSFC), S. D. Barthelmy (GSFC), W. Baumgartner (CRESST/GSFC/UMBC), J. Cummings (CRESST/GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC), C. B. Markwardt (CRESST/GSFC/UMD), D. Palmer (LANL), T. Sakamoto (CRESTT/GSFC/UMBC), G. Skinner (CRESST/GSFC/UMD), M. Stamatikos (OSU/GSFC), J. Tueller (GSFC), T. Ukwatta (GSFC/GWU)\nDate: 17 Nov 2009; 04:38 UT\nProvenance: Hans A. Krimm (Hans.Krimm@nasa.gov)\nSubjects: X-ray, Request for Observations, Binary, Black Hole, Variables\nDescription: Referred to by ATel #: 13169, 13247, 13250\nThe hard X-ray transient monitor of the Swift Burst Alert Telescope (BAT) has detected a previously unknown transient source. This source, Swift J1713.4-4219, was first detected at a daily average rate of 0.0048 ± 0.0017 counts/sec/cm2 (21 mCrab) in the 15-50 keV band on 2009 Nov 13 (MJD 55148). It was visible at a lower significance for four days prior and has remained at roughly the same brightness for the past three days. \nObserving constraints prevent an observation with the Swift X-Ray Telescope (XRT) until 2010 Jan 23. The BAT position was determined to be: \nRA (J2000): 17 13 26.6 (258.361 deg) \nDEC (J2000): -42 19 37.2 (-42.327 deg) \nThe estimated error is 3.0 arc minutes (radius, 90% confidence). \nThe position of the new hard X-ray transient Swift J1713.4-4219 was observed with RXTE for 1.5 ksec beginning on 2009 Nov 16 at 19:41:38 UTC. The source is detected in the PCA with an average rate of 17.0 +- 0.2 counts/s/PCU (full PCA band). Strong flickering is evident in the light curve, with peak rates approaching 70 counts/s/PCU. Timing analysis reveals no significant periodicities, but the strong, aperiodic variability is easily detected in the power spectrum. The PCA spectrum is well fitted (2.5-30 keV) with a column density of 1.2+-0.4 x 10^22 cm2 and power-law index of 1.68 +- 0.04. The average flux is approximately 5.4 mCrab. The present data are consistent with a black hole transient in the low-hard state. Additional RXTE observations are planned over the next few days before the source is too close to the Sun for RXTE to observe. \nSwift/BAT Hard X-ray Transient light curve for Swift J1713.4-4219", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Black hole", "Repeater", "Nova" ] }, "answerKey": "B" }, { "id": "atel_2370", "message": "Title: ATCA non detection of 4U 1630-47 in outburst\nAuthors: D. E. Calvelo (University of Southampton), R. P. Fender (University of Southampton), S. Corbel (CEA Saclay & Université Paris Diderot), C. Brocksopp (UCL-MSSL), T. Tzioumis (ATNF)\nDate: 5 Jan 2010; 19:32 UT\nProvenance: S. CORBEL (corbel@discovery.saclay.cea.fr)\nSubjects: Radio, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 13592\nIn response to the X-ray flux rise reported by MAXI/GSC (ATEL #2363, followed up by RXTE; ATEL #2365) we observed the Galactic black hole candidate 4U 1630-47 with the Australia Telescope Compact Array (6A configuration) on 2010 January 2.90 and 3.04 at 5.5 and 9 GHz for a total of 2880 seconds (1440 s per observation). We do not detect a radio source in either band at the system co-ordinates. The estimated flux density upper limits (3 x R.M.S.) are 93 microJy and 126 microJy at 5.5 and 9 GHz respectively.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Accreting object", "Galaxy", "Near-Earth object" ] }, "answerKey": "A" }, { "id": "atel_2430", "message": "Title: Emergence of the Supersoft X-ray Phase of U Sco\nAuthors: Eric M. Schlegel (UT-San Antonio); Brad Schaefer and Ashley Pagnotta (LSU); Kim Page and Julian Osborne (Leicester); Jeremy Drake (SAO); Marina Orio (Wisconsin), Dai Takei (Rikkyo Univ.), Erik Kuulkers and Jan-Uwe Ness (ESA/ESAC), and Sumner Starrfield (ASU) for a larger collaboration\nDate: 10 Feb 2010; 20:18 UT\nProvenance: Eric M. Schlegel (eric.schlegel@utsa.edu)\nSubjects: X-ray, Cataclysmic Variable, Nova\nDescription: Referred to by ATel #: 2442, 2452, 2477, 3038, 5627\nU Sco has been detected as a supersoft source in the X-ray band using the Swift satellite following the initial discovery as an X-ray source (ATel 2419). The Swift X-ray Telescope (XRT) has been monitoring U Sco since shortly after the optical discovery with the exception of ~5 days when the field-of-view was unavailable because of Swift's lunar constraint. An observation, obtained 2010 Feb 9 13:00 UT or 12 days after the outburst, reveals strong soft emission. The XRT spectrum may be fit with a blackbody of temperature 28+/-8 eV and a column density NH of 3.8(+1.6,-1.2)x10^21 cm^-2. The detected count rate is 0.34+/-0.02 cts/s in contrast to the ~0.002 cts/s of the initial hard phase. The X-ray light curve is essentially flat from days 2 to 8. U Sco is then detected at about 100 times higher count rate at day ~12. The rise phase very likely occurred during the lunar constraint gap but a single point at day 12.1 has a count rate of ~0.1 cts/s and may be the tail of the rise. The observed flux in the 0.3-10 keV band is 9.5x10^-12 erg/s/cm^2. Adopting a column density of 3x10^21 cm^-2 (to be consistent with ATEL 2419) yields an unabsorbed flux of 1.2x10^-9 erg/s/cm^2 in the 0.3-10 keV band. Assuming a distance of 12 kpc (Schaefer 2009, ApJS in press, arXiv:0912.4426), the unabsorbed 0.3-10 keV luminosity is then 2x10^37 erg/s. Fits using WD atmosphere models yield temperatures in the range of 400-700K K, suggesting that the temperature is not tightly constrained and may be higher than the blackbody fit implies. U Sco is expected to remain in a SSS phase for the next approximately 20-30 days, based upon previous outbursts. The details are sufficiently unknown that continued monitoring is highly recommended until U Sco returns to a quiescent state. We thank Neil Gehrels for approving the TOO program and the Swift planning and operations team for their efforts to observe U Sco.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova, Quasar", "Magnetar, Star and stellar system", "Nova, Star and stellar system", "Interstellar medium, Star and stellar system" ] }, "answerKey": "C" }, { "id": "atel_2550", "message": "Title: Spin down rate and inferred dipole magnetic field of the new soft gamma-ray repeater SGR 1833-0832\nAuthors: P. Esposito (INAF-IASF Milano), G. L. Israel (INAF-O. A.Roma), M. Burgay (INAF-O. A.Cagliari), A. Possenti (INAF-O. A.Cagliari), D. Gotz (Irfu/SAp/CEA Saclay), N. Rea (CSIC-ICE Barcelona), S. Mereghetti (INAF-IASF Mi), A. Tiengo (INAF-IASF Mi), L. Stella (INAF-0. A.Roma), R. Turolla (U. Padua), S. Zane (MSSL/UCL) on behalf of a larger collaboration\nDate: 13 Apr 2010; 12:23 UT\nProvenance: Paolo Esposito (paoloesp@iasf-milano.inaf.it)\nSubjects: X-ray, Soft Gamma-ray Repeater, Pulsar\nDescription: Referred to by ATel #: 2553, 2691, 2763\nWe observed the new soft gamma-ray repeater SGR 1833-0832 with XMM-Newton on 2010 March 23 (for about 22 ks) and on 2010 April 02 (for about 21 ks). By merging these data sets with those collected since the discovery of the source (GCN #10526) with RossiXTE and Swift, we were able to refine the period measurement reported in ATEL #2494 (see also ATEL #2493), also including in the phase-coherent timing solution a first period derivative component.\nAccording to our preliminary analysis the period and first period derivative of SGR 1833-0832 are: P= 7.565406(2) s and Pdot= 7.4(2) x 10^-12 s/s (1 sigma uncertainties; epoch 55274.0 MJD). Under the standard assumption that the neutron star slows down because of magnetic braking, we infer a dipole magnetic field of B = 2.4(3) x 10^14 G for a neutron star with radius of 10 km and mass of 1.4 solar masses, confirming the SGR as a new magnetar candidate.\nWe will monitor the source both with XMM-Newton and Swift until the end of the current observability window (about end of April 2010).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Accreting object", "Near-Earth object", "Neutron star" ] }, "answerKey": "D" }, { "id": "atel_2610", "message": "Title: Discovery of VHE gamma-ray emission from PKS 0301-243 with Fermi\nAuthors: A. Neronov (ISDC) D. Semikoz (APC), Ie. Vovk (ISDC)\nDate: 11 May 2010; 10:14 UT\nProvenance: Andrii Neronov (andrii.neronov@obs.unige.ch)\nSubjects: Gamma Ray, >GeV, AGN\nDescription: We report the discovery of VHE (E>100 GeV) emission from the BL Lac type blazar PKS 0301-243 (z=0.26, RA 03:03:26.50, DEC -24:07:11.5, J2000). Evidence for the VHE gamma-ray emission from this source was previously found in the 100-300 GeV band data of Fermi telescope (Neronov et al. arXiv:1004.3767). The source has recently experienced a bright flare in the energy band above 100 MeV detected by Fermi telescope (Cannon A., ATEL #2591). We have analyzed Fermi data collected during the period between April 29 and May 7, 2010, corresponding to the flare, and found that the flaring activity of the source was accompanied by gamma-ray emission in the VHE energy band with the source flux reaching the level of ~1 Crab unit at the energies above 100 GeV. The overall significance of detection of the source above 100 GeV is 6.8 sigma (the standard Fermi likelihood analysis of the entire Fermi exposure starting from August 4, 2008, gives the Test Statistics value TS=45.7 at the source position in the 100-300 GeV energy band ). Additional information about the source properties (TS map, lightcurve and spectrum) could be found at http://www.isdc.unige.ch/vhe/Objects/1FGL_J0303.5-2406/page.html", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium, Black hole", "Active galactic nucleus, Black hole", "Black hole, Black hole", "Active galactic nucleus, Quasar" ] }, "answerKey": "B" }, { "id": "atel_2675", "message": "Title: PTF discovery of PTF10jkx, a type II supernova\nAuthors: A. Gal-Yam, I. Arcavi (Weizmann Institute of Science), D. A. Howell, (LCOGT/UCSB), P. Nugent (LBNL), M. Sullivan (Oxford), M. M. Kasliwal, R. M. Quimby, E. O. Ofek, S. R. Kulkarni (Caltech), J. Bloom (UCB), N. M. Law (U. Toronto), R. G. Dekany, G. Rahmer, David Hale, R. Smith, J. Zolkower, V. Velur, R. Walters, J. Henning, K. Bui, D. McKenna (Caltech), and J. Jacobsen (LBNL) on behalf of the Core-Collapse working group of the Palomar Transient Factory (ATEL#1964)\nDate: 14 Jun 2010; 21:19 UT\nProvenance: Avishay Gal-Yam (avishay.gal-yam@weizmann.ac.il)\nSubjects: Optical, Supernovae\nDescription: The PTF (ATEL #1964; http://www.astro.caltech.edu/ptf/ ) reports the discovery of a new supernova, PTF10jkx. The supernova was discovered by Oarical, an autonomous software framework of the PTF collaboration, on June 10 UT at RA(J2000) = 13:32:57.11 and DEC(J2000) = +48:18:54.5 at a magnitude of 19.8 in R-band (calibrated with respect to the USNO catalog) in the galaxy SDSS J133257.67+481855.7 (z=0.028). The supernova was not detected down to mag 21.5 in previous PTF images taken during May 2010 (3-sigma). A spectrum was obtained using the GMOS Spectrograph (Hook et al. 2004, PASP, 116, 425) on the Gemini North 8-m telescope on June 10 UT, revealing the supernova to be of type II. The superfit program (Howell et al. 2005, ApJ 634, 1190) finds a good match to the type II-P SN 1999em at 9 days post-peak.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova, Black hole", "Quasar, Supernova", "Black hole, Supernova", "Supernova, Supernova" ] }, "answerKey": "D" }, { "id": "atel_2790", "message": "Title: ROTSE-III Discovery of a Supernova Candidate\nAuthors: W. Zheng and R. Anastasiya (University of Michigan); J. Vinko (University of Szeged); R. Quimby (California Institute of Technology); F. Yuan, N. Whallon, Y. Chen, C. Akerlof, and S. B. Pandey (University of Michigan); J. C. Wheeler and E. Chatzopoulos (University of Texas), on behalf of the ROTSE collaboration\nDate: 15 Aug 2010; 15:06 UT\nProvenance: Weikang Zheng (zwk@umich.edu)\nSubjects: Optical, Nova, Supernovae, Transient\nDescription: We report the discovery of a SN candidate, ROTSE3 J235704.6-341106, in unfiltered CCD images taken on July 17.02 UT with the 0.45-m ROTSE-IIIc telescope at the H.E.S.S. site in Namibia at about 18.0 mag. The transient was detected on the following days from ROTSE-IIIc, and the light curve showed it reached peak around July 23th with mag about 16.8 and then decayed after that to about 18.0 mag on Aug. 12.98 UT. The new object is located at RA= 23h57m04s.57, Dec= -34o11'05\".5, which is 0\" east and 0.5\" south to the center of galaxy 6dFGS gJ235704.6-341105 (z~0.0470 according to SIMBAD). No source was detected at this location in the ROTSE-IIIc image (limit ~18.5 mag) before July 16th UT. A finding chart of the transient is posted at the following website URL: http://www.rotse.net/rsvp/j235704.6-341106/j235704.6-341106.jpg", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Exoplanet", "Supernova", "Repeater", "Accreting object" ] }, "answerKey": "B" }, { "id": "atel_2880", "message": "Title: AGILE upper limits above 100 MeV regarding the recent transient MAXI J1659-152\nAuthors: F. Lucarelli, F. Verrecchia (ASDC), A. Chen (INAF/IASF-Mi), M. Tavani (INAF/IASF-Rm, and Univ. Tor Vergata), C. Pittori (ASDC), A. Bulgarelli, F. Gianotti, M. Trifoglio (INAF/IASF-Bo), A. Giuliani, S. Mereghetti, P. Caraveo, F. Perotti (INAF/IASF-Mi), I. Donnarumma (INAF/IASF-Rm), F. D'Ammando, S. Vercellone (INAF/IASF-Pa), E. Del Monte, Y. Evangelista, M. Feroci, F. Lazzarotto, L. Pacciani, P. Soffitta, E. Costa, I. Lapshov, M. Rapisarda, A. Argan, G. Piano, G. Pucella, S. Sabatini, A. Trois, V. Vittorini (INAF/IASF-Rm), F. Fuschino, M. Galli, C. Labanti, M. Marisaldi, G. Di Cocco (INAF/IASF-Bo), A. Pellizzoni, M. Pilia (INAF/OA-Cagliari), G. Barbiellini, F. Longo, E. Moretti, E. Vallazza (INFN Trieste), A. Morselli, P. Picozza, E. Striani (INFN and Univ. Roma Tor Vergata), M. Prest (Universita` dell'Insubria), P. Lipari, D. Zanello (INFN and Univ. Roma Sapienza), P. W. Cattaneo, A. Rappoldi (INFN Pavia), P. Santolamazza, S. Colafrancesco, P. Giommi (ASDC), L. Salotti (ASI)\nDate: 28 Sep 2010; 16:34 UT\nProvenance: Fabrizio Lucarelli (fabrizio.lucarelli@asdc.asi.it)\nSubjects: Gamma Ray, >GeV, Transient\nDescription: Referred to by ATel #: 2881\nFollowing the detection of the new hard X-ray transient by MAXI/GSC (ATel #2873) confirmed by INTEGRAL (ATel #2875) and in the radio band by WSRT (ATel #2874), we searched for significant excess in the AGILE data at the MAXI source position (R.A., Dec = +254.79 deg, -15.27 deg, J2000). \nIntegrating from 2010-09-25 00:00 UT to 2010-09-26 14:00 UT, a maximum likelihood analysis yields a 95 % C.L. upper limit of 80 e-8 ph/cm2/s (E > 100 MeV). \nNo significant detection is obtained for a longer 7-day integration, from 2010-09-20 00:00 UT to 2010-09-27 00:00 UT, yielding a 95 % C.L. upper limit of 40 e-8 ph/cm2/s (E > 100 MeV). \nAGILE will continue to monitor the MAXI transient region. This measurement was obtained with AGILE observing a large portion of the sky in spinning mode.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system", "Galaxy", "Interstellar medium", "Repeater" ] }, "answerKey": "B" }, { "id": "atel_2950", "message": "Title: AGILE detection of prolonged gamma-ray activity from the blazar PKS 1830-211\nAuthors: I. Donnarumma (INAF/IASF-Rm), S. Vercellone (INAF/IASF-Pa), M. Tavani (INAF/IASF-Rm, and Univ. Tor Vergata), C. Pittori, F. Lucarelli, F. Verrecchia (ASDC), A. Chen (INAF/IASF-Mi), A. Bulgarelli, F. Gianotti, M. Trifoglio (INAF/IASF-Bo), A. Giuliani, S. Mereghetti, P. Caraveo, F. Perotti (INAF/IASF-Mi), F. D'Ammando (INAF/IASF-Pa), E. Del Monte, Y. Evangelista, M. Feroci, F. Lazzarotto, L. Pacciani, P. Soffitta, E. Costa, I. Lapshov, M. Rapisarda, A. Argan, G. Piano, G. Pucella, S. Sabatini, A. Trois, V. Vittorini (INAF/IASF-Rm), F. Fuschino, M. Galli, C. Labanti, M. Marisaldi, G. Di Cocco (INAF/IASF-Bo), A. Pellizzoni, M. Pilia (INAF/OA-Cagliari), G. Barbiellini, F. Longo, E. Moretti, E. Vallazza (INFN Trieste), A. Morselli, P. Picozza, E. Striani (INFN and Univ. Roma Tor Vergata), M. Prest (Universita` dell'Insubria), P. Lipari, D. Zanello (INFN and Univ. Roma Sapienza), P. W. Cattaneo, A. Rappoldi (INFN Pavia), P. Santolamazza, S. Colafrancesco, P. Giommi (ASDC), L. Salotti (ASI)\nDate: 17 Oct 2010; 18:59 UT\nProvenance: Donnarumma Immacolata (immacolata.donnarumma@iasf-roma.inaf.it)\nSubjects: Gamma Ray, >GeV, Request for Observations, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 4158, 6361, 12252\nThe AGILE Gamma-Ray Imaging Detector (GRID) has been detecting prolonged gamma-ray emission above 100 MeV from a source at (l,b)=(12.17,-6.25) [RA(J2000)=18h 35m 44.07s, DEC(J2000)=-21h 18m 00.7s] positionally consistent with the high z blazar (z=2.507) PKS 1830-211. \nIntegrating from 2010-10-15 00:00UT to 2010-10-17 00:00UT, a quick-look maximum likelihood analysis yields a source flux of about (5.7+-1.8)E-6 ph/cm2/sec (E > 100 MeV). This flux value is, within the statistical errors, comparable to the daily flux value detected by Fermi/LAT on 2010-10-14, and reported in ATel #2943. \nIt is worth noting that an enhancement in the gamma-ray activity of this blazar was detected by AGILE on 2009-10-12 (see ATel #2242), when it was detected at a flux level about 3.5 times lower than the current one. \nThe AGILE-GRID detection was obtained while AGILE is observing in spinning mode, surveying a large fraction of the sky each day. \nMulti-frequency observations of PKS 1830-211 are strongly encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Active galactic nucleus", "Accreting object", "Magnetar" ] }, "answerKey": "A" }, { "id": "atel_3060", "message": "Title: Swift detection of an ~500s period in MAXI J1409-619\nAuthors: J. A. Kennea (PSU), P. Curran (CEA/Saclay), H. Krimm (CRESST/GSFC/USRA), P. Romano, V. Mangano (INAF-IASFPA), P. A. Evans (U Leicester), K. Yamaoka (Aoyama Gakuin U) and D. N. Burrows (PSU) \nDate: 1 Dec 2010; 01:40 UT\nProvenance: Jamie A. Kennea (kennea@astro.psu.edu)\nSubjects: X-ray, Transient\nDescription: Referred to by ATel #: 3067, 3069, 3070\nAt 15:35UT on November 30th, 2010 Swift/BAT triggered on an outburst from MAXI J1409-619 (Mangano et al., GCN #11428), and it was observed by Swift for a total of 2ks in a combination of PC and WT mode. MAXI J1409-619 was first discovered by MAXI on October 18th, 2010 (Yamaoka et al., ATEL #2959) and followed up by Swift, which accurately localized and confirmed the new transient (Kennea et al., ATEL #2962). \nThe XRT PC mode data reveal an enhanced emission state over the previous detection, with a mean flux of 7 x 10^-10 erg/s/cm^2 (0.3-10 keV, uncorrected for absorption), ~7 times brighter than the flux reported by Swift on October 20th, 2010 (Kennea et al., ATEL#2962). \nThe PC mode pile-up corrected light-curve reveals a sinusoidal periodicity, not previously detected, with a period of 503 +/- 10 s. 4 clear cycles are seen in the second orbit consisting of 1.9ks of PC mode data taken between 16:55 and 17:28UT, with a sinusoidal peak-to-trough modulation of 42% of the mean flux. \nRXTE observations taken October 22-23, 2010 (Yamaoka et al, ATEL #2969) reported no detection of this periodicity, and we have analyzed the previous Swift/XRT data using the Lomb-Scargle method and have also found no evidence of this periodicity. Therefore this periodicity is a transient feature, most likely due to the accretion event that triggered BAT. We suggest that this periodicity is the rotation period of the compact object in MAXI J1409-619, most likely a neutron star, and that MAXI J1409-619 is a candidate HMXB system.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system", "Neutron star", "Nova", "Variable star" ] }, "answerKey": "B" }, { "id": "atel_3175", "message": "Title: New optical nova candidate in the outer disk of M 31\nAuthors: W. Pietsch, M. Henze, V. Burwitz (Max-Planck-Institut fuer extraterrestrische Physik), A. Kaur, D. H. Hartmann (Clemson University), P. Milne, G. Williams (University of Arizona)\nDate: 18 Feb 2011; 14:09 UT\nProvenance: Wolfgang Pietsch (wnp@mpe.mpg.de)\nSubjects: Optical, Nova\nDescription: We report the discovery of a possible nova in the outer disk of M 31 on two 15x60s and 7x60s stacked R filter CCD images obtained with the robotic 60cm telescope with an E2V CCD (2kx2k, 13.5 micron sq. pixels) of the Livermore Optical Transient Imaging System (Super-LOTIS, located at Steward Observatory, Kitt Peak, Arizona, USA) on 2011 February 15.127 and 18.121 UT with magnitude of 18.7 and 18.0, respectively. The position for the nova candidate is RA = 00h42m02.33s, Dec = +41d29'15.6\"(J2000, accuracy of 0.3\"), which is 473\" west and 787\" north of the core of M 31. \n \nWe do not detect the object on a 10x60s stacked SLOTIS CCD image obtained on 2011 February 6.148 UT (limiting R magnitude at the position of 19.5). \n \nThere is no entry in VizieR/CDS for this object and no minor planet could be found on this position using the MPC/IAU Minor Planet Checker (see http://scully.harvard.edu/~cgi/CheckMP ). \n \nAll magnitudes given are obtained from a photometric solution using R magnitudes of the Local Group Survey M 31 catalogue (Massey et al. 2006, AJ, 131, 2478).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy", "Minor body", "Nova", "Repeater" ] }, "answerKey": "C" }, { "id": "atel_3250", "message": "Title: Swift J164449.3+573451/GRB 110328A: Continued Swift Monitoring\nAuthors: J. A. Kennea (PSU), P. Romano (INAF-IASF Palermo), H. A. Krimm (CRESST/GSFC/NASA), J. Cummings (NASA/UMBC), D. N. Burrows (PSU), G. Tagliaferri (INAF-OAB), P. A. Evans (U Leicester), S. D. Barthelmy (NASA/GSFC), A. A. Breeveld (UCL-MSSL), J. M. Gelbord (PSU), G. Israel (INAF-OAR), P. Esposito (INAF-OAC), T. Sakamoto (GSFC/UMBC), M. M. Chester (PSU), S. T. Holland (CRESST/USRA/GSFC), C. Wolf (PSU), N. Gehrels (NASA/GSFC)\nDate: 30 Mar 2011; 19:25 UT\nProvenance: Jamie A. Kennea (kennea@astro.psu.edu)\nSubjects: X-ray, Transient\nDescription: Referred to by ATel #: 3251\nWe report on continued monitoring of the new X-ray transient Swift J164449.3+573451/GRB 110328A (e.g. Kennea et al, ATEL #3242) by Swift. During 2011-Mar-29, Swift J164449.3+573451/GRB 110328A brightened significantly, triggering the Swift/BAT twice, at 18:26:25.19UT and 19:57:45.19UT respectively (see Sakamoto et al., GCN Circ #11842 for more details on the BAT characteristics). \nThe XRT light-curve shows significant variability, and is characterized by periods of bright flares, with the XRT measured brightness varying with a dynamic range of ~400 (~0.2 XRT c/s to ~80 XRT c/s). These flaring episodes last of the order of 2-3 x 10^4 seconds, with many flares occurring within these time periods. In the XRT light-curve, which currently covers from 2011-Mar-28 12:57UT to 2011-Mar-30 13:46UT, ~2 days, we see evidence for 5 major flaring outbursts, the timing of these outbursts does not appear to be periodic. These outburst events are seen in both XRT and BAT light-curves, which are well correlated. The underlying light-curve shows no evidence for a fading trend. \nThe source shows hardness changes that are correlated with the source brightness, with a correlation coefficient of r=0.71 when comparing the XRT count rate to the ratio of the 1.5-10 keV and 0.3-1.5 keV bands. \nA Fourier analysis of the first set of WT data (1.3 ks, MJD 55648.559-55648.946) was performed and no significant periodicity was found. The 3-sigma upper limits on the pulsed fraction, defined as semi-amplitude of the modulation divided by the mean source count rate, computed according to Israel & Stella 1996,ApJ, 468, 369 for a sinusoidal signal is 12% for periods between 3.5ms to 3s (we could not set meaningful upper limits on the pulsed fraction above 3s because of substantial red noise). Further timing analysis is ongoing. \nSummed UVOT observations of the source reveal no detection of an optical counterpart in any filter. The deepest images obtained are in the UVOT white and u filters; co-added images give the following upper limits: white (11.3ks) > 23.4 mag; u (23.6ks) > 22.9 mag. Photometry was performed using the UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627). \nThe source has a very atypical light-curve if it is a GRB. MAXI reports detection of this transient ~4 hours before the initial BAT trigger (Kimura et al., ATEL #3244), suggesting that the source was rising from quiescence at the time of the initial BAT trigger. This behavior is much more typical of a Galactic X-ray transient or some AGN flares. For example in the case of MAXI J1659-152, MAXI detected the rising flux ~5.5 hours before the source had reached sufficient brightness to trigger BAT (Negoro et al., ATEL #2873), although we note that an apparent associated optical counterpart with a measured redshift of z=0.35 (Levan et al., GCN Circ #11833, Thoene et al., GCN Circ #11834), and the detection of a bright radio source at a location consistent with this optical afterglow, are consistent with the transient being extragalactic in origin. We also note that the properties of the X-ray light-curve are becoming less consistent with those of an SFXT, which this source was previously suggested to be (Kennea et al., ATEL #3242), and this combined with the lack of a bright optical companion and the high galactic latitude, make the SFXT hypothesis less likely. \nMonitoring observations of this source by Swift are on-going.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy, Circumstellar disk", "Galaxy, Active galactic nucleus", "Galaxy, Binary system", "Magnetar, Active galactic nucleus" ] }, "answerKey": "B" }, { "id": "atel_3375", "message": "Title: NIR Flaring of BL Lac\nAuthors: L. Carrasco, A. Carraminana, G. Escobedo, E. Recillas, A. Porras, D. Y. Mayya. (INAOE, Mexico)\nDate: 24 May 2011; 05:51 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Millimeter, Infra-Red, Optical, Gamma Ray, TeV, VHE, UHE, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 3377, 3380, 3459\nFollowing the Fermi LAT report (ATel#3368) of increased activity of BL Lac. We carried out NIR Photometry of this object and found on May,23rd, 2011 (JD 2455704.991690) that the object was indeed brighter (H = 10.08 +/- 0.06) than our previous determination on JD 2455575.609653 when it had a flux corresponding to H = 11.439 +/- 0.05. This is consistent with the increase in flux in the optical reported in ATel #3371.Observations were carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We encourage further multi wavelength coverage.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Quasar", "Galaxy, Quasar", "Active galactic nucleus, Interstellar medium", "Supernova, Quasar" ] }, "answerKey": "A" }, { "id": "atel_3425", "message": "Title: Continued Swift and GROND observations of Swift J2058+0516 \nAuthors: Arne Rau, Jochen Greiner, Patricia Schady, Felipe Olivares E (all MPE Garching), Hans Krimm, Stephen Holland (both CRESST/GSFC/USRA)\nDate: 11 Jun 2011; 18:59 UT\nProvenance: Arne Rau (arau@mpe.mpg.de)\nSubjects: Infra-Red, Optical, X-ray, Transient\nDescription: Referred to by ATel #: 3426\nWe report further observations of the transient Swift J2058+0516 (Krimm et al. 2011, ATEL #3384; Greiner et al. 2011, ATEL #3385, Rau et al. 2011, ATEL #3390) by Swift and GROND. \n \nSwift J2058.4+0516 has now faded below detectability in the Swift/BAT (15-50 keV). The last significant detection was for the 4-day period 30 May - 2 June 2011 (0.0022 +/- 0.0004 ct/s/cm^2; ~10 mCrab). The 1-sigma upper limit for 10 June 2011 is 0.003 ct/s/cm^2. \n \nWe obtained 4 Swift/XRT observations over the last 10 days, sometimes stretching over several orbits. We detect seemingly stochastic variability by a factor of two within hours. There is also a long-term trend of a decreasing X-ray intensity from 1.5 ct/s at maximum to 0.5 ct/s maximum of the short-term variations. \n \nIn a stack of the recent Swift observations, Swift J2058+0516 is also detected in UVOT, at the following magnitudes (in Vega system, uncorrected for Galactic foreground extinction): \n \nuvm2 = 21.9 +/- 0.4 \nuvw2 = 22.2 +/- 0.4 \nuvw1 = 21.9 +/- 0.4 \nu = 21.1 +/- 0.3 \nb > 22.4 \n \nThe UVOT position is: \n \nRA (J2000) 20:58:19.87 = 314.58279 (deg) \nDec (J2000) +05:13:32.8 = +5.22578 (deg) \n \nwith an estimated uncertainty of 0.83 arcsec (radius, 90% confidence, statistical + systematic), fully consistent with the earlier reported GROND position (Rau et al. 2011, ATEL #3390). \n \nWe also continued observations of Swift J2058.4+0516 with GROND (Greiner et al. 2008, PASP 120, 405), the 7-channel imager mounted at the 2.2m MPI/ESO telescope at La Silla Observatory (Chile) on June 3, 2011 at 09:32 UT. \n \nIn a 24-min exposure we detect the candidate counterpart reported by Rau et al. 2011 (ATEL #3390) with the following magnitudes (all in the AB system): \n \ng = 22.54 +/- 0.05 \nr = 22.75 +/- 0.09 \ni = 22.81 +/- 0.14 \nz > 23.2 \nJ > 21.8 \nH > 21.3 \nK > 19.2 \n \nThese magnitudes were derived by calibrating the images against SDSS and 2MASS field stars and are not corrected for Galactic foreground reddening of E(B-V)~0.1mag (Schlegel et al. 1998). Upper limits are 3-sigma. \n \nComparison with the previous GROND observation indicates that the optical emission of the source did not change from May 28th to June 3rd. (Note, that the photometry given in Rau et al. 2011, ATEl #3390 suffered from a problem in the reduction and that the corrected magnitudes are consistent with the results reported above.) \n \nThe GROND observations have been obtained ~12hr after a 3ks Swift/XRT pointing (00032004003) starting on June 2rd at 09:50 UT and lasting until 21:18 UT. The XRT spectrum is best fit with a powerlaw with slope 1.51 +/- 0.04 and N_H=(7.4 +/- 0.3)E20 cm^-1, the latter largely consistent with the Galactic foreground column density of N_H= 6.5E20 cm^-1 (Kalberla et al. 2005). The count rate was 1.1 ct/s corresponding to an unabsorbed 0.3-10 keV flux of 5.8E11 erg/s/cm^2. Given the short-term X-ray variations and the 12hr time difference between the Swift and GROND observation, the X-ray-to-optical flux ratio remains high at approx. 12,000.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star, Variable star", "Globular cluster, Accreting object", "Variable star, Accreting object", "Interstellar medium, Accreting object" ] }, "answerKey": "C" }, { "id": "atel_3510", "message": "Title: PTF discovers a young type IIn SN in NGC 151\nAuthors: J. Parrent (LCOGT), D. Levitan (Caltech), A Howell (LCOGT), R. C. Thomas, P. Nugent (LBL), M. Sullivan (Oxford), M. Kasliwal, E. O. Ofek, R. Quimby (Caltech), S. Ben-Ami, D. Xu, I. Arcavi, A. Gal-Yam (Weizmann), C. B. Cenko, W. Li and A. V. Filippenko (UCB) report for the PTF\nDate: 26 Jul 2011; 19:22 UT\nProvenance: Avishay Gal-Yam (avishay.gal-yam@weizmann.ac.il)\nSubjects: Optical, Supernovae\nDescription: Referred to by ATel #: 3511, 3512\nThe PTF (ATEL #1964, #3253; www.astro.caltech.edu/ptf; Law et al. 2009, PASP, 121, 1395; Rau et al. 2009, PASP, 121, 1334) reports the discovery of a new supernova in NGC 151. PTF discoveries are made by autonomous PTF software (Bloom et al. 2011, http://adsabs.harvard.edu/abs/2011arXiv1106.5491B ), as well as by the Galaxy Zoo Supernova Project (Smith et al. 2011, MNRAS, 412, 1309; http://supernova.galaxyzoo.org ). \n \n \n \n Name | RA (J2000) | Dec (J2000) | Discovery | Mag | Redshift | Type | Spec. | Phase | Instrument | Notes \n PTF11iqb | 00 34 04.84 | -09 42 17.9 | Jul 23.41 | 16.8 | 0.0125 | SN IIn | Jul 24 | | P200+DBSP | Observed and reduced by D. Levitan \n | | | | | | | Jul 24 | | Gemini S+GMOS | Reduced by J. Parrent \n \nThe object is not seen down to unfiltered magnitude 18.8 on recent images from KAIT obtained on July 17.47 UT, 2011. PTF is a collaboration of Caltech, LCOGT, the Weizmann Institute, LBNL, Oxford, Columbia, IPAC, and Berkeley.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Neutron star", "Circumstellar disk", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_3600", "message": "Title: Unusually strong X-ray pulsations from Swift J1834.9-0846\nAuthors: Oleg Kargaltsev (UF), Ersin Gogus (Sabanci Univ. Istanbul), Chryssa Kouveliotou (NASA/MSFC), and George Pavlov (PSU)\nDate: 27 Aug 2011; 18:24 UT\nProvenance: Oleg Kargaltsev (oyk100@astro.ufl.edu)\nSubjects: X-ray, Neutron Star, Soft Gamma-ray Repeater, Transient, Pulsar\nDescription: The newest magnetar candidate Swift J1834.9-0846 (D'Elia et al. GCN Circ. #12253, Guiriec et al. #12255) was observed with Chandra/ACIS-S for 13 ks on 2011 August 22, with time resolution of 0.44 s. The timing analysis of the barycentered data reveals an unusually high pulsed fraction at the previously reported frequency of 0.402850 Hz (Gogus et al. ATels #3542, #3576). The pulsed fraction in 2-10 keV for the 733 events extracted from r=1'' circular aperture, centered on the source, exceeds 80%. The RMS measure of pulsation strength exceeds 0.7. The background contribution in the chosen extraction aperture and energy range is essentially zero. The detected pulsations, with a single broad peak per period, are much stronger then those observed from any other magnetar in this energy range. The average source flux during the ACIS observation was 2.4e-12 erg/s/cm2 (absorbed, in 2-9 keV). No noticeable flaring activity was seen during the observation. We have also performed phase-connected timing analysis of the RXTE and Chandra data and produced the following spin ephemeris spanning over a time baseline of ~15 days: nu = 0.40285190(6) Hz and nu-dot = -1.3(1)E-12 Hz/s (Epoch 55783 MJD), consistent with those reported by Kuiper & Hermsen (ATel #3577).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Binary system", "Nova", "Circumstellar disk" ] }, "answerKey": "A" }, { "id": "atel_3660", "message": "Title: NIR and Radio follow-up of PKS0402-362\nAuthors: Roberto Nesci (University La Sapienza, Italy); Roopesh Ojha (NASA Goddard Space Flight Center, USA); Matthias Kadler (University of Wurzburg, Germany); Tapio Pursimo (Nordic Optical Telescope, Santa Cruz de La Palma, Spain); Gino Tosti (Perugia University, Italy); Michael Dutka (Catholic University, USA); J. Blanchard (Department of Physics, University of Tasmania, Hobart, Tasmania, 7001, Australia); J. Lovell (School of Mathematics & Physics, Private Bag 37, University of Tasmania, Hobart, TAS, 7001, Australia).\nDate: 25 Sep 2011; 04:43 UT\nProvenance: Roberto Nesci (roberto.nesci@uniroma1.it)\nSubjects: Radio, Infra-Red, AGN, Blazar\nDescription: The blazar PKS 0402-362 (RA: 04h02m02.5994s, Dec: -36d13m11.947s) is being monitored by the TANAMI project (http://pulsar.sternwarte.uni-erlangen.de/tanami/) in NIR with the REM telescope (http://www.rem.inaf.it) since February 2011. A Gamma-ray flare has been detected by Fermi-LAT (ATel #3655) on 2011-09-22 (JD 55827): Swift follow-up is reported in ATel #3659. We recorded J=15.60 (+/-0.17) on 2011-09-21, UT 09:18 (MJD 55825.38) pratically simultaneous with the Gamma-ray flare, using a sequence of 4 comparison stars taken from the 2MASS for differential photometry. In the 2MASS catalogue the source is reported at J=16.20. During our monitoring PKS 0402-362 was generally below the detection threshold. We detected the source also on 2011-04-11 (MJD 55662.06) at J=15.14 (+/-0.16), and on 2011-08-10 (MJD 55783) at J=15.62 (+/-0.20): in neither case Gamma-ray flares were reported. Preliminary radio observations from Ceduna telescope suggests that the radio flux has been increasing from about 1.8 Jy to 2.44 Jy on 2011-09-15. Further multiwavelength observations are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Interstellar medium", "Galaxy", "Minor body" ] }, "answerKey": "A" }, { "id": "atel_3775", "message": "Title: Extremely high cm-band radio flux level of the gamma-ray flaring FSRQ PKS 1510-089\nAuthors: M. Orienti (University of Bologna, INAF-IRA Bologna), F. D'Ammando (INAF-IRA Bologna), M. Giroletti (INAF-IRA Bologna), and A. Orlati (INAF-IRA Medicina) on behalf of the ESCS-Development-Team \nDate: 21 Nov 2011; 10:21 UT\nProvenance: Filippo D'Ammando (filippo.dammando@iasf-roma.inaf.it)\nSubjects: Radio, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 3799\nThe 32-m single dish antenna located at Medicina has been observing the flat spectrum radio quasar PKS 1510-089 starting from July 2011 with monthly frequency. The observations were organised as a follow-up of the gamma-ray flaring event reported in July 2011 by AGILE (ATel #3470) and Fermi (ATel #3473). \nRecently, radio observations were performed at 4.9 GHz and 8.0 GHz on 2011 November 16. The observations have been carried out using the new Enhanced Single-dish Control System (ESCS; for details about ESCS please contact: Andrea Orlati 3698). \nThe observed flux density levels are 2.49+/-0.17 Jy at 4.9 GHz, and 3.72+/-0.22 Jy at 8.0 GHz. As a comparison, on 2011 October 13 the flux densities measured with the Medicina antenna were 1.53+/-0.05 Jy at 4.9 GHz, and 2.08+/-0.05 Jy at 8.0 GHz. \nThe increase of the radio flux density may be related to the high activity level recently observed in gamma rays. Further multifrequency observations are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Binary system", "Quasar", "Accreting object" ] }, "answerKey": "C" }, { "id": "atel_3850", "message": "Title: Spectroscopic classification of PTF12js as an Fe II nova in M31\nAuthors: A. W. Shafter (SDSU), M. J. Darnley, M. F. Bode (Liverpool JMU, UK), R. Ciardullo (PSU), K. Hornoch (Astronomical Institute, Ondrejov, Czech Republic)\nDate: 7 Jan 2012; 12:40 UT\nProvenance: Allen W. Shafter (aws@nova.sdsu.edu)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 3851\nWe report spectroscopic observations of the M31 nova candidate PTF12js (M31N 2012-01a?) recently reported by Cao & Kasliwal (ATel #3846). At our request, a spectrum (410–900 nm) was obtained by J. Caldwell on 2012 Jan. 07.14 UT with the 9.2-m Hobby-Eberly Telescope (+ Marcario Low-Resolution Spectrograph). The spectrum reveals narrow Balmer and Fe II emission lines (FWHM Hα ~ 800 km/s; EW Hα ~ -2.0 nm) with pronounced P Cygni profiles superimposed on a blue continuum. These observations confirm that PTF12js is an Fe II nova in M31 observed near maximum light. Inspection of an image of the field taken with the 0.65-m telescope at Ondrejov on the night of Jan. 04.84 UT reveals the nova on the rise at R = 19.7 +/- 0.3. \nA.W.S. thanks the NSF for support through AST-1009566. \nHET Spectra of Local Group Novae", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Near-Earth object", "Galaxy", "Exoplanet" ] }, "answerKey": "A" }, { "id": "atel_4000", "message": "Title: INTEGRAL Galactic Bulge monitoring detects activity from XMMU J174445.5-295044 with JEM-X\nAuthors: J. Chenevez (DTU Space, Denmark), E. Kuulkers (ESA/ESAC, Spain), J. Alfonso-Garzon (CAB/INTA-CSIC, Spain), V. Beckmann (APC, France), T. Bird (Southampton, UK), S. Brandt (DTU Space, Denmark), M. Del Santo (INAF/IASF-Roma, Italy), A. Domingo (CAB/INTA-CSIC, Spain), K. Ebisawa (ISAS, Japan), P. Jonker (SRON, The Netherlands), P. Kretschmar (ESA/ESAC, Spain), C. Markwardt (GSFC, USA), T. Oosterbroek (ESA/ESTEC, The Netherlands), A. Paizis (INAF-IASF, Italy), K. Pottschmidt (UMBC/NASA GSFC, USA), C. Sanchez-Fernandez (ESA/ESAC, Spain), R. Wijnands (UvA, The Netherlands)\nDate: 24 Mar 2012; 21:59 UT\nProvenance: Jerome CHENEVEZ (jerome@space.dtu.dk)\nSubjects: X-ray, Gamma Ray, Transient\nDescription: Referred to by ATel #: 4924, 15236\nDuring INTEGRAL Bulge monitoring (ATel #438; Kuulkers et al. 2007, A&A, 466, 595) observations performed on March 23, 2011, between 6:52 and 10:33 (UTC), the twin X-ray monitor JEM-X detected an X-ray transient source at the position: \nRA= 266.20 (17h 44m 48s) \nDEC=-29.85 (-29d 51' 00\") \n(J2000) with an uncertainty of 1.3 arcmin at 95% confidence level. \nThe Galactic coordinates are: (l, b)= (359.13, -0.32). \n \nThe source is detected at 5 σ between 10-25 keV (for 12.3 ks effective exposure), and measured at a flux of 13±3 mCrab (1.5±0.3 ×10-10 erg/cm2/s). It is not detected in other energy bands, leading to a 3 σ upper limit of 5 mCrab between 3-10 keV, which suggests a large amount of absorption. The source is not detected by the IBIS/ISGRI instrument with 5 σ upper limits of about 5 mCrab and 10 mCrab between 18-40 keV and 40-100 keV, respectively. \n \nBoth the source position and its high absorption are consistent with the X-ray transient XMMU J174445.5-295044 reported by Heinke et al. 2009, ApJ 701, 1627. \n \nINTEGRAL will continue to monitor the Galactic bulge on March 29 and 31, and observation results from near real time data will be made available at: http://integral.esac.esa.int/BULGE/index.html \nMulti-wavelength follow-up observations are encouraged to constrain the nature of this transient.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object, Binary system", "Galaxy, Binary system", "Repeater, Binary system", "Accreting object, Black hole" ] }, "answerKey": "A" }, { "id": "atel_4080", "message": "Title: X-ray Flux Enhancement from 1E 2259+586 in Swift XRT Monitoring\nAuthors: R. F. Archibald, V. M. Kaspi (McGill U.), A. P. Beardmore (U. Leicester), N. Gehrels (NASA-GSFC), J. Kennea (PSU)\nDate: 30 Apr 2012; 20:04 UT\nProvenance: Victoria Kaspi (vkaspi@physics.mcgill.ca)\nSubjects: X-ray, Neutron Star, Soft Gamma-ray Repeater, Pulsar\nDescription: Referred to by ATel #: 4101\nWe report an increase in the X-ray flux from 1E 2259+586 in our most recent Swift XRT monitoring observation on April 28, 2012 (MJD 56045.00889). We measure a 1-10 keV flux of (5.0+/-0.2)x10^-11 erg/s/cm2, which represents a factor of 2.00+/-0.09 increase relative to the long-term average, and to the flux measured in the previous Swift observation on April 14, 2012. In addition, the 1-10 keV pulse profile shows a modest deviation from the quiescent profile, with the ratio of the amplitudes of the two pulse peaks closer to unity. We detect no bursts in the April 28 observation. We encourage observations of the source at other wavelengths.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Magnetar", "Supernova", "Neutron star" ] }, "answerKey": "D" }, { "id": "atel_4170", "message": "Title: MAXI/GSC detection of a renewed activity from IGR J17191-2821\nAuthors: J. Sugimoto (RIKEN), H. Negoro (Nihon U.), M. Serino, T. Mihara, M. Sugizaki, T. Yamamoto, M. Matsuoka (RIKEN), S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa (JAXA), N. Kawai, M. Morii, R. Usui, K. Ishikawa (Tokyo Tech), A. Yoshida (AGU), H. Tsunemi, M. Kimura (Osaka U.), M. Nakajima, M. Asada, H. Sakakibara, N. Serita (Nihon U.), Y. Ueda, K. Hiroi, M. Shidatsu, R. Sato (Kyoto U.), Y. Tsuboi, M. Higa (Chuo U.) M. Yamauchi, Y. Nishimura, T. Hanayama, K. Yoshidome (Miyazaki U.), K. Yamaoka (Waseda U.) report on behalf of the MAXI team\nDate: 13 Jun 2012; 05:25 UT\nProvenance: Tatehiro Mihara (mihara@crab.riken.jp)\nSubjects: X-ray, Binary, Neutron Star, Transient\nDescription: At 2012/06/12 17:17:52 UT, the MAXI/GSC nova alert system triggered on enhanced X-ray emission from the position (259.66,-28.30) with a statistical uncertainty of 10 arcmin at the 90% confidence limit and an additional systematic uncertainty of 0.1 deg (90% containment radius). The position is consistent with IGR J17191-2821. \nThe one-day average X-ray flux from 2012/06/11 18:00 to 6/12 18:00 UT is about 43 +- 17 mCrab in 4-10 keV band. The source had been in invisible area for MAXI/GSC near the ISS rotation pole during June 6 - 10, 2012. The MAXI/GSC, however, detected the beginning of the outburst at June 4 00:00 (UT). The brightening of the source can also be seen in the Swift/BAT light curve ( http://heasarc.gsfc.nasa.gov/docs/swift/results/transients/weak/IGRJ17191-2821/ ). \nIGR J17191-2821 was discovered with INTEGRAL in March 2007 (ATel #1021, #1022, #1025, #1065, #1068, #1070, #1075, #1096). No outburst was reported since then. The source was found to be a neutron star system showing a kH-QPO (ATel #1075) and an X-ray burst (ATel #1065). \nThe latest light curves and images of IGR J17191-2821 by MAXI/GSC are placed at the following URL: \nhttp://maxi.riken.jp/top/index.php?cid=1&jname=J1719-283", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system", "Nova", "Minor body", "Neutron star" ] }, "answerKey": "D" }, { "id": "atel_4325", "message": "Title: Fermi LAT detection of a GeV flare from PMN J1626-2426\nAuthors: Michael Dutka (Catholic U.) and Roopesh Ojha (NASA/GSFC) on behalf of the Fermi Large Area Telescope Collaboration\nDate: 21 Aug 2012; 16:36 UT\nProvenance: Roopesh Ojha (Roopesh.Ojha@gmail.com)\nSubjects: Gamma Ray, >GeV, Request for Observations, AGN, Blazar, Quasar\nDescription: The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed gamma-ray flaring activity from the position R.A.=16h24m53.04s, Dec.=-24d18m32.0s (95% radius: 0.25 degrees). This is in the vicinity of the flat spectrum radio source PMN J1626-2426 (also known as 2FGL J1627.0-2425c, Nolan et al. 2012, ApJS, 199, 31; R.A.= 16h27m00.010s, Dec.= -24d26m40.50s, J2000.0, Healey et al. 2007, ApJS, 171, 61). There does not appear to be any optical information, including redshift, in the literature. There is an HII region located at this R.A. and Dec as well which makes optical observations of this source very difficult. \nPreliminary analysis indicates that the source brightened in gamma rays with a daily averaged flux (E > 100 MeV) of (1.0+/-0.3) x10^-6 ph cm^-2 s^-1 (errors are statistical only) on 19 August 2012, a factor of 17 greater than the average flux reported in the second Fermi LAT catalog (2FGL, Nolan et al. 2012, ApJS, 199, 31). This is the highest flux observed for this source since the beginning of the Fermi mission. \nBecause Fermi operates in all-sky survey mode, gamma-ray monitoring of this source will continue. In consideration of the activity of this source we encourage multiwavelength observations. The Fermi LAT contact person for this source is Michael Dutka (ditko86@gmail.com). \nThe Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Magnetar", "Active galactic nucleus, Black hole", "Active galactic nucleus, Repeater", "Active galactic nucleus, Stellar evolution" ] }, "answerKey": "B" }, { "id": "atel_4410", "message": "Title: Follow-up ATCA radio observations of the black hole candidate Swift J174510.8-262411 \nAuthors: S. Corbel (Univ. Paris Diderot & CEA Saclay), P. Edwards, T. Tzioumis (ATNF), M. Coriat, R. Fender (Univ. Southampton) & C. Brocksopp (MSSL) \nDate: 21 Sep 2012; 22:39 UT\nProvenance: Mickael Coriat (mickael@coriat.eu)\nSubjects: Radio, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 4450, 4456\nFollowing the discovery of Swift J174510.8-262411 (GCN #13774, GCN #13775, ATEL #4380) and the report of a radio counterpart (ATel # 4394), we have conducted radio observations with the Australia Telescope Compact Array on 2012 September, 19. \n \nA bright radio source is detected at a position consistent with Swift J174510.8-26241 with preliminary flux densities of 13.2 +/- 0.20 mJy at 5.5 GHz and 13.5 +/- 0.20 mJy at 9.0 GHz, giving a spectral index of +0.05+/- 0.04. This radio spectral index during this ATCA observation clearly favours optically thick synchrotron emission from self-absorbed compact jets, which is fully consistent with the source being in the hard state at the time of the ATCA radio observations (e.g. ATel #4393). \n \nA comparison with the radio observation on the previous day (ATel # 4394) indicates that the flux densities have doubled in less than a day. Follow up radio observation are important to catch the possible radio flare that could occur in the next days.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Repeater", "Globular cluster", "Black hole" ] }, "answerKey": "D" }, { "id": "atel_4500", "message": "Title: Swift observation of Nova OGLE-2012-NOVA-002\nAuthors: N. Masetti (INAF/IASF, Bologna), A. Paggi (CfA, Harvard), F. Massaro (Stanford Univ.), P. Parisi (INAF/IAPS, Roma) and R. Angeloni (PUC, Santiago)\nDate: 19 Oct 2012; 16:24 UT\nProvenance: Nicola Masetti (masetti@iasfbo.inaf.it)\nSubjects: Ultra-Violet, X-ray, Nova, Transient\nDescription: The nova OGLE-2012-NOVA-002 (ATels #4483, #4485, #4487) was observed with the XRT and UVOT instruments onboard the Swift satellite. Observations began on October 18, 2012, at 16:33 UT and lasted about 3800 seconds for both instruments. \nThe UVOT data, acquired in the UVW2 filter (central wavelength: 1928 Angstroms; Poole et al. 2008, MNRAS, 383, 627), allow a detection of the source at magnitude 14.44 +- 0.04 (Vega system); this indicates that the nova is relatively quite bright in the ultraviolet. \nOn the contrary, with the XRT pointing we do not detect the source down to a 3-sigma upper limit of 0.005 counts s-1 in the 0.3-10 keV band. \nThis, assuming a blackbody spectrum with temperature 0.5 keV implies a flux limit of 1.4e-13 erg cm-2 s-1 which, at the distance of the SMC (60.6 kpc; Hilditch et al. 2005, MNRAS, 357, 304), corresponds to a luminosity upper limit of about 6e34 erg s-1 in that band. \n \n \nWe thank Neil Gehrels, Jamie Kennea and the Swift team for having quickly set up and performed the requested Target-of-Opportunity observation.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Exoplanet", "Circumstellar disk", "Repeater", "Nova" ] }, "answerKey": "D" }, { "id": "atel_4600", "message": "Title: RATAN-600 multi-frequency measurements of the gamma-ray blazar BL Lacertae\nAuthors: M. Mingaliev, S. Trushkin, J. Sotnikova, A. Erkenov, T. Mufakharov (SAO RAS)\nDate: 22 Nov 2012; 13:58 UT\nProvenance: Sergei Trushkin (satr@sao.ru)\nSubjects: Radio, Millimeter, Infra-Red, Gamma Ray, Blazar\nDescription: Referred to by ATel #: 4973, 5002\nWe have measured radio flux densities of BL Lac (B2200+420) with the RATAN-600 radio telescope at 4.8, 7.9, 11.2 and 21.7 GHz during 6 October - 20 November, 2012 to study the detected (ATel #4557, #4565, and #4568) flare. In the rest of October BL Lac became bright in X-ray, FIR, microwave and radio bands. Our data agree with the OVRO radio flux 9.6 Jy at 15 GHz by Hovatta et al. (ATEL #4565) on 7 November. We have measured 5.29 +/- 0.1 Jy at 4.8 GHz, 6.85 +/- 0.2 Jy at 7.9 GHz, 7.27 +/- 0.2 Jy at 11.2 GHz and 7.00 +/- 0.3 Jy at 21.7 GHz on 14 October. On 12 November flux density had notably risen to 8.30 +/- 0.19 Jy at 7.7 GHz, to 9.86 +/- 0.2 Jy at 11.2 GHz and to 11.70 +/- 0.3 Jy at 21.7 GHz. Our further observations show the higher fluxes at high frequencies (20 November): 8.83 +/- 0.34 Jy at 7.7 GHz, 11.19 +/- 0.39 Jy at 11.2 GHz and 12.6 +/- 0.6 Jy at 21.7 GHz. Growth of the flux densities has been detected after 15 November at all frequencies, meanwhile the flaring event began during MJD56225-56230 probably. The spectral index changed from -0.08 +/- 0.02 to +0.23 +/- 0.02 at 11.2-21.7 GHz for October to November flux points. The mean spectra in October and November 2012 and the updated light curves are accessed: http://www.sao.ru/hq/giag/new1-en.html", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Circumstellar disk", "Active galactic nucleus, Repeater", "Active galactic nucleus, Black hole", "Active galactic nucleus, Near-Earth object" ] }, "answerKey": "C" }, { "id": "atel_4675", "message": "Title: Bright OT detected by MASTER\nAuthors: S. Shurpakov, D. Denisenko, P. Balanutsa, V. Lipunov, E. Gorbovskoy, N. Tiurina, V. Kornilov, A. Belinski, N. Shatskiy, V. Chazov, A. Kuznetsov, D. Zimnukhov (Moscow State University, SAI), V. Krushinsky, I. Zalozhnih, A. Popov, A. Bourdanov, A. Punanova (Ural Federal University), K. Ivanov, S. Yazev, N. Budnev, E. Konstantinov, O. Chuvalaev, V. Poleshchuk, O. Gress (Irkutsk State University), A. Parkhomenko, A. Tlatov, D. Dormidontov, V. Senik (Kislovodsk solar station of the Pulkovo observatory RAS), V. Yurkov, Y. Sergienko, D. Varda, E. Sinyakov (Blagoveshchensk Educational University), V. Shumkov, P. Podvorotny, (MASTER team members), H. Levato, C. Saffe (ICATE), C. Mallamaci, C. Lopez and F. Podest (Observatorio Astronomico Felix Aguilar; OAFA)\nDate: 24 Dec 2012; 08:07 UT\nProvenance: Vladimir Lipunov (lipunov2007@gmail.com)\nSubjects: Optical, Cataclysmic Variable\nDescription: Referred to by ATel #: 4679\nMASTER OT J211322.92+260647.4 - new bright CV\nMASTER-Amur auto-detection system discovered OT source at (RA, Dec) = 21h 13m 22.92s +26d 06m 47.4s on 2012-12-21.46578 UT. The OT unfiltered magnitude is 15.2m (limit 16.1m). The OT is seen in 4 images. We have reference image without OT on 2011-08-21.64619 UT with unfiltered magnitude limit 19.6m. \nThere is a faint star at the position of OT on blue digitized POSS plates. Color-combined finder chart is uploaded to http://master.sai.msu.ru/static/OT/J211322+260647-BRIR5x5.jpg The star is present in GSC 2.3.2 with the coordinates (J2000.0) 21 13 22.953 +26 06 47.02 and magnitude Jmag=21.69. It is also identical to the UV source GALEX J211322.8+260647 (FUV=21.97+/-0.31, NUV=22.84+/-0.48). \nNothing is present at this position in 2MASS, USNO-B1.0, 1RXS, GCVS catalogs and in AAVSO VSX. This area of sky is not covered by SDSS and CRTS. No previous outbursts were detected on 9 Palomar/NEAT images obtained on 2001 Aug. 12, 18 and 2002 July 27. \nBased on the amplitude of variability (more than 6m) we conclude that MASTER OT J211322.92+260647.4 is a new cataclysmic variable of SU UMa or WZ Sge type in superoutburst. Follow up observations are required. The discovery and reference images are available at: http://master.sai.msu.ru/static/OT/211322.92260647.4.png \nList of optical transients discovered by MASTER\nGlobal MASTER Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater", "Nova", "Variable star", "Near-Earth object" ] }, "answerKey": "C" }, { "id": "atel_4750", "message": "Title: EVN detection of a compact radio source as a counterpart to Fermi J1418+3541\nAuthors: Sandor Frey (FOMI Satellite Geodetic Obs.), Zsolt Paragi (JIVE), Krisztina Gabanyi (Konkoly Obs.), Tao An (Shanghai Astronomical Obs.)\nDate: 20 Jan 2013; 11:44 UT\nProvenance: Zsolt Paragi (zparagi@jive.nl)\nSubjects: Radio, AGN, Blazar\nDescription: Fermi J1418+3541 is a suspected blazar recently detected as a flaring gamma-ray point source, identified with likely radio, optical and infrared counterparts within the Fermi LAT error circle (Dutka et al. 2012, ATEL #4643; Mahabal et al. 2012, ATEL #4645; Bernieri et al. 2013, A&A, in press, arXiv:1212.6868). \nWe detected the proposed radio counterpart of Fermi J1418+3541 with the European VLBI Network (EVN), in real-time e-VLBI mode at 5 GHz on 2013 Jan 16 (project code RSF07). The source is dominated by a compact radio core, practically unresolved on intercontinental baselines from Europe to South Africa. The \"core\" flux density (34 +/- 2 mJy) is consistent with the historical single-dish values. The upper limit to its fitted angular size (Gaussian FWHM) is estimated as 0.20 mas in the ~E-W and 0.06 mas in the ~N-S direction. We derived a lower limit to its brightness temperature, ~1011 K, which suggests Doppler-boosted radio emission from a relativistic jet oriented close to the line of sight, another strong indication of its blazar nature. There is a weak mas-scale jet-like extension seen in the W-NW direction from the core. The accurate position of the brightness peak is RA 14h18m28.58178s, Dec 35d42'49.4618\" (J2000; formal uncertainty ~0.8 mas). \nWe thank the EVN PC chairman, Tom Muxlow for approving the short e-EVN observations, and the staff of the EVN and the observatories for carrying out the experiment. e-VLBI research infrastructure in Europe is supported by the European Union's Seventh Framework Programme (FP7/2007-2013) under grant agreement RI-261525 NEXPReS. The European VLBI Network is a joint facility of European, Chinese, South African and other radio astronomy institutes funded by their national research councils. We thank for the OTKA grant K104539.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Stellar evolution", "Active galactic nucleus", "Black hole" ] }, "answerKey": "D" }, { "id": "atel_4830", "message": "Title: VVV-NOV-002: the second Galactic nova candidate discovered in the Milky Way bulge by the VVV Survey\nAuthors: R. K. Saito (Pontificia Universidad Catolica de Chile, Universidad de Valparaiso, The Milky Way Millennium Nucleus), D. Minniti (Pontificia Universidad Catolica de Chile, Vatican Observatory, The Milky Way Millennium Nucleus), R. Angeloni (Pontificia Universidad Catolica de Chile) and M. Catelan (Pontificia Universidad Catolica de Chile, The Milky Way Millennium Nucleus)\nDate: 21 Feb 2013; 12:30 UT\nProvenance: Roberto Saito (rsaito@astro.puc.cl)\nSubjects: Infra-Red, Nova, Transient\nDescription: Referred to by ATel #: 4879, 7124\nWe report the discovery of the second likely Galactic nova in the VVV Survey data (vvvsurvey.org; Minniti et al. 2010, New Astronomy, 15, 433). Observations taken during 2012 show the presence of a stellar source fading in brightness from March 1st 2012 to October 08 2012 (see table below). The light curve follows the expected behavior of the early stages of a nova outburst, with VVV-NOV-002 fading by Delta_Ks>5.7 mag over 221 days. \nThe coordinates of VVV-NOV-002 are RA, DEC= 17:32:23.10, -29:48:38.5 (J2000), corresponding to (l,b)= -2.277,1.973 deg. Previous VVV observations taken during 2011 show no detection at the target position, which allow us to infer the nova remnant was fainter than the limiting magnitude of Ks=16.76 mag in the field. The nova outburst occurred between September 24 2011, the last 2011 observation with no detection, and March 1st 2012, when the object is first detected as a saturated source with Ks=8.15 mag. \nAccording to the VVV reddening maps (Gonzalez et al., 2012, A&A, 543, 13) assuming the Cardelli et al. (1989, ApJ, 345, 245 2009) extinction law, the extinction for a 2 arcmin region around the target position is E(J-Ks)=0.54, corresponding to AV=6.67 mag. \nThere are no previous entries in the literature for the target position. \n \n \n VVV-NOV-002 Table of Observations \n \n Date (UT) filter mag flag \n 2011-05-07.3390 Ks beyond detection \n 2011-07-26.2299 Ks beyond detection \n 2011-08-30.1265 Ks beyond detection \n 2011-09-04.0604 Ks beyond detection \n 2011-09-13.0354 Ks beyond detection \n 2011-09-24.0046 Ks beyond detection \n 2012-03-01.3514 Ks 8.149+/-0.010 -9 \n 2012-03-24.2745 Ks 8.869+/-0.010 -9 \n 2012-06-07.1976 Ks 11.586+/-0.010 -1 \n 2012-06-08.2327 Ks 11.628+/-0.010 -1 \n 2012-06-21.0333 Ks 11.937+/-0.010 -1 \n 2012-06-26.0726 Ks 12.122+/-0.010 -1 \n 2012-07-12.1512 Ks 12.477+/-0.010 +1 \n 2012-07-14.1707 Ks 12.505+/-0.010 +1 \n 2012-07-17.1685 Ks 12.558+/-0.010 +1 \n 2012-07-17.9939 Ks 12.609+/-0.010 +1 \n 2012-07-27.1015 Ks 12.791+/-0.012 +1 \n 2012-08-01.0482 Ks 12.931+/-0.012 +1 \n 2012-08-02.1506 Ks 12.894+/-0.012 +1 \n 2012-08-12.0111 Ks 13.121+/-0.015 +1 \n 2012-08-13.1334 Ks 13.078+/-0.015 +1 \n 2012-08-16.9878 Ks 13.100+/-0.018 +1 \n 2012-09-10.0695 Ks 13.463+/-0.022 +1 \n 2012-09-11.9821 Ks 13.557+/-0.022 +1 \n 2012-09-18.0335 Ks 13.587+/-0.023 +1 \n 2012-09-19.0093 Ks 13.534+/-0.024 +1 \n 2012-09-20.0010 Ks 13.651+/-0.024 +1 \n 2012-10-01.0275 Ks 13.743+/-0.028 +1 \n 2012-10-02.0127 Ks 13.819+/-0.028 +1 \n 2012-10-02.0732 Ks 13.771+/-0.027 +1 \n 2012-10-03.0328 Ks 13.751+/-0.028 +1 \n 2012-10-08.9968 Ks 13.861+/-0.029 +1 \n \nThe VVV data are in the natural VISTA Vegamag system. \nPhotometric flags are described in Saito et al. 2012 (A&A, 537, A107): \n-9 saturated source \n-1 stellar object \n+1 non-stellar object \nAcknowledgments: We gratefully acknowledge use of data from the ESO Public Survey programme ID 179.B-2002 taken with the VISTA telescope, and data products from the Cambridge Astronomical Survey Unit.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Variable star", "Stellar evolution", "Exoplanet" ] }, "answerKey": "A" }, { "id": "atel_4920", "message": "Title: Nova SMC 2012: a probable 20.4 hour period detected by Swift in the UV and X-ray\nAuthors: K. L. Page, J. P. Osborne, A. P. Beardmore (U. Leicester) and G. J. Schwarz (AAS)\nDate: 27 Mar 2013; 09:08 UT\nProvenance: Kim Page (kpa@star.le.ac.uk)\nSubjects: Nova\nDescription: Following the detection of Nova SMC 2012 (OGLE-2012-NOVA-002) as a super-soft X-ray source on 2013 March 2, 270 days after optical detection (ATel #4853), Swift has monitored the source, generally daily, and recently also at higher cadences. The X-ray spectrum of this nova has not changed significantly over this time. Periodogram analysis of de-trended UVOT data (collected using the uvw2 filter, central wavelength 1928 Angstrom) since the detection of the super-soft emission (i.e. days 270-294) reveals a strongly-detected sine-like modulation with a period of 20.4 +/- 0.3 hours and an amplitude of 0.11 +/- 0.01 magnitudes. During this interval the mean uvw2 brightness fell from magnitude ~16.1 to ~16.3, while the X-ray count-rate shows no decline over this interval, having a mean of ~0.1 count s-1. The highest peak in the X-ray periodogram is at the same frequency as detected in the UV. Folded at the UV period, the X-ray count-rate shows a modulation with an amplitude of 0.020 +/- 0.005 count s-1, in phase with the UV brightness variation. \nThis pattern of in-phase X-ray & UV modulation is similar to that seen in Nova Mon 2012 and HV Cet (ATel #4727; Beardmore et al., 2012, A&A, 545, A116). In these objects the modulation was ascribed to a raised portion of an accretion disk rim passing through the line of sight, reducing the observed size of a scattering region around the hot white dwarf, and likely reprocessing the illuminating flux from its inner face. The detected period in this scenario would be the orbital period of the binary system. This result suggests that Nova SMC 2012 has a moderately high orbital inclination, however no strong eclipse is evident in the UV folded light-curve. \nAlthough most novae have orbital periods of a few hours, novae with Porb = 20-50 hours are known (including the well-known recurrent nova U Sco at Porb=29.5 hours). A nova with an orbital period in this range requires an evolved secondary star. \nFurther Swift observations are planned, and follow-up observations at other wavelengths are encouraged. We thank the Swift PI and operations team for their support.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Binary system", "Active galactic nucleus, Binary system", "Nova, Binary system", "Nova, Globular cluster" ] }, "answerKey": "C" }, { "id": "atel_5040", "message": "Title: Detection of radio pulsations from the direction of the NuSTAR 3.76 second X-ray pulsar at 8.35 GHz\nAuthors: Ralph Eatough (Max-Planck-Institut fuer Radioastronomie: MPIfR), Ramesh Karuppusamy (MPIfR), Michael Kramer (MPIfR), Bernd Klein (MPIfR), David Champion (MPIfR), Alex Kraus (MPIfR), Evan Keane (Jodrell Bank Centre for Astrophysics: JBCA), Cees Bassa (JBCA), Andrew Lyne (JBCA), Patrick Lazarus (MPIfR), Joris Verbiest (MPIfR), Paulo Freire (MPIfR), Andreas Brunthaler (MPIfR), Heino Falcke (ASTRON, Nijmegen)\nDate: 2 May 2013; 21:48 UT\nProvenance: Evan Keane (ekean@jb.man.ac.uk)\nSubjects: Radio, Neutron Star, Soft Gamma-ray Repeater, Pulsar\nDescription: Referred to by ATel #: 5043, 5046, 5053, 5058, 5070, 5076, 13042\nAs part of continued efforts to detect radio pulsations from the 3.76-second X-ray pulsar discovered with the NuSTAR telescope (ATels #5020, #5027, #5033, #5035), we have performed a ~2.5 hour observation with the Max Planck Institute for Radio Astronomy (MPIfR) Effelsberg radio telescope at a central frequency of 8.35 GHz. This observation was performed at these observing frequencies to mitigate the expected strong scattering of radio waves in the Galactic Centre region (scattering time ~ freq.^-4). Using a secondary focus cryogenically cooled receiver (system temperature ~22 K) we recorded summed polarisations for 128 spectral channels, across a bandwidth of 500 MHz, and with a data sampling interval of ~65 microseconds. Observations started on 2013-05-02 at 01:11:20 UTC on the updated source position provided in ATel #5032. We have detected a narrow (duty cycle ~ 2%) bright (signal-to-noise ratio ~140) pulse with a spin period matching the NuSTAR discovery period (see link to pulsar diagnostic plot generated with the psrchive software package: http://psrchive.sourceforge.net/ ). Assuming typical contributions to the system temperature from spillover, we estimate the flux density at 8.35 GHz to be ~0.2 mJy. Note, this signal is not seen in two 30 minute off-source observations at the same telescope elevation. Compared with the previously reported detections at lower frequencies (Atel #5035), the duty cycle of the pulse is markedly smaller, and in addition, we do not observe any changes in the spin period over the 2.5 hr observation. We also note that the dispersion measure appears to be high (DM~4000 pc cm^-3) however the small dispersive delays at this frequency result in large uncertainties. Such a large dispersion measure would plausibly place this source at the Galactic Centre. We continue to work on constraining this further. We note that without a multi-beam receiver (where multiple sky positions are recorded simultaneously) we cannot yet conclusively rule out the possibility that the signal reported here is caused by terrestrial RFI in the primary telescope beam, however, we find the evidence of this source's authenticity to be compelling. Diagnostic plot: www.mpifr-bonn.mpg.de/staff/reatough/public/pdmp-cand.pdf \nDiagnostic Plot", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Interstellar medium", "Active galactic nucleus", "Black hole" ] }, "answerKey": "A" }, { "id": "atel_5130", "message": "Title: Optical brightening of the Quasar PKS2209+236 detected by MASTER\nAuthors: V. Yecheistov, D. Denisenko, E. Gorbovskoy, V. Lipunov, P. Balanutsa, V. Kornilov, N. Tiurina, N. Shatskiy, V. Chazov, A. Kuznetsov (Moscow State University, SAI), K. Ivanov, S. Yazev, N. Budnev, E. Konstantinov, O. Chuvalaev, V. Poleshchuk, O. Gress, A. Frolova (Irkutsk State University), V. Krushinsky, I. Zalozhnih, A. Popov, A. Bourdanov (Ural Federal University), A. Parkhomenko, A. Tlatov, D. Dormidontov, V. Senik (Kislovodsk solar station of the Pulkovo observatory RAS), V. Yurkov, Y. Sergienko, D. Varda, E. Sinyakov, A. Gabovich (Blagoveshchensk Educational University), P. Podvorotny, V. Shumkov, S. Shurpakov (MASTER team members), H. Levato, C. Saffe (ICATE), C. Mallamaci, C. Lopez and F. Podest (OAFA)\nDate: 14 Jun 2013; 12:51 UT\nProvenance: Vladimir Lipunov (lipunov2007@gmail.com)\nSubjects: Optical, Blazar, Quasar\nDescription: Referred to by ATel #: 5149\nMASTER OT J221205.95+235541.0 discovery \nMASTER-Kislovodsk auto-detection system discovered OT source at (RA, Dec) = 22h 12m 05.95s +23d 55m 41.0s (error = 0.5 arcsec) on 2013-06-13.87596 UT. The OT unfiltered magnitude is 17.3m (limit 19.0m). The OT is seen in 5 images. There is no minor planet at this place. \nWe have reference unfiltered image without OT on 2011-07-06.99191 UT with magnitude limit 21.0m. \nThere is Quasar PKS2209+236 inside our error box which variability detected before ( L. Carrasco, A. Luna, G. Escobedo, D. Y. Mayya, A. Carraminana, V. et al. ATel #4559). \nFollow up observations are required. \nThe discovery and reference images are available at: http://master.sai.msu.ru/static/OT/221205.95235541.0_1.png \nList of Optical Transients discovered by MASTER\nGlobal MASTER Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Neutron star", "Quasar", "Exoplanet" ] }, "answerKey": "C" }, { "id": "atel_5190", "message": "Title: Swift observations of a new outburst of the SFXT IGR J08408-4503\nAuthors: P. Romano (INAF-IASF Palermo), A. Y. Lien (NASA/GSFC/ORAU), P. A. Evans (LU), S. D. Barthelmy (GSFC), D. N. Burrows (PSU), P. Esposito (INAF-IASFMI), N. Gehrels (GSFC), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), D. Malesani (DARK/NBI), V. Mangano (PSU), S. Vercellone (INAF-IASF Palermo) \nDate: 3 Jul 2013; 14:13 UT\nProvenance: Pat Romano (romano@ifc.inaf.it)\nSubjects: X-ray, Gamma Ray, Binary, Transient\nDescription: The Swift Burst Alert Telescope (BAT) triggered on a new outburst from the Supergiant Fast X-ray Transient (SFXT) IGR J08408-4503 on 2013 July 2 at 08:10:45 UT (image trigger=00559642). Swift immediately slewed to the BAT position, and the narrow field instruments started observing about 130 s after the trigger. \nUsing the BAT data set from T-239 to T+963 s from the recent telemetry downlink, we report that the time-averaged spectrum from T-79.0 to T+497.0 s is best fit by a power law with an exponential cutoff. This fit gives a photon index 0.8+/-1.2, and Epeak of 23 keV. The total fluence in the 15-150 keV band is (2.1+/-0.3)E-06 erg/cm2. All the quoted errors are at the 90% confidence level. \nThe XRT began observing the field 135 seconds after the BAT trigger. The light curve shows several flares and reached 20 counts/s. The mean XRT/WT spectrum (T+135 to 554 s, 418 s exposure) can be fitted with an absorbed power-law with a photon index of 0.5+/-0.1 and an absorbing column density of NH=(4 +/- 1)E21 cm-2. The mean observed (unabsorbed) flux is about 1.4E-9 (1.5E-9) erg/cm2/s (0.3-10 keV). The mean XRT/PC spectrum (T+ 556 to 1965 s, 1.4 ks exposure) can be fitted with an absorbed power-law with a photon index of 0.6+/-0.2 and an absorbing column density of NH=(5 +/- 2)E21 cm-2. The mean observed (unabsorbed) flux is about 2.6E-10 (2.8E-10) erg/cm2/s (0.3-10 keV). \nPreviously, Swift observed flares from this source on 2006 October 4 (Gotz et al. 2007,ApJ,655,L101; Romano et al. 2009,MNRAS,392,45), 2008 July 05 (Romano et al. 2009,MNRAS,392,45), 2008 September 21 (Sidoli et al. 2009,MNRAS,397,1528), 2009 August 28 (Barthelmy et al. 2009, ATel #2178), 2010 March 28 (Romano et al. 2010, ATel #2520), and 2011 August 25 (Mangano et al. 2011, ATel #3586). The historical light curve from the BAT hard X-ray transient monitor (Krimm et al, 2006, ATel #904; 15-50 keV) can be found at http://swift.gsfc.nasa.gov/docs/swift/results/transients/weak/IGRJ08408-4503 . \nScaled Map Transient Analysis for IGR J08408-4503", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Circumstellar disk", "Active galactic nucleus", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_5310", "message": "Title: Addendum to ATel 5304\nAuthors: U. Munari (INAF Padova-Asiago), S. Dallaporta, G. Cherini, P. Valisa, G. Cetrulo, A. Milani, L. Ghirotto (ANS Collaboration)\nDate: 22 Aug 2013; 17:24 UT\nProvenance: U. Munari (ulisse.munari@oapd.inaf.it)\nSubjects: Optical, Nova\nDescription: The following information was missing from ATel #5304, and it is provided here following a request from ATel Editors.\nWe are collecting photometry of Nova Del 2013 every night since its discovery was posted to TOCP web page (http://www.cbat.eps.harvard.edu/unconf/tocp.xml). Given the large brightness of the nova, we are forced to use as local standards the bright stars HR 7811, HD 194841, HD 194113, HD 194631 and HD 194072 with their Cousins Ic magnitude taken from the Hipparcos Input Catalog and the B,V magnitudes from Tycho-2 catalog transformed to Johnson following Bessell (2000, PASP 112, 961). These five standard stars span a wide range in color to assure a good determinations of the coefficients of the instantaneous color equations transforming to the standard system. These preliminary B,V,Ic magnitudes are being checked against Landolt (2009) equatorial standards, and we are also deriving the magnitude of the standard stars in the Johnson U, Cousins Rc and Stromgren b,y bands in which we are also monitoring the nova. The high brightness of the nova and the large distance of the standard stars from it, force us to use short focal length refractors with their apertures reduced to a few cm in diameter, so that the exposure times are long enough with respect to CCD camera shutter opening/closing times. In addition, photoelectric photometry in the Johnson B,V bands is obtained with an Optec SSP-5 photometer attached to a 35cm telescope, using the same standards as for the CCD photometry.\nWe are also obtaining every night spectroscopy of the nova with four different telescopes located in northern Italy (cf ATel #5297). The Varese 0.61m telescopes, equipped with the Multi Mode Spectrograph, is used to record both Echelle (res.pow. 18000, range 3900-8600 Ang, 30 orders) and low resolution spectra (dispersion 2.1 Ang/pix, range 3900-8600 Ang). The Asiago 1.22m telescope + B&C spectrograph obtains low resolution spectra (dispersion 2.3 Ang/pix, range 3200-7700 Ang) while the Asiago 1.82m telescope + Echelle spectrograph secures high resolution ones (res.pow. 22000, range 3400-7300 Ang, 32 orders). Finally, low resolution spectra are also obtained in the far red with the Polse di Cougnes 0.70m telescope (1.1 Ang/pix, range 6500-9700 Ang, Schott 2mm OG5 2nd order cutting filter). At all sites the spectra are absolutely fluxed against the spectrophotometric standard stars HR 8004 (A1V) and HR 7596 (A0III), which have an energy distribution similar to that of the nova and are observed every night along with it.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Active galactic nucleus", "Pulsar", "Nova" ] }, "answerKey": "D" }, { "id": "atel_5375", "message": "Title: Limits on non-thermal radio emission from Nova Cephei 2013\nAuthors: Prasun Dutta (NCRA-TIFR), Nimisha G. Kantharia (NCRA-TIFR), Nirupam Roy (MPIfR), G. C. Anupama (IIA), N. M. Ashok (PRL), Dipankar P. K. Banerjee (PRL)\nDate: 8 Sep 2013; 11:56 UT\nProvenance: Nirupam Roy (roy.nirupam@gmail.com)\nSubjects: Radio, Nova\nDescription: Referred to by ATel #: 5389\nNova Cephei 2013, discovered on 2013 Feb. 02 (CBET #3397), was observed at low radio frequency with the Giant Metrewave Radio Telescope (GMRT) on 2013 June 1 (at 1.3 GHz) and Aug 23 (610 MHz) using director's discretionary time. No radio emission was detected in either epochs down to the rms noise level of 120 microJy at 1.3 GHz and 70 microJy at 610 MHz. Observations at other wavelengths earlier reported no detectable X-ray emission (ATel #4950), but clear indication of ongoing dust formation (ATel #4893, #5026 and #5269). VLA observations at higher radio frequencies reported detection at 7.4 and 36.5 GHz (ATel #4950). Using this, and assuming an early-time S_\\nu ~ t^2 \\nu^2 behaviour, the GMRT observations rule out, at 3sigma level, any non-thermal emission brighter than 330 and 190 microJy, respectively, for these two epochs of observation. \nWe thank the staff of the GMRT who made these observations possible. The GMRT is operated by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research (NCRA-TIFR).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Nova", "Binary system", "Minor body" ] }, "answerKey": "B" }, { "id": "atel_5450", "message": "Title: Discovery of a Probable Nova in M31\nAuthors: K. Hornoch (Astronomical Institute, Ondrejov, Czech Republic), J. Vrastil (Astronomical Institute, Charles U., Prague, Czech Republic)\nDate: 7 Oct 2013; 15:07 UT\nProvenance: Allen W. Shafter (aws@nova.sdsu.edu)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 5503\nWe report the discovery of a probable nova in M31 on a co-added 1530-s R-band CCD frame taken on 2013 Oct. 6.740 UT with the 0.65-m telescope at Ondrejov. \nThe object designated PNV J00424654+4117006 is located at R.A. = 0h42m46s.54, Decl. = +41o17'00\".6 (equinox 2000.0), which is 25.0\" east and 52.1\" north of the center of M31 (see link to discovery image below). \nThe following R-band magnitudes were obtained using the 0.65-m telescope at Ondrejov: \n2013 Oct. 3.739 UT, [19.6; 4.739, [19.4; 6.740, 18.3 ± 0.25; 6.753, 18.3 ± 0.3; 6.772, 18.2 ± 0.25. \nDiscovery image", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Globular cluster", "Accreting object", "Nova", "Black hole" ] }, "answerKey": "C" }, { "id": "atel_5550", "message": "Title: NIR brightening of BL LAC\nAuthors: L. Carrasco, E. Recillas, A. Porras, V. Chavushyan, A. Carraminana (INAOE, Mexico)\nDate: 6 Nov 2013; 05:22 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Infra-Red, Gamma Ray, AGN, Blazar\nDescription: Referred to by ATel #: 5558\nWe report on the recent observation that revealed a NIR brightening of the prototype blazar, BL LAC itself. On October 30th,2013 (JD 2456595.735567), its flux in the H band corresponded to the magnitude H = 10.124 +/- 0.03. It is brightest since the time we started monitoring his object in the NIR (JD2454358.657246). Our observations were carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We strongly encourage further multi-wavelength coverage.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Active galactic nucleus", "Black hole", "Pulsar" ] }, "answerKey": "C" }, { "id": "atel_5640", "message": "Title: M31N 2013-11b is Likely a Red LPV\nAuthors: K. Hornoch (Astronomical Institute, Ondrejov, Czech Republic)\nDate: 8 Dec 2013; 21:35 UT\nProvenance: Allen W. Shafter (aws@nova.sdsu.edu)\nSubjects: Optical, Nova, Transient, Variables\nDescription: Referred to by ATel #: 5744, 9470, 9554\nInformation about the discovery by E. Ovcharov et al. of a faint (R = 20.3 ± 0.2) probable nova in M31 on 2013 Nov. 7.780 UT was published in ATel #5569. \nI observed the object on 2013 Nov. 13.770 - 13.791 UT using the 0.65-m telescope at Ondrejov and Dec. 1.025 - 1.027 UT using the Danish 1.54-m telescope at La Silla. The following magnitudes were obtained: \n2013 Nov. 13.770 UT, I = 18.9 ± 0.15; 13.791, R = 20.4 ± 0.25; Dec. 1.025, I = 18.52 ± 0.06; 1.027, R = 19.49 ± 0.08. \nThe significantly red color of the object is not typical for a classical nova unless it is highly reddened, which is not expected in the line of sight to the object. Thus, a more likely classification of the object is that it is a red LPV which is supported also by its very slow brightening. \nBased (in part) on data collected with the Danish 1.54-m telescope at the ESO La Silla Observatory.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Pulsar", "Near-Earth object", "Black hole", "Nova" ] }, "answerKey": "D" }, { "id": "atel_5750", "message": "Title: MAXI/GSC discovery of a new soft X-ray transient MAXI J1421-613\nAuthors: Y. Morooka, Y. Ogawa (Miyazaki U.), H. Negoro (Nihon U.), M. Serino (RIKEN), S. Ueno, H. Tomida, S. Nakahira, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA), T. Mihara, M. Sugizaki, M. Morii, J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN), N. Kawai, R. Usui, K. Ishikawa, T. Yoshii, Y. Tachibana (Tokyo Tech), A. Yoshida, T. Sakamoto, Y. Nakano, Y. Kawakubo, H. Ohtsuki (AGU), H. Tsunemi, M. Sasaki, D. Uchida (Osaka U.), M. Nakajima, H. Sakakibara, K. Fukushima, T. Onodera, K. Suzuki (Nihon U.), Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.), Y. Tsuboi, M. Higa, A. Kawagoe (Chuo U.), M. Yamauchi, K. Yoshidome, H. Yamada (Miyazaki U.), K. Yamaoka (Nagoya U.) report on behalf of the MAXI team\nDate: 9 Jan 2014; 23:53 UT\nProvenance: Hitoshi Negoro (negoro@phys.cst.nihon-u.ac.jp)\nSubjects: X-ray, Binary, Black Hole, Cataclysmic Variable, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 5751, 5759, 5765, 5780, 5802, 5894\nThe MAXI/GSC nova alert system triggered an uncatalogued X-ray transient source at 01:13:07 UT on 2014-01-09. Assuming that the source flux was constant over the transit, we obtain the source position at \n \n(R.A., Dec) = (215.413 deg, -61.345 deg) = (14 21 39, -61 20 41) (J2000) \n \nwith a statistical 90% C.L. elliptical error region with long and short radii of 0.55 deg and 0.39 deg respectively. The roll angle of the long axis from the north direction is 118.0 deg counterclockwise. There is an additional systematic uncertainty of 0.2 deg (90% containment radius). \n \nMAXI scanned the region only a few times a day in recent days, but count excesses in the 2-4 keV and 4-10 keV bands had been recognized since the beginning of Jan. 7th. The 4-10 keV X-ray flux averaged over 4 scan transits from 23:40 on Jan. 8th to 04:18 on Jan. 9th was 40+-11 mCrab. \n \nWe tentatively name the source MAXI J1421-613. Followup observations are strongly encouraged to reveal the nature of the source.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Black hole, Neutron star, Variable star, Pulsar", "Accreting object, Black hole, Galaxy, Variable star, Pulsar", "Accreting object, Black hole, Neutron star, Variable star, Pulsar", "Accreting object, Black hole, Accreting object, Variable star, Pulsar" ] }, "answerKey": "C" }, { "id": "atel_5825", "message": "Title: CSP spectroscopic classification of LSQ14jp\nAuthors: F. Taddia (OKC/Stockholm), M. Stritzinger (Aarhus), N. Morrell, E. Y. Hsiao (LCO), E. Hadjiyska, E. S. Walker, D. Rabinowitz, C. Baltay, N. Ellman, R. McKinnon (Yale), U. Feindt (U. Bonn), P. Nugent (LBNL/UCB)\nDate: 28 Jan 2014; 11:27 UT\nProvenance: Francesco Taddia (ftadd@astro.su.se)\nSubjects: Optical, Supernovae\nDescription: Carnegie Supernova Project reports the spectroscopic classification of LSQ14jp using an optical spectrum obtained with the Nordic Optical Telescope (+Alfosc). The target was supplied by the La Silla-Quest survey (Hadjiyska et al., ATel #3812). \n \n \n Name | RA | DEC | Disc. date | Spec. date | Tele+Inst | Type |z | Phase | \n LSQ14jp | 12 57 21.5 | -15 47 33.5 | 2014 01 25 | 2014 01 28 | NOT+ALFOSC | Ia |0.045 | 1 week before max |", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Nova", "Exoplanet", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_5940", "message": "Title: NIR brightening of the Quasar PKS0306+102\nAuthors: L. Carrasco, E. Recillas, A. Porras, V. Chavushyan, A. Carraminana, D. Mayya (INAOE, Mexico)\nDate: 2 Mar 2014; 18:42 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Infra-Red, Optical, Gamma Ray, Request for Observations, AGN, Blazar, Quasar\nDescription: We report on a NIR brightening of the intermediate redshift quasar PKS0306+102 (z=0.863), also known as CGRaBSJ0309+1029, associated with the gamma-ray source 2FGL0309.1+1027. Our NIR photometry for this source shows that, on February 18th,2014 (JD2456706.6940), the object brightness corresponded to H = 15.72 +/- 0.04. This value is about 0.7 magnitudes brighter than our previous photometry, obtained on JD2456678.73 (H = 16.38 +/- 0.07), for this field. Hence, it has doubled its flux in a lapse of 28 days. The object is brightest since we started monitoring it on JD 24546324. Our observations are carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We strongly encourage further multiwavelength coverage.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Minor body", "Stellar evolution", "Magnetar" ] }, "answerKey": "A" }, { "id": "atel_6090", "message": "Title: Broad-band photometry of NHATS target 387733 (2003 GS)\nAuthors: M. Hicks (JPL/Caltech), J. Frederick (PCC), I. Harley (PCC)\nDate: 23 Apr 2014; 17:57 UT\nProvenance: Michael D. Hicks (Michael.Hicks@jpl.nasa.gov)\nSubjects: Optical, Asteroid, Planet (minor), Solar System Object, Near-Earth Object\nDescription: The near-Earth asteroid (2003 GS) was discovered by the LONEOS Sky Survey on April 12, 2003 (MPEC 2003-G25). The object passed within 0.0875 AU on April 12, 2014 and is scheduled to be observed at radar wavelength at Arecibo on April 18-20 (E. Howell, personal communication). 2003 GS has been flagged by NASA's Near-Earth Object Human Space Flight Accessible Targets Study (NHATS) as a potentially attractive mission target. Though close to full moon, we took advantage of the object's 2014 apparition to obtain three partial nights of time-resolved photometry (April 12-14 2014 UT) at the JPL Table Mountain Observatory 0.6-m telescope, as summarized in Table 1 and Figures 1-3 [1] [2] [3]. \n \nThe rotationally averaged colors of the asteroid (B-R=1.233+/-0.012 mag; V-R=0.466+/-0.012 mag; R-I=0.361+/-0.034 mag) were found most compatible with an S-type spectral classification, an association obtained through a comparison of our colors with the 1341 asteroid spectra in the SMASS II database (Bus & Binzel 2002) [Figure 4 and Table 2]. As shown in Figure 5 , our solar phase coverage allow the determination of absolute magnitude (H_R=18.50 mag) and solar phase parameter g=0.17, consistent with an S-Family taxonomic classification. Using our V-R color, we measured an absolute magnitude in the V band H_V=18.97+/-0.02 mag. \n \nAfter converting our observed flux to normalized flux, we performed a rotational period search using standard Fourier techniques. Figure 6 plots chi-squared 2nd and 3rd order Fourier model misfit as a function of assumed rotation period, with a clear minimum near 2.5 hr. Assuming a double-peaked lightcurve, we found a best-fit synodic period P_syn = 2.469+/-0.001 hr, as shown in Figure 7 . The rapid rotation and low lightcurve amplitude suggests a potential binary NEO system; there was no clear evidence of a two-period system in our data. \n \n \nCopyright 2014. All rights reserved. The research described in this telegram was carried out at the Jet Propulsion Laboratory, under a contract with the National Aeronautics and Space Administration. The student participation was supported by the National Science Foundation under REU grant AST-1156756 to Los Angeles City College. \n \n\n \n \n Table 1: Observational summary. \n \n Solar Lunar . \n UT Date r delta Phase V Elong. Filters Observers \n [AU] [AU] [deg] [mag] [deg] \n Apr 12.40 1.087 0.087 15.0 14.7 41.6 BVRI Hicks \n Apr 13.31 1.086 0.088 16.7 14.8 31.1 R Harley, Frederick, Hicks \n Apr 14.26 1.086 0.088 18.7 14.9 23.6 R Hicks \n \n \n \n Table 2: Best-fit SMASS II spectral analogs. \n \n TAXONOMIC CLASS \n MISFIT OBJECT NAME (THOLEN) (BUS) \n \n 1.983 39 Laetitia S S \n 2.988 3198 Wallonia S \n 3.037 1351 Uzbekistania Xk \n 3.218 6704 1988 CJ K \n 3.449 56 Melete P Xk", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Neutron star", "Supernova", "Minor body" ] }, "answerKey": "D" }, { "id": "atel_6175", "message": "Title: Discovery and classification of a young Type Ia supernova in UGC 8503\nAuthors: Y. Cao, D. Perley (Caltech), M. Kasliwal (Carnegie), J. Johansson, A. Goobar (OKC), R. Quimby (IPMU) A. Horesh, I. Sagiv, Y. Ofer, E. Ofek, A. Gal-Yam (Weizmann) P. Nugent (LBL), D. Fox (PSU) on behalf of the intermediate Palomar Transient Factory collaboration\nDate: 27 May 2014; 16:39 UT\nProvenance: Yi Cao (ycao@astro.caltech.edu)\nSubjects: Optical, Supernovae\nDescription: The intermediate Palomar Transient Factory (Law et al. 2009; ATel#4807) reports discovery of a young supernova, iPTF14bdn, at RA=13:30:44.88 and Dec=+32:45:42.4 (J2000) in UGC 8503 at z=0.01558. It was discovered at r=19.1 mag on UT 2014 May 27.24. Nothing was found at the same location down to r~21.4 mag on UT 2014 May 26.28 and in the PTF/iPTF archive down to a similar depth. \nWe took a spectrum of this young supernova candidate with the Low Resolution Imaging Spectrometer (LRIS) mounted on the Keck I telescope on UT 2014 May 27.40. The spectrum shows a Si II 6150 absorption feature relatively weaker than a normal Type Ia. The minimum of the Si II absorption corresponds to a velocity of ~15,000 km/s. No sign of strong extinction was seen in the spectrum. Hence, the Si II feature in the spectrum and the absolute magnitude of -15 mag together suggest that iPTF14bdn is probably a SN1991T/SN1999aa-like event at least two weeks before maximum.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Supernova", "Neutron star", "Stellar evolution" ] }, "answerKey": "B" }, { "id": "atel_6250", "message": "Title: MAXI/GSC detection of a hard-to-soft transition of NS-LMXB GS 1826-238 \nAuthors: S. Nakahira (JAXA), T. Mihara, M. Sugizaki, M. Serino, M. Morii, J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN), N. Kawai, T. Yoshii, Y. Tachibana (Tokyo Tech), S. Ueno, H. Tomida, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA), H. Negoro, M. Nakajima, K. Fukushima, T. Onodera, K. Suzuki, M. Fujita, T. Namba, F. Honda (Nihon U.), A. Yoshida, T. Sakamoto, Y. Kawakubo, H. Ohtsuki (AGU), H. Tsunemi, D. Uchida (Osaka U.), Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.), A. Kawagoe, Y. Tsuboi (Chuo U.), M. Yamauchi, Y. Morooka (Miyazaki U.), K. Yamaoka (Nagoya U.), report on behalf of the MAXI team\nDate: 20 Jun 2014; 04:50 UT\nProvenance: Satoshi NAKAHIRA (nakahira@crab.riken.jp)\nSubjects: X-ray, Binary, Neutron Star\nDescription: Referred to by ATel #: 10117\nWe report on a hard-to-soft spectral transition of an X-ray burster GS 1826-238 detected with MAXI/GSC. \nThis source had been consistently observed in the hard state for more than 25 years since the discovery in 1988 (Tanaka 1989, Barret et al. 1995, Ubertini et al. 1999, Cocchi et al. 2010), including the recent five years monitored by MAXI. \nOn 2014 June 8, the MAXI/GSC hardness ratio (7-20keV / 2-7 keV) suddenly decreased from ~ 0.4 to 0.1. According to the hardness change, the 2-10 keV X-ray flux increased from 50 mCrab (before May 2014) to 140 mCrab (15 June 2014), while the 15-50 keV flux monitored by Swift BAT decreased. All these results indicate that the source entered into the soft state. \n \nMAXI light curves are in \nhttp://maxi.riken.jp/top/index.php?cid=1&jname=J1829-237 \nMAXI and BAT light curves and MAXI spectra are in \nhttp://maxi.riken.jp/news/en/?p=1112 \nMulti-wavelength observations are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Binary system", "Star and stellar system", "Quasar" ] }, "answerKey": "A" }, { "id": "atel_6350", "message": "Title: PNV J01340288+3035111 is Likely a Nova in M33\nAuthors: K. Hornoch (Astronomical Institute, Ondrejov, Czech Republic), M. Rabus (Instituto de Astrofisica, Pontificia Universidad Catolica de Chile, Chile, and MPI, Heidelberg, Germany), M. Hundertmark and U. G. Jorgensen (Niels Bohr Institute, University of Copenhagen, Denmark), M. Dominik (University of St Andrews, UK), J. Vrastil and H. Kucakova (Astronomical Institute, Charles U., Prague, Czech Republic)\nDate: 28 Jul 2014; 21:18 UT\nProvenance: Allen W. Shafter (aws@nova.sdsu.edu)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 6356\nIn order to search for a known counterpart of the PNV J01340288+3035111 (see ATel #6331), we obtained additional images of M33 at higher spatial resolution using the Danish 1.54-m telescope at La Silla and the 0.65-m telescope at Ondrejov. These data also allowed us to determine color index and brightness evolution of the object. Our search for a counterpart was facilitated by the use of the Survey of Local Group Galaxies Currently Forming Stars: I. UBVRI Photometry of Stars in M31 and M33 by Massey et al. (2006, AJ, 131, 2478), which provided deep comparison images. \nThe following magnitudes were obtained using the 1.54-m (D) and the 0.65-m (O) telescopes: \n2014 Jul. 21.047 UT, R = 18.9 ± 0.15 (O); 23.060, R = 19.1 ± 0.15 (O); 23.071, I = 18.8 ± 0.2 (O); 24.074, V = 18.8 ± 0.15 (O); 24.085, R = 18.6 ± 0.15 (O); 24.416, R = 18.82 ± 0.10 (D); 24.427, I = 18.58 ± 0.10 (D); 25.021, R = 19.5 ± 0.2 (O); 26.027, R = 19.7 ± 0.25 (O); 27.008, R = 20.1 ± 0.3 (O). \nR-band and I-band images obtained around July 24.42 UT with the Danish 1.54-m telescope under ~1.3\" seeing show that the PNV J01340288+3035111 is located ~ 0.5\" away from the closest object visible on R-band and I-band Massey's images (i.e., no counterpart is visible there down to ~ 23rd magnitude). It confirms the suspicion from ATel #6331, that the nova candidate is not connected to the 21st magnitude variable No. 236977 listed in Hartman et al. (2006, MNRAS, 371, 1405). The lack of an optical counterpart brighter than ~ 23 mag at the location of the PNV J01340288+3035111, along with the observed color indicies [(V-R) ~ 0.2; (R-I) ~ 0.3 mag] and brightness evolution, is consistent with the nova nature of the object. Taken together, these findings strongly suggest that the PNV J01340288+3035111 is a nova in M33, discovered probably a few days after outburst. \nThis work is based (in part) on data collected with the Danish 1.54-m telescope at the ESO La Silla Observatory.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Quasar", "Nova", "Circumstellar disk" ] }, "answerKey": "C" }, { "id": "atel_6475", "message": "Title: Follow-up of ASASSN-14ei show He lines in the spectra and Swift/XRT X-ray detection\nAuthors: J. L. Prieto (Universidad Diego Portales; MAS), N. Morrell (LCO), D. Grupe (Morehead State), K. Z. Stanek, C. S. Kochanek, T. W.-S. Holoien, A. B. Davis, U. Basu, J. F. Beacom (Ohio State), D. Bersier (LJMU), B. J. Shappee (Carnegie Observatories), J. Brimacombe (Coral Towers Observatory), D. Szczygiel, G. Pojmanski (Warsaw University Observatory)\nDate: 15 Sep 2014; 21:50 UT\nProvenance: Jose L. Prieto (jose.prietok@mail.udp.cl)\nSubjects: Optical, Ultra-Violet, X-ray, Cataclysmic Variable, Transient\nDescription: We report follow-up optical spectra and Swift X-ray/UV/optical imaging of the unusual optical transient ASASSN-14ei (ATel #6340). We obtained medium/low resolution optical spectra on UT 2014 Jul 28.4 and Aug 01.4 with the B&C spectrograph mounted on the du Pont 2.5m telescope at LCO. The spectra show a blue continuum with relatively narrow He I and He II lines in emission at redshift z=0 (see this figure). This is consistent with a He dwarf nova (AM CVn system in outburst) classification for the object, which was proposed from the periodic variations observed in the optical light curve of ~43 min and other light curve characteristics (see vsnet-alerts 17575 and CBA news). The optical light curve of ASASSN-14ei from AAVSO and ASAS-SN shows 6 short brightening episodes since 2014 July 5 (UT July 10.4, July 24.4, August 03.4, August 14.2, August 28.2, and September 10.5) with V = 11.9-13.2 mag at peak brightness and V ~ 15-17 mag between outbursts (see the optical light curve here, with the dashed vertical lines showing the times when spectra were obtained). The times between consecutive brightening peaks in the optical light curve observed so far is between 10 and 14 days. \nWe also obtained TOO observations of ASASSN-14ei with Swift UVOT and XRT on four epochs between UT July 24.9 and UT July 26.5, within 2 days of the peak of the second recorded outburst. The source was bright and blue in UVOT photometry, with v=12.35 +/- 0.04, b=12.15 +/- 0.03, uvw1=10.27 +/- 0.04, uvm2=10.08 +/- 0.04, uvw2=10.04 +/- 0.04 on UT July 26.1. It was also strongly detected in X-rays with the XRT in 1ks exposures. The XRT data is well-modeled with a power-law with photon index of 1.7-2.0 and flux of 3.7-4.2 x 10-12 erg/cm2/s (0.3-10 keV). \nWe thank the Swift team for making these observations possible. For more information about the ASAS-SN project see the ASAS-SN Homepage and also ASAS-SN Transients.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Exoplanet", "Near-Earth object", "Variable star", "Galaxy" ] }, "answerKey": "C" }, { "id": "atel_6575", "message": "Title: Fermi-LAT detection of a GeV gamma-ray flare from blazar PKS B1908-201\nAuthors: Stefano Ciprini (ASI Science Data Center and INAF Observatory of Rome, Italy), on behalf of the Fermi Large Area Telescope Collaboration.\nDate: 13 Oct 2014; 20:19 UT\nProvenance: Stefano Ciprini (stefano.ciprini@asdc.asi.it)\nSubjects: Gamma Ray, >GeV, Request for Observations, AGN, Blazar, Quasar\nDescription: The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed increasing gamma-ray flux from a source positionally consistent with the flat spectrum radio quasar PKS B1908-201 (also known as PKS 1908-201, TXS 1908-201, OV -213), with radio coordinates R.A.: 287.79022 deg, Dec: -20.11531 deg (J2000.0, Johnston et al. 1995, AJ, 110, 880). This FSRQ has a redshift of 1.119 (Halpern, Eracleous & Mattox 2003, AJ, 125, 572). \nPreliminary analysis indicates that PKS B1908-201 on October 12, 2014, was in a high state with a daily averaged gamma-ray flux (E>100MeV) of (1.3+/-0.3)X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only), about 10 times greater than the average flux reported in the second Fermi-LAT catalog (2FGL J1911.1-2005 , Nolan et al. 2012, ApJS, 199, 31). PKS B1908-201 is a known EGRET blazar (3EG J1911-2000) and is monitored by VLBA (MOJAVE program). \nBecause Fermi operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. The source will be inserted in the \"LAT Monitored Source\", consequently a quick look estimation of the daily gamma-ray flux observed by Fermi LAT will be publicly available (fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/). In consideration of the ongoing activity of this source, we encourage multiwavelength observations. For this source the Fermi LAT contact person is David J. Thompson (David.J.Thompson@nasa.gov). \nThe Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Globular cluster", "Nova", "Stellar evolution", "Black hole" ] }, "answerKey": "D" }, { "id": "atel_6675", "message": "Title: Liverpool Telescope Discovery of a Possible Nova in M31 \nAuthors: S. C. Williams (LJMU), M. J. Darnley (LJMU), M. F. Bode (LJMU)\nDate: 8 Nov 2014; 14:11 UT\nProvenance: Matt Darnley (M.J.Darnley@ljmu.ac.uk)\nSubjects: Optical, Nova\nDescription: Referred to by ATel #: 6689, 6704, 6759\nWe report the discovery of a possible nova in M31 in Liverpool Telescope (LT; Steele et al. 2004) IO:O data taken on 2014 November 7.98 UT. \nThis potential nova was discovered in observations taken while following the decline of the nearby M31 nova PNV J00423972+4120117 (see ATel #6563, #6616). \nWe measured the position of this new transient to be RA = 0:42:52.76 Dec. = +41:17:19.7, with an accuracy of 0.2''. The possible nova had a V-band magnitude of 19.03 ± 0.04 on November 7.98 UT and an r'-band magnitude of 19.02 ± 0.03 on November 7.99 UT. \nThe possible nova is also visible in a second epoch of LT data taken on November 8.11 UT, when it had a magnitude of V = 19.00 ± 0.05 and r' = 18.84 ± 0.03 on November 8.12 UT. The source is not visible on frames taken 2014 October 17.04 UT down to a V-band limiting magnitude of 20.4.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Magnetar", "Nova", "Active galactic nucleus" ] }, "answerKey": "C" }, { "id": "atel_6800", "message": "Title: Chandra LETG Spectroscopy of the Tidal Disruption Candidate ASASSN-14li\nAuthors: J. M. Miller (Michigan), B. Cenko (GSFC), S. Gezari (Maryland), K. Gultekin (Michigan), J. A. Irwin (Alabama), J. Kaastra (SRON), P. Maksym (Alabama), R. Mushotzky (Maryland), F. Paerels (Columbia), E. Ramirez-Ruiz (UCSC), M. Reynolds (Michigan)\nDate: 10 Dec 2014; 22:58 UT\nProvenance: Jon Miller (jonmm@umich.edu)\nSubjects: X-ray, AGN, Black Hole, Transient\nDescription: Referred to by ATel #: 6825, 6834\nWe report on a Chandra observation of the candidate tidal disruption flare ASASSN-14li (Jose et al. 2014, ATEL #6777). The high flux from this nearby event offered an excellent opportunity to search for lines that might illuminate the aftermath of the disruption. Owing to the negligible column density to this source and its intrinsically soft spectrum, we requested an 80 ks DDT observation using the LETG+HRC-S. The first 35 ks was obtained starting on Dec 8 2014, and we report on a first analysis of the summed first-order spectra from this segment. \n \nThe source appears to be detected out to 170 Angstroms (0.073 keV). There is no evidence of neutral obscuration from gas along the line of sight. Ultraviolet observations are again strongly encouraged. \n \nAbove and below the 20-40 Angstroms band, the spectrum diverges from a blackbody; it is not clear if this is astrophysical. Within the 20-40 Angstroms (0.3-0.62 keV) band, the source is well described by a fiducial blackbody, kT = 67 +/- 1 eV, giving a flux of 2.8 E-11 erg/cm/cm/s (extrapolated over the 0.3-1 keV band), corresponding to L ~ 2.8 E+43 erg/s for a host galaxy at 90 Mpc. \n \nHighly ionized charge states of C, N, and O fall within this band, but there is no clear evidence of emission or absorption features in this segment of the spectrum. The strongest feature is a putative absorption line at 31 Angstroms that could correspond to N I; however, the absence of other neutral lines in absorption, and the lack of edges associated with neutral gas along the line of sight, renders this identification unlikely. The Fe L band is similarly free of atomic features. \n \nOngoing Swift observations show a relatively steady flux over many days. If ASASSN-14li is indeed a tidal disruption event, this would indicate an extended Eddington-limited phase, and the implied luminosity would then signal a log(M/Msun) ~ 6 black hole after bolometric corrections. The cool thermal emission could plausibly represent a newly-formed accretion disk, or an optically-thick photosphere if the source is in an extreme super-Eddington state. \n \nWe thank Belinda Wilkes and the Chandra mission for quickly executing observations of a particularly special source.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova, Black hole", "Quasar, Black hole", "Accreting object, Globular cluster", "Accreting object, Black hole" ] }, "answerKey": "D" }, { "id": "atel_6930", "message": "Title: A Strong Optical Flare from QSO B2 1633+38\nAuthors: A. B. Danilet, K. Z. Stanek, C. S. Kochanek, T. W.-S. Holoien, G. Simonian, U. Basu, N. Goss, J. F. Beacom (Ohio State), B. J. Shappee (Hubble Fellow, Carnegie Obsrvatories), J. L. Prieto (Diego Portales; MAS), D. Bersier (LJMU), Subo Dong (KIAA-PKU), P. R.Wozniak (LANL), J. Brimacombe (Coral Towers Observatory), D. Szczygiel, G. Pojmanski (Warsaw University Observatory)\nDate: 15 Jan 2015; 20:16 UT\nProvenance: Krzysztof Stanek (stanek.32@osu.edu)\nSubjects: Optical, Blazar\nDescription: Referred to by ATel #: 6942, 6954, 7004\nB2 1633+38 (4C +38.41) is in a field observed by the 14-cm ASAS-SN quadruple \"Brutus\" telescope with a 2-3 day cadence, typical for our all-sky survey. The largest flare of B2 1633+38 in the ASAS-SN data was discovered on UT 2015-01-14.64 at V~14.9 mag. This figure shows the complete ASAS-SN V-band photometry for this interesting object, spanning more than 1000 days. In the last three epochs ASAS-SN measured the following V-band brightness \n \n \n UT Date V \n 2015-01-01.660 17.0 \n 2015-01-09.654 16.2 \n 2015-01-14.635 14.9 \n \nwith the last data point significantly brighter than any previous ASAS-SN measurement. \nWe thank LCOGT and its staff for their continued support of ASAS-SN. ASAS-SN is supported in part by Mt. Cuba Astronomical Foundation. For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Interstellar medium", "Star and stellar system", "Quasar" ] }, "answerKey": "D" }, { "id": "atel_7000", "message": "Title: ASAS-SN Discovery of A Probable Supernova in CGCG 064-017\nAuthors: E. Conseil (Association Francaise des Observateurs d'Etoiles Variables), J. M. Fernandez (Observatory Inmaculada del Molino), R. A. Koff (Antelope Hills Observatory), J. Brimacombe (Coral Towers Observatory), C. Gonzalez, C. Contreras (Las Campanas Observatory), Eric Y. Hsaio (Aarhus University) T. W.-S. Holoien, K. Z. Stanek, C. S. Kochanek, A. B. Danilet, G. Simonian, U. Basu, N. Goss, J. F. Beacom (Ohio State), B. J. Shappee (Hubble Fellow, Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), D. Bersier (LJMU), Subo Dong (KIAA-PKU), P. R. Wozniak (LANL), E. Falco (CfA), D. Szczygiel, G. Pojmanski (Warsaw University Observatory), S. Kiyota (Variable Star Observers League in Japan), B. Nicholls (Mt. Vernon Obs., New Zealand)\nDate: 27 Jan 2015; 20:03 UT\nProvenance: Thomas Holoien (tholoien@astronomy.ohio-state.edu)\nSubjects: Optical, Supernovae, Transient\nDescription: During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or \"Assassin\"), using data from the quadruple 14-cm \"Brutus\" telescope in Haleakala, Hawaii, we discovered a new transient source, most likely a supernova, in the galaxy CGCG 064-017: \n \n \n Object RA (J2000) DEC (J2000) Disc. UT Date Disc. V mag \n ASASSN-15cd 09:59:14.99 +12:59:18.27 2015-01-26.46 17.0 \n \nASASSN-15cd was discovered in images obtained on UT 2015-01-26.46 at V~17.0 mag. We also detect the object in images obtained on UT 2015-01-23.46 (V~17.1), UT 2015-01-21.46 (V~17.4), and UT 2015-01-19.49 (V~17.2). We do not detect (V>17.7) the object in images taken on UT 2015-01-16.48 and before. Images obtained on UT 2015-01-27.33 with the Swope 1-m telescope at Las Campanas Observatory and at earlier times on 2015-01-26 and 2015-01-27 by multiple other observers and telescopes confirm the discovery of the transient. This figure shows the archival SDSS g-band image of the host (left) and the Swope i-band confirmation image (right). The red circle has a radius of 2.0\" and is centered on the position of the transient in the Swope image. \nThe position of ASASSN-15cd is approximately 1.8\" North and 3.4\" East from the center of the starburst galaxy CGCG 064-017 (z=0.034352, d=150 Mpc, via NED), giving an absolute V-band magnitude of approximately -19.0 (m-M=35.88, A_V=0.083). Follow-up observations are encouraged. \nWe thank LCOGT and its staff for their continued support of ASAS-SN. ASAS-SN is supported in part by Mt. Cuba Astronomical Foundation. For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Magnetar", "Supernova", "Binary system" ] }, "answerKey": "C" }, { "id": "atel_7080", "message": "Title: Discovery of Very High Energy Gamma-Ray Emission from the FSRQ S4 0954+65 with the MAGIC telescopes\nAuthors: Razmik Mirzoyan (Max-Planck-Institute for Physics) on behalf of the MAGIC collaboration\nDate: 15 Feb 2015; 19:44 UT\nProvenance: Razmik Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de)\nSubjects: Radio, Optical, Ultra-Violet, X-ray, Gamma Ray, >GeV, TeV, VHE, UHE, AGN, Black Hole, Blazar, Cosmic Rays\nDescription: Referred to by ATel #: 7093\nThe MAGIC collaboration reports the discovery of very high energy (VHE; E>100 GeV) gamma-ray emission from the FSRQ S4 0954+65 (RA=+9:58:47.00, DEC=+65:33:55.00, J2000.0), located at redshift z=0.368. The object was observed with the MAGIC telescopes for ~2 hours during the night 2015 February 13/14 (MJD 57067). A preliminary analysis of the data yields detection with a statistical significance of more than 5 standard deviations. This is the first time a significant signal at VHE gamma rays has been seen from S4 0954+65. The flux above 150GeV is estimated to be about 2e-11 cm^-2 s^-1. S4 0954+65 is entered an exceptionally high state at optical and near infrared frequencies (ATels #7057; #7055; #7046, #7001; #6996), which triggered the MAGIC observations. Optical observations performed with the KVA telescope suggests that this is the brightest state ever observed from this source since November 2006 (beginning of KVA observations). The preliminary lightcurve is available at: http://users.utu.fi/kani/1m/S4_0954+65.html. During the preparation of this ATel, we were informed by Fermi-LAT collaboration that the gamma-ray flux above 100 MeV from S4 0954+65 also increased substantially during the last few days. MAGIC observations on S4 0954+65 will continue during the following nights, and multiwavelength observations are encouraged. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and E. Lindfors (elilin@utu.fi). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Active galactic nucleus", "Repeater", "Neutron star" ] }, "answerKey": "B" }, { "id": "atel_7150", "message": "Title: M31N 2015-01a - A Luminous Red Nova\nAuthors: A. Kurtenkov (University of Sofia, Bulgaria), T. Tomov (Uniwersytet Mikolaja Kopernika, Torun, Poland), S. Fabrika, E. A. Barsukova, A. F. Valeev (Special Astrophysical Observatory), P. Pessev (GRANTECAN, IAC), K. Vida, L. Molnar, K. Sarneczky (Konkoly Observatory, Hungary), V. P. Goranskij (SAI, Moscow University), K. Hornoch (Astronomical Institute, Ondrejov), M. Henze (ESA/ESAC, Spain), A. W. Shafter (SDSU), E. Ovcharov, P. Nedialkov (University of Sofia, Bulgaria), A. Kostov (IA BAS, Bulgaria), S. Valenti (LCOGT), M. Stritzinger (Aarhus University)\nDate: 27 Feb 2015; 10:31 UT\nProvenance: Toma Tomov (tomtom@astri.uni.torun.pl)\nSubjects: Optical, Nova, Variables\nDescription: Referred to by ATel #: 7173, 7236, 7272, 7555, 7572, 7624, 8059, 8220\nPreliminary results of the ongoing optical monitoring of M31N 2015-01a = MASTER J004207.99+405501.1 (ATel #6911, #6924, #6941, #6951, #6952, #6985) are reported. Throughout February the colors of the object have been consistently shifting to the red. In just one month B-R has changed from 0.8 to 2.9 mag. The following magnitudes are reported: \ndate,UT filter mag err telescope\n2015-01-24.11 B 16.00 0.04 McDonald 1 m, Fort Davis, Texas\n2015-01-24.12 R 15.24 0.02 McDonald 1 m, Fort Davis, Texas\n2015-02-07.74 B 17.86 0.05 Konkoly 60/90 cm Schmidt, Hungary\n2015-02-07.74 R 15.74 0.03 Konkoly 60/90 cm Schmidt, Hungary\n2015-02-18.7 B 18.48 0.12 Konkoly 60/90 cm Schmidt, Hungary\n2015-02-18.7 V 16.87 0.04 Konkoly 60/90 cm Schmidt, Hungary\n2015-02-18.7 R 15.90 0.03 Konkoly 60/90 cm Schmidt, Hungary\n2015-02-18.7 I 15.22 0.03 Konkoly 60/90 cm Schmidt, Hungary\n2015-02-21.72 B 18.77 0.09 6 m BTA, Russia\n2015-02-21.72 V 16.84 0.03 6 m BTA, Russia\n2015-02-21.72 R 15.84 0.03 6 m BTA, Russia\nAdditional spectroscopic observations were performed on Feb 21.79 and Feb 22.71 UT with the Russian 6m BTA telescope, equipped with the SCORPIO spectrograph. The spectral ranges were 3720 - 5530 Å and 5750 - 7500 Å with a resolution of about 5 Å. The spectrum shows a strong continuum with multiple deep absorption lines. The only emission observed is the Ca II doublet 3933 and 3968 Å. \nSpectra with the 10.4m Gran Telescopio Canarias and the OSIRIS instrument were obtained on Feb 24. The spectral range of 5000-10000 Å was covered by three individual setups utilizing the R2500V, R and I grisms. The spectrum is dominated by absorption lines with weaker molecular bands (mainly TiO). The only emission seen in the OSIRIS spectra is weak Hα with a central absorption component. \nThe object displayed an unusual absorption-line F5I type spectrum in January 2015 (ATel #6985). During the February 2015 spectroscopic observations the object shows spectral features typical for a K supergiant. Furthermore, distinct similarities are found to the V838 Mon spectra taken in the second part of March - beginning of April 2002. Based on the extreme luminosity at maximum (L>3x10^5 Lsun), the initial slow decline, observed shift of colors, and spectral information we conclude that the object is a Luminous Red Nova (LRN). \nThis red nova may be entering a stage of rapid and deep fading. Taking into account the limited visibility of M31, we strongly encourage follow-up observations be made as soon as possible.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Variable star", "Exoplanet", "Binary system" ] }, "answerKey": "B" }, { "id": "atel_7275", "message": "Title: INTEGRAL detects a new outburst from the millisecond X-ray pulsar IGR J17511-3057\nAuthors: E. Bozzo (ISDC, Switzerland), E. Kuulkers (ESA/ESAC, Spain), A. Bazzano (INAF/IAPS, Italy), V. Beckmann (APC, France), T. Bird (Southampton, UK), A. Bodaghee (GCSU, USA), J. Chenevez (DTU Space, Denmark), M. Del Santo (INAF/IASF-Palermo, Italy) , A. Domingo (CAB/INTA-CSIC, Spain), P. Jonker (SRON, The Netherlands), P. Kretschmar (ESA/ESAC, Spain), C. Markwardt (GSFC, USA), A. Paizis (INAF/IASF-Milano, Italy), K. Pottschmidt (UMBC/NASA GSFC, USA), C. Sanchez-Fernandez (ESA/ESAC, Spain), R. Wijnands (UvA, The Netherlands), C. Ferrigno, M. Tuerler (ISDC, Switzerland)\nDate: 23 Mar 2015; 12:13 UT\nProvenance: E. Bozzo (enrico.bozzo@unige.ch)\nSubjects: X-ray, Binary, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 7288\nDuring the observations performed in the direction of the Galactic Bulge on 2015 March 23 from 02:49 to 07:26 (UTC), the instruments on-board INTEGRAL detected a new outburst from the millisecond X-ray pulsar IGR J17511-3057 (ATel #2196, #2197; Papitto et al., 2010, MNRAS, 407, 2575).\nThe source was included in both the IBIS and JEM-X field of views. IGR J17511-3057 is detected by IBIS/ISGRI at a flux of 18+/-2 mCrab in the 20-40 keV energy band and 24+/-2 mCrab in the 40-80 keV energy band. The fluxes estimated from the JEM-X data were 18+/-3 mCrab in the 3-10 keV energy band and 24+/-5 mCrab in the 10-20 keV energy band. All uncertainties on the fluxes are quoted at 1 sigma c.l. The IBIS/ISGRI spectrum (effective exposure time 9.1 ks) could be reasonably well described by using a power-law model with photon index 2.3+/-0.4. The 20-100 keV X-ray flux estimated from the spectral fit is 4.5E-10 ergs/cm^2/s.\nFurther INTEGRAL observations in the direction of the source are already planned for the next days. The INTEGRAL monitoring of the Galactic bulge will also continue in the coming weeks, and the observational results from near real time data will be made available HERE.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Pulsar", "Star and stellar system", "Magnetar", "Accreting object" ] }, "answerKey": "A" }, { "id": "atel_7350", "message": "Title: ASASSN-15fd = Nova LMC 2015\nAuthors: Frederick Walter (Stony Brook University)\nDate: 7 Apr 2015; 00:33 UT\nProvenance: Fred Walter (frederick.walter@stonybrook.edu)\nSubjects: Optical, Nova\nDescription: Novae in the LMC are astrophysically-useful because they form a subset of galactic novae at a common distance and low extinction. K.Z. Stanek et al (ATel #7313) suggested, based on its light curve and spatial location, that ASASSN-15fd might be a nova in the LMC. They were correct. \nWe obtained an R=28,000 spectrum using the SMARTS Chiron Spectrograph on the SMARTS/CTIO 1.5m on UT 2015 April 3.0. The Balmer lines and a number of Fe II lines were in emission at that time. The radial velocities of the emission lines, excepting H-alpha, were consistent with the +278 km/s radial velocity of the LMC. The spectrum is consistent with a classical Fe II nova near maximum light. A phenomenological description of the spectra follow. \nH-alpha has a FWHM about 850 km/s; strong P Cyg absorption superposed on the blue emission wing has a mean velocity of -750 km/s in the rest frame of the LMC. H-beta is asymmetric, with a steeper blue side, but showed no discrete absorption components. \nNo emission is seen at He I, but broad absorption lines are seen blueward of the 588 and 668 nm He I lines. No such absorption is seen to the blue of the 707 nm line. \nThe Fe II lines have a sharp (70 km/s FWHM) absorption component blueshifted by 750 km/s (rest velocities). The strong multiplet 42 lines also exhibit a broad blueshifted absorption feature extending to about -1650 km/s. About ten Fe II lines between 450 and 470 nm are seen only in this narrow absorption component, and lack evidence of any emission. The Na D lines show similar sharp absorption features superposed on a broad emission pedestal. O I 774 nm is in emission, and shows an absorption trough extending outwards to about 1150 km/s. \nContinuing observations of novae at Stony Brook are made possible by generous support from the Provost of Stony Brook University, Dennis Assanis.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system", "Black hole", "Nova", "Globular cluster" ] }, "answerKey": "C" }, { "id": "atel_7475", "message": "Title: MASTER-SAAO: last images and coordinates of PROGRESS M27M\nAuthors: E. Gorbovskoy, V. Lipunov (Lomonosov MSU), D. Buckley (SAAO), V. Chazov, V. Kornilov, N. Tiurina, A. Kuznetsov, P. Balanutsa (Lomonosov Moscow State University, SAI), N. Budnev, O. Gress, K. Ivanov, S. Yazev, V. Poleschuk (Irkutsk State University), A. Tlatov, V. Senik, D. Dormidontov (Kislovodsk Solar Station), Yu. Sergienko, V. Yurkov, A. Gabovich (Blagoveschensk State Educational University)\nDate: 5 May 2015; 21:02 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Near-Earth Object\nDescription: MASTER-SAAO auto-detection system detected Russian Space Ship Progress M27M on 2015-05-05 17:05:52.524 UT. \nThe position of MASTER-SAAO (K95 observatory) is the following: \nLONG 20.810682 \nLAT -32.379369 \nAltitude 1760m \nPROGRESS M27M astrometrical positions are the following \n \n \n Date,Time Ra Dec mag \n \n 2015-05-05.7124134722222222 84.8057334895609 37.4282150664347 9.4 \n \n 2015-05-05.7124250462962963 84.9080081171341 37.3756685252052 7.5 \n \n 2015-05-05.7133435763888889 95.8331960143204 31.3990586458172 12.3 \n \nPhotometry shows fast rotation. \nThe part of the detection image (5-s exposition) is available at http://www.pereplet.ru/lipunov/images/MASTER_SAAO_ProgresM27M.jpg\nThe video is available at http://www.pereplet.ru/lipunov/images/PROGRESS_MASTER.gif\nGlobal MASTER Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Near-Earth object", "Black hole", "Exoplanet" ] }, "answerKey": "B" }, { "id": "atel_7600", "message": "Title: FLOYDS Classification of ASASSN-15ki as a Galactic Source\nAuthors: G. Hosseinzadeh, S. Valenti, D. A. Howell, I. Arcavi, C. McCully (LCOGT/UCSB)\nDate: 7 Jun 2015; 00:47 UT\nProvenance: Iair Arcavi (iarcavi@lcogt.net)\nSubjects: Optical, Cataclysmic Variable, Star, Variables\nDescription: We obtained a spectrum of ASASSN-15ki (ATel #7583) on 2015 June 5.3 UT with the robotic FLOYDS instrument mounted on the Faulkes Telescope North. The spectrum is that of a hot blackbody with hydrogen absorption lines at redshift z=0. Apart from the galaxy, there is only one object visible, both in the spectrum and the acquisition images. We therefore conclude that this transient is a brightening of the source identified in the archival DSS image in the ASAS-SN ATel.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Circumstellar disk", "Black hole", "Galaxy" ] }, "answerKey": "D" }, { "id": "atel_7675", "message": "Title: ASASSN-15lo is a Post-Maximum Normal Type Ia Supernova\nAuthors: D. C. Leonard (San Diego State University), P. Sheehan, D. McCarthy (University of Arizona), K. Follette (Stanford University), J. Moustakas (Siena College), D. Cantillo, A. Cazares-Kelly, S. Cazares-Kelly, Y. Cendes, N. Damm, A. Donati, E. Douglas, L. Ferrell, H. Fosbiner-Elkins, C. Fox, M. Greenberg, K. Hart, H. Hensley, A. Holt, E. Hooper, C. Juran, J. Keane, K. Key, L. Korus, T. Lee, K. Leidig, E. Merchak, K. Nessmann, S. Pendyala, S. Pirkl, J. Reeder, A. Roos, S. Rounseville, E. Ruddy, A. Schlingman, W. Schlingman, W. Schlingman, E. Schwartzman, V. Shanmugam, E. Silver, A. Stein, N. Stock, B. Svoboda, B. Thomas, N. Thomas, K. Thompson-Taylor, H. Walton (2015 Advanced Teen Astronomy Camp)\nDate: 20 Jun 2015; 17:28 UT\nProvenance: D. C. Leonard (leonard@astro.caltech.edu)\nSubjects: Optical, Supernovae\nDescription: We report spectroscopic classification of ASASSN-15lo (ATel #7673) through inspection of a low-dispersion optical spectrum (range 370-680 nm), obtained with the 2.3-m Bok telescope (+ Boller & Chivens spectrograph) at Kitt Peak on 2015 June 20 UT. \nASASSN-15lo is a Type Ia supernova; cross-correlation with a library of supernova spectra using the \"Supernova Identification\" code (SNID; Blondin and Tonry 2007, ApJ, 666, 1024) finds best matches with a number of normal type-Ia supernovae at a redshift of 0.04 roughly 11 days after maximum light. An expansion velocity of 10,078 km/s is derived from the position of the Si-II (rest 635.5 nm) minimum. We note that the spectroscopically derived (post-maximum) age of this supernova is in some tension with the discovery photometry described by ATel #7673, which would suggest a pre-maximum phase at the time of our observation; the uncertainties on the preliminary photometric measurements (not explicitly given by ATel #7673), however, may be quite large and so the increasing brightness indicated over the past several days may not be significant.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus", "Supernova", "Exoplanet", "Near-Earth object" ] }, "answerKey": "B" }, { "id": "atel_7740", "message": "Title: Significant Decrease in Intensity and Variability of Millimeter Emission from V404 Cyg\nAuthors: A. Tetarenko, G. R. Sivakoff (Alberta), M. Bremer (NOEMA), J. C. Miller-Jones (Curtin), K. Mooley, R. Fender, T. Staley, G. Anderson (Oxford) on behalf of a larger XRB collaboration\nDate: 1 Jul 2015; 14:45 UT\nProvenance: Gregory R Sivakoff (sivakoff@ualberta.ca)\nSubjects: Radio, Millimeter, Request for Observations, Black Hole, Transient\nDescription: Referred to by ATel #: 7763, 7959\nWe report follow up mm observations (ATel #7671, #7661, #7708) of the current outburst of the black hole X-ray binary, V404 Cyg, with the NOrthern Extended Millimeter Array (NOEMA; formerly the Plateau de Bure Interferometer). While V404 Cyg has shown strong variable multiwavelength emission (GCN #17929, #17931, #17929, #17931, #17933, #17938, #17940, #17944, #17945, #17946, #17948, #17949, #17956; ATel #7646, #7647, #7650, #7655, #7658, #7659, #7661, #7662, #7665, #7666, #7667, #7669, #7674, #7677, #7678, #7681, #7686, #7688, #7693, #7694, #7695, #7696, #7699, #7701, #7702, #7703, #7706, #7709, #7710, #7714, #7715, #7717, #7718, #7720, #7721, #7722, #7725, #7726, #7727, #7728), recently, dramatic decreases in flux at radio (ATel #7733), optical (ATel #7729, #7737), UV (ATel #7734), and X-ray (ATel #7731) frequencies have been reported. \nOur NOEMA observations occurred on 2015 June 26/27, June 27/28, and June 29/30 (Epochs 1-3). Data were taken between June 26 22:24 - June 27 02:42 UTC (MJD=57199.9333-57200.1125), June 27 23:17 - June 28 03:05 UTC (MJD=57200.9701-57201.1285), and June 29 22:12 UTC - June 30 02:55 UTC (MJD=57202.9250-57203.1215). Data in Epochs 1 and 3 were taken in the 3mm (97.5 GHz for ~1.5 hours) and the 2mm (140.5 GHz for ~2.5 hours) bands in sequence, while only 2mm band data were taken in Epoch 2. \nWe observed multiple flares during Epochs 1 and 2 at 140.5 GHz, but not at 97.5 GHz, while Epoch 3 detected no flaring activity in either band. The average flux level declined from Epoch 1 to Epoch 3; all flux densities reported below are found from fitting a point source in the UV plane to the complete data sets. The errors reported do not include the ~15/10% systematic errors for absolute flux calibration in the 2mm/3mm bands. \n \n \n Epoch Frequency (GHz) Flux Density (mJy) \n ---------------------------------------------------------------- \n 1 97.5 65.2 +/- 0.2 \n 1 140.5 46.9 +/- 0.3 \n 2 140.5 16.4 +/- 0.09 \n 3 97.5 5.3 +/- 0.1 \n 3 140.5 6.0 +/- 0.1 \n \nOur NOEMA observations show much fainter flux densities, compared to the Jy level mm/sub-mm emission we observed with the SMA/JCMT on June 22 (ATel #7708). By combining the NOEMA data with simultaneous AMI-LA data at 16 GHz, we measure simultaneous spectral indices of: alpha_{16,97.5 GHz} = -0.65 +/- 0.06 and alpha_{16,140.5 GHz} = -0.61 +/- 0.08 in Epoch 1; alpha_{16,140.5 GHz} = -0.39 +/- 0.08 in Epoch 2; and alpha_{16,97.5 GHz} = -0.25 +/- 0.06 and alpha_{16,140.5 GHz} = -0.11 +/- 0.08 in Epoch 3, where flux density (f_nu) is proportional to nu^alpha. This suggests the radio through mm emission switched from being dominated by optically thin synchrotron jet ejecta to being dominated by an optically thick compact synchrotron jet. \nThis could represent the reestablishment of a compact jet associated with a transition from the soft to the hard accretion state. The latest X-ray spectra and flux reported (ATel #7731) are consistent with the source being in the hard state and at about 0.1% Eddington (given a 12 solar mass black hole; e.g., Shahbaz et al. 1994, MNRAS, 271, L10). It is unclear at this time whether V404 Cyg will continue to decay in the hard state (possibly following a similar decay pattern as the 1989 outburst; Han & Hjellming 1992, ApJ, 400, 304) or whether it will brighten and/or undergo other state transitions. \nObservers with data between 2015 June 26 - 30 during the times listed above are encouraged to contact sivakoff@ualberta.ca to coordinate joint analyses. \nGiven the significant decline in intensity and variability activity reported here and at other wavelengths, further multi-wavelength observations are highly recommended. \nWe thank the NOEMA staff for rapidly scheduling our observations and the AMI scheduling team for their continued monitoring of the source.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Accreting object, Exoplanet", "Black hole, Magnetar, Star and stellar system", "Black hole, Accreting object, Star and stellar system", "Active galactic nucleus, Accreting object, Star and stellar system" ] }, "answerKey": "C" }, { "id": "atel_7875", "message": "Title: Significant colour change of ASASSN-15ni observed with the UCD Watcher telescope\nAuthors: A. Martin-Carrillo (University College Dublin, UCD), D. Murphy (UCD), L. Hanlon (UCD), M. Topinka (CTU), H. J. van Heerden (UFS), B. van Soelen (UFS) and P. J. Meintjes (UFS)\nDate: 5 Aug 2015; 23:07 UT\nProvenance: Antonio Martin-Carrillo (antonio.martin-carrillo@ucd.ie)\nSubjects: Optical, Cataclysmic Variable\nDescription: We continue to monitor the cataclysmic variable ASASSN-15ni (ATel #7850) with the 0.4m UCD Watcher robotic telescope at Boyden Observatory (South Africa). Observations are carried out using 3 filters (SDSS g', r' and i') with exposure times ranging from 10 to 30 seconds. \nIn our first set of observations from July 28 (ATel #7855), ASASSN-15ni appeared as a blue source with a colour index of r' - g' = 0.14 +/- 0.04 and i' - g' = 0.35 +/- 0.04, consistent with ATels #7854 and #7859. Using data obtained for 9 nights from July 28th to August 5, we observe that the brightness of the source was decaying as a power-law until August 4. No significant change in brightness is seen between August 4 and August 5 suggesting a possible flattening. No significant variability is seen in any filter at short timescales. \nThe current average magnitudes obtained on August 5 (18:21 - 19:21 UT) are r' = 14.39 +/- 0.04, i' = 14.41 +/- 0.07, g' = 14.44 +/- 0.02. These new magnitudes suggest a spectral change where the source is significantly redder than on July 28, with colour indices of r' - g' = -0.05 +/- 0.05 and i' - g' = -0.03 +/- 0.07. \nWe plan to continue observing ASASSN-15ni.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Magnetar", "Accreting object", "Variable star" ] }, "answerKey": "D" }, { "id": "atel_7950", "message": "Title: Recent NIR photometry of the Flaring Quasar 3C454.3 \nAuthors: L. Carrasco, E. Recillas, A. Porras, D. Y. Mayya, A. Carraminana, (INAOE, Mexico)\nDate: 25 Aug 2015; 20:51 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Infra-Red, Gamma Ray, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 7981\nFollowing the report of enhanced Gamma-ray activity by Fermi LAT, we observe the quasar 3C454.3 at NIR wavelengths, finding it with increased flux. On August 22nd, 2015 (MJD 2457256.727951), the object had J = 12.246 +/- 0.04, H = 11.367 +/- 0.04 and Ks = 10.463 +/- 0.05. These values correspond to fluxes about 30% larger than the ones obtained in our previous observations on MJD 2457008. Flaring activity in visible light for this object had been reported by S. Jorstad et al. (Atel#7942). Our observations are carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We strongly encourage further multiwavelength coverage.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Quasar", "Minor body", "Variable star" ] }, "answerKey": "B" }, { "id": "atel_8050", "message": "Title: MAXI/GSC detection of a short X-ray transient MAXI J1714-130 / XRF 150912 and Swift non-detection in XRT follow-up observations\nAuthors: M. Nakajima, H. Negoro (Nihon U.), T. Mihara (RIKEN), J. A. Kennea (PSU), M. Arimoto (Tokyo Tech), S. Ueno, H. Tomida, S. Nakahira, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA), M. Sugizaki, M. Serino, M. Shidatsu, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN), N. Kawai, T. Yoshii, Y. Tachibana, Y. Ono, T. Fujiwara (Tokyo Tech), A. Yoshida, T. Sakamoto, Y. Kawakubo, H. Ohtsuki (AGU), H. Tsunemi, R. Imatani (Osaka U.), K. Tanaka, T. Masumitsu (Nihon U.), Y. Ueda, T. Kawamuro, T. Hori (Kyoto U.), Y. Tsuboi, S. Kanetou (Chuo U.), M. Yamauchi, D. Itoh (Miyazaki U.), K. Yamaoka (Nagoya U.), M. Morii (ISM) report on behalf of the MAXI team:\nDate: 13 Sep 2015; 16:19 UT\nProvenance: Hitoshi Negoro (negoro@phys.cst.nihon-u.ac.jp)\nSubjects: X-ray, Transient\nDescription: The MAXI/GSC nova alert system triggered an uncatalogued faint X-ray transient source at UT 2015-09-12 21:03:00 (MJD 57277.8771). Assuming that the source flux was constant over the transit, we obtain the source position at \n(R.A., Dec) = (258.585 deg, -13.060 deg) = (17 14 20, -13 03 36) (J2000) \nwith a statistical 90% C.L. elliptical error region with long and short radii of 0.41 deg and 0.35 deg, respectively. The roll angle of long axis from the north direction is 7.0 deg counterclockwise. There is an additional systematic uncertainty of 0.1 deg (90% containment radius). \n \nThe 4-10 keV X-ray fluxes in the scan transits at 19:30, 21:03 and 22:35 were 0.047 ± 0.044 photons/cm2/sec, 0.129 ± 0.052 photons/cm2/sec and -0.027 ± 0.032 photons/cm2/sec, respectively. \nWe then requested Swift XRT followup observations, and a 7-point tiling observation of the error circle, with exposures of approximately 500 sec per tile, were performed from 2015-09-13 06:24:27 to 08:24:43. But, there is no new source detected in any of the 7 fields. \n \nThe latest light curves and images of MAXI J1714-130 are available at the URL: \nhttp://maxi.riken.jp/top/index.php?cid=1&jname=J1714-130", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Exoplanet", "Active galactic nucleus", "Nova" ] }, "answerKey": "D" }, { "id": "atel_8150", "message": "Title: Spectrum of V1831 Aql (N Aql 2015) in the short-wave optical range\nAuthors: V. P. Goranskij (SAI, Moscow University), E. A. Barsukova (Special Astrophysical Observatory, Russia)\nDate: 11 Oct 2015; 14:31 UT\nProvenance: Vitaly Goranskij (goray@sai.msu.ru)\nSubjects: Optical, Nova\nDescription: We have taken an optical spectrum of the highly obscured Galactic nova V1831 Aql (PNV J19215012+1509248, ASASSN-15qd; ATel #8126, #8127, #8136, #8142) using the SAO RAS 1-m telescope and the UAGS spectrograph. The exposure of the spectrum was 3.6 ks centered on 2015 Oct 6.72 UT, spectral range 3800-5247 Å, spectral resolution 3 Å, signal-to-noise ratio >10\\. In this spectrum, the stellar continuum is visible by the red side from 4500 Å. The spectrum is dominated by strong lines of H-beta, Fe II 4924, 5018, 5169 (blend), 5235 Å. Equivalent widths of H-beta, FeII 4924 and 5018 Å are the following: 150, 43 and 65 Å, respectively. All the lines have double profiles with a division of peaks at 740 km/s. H-beta and Fe II lines have almost equal half-widths, FWHM ~ 1350 km/s (corrected for resolution). The blue peak in H-beta is more intensive than red one by about 50 per cent, whereas peaks of Fe II lines are of equal intensity. Our observation confirms the Williams Fe II classification based on infrared data published in ATel #8142.\nThe spectrum of V1831 Aql", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova, Stellar evolution", "Interstellar medium, Variable star", "Nova, Variable star", "Binary system, Variable star" ] }, "answerKey": "C" }, { "id": "atel_8200", "message": "Title: Spectroscopic Classification of PS15cku as a Type Ia Supernova\nAuthors: Jujia Zhang (Yunnan Observatories) and Xiaofeng Wang (Tsinghua University)\nDate: 21 Oct 2015; 04:02 UT\nProvenance: Xiaofeng Wang (wang_xf@mail.tsinghua.edu.cn)\nSubjects: Optical, Supernovae, Transient\nDescription: We report an optical spectrum (range 340-900 nm) of PS15cku that was obtained on Oct.20.7 2015 UT with the 2.4-m telescope (+YFOSC) at LiJiang Gaomeigu Station of YNAO. The spectrum is consistent with a type Ia supernova a few days before the maximum light. Cross-correlation with a library of supernova spectra using the \"Supernova Identification\" code (SNID; Blondin and Tonry 2007, Ap.J. 666, 1024) shows that it matches with SN 2003cg at t = -3 days. Adopting a redshift of 0.023 for its host galaxy 2MASX J01242239+0335168 (from the narrow emission of the spectrum), an expansion velocity of about 11000 km/s can be derived from the absorption minimum of Si II 635.5 nm.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Near-Earth object", "Black hole", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_8300", "message": "Title: Spectroscopic Classification of PS15cwx as a Type Ia\nAuthors: Charles Kilpatrick, Peter Milne, Jennifer Andrews, Nathan Smith (University of Arizona)\nDate: 19 Nov 2015; 09:14 UT\nProvenance: Charles Kilpatrick (charlesk@email.arizona.edu)\nSubjects: Optical, Supernovae, Transient\nDescription: Referred to by ATel #: 8301\nThe AZTEC (Arizona Transient Exploration and Characterization) collaboration reports an optical spectrum of PS15cwx (ATEL #8299) obtained on UT 2015 Nov. 19.33 with the 2.3m Bok telescope (+ Boller & Chivens spectrograph) on Kitt Peak, Arizona. Cross-correlation using SNID (Blondin & Tonry 2007) finds good matches with SNe Ia-91T (e.g., SN 1999ac) before optical maximum and with a redshift near 0.046.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Exoplanet", "Black hole", "Near-Earth object", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_8370", "message": "Title: Discovery of a Probable Nova in M81\nAuthors: K. Hornoch (Astronomical Institute, Ondrejov, Czech Republic), H. Kucakova (Astronomical Institute, Charles U., Prague, Czech Republic)\nDate: 5 Dec 2015; 17:41 UT\nProvenance: Allen W. Shafter (ashafter@mail.sdsu.edu)\nSubjects: Optical, Nova, Transient\nDescription: We report the discovery of a probable nova in M81 on a co-added 1440-s unfiltered CCD frame taken on 2015 Nov. 24.064 UT with the 0.65-m telescope at Ondrejov. \nThe new object designated PNV J09552375+6906265 is located at R.A. = 9h55m23s.75, Decl. = +69o06'26\".5 (equinox 2000.0), which is 50.5\" west and 151.4\" north of the center of M81 (see link to discovery image below). \nThe following unfiltered magnitudes were obtained using the 0.65-m telescope at Ondrejov (R-band magnitudes used from comparison stars): \n2015 Oct. 31.163 UT, [21.9; Nov. 24.064, 20.5 ± 0.25; 28.183, 21.6 ± 0.4. \nDiscovery image", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Accreting object", "Active galactic nucleus", "Exoplanet" ] }, "answerKey": "A" }, { "id": "atel_8460", "message": "Title: Discovery and Classification of the z=1.86 SLSNe: DES15E2mlf\nAuthors: Y.-C. Pan, R. J. Foley (University of Illinois), L. Galbany, S. Gonzalez-Gaitan, F. Forster, M. Hamuy (Universidad de Chile), J. L. Prieto (Universidad Diego Portales), F. Yuan, B. E. Tucker (Australian National University), C. Lidman (Australian Astronomical Observatory), P. Martini (Ohio State University), Julia Gshwend (Observatorio Nacional / LIneA), A. Moller, B. Zhang (Australian National University), S. Desai, K. Paech (Ludwig Maximilians University, Munich), R. C. Smith (NOAO/CTIO), M. Schubnell (University of Michigan), R. Kessler, J. Lasker, D. Scolnic (University of Chicago), D. J. Brout, L. Gladney, M. Sako, R. C. Wolf (University of Pennsylvania), P. J. Brown, K. Krisciunas, N. Suntzeff (Texas A&M University), R. Nichol, A. Papadopoulos (University of Portsmouth), M. Childress, C. D'Andrea, S. Prajs, M. Smith, M. Sullivan (University of Southampton), R. Maartens (University of the Western Cape), R. Gupta, E. Kovacs, S. Kuhlmann, H. Spinka (Argonne National Laboratory), E. Ahn, D. A. Finley, J. Frieman, J. Marriner, W. Wester (Fermilab), G. Aldering, A. G. Kim, R. C. Thomas (Lawrence Berkeley National Laboratory), K. Barbary, J. S. Bloom, D. Goldstein, P. Nugent, S. Perlmutter (Lawrence Berkeley National Laboratory + University of California, Berkeley), R. Casas, F. J. Castander (ICE, IEEC/CSIC, Barcelona)\nDate: 23 Dec 2015; 22:59 UT\nProvenance: Mathew Smith (matsmith2@gmail.com)\nSubjects: Optical, Supernovae\nDescription: We report the spectroscopic classification of DES15E2mlf as a superluminous supernova (SLSN) discovered by the Dark Energy Survey (ATEL #4668). DES15E2mlf was discovered on 7 November 2015 at R.A. = 00:41:33.40, Decl = -43:27:17.2 with r = 24.1 mag. We obtained spectra using GMOS on Gemini-South (520-990nm) on 06 December 2015 which indicated a redshift of z = 1.86 from Mg II 2800 absorption. The SN peaked at r = 22.4 mag, which corresponds to M = -22.4 mag at z = 1.86. Further observations were obtained with the AAOmega Spectrograph (Saunders et al. 2004, SPIE, 5492, 389) and the 2dF fibre positioner at the Anglo-Australian Telescope (AAT) on 12 & 14th December 2015 and using GMOS on Gemini-South (380-990nm) on 15 December 2015, the latter of which confirm DES15E2mlf to be a SLSN at z = 1.86 at maximum light, spectroscopically similar to SNLS-06D4eu. While our spectra do not cover hydrogen features and thus cannot rule out DES15E2mlf as a SLSN-II, it is most similar, spectroscopically, to other SLSNe-I. Object classification was performed using superfit (Howell et al, 2005, ApJ, 634, 119), the details of which are reported in the table below. \n \n \n Name | RA (J2000)| Dec (J2000)|Discovery |Discovery|Spectrum |Redshift| Type | Phase |Notes \n | | |Date (UT) |Mag (r) |Date (UT) | | | | \n DES15E2mlf |00:41:33.40|-43:27:17.2 |2015 Nov 07| 24.1 |2015 Dec 06 and 15 (Gemini-S), 2015 Dec 12 and 14 (AAT)| 1.86 | SLSN | max |a,b \n \n a). Redshift from galaxy emission features\t \n b). DES15E2mlf has (g,r,i,z)=(23.3,22.7,22.5,22.7) on 16 Dec 2015 and is rising in i&z. Further spectroscopic observations where possible are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus", "Supernova", "Star and stellar system", "Binary system" ] }, "answerKey": "B" }, { "id": "atel_8525", "message": "Title: Spectroscopic Classification of ASASSN-15uy as a Type IIb Supernova\nAuthors: Liming Rui, Xiaofeng Wang, Fang Huang (Tsinghua University), Tiameng Zhang, Meng Zhai (NAOC)\nDate: 10 Jan 2016; 00:21 UT\nProvenance: Xiaofeng Wang (wang_xf@mail.tsinghua.edu.cn)\nSubjects: Optical, Supernovae, Transient\nDescription: We report an optical spectrum (range 380-850 nm) of ASASSN-15uy (ATEL 8491) that was obtained on UT Jan. 08.9 2015 with the 2.16-m telescope (+BFOSC) at Xinglong Station of National Astronomical Observatories of China. Cross-correlation with a library of supernova spectra using the spectral comparison tool Gelato (Harutyunyan et al., 2008, A&A, 488, 383) shows that the spectrum matches with a few type IIb supernovae within 1-2 weeks from the maximum light.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Circumstellar disk", "Repeater", "Quasar" ] }, "answerKey": "A" }, { "id": "atel_8610", "message": "Title: X-ray detection of the old nova DK Lacertae\nAuthors: S. F. Boardman (Commonwealth School and CfA), D. Takei (RIKEN), J. J. Drake (CfA), T. Sakamoto (AGU), A. Fruscione (CfA)\nDate: 29 Jan 2016; 21:52 UT\nProvenance: Jeremy J. Drake (jdrake@cfa.harvard.edu)\nSubjects: X-ray, Cataclysmic Variable, Nova, Variables\nDescription: We report the detection of the old nova DK Lacertae with Chandra X-Ray Observatory's ACIS-S CCD imaging spectrometer on 3 February 2015. DK Lacertae, located at (J2000) 22:49:46.970 +53:17:19.66, was discovered in 1950 at a brightness of 6 mag (Bertaud, C., 1950, IAUC, 1254, 1). Chandra detected 92.5 +/- 9.6 net counts from the source at a count rate of 0.0306 +/- 0.0032 c/s over an exposure time of 3025.6 s. No significant variability was observed during the length of the observation. With 90% statistical confidence, the size of the source indicates that it is point-like. No evidence for extended emission was found. Best-fit X-ray spectral model parameters were a temperature of kT > 91 keV and an interstellar hydrogen column density of nH = 3.5 +/- 0.52x10^21 cm^-2 for an APEC thermal plasma model and gamma = 0.92 +/- 1.3 and nH <= 3.4x10^21 cm^-2 for a power law model. The flux for the bandpass 0.5-7 keV was 4.23E-13 +/- 7.3E-14 erg/cm2/s. The hardness of the X-ray spectrum suggests the presence of non-thermal emission.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system", "Nova", "Active galactic nucleus", "Globular cluster" ] }, "answerKey": "B" }, { "id": "atel_8725", "message": "Title: MASTER-Kislovodsk: bright high amplitude OT\nAuthors: P. Balanutsa, V. Lipunov, E. Gorbovskoy, N. Tiurina, V. Kornilov, O. Gress, A. Kuznetsov, I. Gorbunov, D. Vlasenko, V. Vladimirov (Lomonosov Moscow State University, SAI), A. Tlatov, V. Senik, D. Dormidontov, A. Parkhomenko (Kislovodsk Solar Station, Pulkovo observatory)\nDate: 24 Feb 2016; 12:30 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Request for Observations, Cataclysmic Variable, Transient, Variables\nDescription: Referred to by ATel #: 8731\nMASTER OT J084140.94+722732.6 discovery - high amplitude dwarf nova outburst(ampl>5.5m) with MASTER archive 6.6mag outburst in 2013y\nMASTER-Kislovodsk auto-detection system ( Lipunov et al., \"MASTER Global Robotic Net\", Advances in Astronomy, 2010, 349171 ) discovered OT source at (RA, Dec) = 08h 41m 40.94s +72d 27m 32.6s on 2016-02-22.89248 UT. \nThe OT unfiltered magnitude is 14.7m. The OT is seen in 3 images. There is no minor planet at this place. \nWe have reference image on 2013-12-30.89828 UT with unfiltered magnitude limit 19.5m, m_OT~19.7. \nWe have archive previous outburst in MASTER-Tunka database on 2013-04-25 19:01:50UT with m_OT=13.1. \nThere is USNO-B1 star with B2=18.70,R2=18.73, I=18.72, so we suggest the dwarf nova outburst with Amplitude more then 5m on 22nd of Feb2016 and Ampl>6.6m in last outburst(2013). \nSpectral observations are required. \nThe discovery and referencei mages are available at http://master.sai.msu.ru/static/OT/MASTER084140.94+722732.6.jpg \nMASTER Global Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system", "Variable star", "Minor body", "Interstellar medium" ] }, "answerKey": "B" }, { "id": "atel_8800", "message": "Title: Swift monitoring observations of 1H 1743-322 and its evolution towards a state transition\nAuthors: Zhen Yan, Jie Lin, Wenfei Yu, Wenda Zhang, Hui Zhang and Dongming Mao (Shanghai Astronomical Observatory)\nDate: 11 Mar 2016; 06:10 UT\nProvenance: Wenfei Yu (wenfei@shao.ac.cn)\nSubjects: X-ray, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 8849\nFollowing the report of the new outburst of black hole X-ray binary H1743-322 (ATel #8751), we requested a series of Swift ToO observations to monitor the X-ray temporal and spectral evolution and potential jet contribution to the UV flux during the outburst. The latest two Swift observations were taken on Mar 7th and Mar 10th, when the hard X-ray (15-50 keV) flux seen from Swift/BAT started to drop. The 0.5-10 keV X-ray spectra of the two observations are quite similar. Both spectra can be fitted well by a power-law model with indices of 1.58+-0.04 and 1.62+-0.05, respectively. Both Fourier power spectra obviously show Type-C low frequency quasi-periodic oscillations (QPOs). The central frequency of the QPO increased from 0.44+-0.03 to 0.75+-0.01 Hz, and the fractional root mean square (RMS) between 0.1 and 10 Hz had dropped from 0.39+-0.02 to 0.32+-0.02. \nWe also investigated the Swift/XRT observations of several previous outbursts of H1743-322 observed with Swift/XRT. In the last two outbursts in 2014 and 2015, H1743-322 stayed in the low-hard state throughout the entire outbursts. Therefore compare the current outburst with the previous two outbursts will tell if the current outburst will be the same low hard state outburst. The Swift/XRT spectrum near the previous outburst peak was also well-fitted by a power-law model with an index ~ 1.55, and the central frequency of the low frequency QPO was about 0.2-0.3 Hz. However, the central frequency of the QPO exponentially evolved from less than 1 Hz to about 3-5 Hz within one week during the hard-to-soft transition of the normal outbursts, at the same time the fractional RMS quickly dropped (Debnath et al. 2013, Zhou et al. 2013). \nBased on the decreasing trend of the hard X-ray flux and the RMS variability, the increasing trend of the QPO frequency, and the higher QPO frequency during the current outburst, we suspect that a hard-to-soft state transition is likely to start in the next few days. The Swift will continue monitor the source and we encourage multi-wavelength observations in X-ray, radio, optical and infrared wavelengths in the next week due to jet activities during the X-ray state transition expected to occur (e.g. Miller-Jones et al. 2012). We thank the Swift PI, Neil Gehrels, for approving these observations and the Swift team for scheduling our observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Exoplanet", "Black hole", "Supernova" ] }, "answerKey": "C" }, { "id": "atel_8910", "message": "Title: Swift follow-up observations of iPTF16abc\nAuthors: Yi Cao, Mansi M. Kasliwal (Caltech), S. Bradley Cenko (GSFC/UMd) on behalf of the intermediate Palomar Transient Factory collaboration\nDate: 5 Apr 2016; 18:30 UT\nProvenance: Yi Cao (ycao@astro.caltech.edu)\nSubjects: Optical, Ultra-Violet, Supernovae\nDescription: Referred to by ATel #: 8937\nWe triggered Swift to observe the young type Ia supernova iPTF16abc (ATel#8907, ATel#8909) under our ToO program (PI: Kasliwal; program ID: 1215232). The first visit was undertaken around UT April 5.4, about 12 hours after our trigger. The UVOT photometry (in AB system) is as follows: \n \n \n UW2 > 22.45 \n UM2 > 22.99 \n UW1 = 21.76 +/- 0.34 \n U = 19.24 +/- 0.11 \n V = 18.37 +/- 0.24 \n B = 18.88 +/- 0.13 \n \nThe supernova is not detected by XRT, leaving a 3-sigma upper limit of 4.26e-3 cts/s. \nMore Swift observations are scheduled in the next few days.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus", "Supernova", "Stellar evolution", "Globular cluster" ] }, "answerKey": "B" }, { "id": "atel_8975", "message": "Title: After the aborted 2015 attempt, the supersoft X-ray symbiotic star AG Dra is finally entering a bright outburst\nAuthors: U. Munari (INAF Padova-Asiago), G. L. Righetti (ANS Collaboration)\nDate: 20 Apr 2016; 19:52 UT\nProvenance: U. Munari (ulisse.munari@oapd.inaf.it)\nSubjects: Optical, Ultra-Violet, X-ray, Cataclysmic Variable, Nova\nDescription: Referred to by ATel #: 10390, 11559\nAfter seven years of flat quiescence following the 2006-08 major outburst, in the late spring of 2015, AG Dra begun rising again in brightness toward what appeared to be a new outburst (#Atel 7582). However, in a few weeks the trend reversed and the object returned to flat quiescence. The peak amplitude of that attempt was 0.3 mag in the B band.\nThis time AG Dra seems doing it right. In a couple of weeks, the brightness in the B band has increased by a whole magnitude, from 11.3 on April 5 to 10.3 on April 19, already covering almost half of the way to the peak B=9.0 reached in September 2006 during the last 2006-08 major outburst (Munari et al. 2009, PASP 121, 1070). We are tightly monitoring AG Dra both photometrically and spectroscopically with various ANS Collaboration telescopes and the Asiago 1.22m and 1.82m telescopes. On April 18.869 UT we measured B=10.351, V=9.360, Rc=8.610, and Ic=8.013, and on April 19.854 UT its was U=9.832, B=10.322, V=9.355, Rc=8.560, and Ic=8.003.\nLarge spectroscopic changes are accompanying the rapid increase in optical brightness. A low resolution spectrum (range 3450-8150 Ang, dispersion 2.31 Ang/pix), obtained on April 19.91 UT with the Asiago 1.22m telescope, shows a strong blue continuum veiling the redder quiescence spectrum, and the Balmer continuum has turned into outstanding emission. Compared to a similar spectrum we obtained a month ago for AG Dra in quiescence (March 19.97 UT), all emission lines have increased their integrated absolute flux. In units of 10(-12) erg cm(-2) sec(-1), Halpha increased from 54 to 70, HeI 5876 from 1.4 to 2.4, Raman 6825 band from 6.2 to 8.1, and HeII 4686 truly jumped up, from 6.8 to 31. Particularly noteworthy is the increase in the HeII/Hbeta ratio from 0.94 to 1.84. Following the nomenclature introduced by Gonzalez-Riestra et al. (1999, A&A 347, 478) the current outburst is of the \"hot\" type. An Echelle spectrum (range 3600-7400 Ang, resolving power 23000) obtained with the Asiago 1.82m telescope on April 19.95 UT, shows the emission lines to be sharp and with simple profiles, and no obvious P-Cyg absorptions. The FWHM of HeI lines is 75 km/s, 120 km/s is that of HeII 4686 and 5412, and 190 km/s for Balmer lines.\nAG Draconis is the brightest symbiotic star in X-rays and one of the prototypes of the supersoft X-ray source class. During the 2006-08 outburst, XMM observations by Gonzalez-Riestra et al. (2008, A&A 481, 725) found a marked anti-correlation between X-ray flux and optical brightness, suggesting that during outburst the WD radiation increases, but is strongly absorbed by the circumstellar ionized gas. New X-ray observations during the current outburst would be relevant to test and refine the picture.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Variable star", "Pulsar", "Near-Earth object" ] }, "answerKey": "B" }, { "id": "atel_9075", "message": "Title: Spectroscopic Classification of ASASSN-16fj/AT2016cmn as a Type Ia SN\nAuthors: D. M. Terndrup, G. Calhoun, R. Cannata, J. Schulze (OSU), S. Dong (KIAA-PKU), J. L. Prieto (UDP; MAS)\nDate: 23 May 2016; 14:44 UT\nProvenance: Jose L. Prieto (jose.prietok@mail.udp.cl)\nSubjects: Optical, Supernovae, Transient\nDescription: We obtained an optical spectrum (range 397-686nm) of ASASSN-16fj/AT2016cmn (ATel #9073) on UT 2016 May. 21.4 with OSMOS mounted on the MDM 2.4-m telescope. The spectrum of ASASSN-16fj/AT2016cmn is that of a normal Type Ia SN before maximum light. Cross-correlation with a library of supernova spectra using the \"Supernova Identification\" code (SNID; Blondin & Tonry 2007, ApJ, 666, 1024) shows that the best match is the normal Type Ia SN1994D at -4 days. After correcting the spectrum for the redshift of the host galaxy, we measure a Si II 635.5nm expansion velocity of 11000 km/s.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Star and stellar system", "Accreting object", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_9150", "message": "Title: An increase of Optical Activity in the Quasar 3C454.3\nAuthors: Svetlana Jorstad (IAR, Boston U., Boston, USA & St. Petersburg State U., St. Petersburg, Russia) \nDate: 14 Jun 2016; 04:57 UT\nProvenance: Svetlana Jorstad (jorstad@bu.edu)\nSubjects: Optical, X-ray, Gamma Ray\nDescription: Referred to by ATel #: 9157, 9176, 9178, 9190, 9192, 9723\nThe quasar 3C454.3 shows an increase of the optical activity during the last three nights. According to our observations at the Perkins telescope of the Lowell Observatory (Flagstaff, AZ) the brightness of the source on June 10 (JD 2457549.8770) in R band was 15.817+-0.018 with a of polarization of 2.27+-0.39%. On June 12 the brightness and degree of polarization increased significantly (R= 15.262+-0.018 and P=13.00+-0.25%) and the last night a new increase of the brightness is observed (R=14.958+-0.020). We encourage multi-wavelength observations of the quasar, well known for its dramatic variability and a good correlation between variations at different wavelengths from gamma-ray to mm-waves.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Black hole", "Repeater", "Active galactic nucleus" ] }, "answerKey": "D" }, { "id": "atel_9225", "message": "Title: Doubling Down: A Dominant, 11.26-Minute Photometric Period in FO Aqr\nAuthors: Colin Littlefield (Notre Dame), Erin Aadland (Minnesota State), Peter Garnavich (Notre Dame), Mark Kennedy (University College Cork)\nDate: 8 Jul 2016; 05:59 UT\nProvenance: Colin Littlefield (clittlef@alumni.nd.edu)\nSubjects: Optical, Request for Observations, Binary, Cataclysmic Variable, Variables\nDescription: We obtained time-resolved photometry of the intermediate polar FO Aqr during its ongoing low state (ATEL #9216) on 2016 July 2, 6, and 7. We observed at a cadence of 8 seconds using the University of Notre Dame's 80-cm Sarah L. Krizmanich Telescope. All data were unfiltered with a Johnson V zeropoint. A representative light curve, along with a Lomb-Scargle periodogram of the combined dataset, is available at this link.\nThe most surprising feature of our data is the presence of a very prominent 11.26-minute periodicity, corresponding with one-half of the beat period between the spin and orbital periods. To check the stability of this period, we computed a power spectrum for each individual time series, and the 11-minute signal was by far the strongest period in all three light curves. Interestingly, there is little evidence of the beat period itself. The 20.9-minute spin period of the white dwarf (WD) is also conspicuous in the power spectrum, although the 11-minute signal is much stronger. For comparison, during FO Aqr's bright state, the spin modulation of the WD was the dominant source of photometric variation on timescales of less than the orbital period, and the 11-minute signal was comparatively weak (Kennedy et al. 2016, MNRAS, 459, 3622). Such a strong signal at half of the beat period suggests an interaction between the rotating WD and structures fixed within the binary rest frame. For example, if the accretion stream were to overflow the disk and travel to the WD's magnetosphere, it is conceivable that the overflowing stream would be channeled onto alternating magnetic poles as a consequence of the WD's rotation with respect to the stream. As a result, the stream might alternate between magnetic poles twice each beat period, possibly producing the observed signal. Regardless of the exact cause of the 11.26-minute period, the reduced accretion rate has clearly resulted in dramatic changes in the system's accretion processes. FO Aqr merits continued photometric and spectroscopic monitoring. \nPower spectrum and a representative light curve", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star, Black hole", "Variable star, Binary system", "Accreting object, Binary system", "Variable star, Circumstellar disk" ] }, "answerKey": "B" }, { "id": "atel_9330", "message": "Title: MAXI/GSC detection of a new X-ray outburst from the LMXB 4U 1608-52\nAuthors: Y. Ono, Y. Tachibana, N. Kawai (Tokyo Tech), H. Negoro, M. Nakajima (Nihon U.), T. Mihara (RIKEN), S. Ueno, H. Tomida, S. Nakahira, M. Ishikawa, Y. Sugawara (JAXA), Y. E. Nakagawa (JAMSTEC), M. Sugizaki, M. Serino, W. Iwakiri, M. Shidatsu, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN), N. Isobe, S. Sugita, T. Yoshii, T. Fujiwara (Tokyo Tech), A. Yoshida, T. Sakamoto, Y. Kawakubo, Y. Kitaoka (AGU), H. Tsunemi, R. Shomura (Osaka U.), K. Tanaka, T. Masumitsu, T. Kawase (Nihon U.), Y. Ueda, T. Kawamuro, T. Hori, A. Tanimoto (Kyoto U.),Y. Tsuboi, Y. Nakamura, R. Sasaki (Chuo U.), M. Yamauchi, K. Furuya (Miyazaki U.), K. Yamaoka (Nagoya U.) report on behalf of the MAXI team:\nDate: 6 Aug 2016; 09:44 UT\nProvenance: Yutaro Tachibana (tachibana@hp.phys.titech.ac.jp )\nSubjects: X-ray, Binary, Neutron Star\nDescription: Referred to by ATel #: 9356\nThe MAXI/GSC nova-alert system detected renewed X-ray activity from the low mass X-ray binary 4U 1608-52 (H 1608-522) at UT 11:30 on 2016 August 5 (MJD 57605). The 4-10 keV X-ray fluxes obtained with MAXI/GSC were 255 +- 17 mCrab averaged over four scan transits centered on 11:25 and 16:02 on August 5. Swift/BAT also detected the beginning of this outburst on August 5 (http://swift.gsfc.nasa.gov/docs/swift/results/transients/H1608-522/). This is the 7th outburst from the source since the long outburst in 2007-2009 (Linares et al. ATel #2264). The previous outbursts started on 2010 March 2 (ATel #2462, Asai et al. 2012), 2011 March 24 (ATel #3237, Asai et al 2012), 2012 October 10 (ATel #4478), 2013 May 27 (ATel #5094) ,2014 January 16 (ATel #5990) and 2014 October 7 (ATel #6550).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Galaxy", "Black hole", "Neutron star" ] }, "answerKey": "D" }, { "id": "atel_9420", "message": "Title: Asiago spectroscopic classification of ASASSN-16jj\nAuthors: L. Tomasella, S. Benetti, E. Cappellaro, N. Elias-Rosa, P. Ochner, A. Pastorello, G. Terreran, M. Turatto (INAF OAPd)\nDate: 28 Aug 2016; 00:13 UT\nProvenance: Lina Tomasella (lina.tomasella@oapd.inaf.it)\nSubjects: Optical, Supernovae, Transient\nDescription: Referred to by ATel #: 9422\nThe Asiago Transient Classification Program (Tomasella et al. 2014, AN, 335, 841) reports the spectroscopic classification of ASASSN-16jj (SN 2016flu) in SDSS J234711.91+100459. \nThe observations were performed with the Asiago 1.82 m Copernico Telescope equipped with AFOSC (range 340-820 nm; resolution 1.4 nm). \n \n \n Survey Name | IAU Name | Host galaxy | Discovery (UT) | Discovery mag | Observation (UT) | Redshift | Type | Phase | Notes \n ASASSN-16jj | SN 2016flu |SDSS J234711.91+100459|2016-08-27 13:40:47| 17.1 | 2016-08-27.87 | 0.034 | SN Ia | before max | (1) \n \n(1) The best match is with the Type Ia SN 2003du and SN 2003kf about one week before B-band maximum light. Using the redshift 0.034 (suggested by SNID), from the position of the minimum of the Si II 635nm feature, we infer an expansion velocity of ~12600 km/s for the ejected material. \nThe classification was performed using the GELATO (Harutyunyan et al. 2008, A&A, 488, 383) and SNID (Blondin and Tonry 2007, ApJ, 666, 1024) tools. The Asiago classification spectra are posted at the website http://sngroup.oapd.inaf.it. \nPadova-Asiago SN group", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Exoplanet", "Supernova", "Quasar" ] }, "answerKey": "C" }, { "id": "atel_9480", "message": "Title: The progenitor of Nova ASASSN-16kd\nAuthors: R. K. Saito (Universidade Federal de Santa Catarina), D. Minniti (Univ. Andres Bello, Millennium Institute of Astrophysics, Vatican Observatory), M. Catelan (Pontificia Univ. Catolica de Chile, Millennium Institute of Astrophysics), R. Angeloni (Gemini Observatory), L. A. Gutierrez (Univ. Andres Bello, Millennium Institute of Astrophysics)\nDate: 9 Sep 2016; 17:50 UT\nProvenance: Roberto Saito (saito@astro.ufsc.br)\nSubjects: Infra-Red, Nova\nDescription: Referred to by ATel #: 9482\nStanek et al. (ATel #9469) recently reported on the discovery of a likely classical Nova in the Milky Way bulge, confirmed by spectroscopic observations by the ARAS Group (Bohlsen 2016, ATel #9477). Nova ASASSN-16kd is located at coordinates RA,DEC (J2000) = 17:22:51.426,-31:58:36.28, corresponding to l,b = -5.220,2.463, within the area covered by the VVV Survey (vvvsurvey.org; Minniti et al. 2010, New Astronomy, 15, 433). \nMultiband near-IR VVV observations taken in 2010 show the presence of a faint source 0.94 arcsec apart from the reported target position. According to the VVV reddening maps (Gonzalez et al., 2012, A&A, 543, 13) assuming the Cardelli et al. (1989, ApJ, 345, 245) extinction law, the mean extinction for a 2 arcmin region around the source position is A_K=0.45 mag, corresponding to A_V=3.8 mag. \nThe VVV coordinates and magnitudes for the likely progenitor of Nova ASASSN-16kd are listed below. \n \n \n VVV ID: VVV J172251.46-315837.1 \n RA,DEC(J2000) = 17:22:51.465, -31:58:37.08 \n L,B = -5.216, 2.470 \n Z = 19.41+/-0.19 \n Y = 18.67+/-0.17 \n J = 17.69+/-0.15 \n H = 16.85+/-0.17 \n Ks = 16.53+/-0.21 \n \nWe gratefully acknowledge use of data from the ESO Public Survey programme ID 179.B-2002 taken with the VISTA telescope, and data products from the Cambridge Astronomical Survey Unit. R.K.S. acknowledges support from CNPq/Brazil.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Minor body", "Galaxy", "Exoplanet" ] }, "answerKey": "A" }, { "id": "atel_9600", "message": "Title: Optical Observations of Correlated Outburst Activity in BL Lacertae\nAuthors: Thomas J. Balonek, Ryan W. Stahlin, Katie J. Chapman, Alina Sabyr, Saiyang Zhang (Colgate Univ)\nDate: 6 Oct 2016; 06:13 UT\nProvenance: Thomas J. Balonek (tbalonek@colgate.edu)\nSubjects: Optical, AGN, Blazar, Quasar\nDescription: We report an optical (R) outburst in the blazar BL Lacertae likely associated with the recently reported gamma ray flare on 2016 October 5 (Mukherjee, ATel #9599). Since early September, when BL Lac was at a local minimum (R ~ 14.1-14.2), it has increased in brightness, rising to R ~ 12.9-13.0 on 2016 October 4, 5, 6 (UT). On 2016 October 6, continuous observations over 6 hours show only minor variations (ΔR < 0.1). Several smaller flares were were superimposed on the month-long rise, the brightest peaking around September 22-23 at R ~ 13.2, followed by a fading of 0.4 magnitude in 2 days. The pre-outburst minimum corresponds to the faintest we have observed BL Lac since a local minimum of similar brightness in mid-2014; the peak is the brightest we have observed since a comparable outburst that peaked in late May 2016. All observations were obtained using the Ferson 0.4-m telescope equipped with a FLI PL1001 CCD camera at Colgate University's Foggy Bottom University in Hamilton, NY.\nStudent research participation at Colgate University is supported by the NASA / New York Space Grant, and Colgate University Schlichting fellowships and a Research Council grant.\nFurther observations are encouraged, as this source frequently exhibits multi-wavelength intra-day variability.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus", "Supernova", "Black hole", "Star and stellar system" ] }, "answerKey": "C" }, { "id": "atel_9690", "message": "Title: VERITAS detection of the radio galaxy NGC 1275 with elevated very-high-energy gamma-ray emission\nAuthors: Reshmi Mukherjee (Barnard College) for the VERITAS Collaboration\nDate: 30 Oct 2016; 22:15 UT\nProvenance: Reshmi Mukherjee (muk@astro.columbia.edu)\nSubjects: Gamma Ray, >GeV, TeV, VHE, AGN\nDescription: Referred to by ATel #: 9791, 9931\nOn October 29, 2016 UTC (MJD 57690), the radio galaxy NGC 1275 (z = 0.01756) was detected with elevated very-high-energy gamma-ray emission during routine snapshot monitoring with the VERITAS array of atmospheric Cherenkov telescopes. Further observations by VERITAS were taken on October 30, 2016 UTC (MJD 57691) resulting in a total of ~5 hours (~5:00 UTC to ~10:00 UTC) of data. A preliminary analysis of these data yields a significant detection with the peak flux (from a run-by-run light curve) being (2.7 +/- 0.67) x 10^-11 cm^-2 s^-1 above 250 GeV (corresponding to 15% of the flux from the Crab Nebula). This is the brightest VHE detection of this source recorded; previous detections are at ~3% of the Crab Nebula from MAGIC (Aleksic et al. 2014, A&A 564, A5) and ~1% Crab Nebula flux from VERITAS (Benbow et al. 2015 https://arxiv.org/abs/1508.07251). We note that an increased activity from NGC 1275 at very-high-energy gamma rays was also reported by MAGIC for the same dates (ATel #9689). VERITAS will continue to observe NGC 1275 and multi-wavelength observations are encouraged. Questions regarding the VERITAS observations should be directed to Reshmi Mukherjee (muk@astro.columbia.edu). VERITAS (Very Energetic Radiation Imaging Telescope Array System) is located at the Fred Lawrence Whipple Observatory in southern Arizona, USA, and is most sensitive to gamma rays between ~85 GeV and ~30 TeV (http://veritas.sao.arizona.edu).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Galaxy", "Star and stellar system", "Magnetar" ] }, "answerKey": "B" }, { "id": "atel_9800", "message": "Title: PESSTO spectroscopic classification of optical transients\nAuthors: Felipe Olivares (MAS, Univ. de Chile), Lingzhi Wang (CASSACA), Lixin Yu (CASSACA), Giuliano Pignata (UNAB, MAS), Osmar Rodriguez (UNAB, MAS), Lluís Galbany (Pitt), Ting-Wan Chen (MPE), C. Inserra (QUB), E. Kankare (QUB), K. Maguire (QUB), S. J. Smartt (QUB), K. W. Smith (QUB), M. Sullivan (Southampton), S. Valenti (UC Davis), O. Yaron (Weizmann), D. Young (QUB), I. Manulis (Weizmann), L. Wyrzykowski,(Warsaw, Observatory, Poland)\nDate: 28 Nov 2016; 18:26 UT\nProvenance: Giuliano Pignata (pignago@gmail.com)\nSubjects: Optical, Supernovae\nDescription: PESSTO, the Public ESO Spectroscopic Survey for Transient Objects (see Smartt et al. 2015, A&A, 579, 40 http://www.pessto.org ), reports the following supernova classifications. Targets were supplied by OGLE-IV Real-time Transient Search (Wyrzykowski et al., 2014 arxiv:1409.1095; http://ogle.astrouw.edu.pl/. All observations were performed on the ESO New Technology Telescope at La Silla on 2012 November 27th, using EFOSC2 and Grism 13 (3985-9315A, 18A resolution). Classifications were done with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024) and GELATO (Harutyunyan et al., 2008, A&A, 488, 383). Classification spectra and additional details can be obtained from http://www.pessto.org (via WISeREP) and the IAU Transient Name Server. \n \n \n Survey Name | IAU Name | RA (J2000) | Dec (J2000) | Disc. Date | Source | Disc Mag | z | Type | Phase | Notes \n OGLE16fsn | | 05:55:38.77 | -64:37:57.5 | 20161117 | OGLE | 19.6 | 0.075 | Ia | +1d |", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Black hole", "Supernova", "Globular cluster" ] }, "answerKey": "C" }, { "id": "atel_9870", "message": "Title: Magnetar-like Spectral Index Flattening of the High Magnetic Field Pulsar PSR J1119- 6127\nAuthors: Aaron B. Pearlman (Caltech, JPL), Walid A. Majid (JPL, Caltech), Shinji Horiuchi (CSIRO), Jonathon Kocz (Caltech), Jonas Lippuner (Caltech, JPL), Thomas A. Prince (Caltech, JPL)\nDate: 17 Dec 2016; 00:55 UT\nProvenance: Walid Majid (majidw@gmail.com)\nSubjects: Radio, X-ray, Gamma Ray, Neutron Star, Transient, Pulsar, Magnetar\nDescription: Dramatic changes in pulsed radio emission have been reported by Majid et al. (2016; arXiv:1612.02868) from the high magnetic field pulsar PSR J1119-6127 at S-band (2.3 GHz) and X-band (8.4 GHz) following the reactivation of its radio emission (Burgay et al., ATel #9366). Magnetar-like outbursts have also been observed in X-rays and gamma-rays (Kennea et al., GCN Circular #19735; Younes et al., GCN Circular #19736; Kenna et al., ATel #9274; Archibald et al. (2016); Go?g?u?s? et al. (2016)). We report our observations of PSR J1119-6127, spanning 1.7 hours on 03 December 2016 starting at UT 15:36:52, using the 70-m diameter Deep Space Network (DSN) radio dish (DSS- 43) in Canberra, Australia. The data were recorded in filterbank search mode using 512 us time resolution. The receivers and data acquisition system are described in detail in Majid et al. (2016; arXiv:1612.02868). Pulsations were detected at S-band (2.3 GHz, 96 MHz bandwidth) and X-band (8.4 GHz, 480 MHz bandwidth) in dual circular polarization mode at a period of 0.40996974(6) s using the PRESTO pulsar search package (http://www.cv.nrao.edu/~sransom/presto). Both polarizations were combined in quadrature, and pulsed emission was seen at S/X-band with a peak signal-to- noise ratio (SNR) of 17.2/54.5. The pulse profile at S-band appears roughly singly peaked, with a smaller secondary peak near the dominant emission component. At X-band, the pulse profile shows a strong, narrow single peak. We measure a mean flux density of 0.18(4)/0.08(2) mJy at S/X-band, which represents an order of magnitude decrease at S-band and roughly a factor of 2 decrease at X-band compared to previous measurements by Majid et al. (2016; arXiv:1612.02868). Using these flux density values, we derive a spectral index -0.6(2). We also divided the X-band data into five equal 96 MHz bandwidths and detected pulsations in each subband. Mean flux densities at each subband were measured, and together with our mean flux density value at S-band, we find a spectral index of -0.52(6) in agreement with our initial result. The spectral index has flattened by a factor of approximately 4 compared to previous measurements by Majid et al. (2016; arXiv:1612.02868) across these frequency bands. We interpret this change as evidence of additional magnetar-like behavior from PSR J1119-6127, as these spectral index measurements are similar to those observed from other magnetars, such XTE J1810-197 (Camilo et al. (2007); Lazaridis et al. (2008)), SGR J1745-2900 (Torne et al. (2015)), and PSR J1622-4950 (Anderson et al. (2012)). We are continuing to monitor changes in the spectrum of PSR J1119-6127 at S-band and X-band, and we encourage further observations across multiple wavelengths. We thank the DSN and Canberra Deep Space Communication Complex teams for scheduling these observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Pulsar", "Near-Earth object", "Neutron star" ] }, "answerKey": "B" }, { "id": "atel_10025", "message": "Title: ATCA non-detection of TDE candidate OGLE17aaj\nAuthors: E. R. Stanway (Warwick), A. J. Levan (Warwick), G. C. Brown (Warwick)\nDate: 30 Jan 2017; 13:52 UT\nProvenance: Andrew Levan (A.J.Levan@warwick.ac.uk)\nSubjects: Radio, AGN, Transient, Tidal Disruption Event\nDescription: We observed TDE candidate OGLE17aaj (A-Tels #10006, #9977) at 5.5 and 9.0 GHz with the Australia Telescope Compact Array (ATCA). The simultaneous observations commenced at 2017 Jan 28 06:06UT and continued for 90 minutes on-source, ending at 08:02UT. The standard source PKS1934-638 was used for flux calibration, and J0252-712 for phase calibration. The array was in the 750B configuration, giving a beam of 39 x 4.9 arcseconds at a position angle of -6.4 degrees. \nWe do not detect the target source at either frequency.\nWe note that assigning an absolute flux limit is complicated by the large beam and the presence of an unrelated 14mJy source at RA,Dec=01:56:21.9,-71:05:43.19. We measure a local rms at the location of the TDE of 46 microJy at 5.5 GHz and 53 microJy at 9.0 GHz. \nThese observations were associated with NAPA programme C3098 (PI: Stanway).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object, Accreting object, Neutron star", "Repeater, Black hole, Neutron star", "Accreting object, Black hole, Accreting object", "Accreting object, Black hole, Neutron star" ] }, "answerKey": "D" }, { "id": "atel_10125", "message": "Title: ASASSN-17cz: Discovery of A Probable Supernova in 2MASX J17503055-0148023\nAuthors: J. Brimacombe (Coral Towers Observatory), J. S. Brown, K. Z. Stanek, T. W.-S. Holoien, C. S. Kochanek, J. Shields, T. A. Thompson (Ohio State), B. J. Shappee (Hubble Fellow, Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), D. Bersier (LJMU), Subo Dong, S. Bose, Ping Chen (KIAA-PKU), P. Cacella (DogsHeaven Observatory), J. M. Fernandez (Observatory Inmaculada del Molino), S. Kiyota (Variable Star Observers League in Japan), R. A. Koff (Antelope Hills Observatory), P. Marples (Leyburn Observatory, Australia), R. S. Post (Post Astronomy)\nDate: 24 Feb 2017; 19:14 UT\nProvenance: Jonathan Brown (brown@astronomy.ohio-state.edu)\nSubjects: Optical, Supernovae, Transient\nDescription: During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014), using data from the quadruple 14-cm \"Brutus\" telescope in Haleakala, Hawaii, we discovered a new transient source, most likely a supernova, in the galaxy 2MASX J17503055-0148023. \nASASSN-17cz (AT 2017bkc) was discovered in images obtained on UT 2017-02-23.65 at V~16.9 mag. We do not detect (V>17.6) the object in images taken on UT 2017-02-15.64 and before. An image obtained on 2017-02-24 by J. Brimacombe confirms the discovery of the transient. This figure shows the archival Pan-STARRS (Chambers et al. 2016, arXiv:1612.05560) g-band image of the host (left) and the J. Brimacombe confirmation image (right). The red circle has a radius of 5\" and is centered on the position of the transient in the J. Brimacombe image. \nThe position of ASASSN-17cz is approximately 4.9\" South and 7.0\" West from the center of the galaxy 2MASX J17503055-0148023 (z=0.017382, d=71.5 Mpc, via NED), giving an absolute V-band magnitude of approximately -18.5 (m-M=34.24, A_V=1.138). Properties of the new source and photometry are summarized in the tables below: \n \n \n Object RA (J2000) DEC (J2000) Disc. UT Date Disc. V mag Approx. Abs. Mag Offset from Host (\") \n ASASSN-17cz 17:50:30.103 -01:48:07.37 2017-02-23.65 16.9 -18.5 8.54 \n \n \n \n Obs. UT Date V mag \n 2017-02-15.64 >17.6 \n 2017-02-23.65 16.9 \n \nFollow-up observations are encouraged. \nWhile we are participating in the TNS system to minimize potential confusion, ASAS-SN will continue using ASASSN-17xx transient names as our primary nomenclature (including supernovae, but also other classes of transients), and we encourage others to do the same. We prefer merging the names as ASASSN-17xx (AT 2017xyz) to preserve, rather than anonymize, the origin of the transient. \nWe thank Las Cumbres Observatory and its staff for their continued support of ASAS-SN. ASAS-SN is funded in part by the Gordon and Betty Moore Foundation through grant GBMF5490 to the Ohio State University, NSF grant AST-1515927, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, the Chinese Academy of Sciences South America Center for Astronomy (CASSACA), and the Mt. Cuba Astronomical Foundation. For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Neutron star", "Supernova", "Accreting object" ] }, "answerKey": "C" }, { "id": "atel_10175", "message": "Title: Swift/XRT detects renewed activity of the Galactic center transient CXOGC J174540.0-290005\nAuthors: N. Degenaar (U. of Amsterdam), M. T. Reynolds (U. of Michigan), R. Wijnands (U. of Amsterdam), J. M. Miller (U. of Michigan), J. A. Kennea (PSU), on behalf of a larger collaboration\nDate: 16 Mar 2017; 20:34 UT\nProvenance: Nathalie Degenaar (degenaar@uva.nl)\nSubjects: X-ray, Binary, Black Hole, Neutron Star, Transient\nDescription: In our daily Swift/XRT monitoring observations of the Galactic center (Degenaar et al. 2015, JHEAp, 7, 137) we detect X-ray activity of a transient source located ~20\" to the north of Sgr A*, at a position consistent with that of the known X-ray transient CXOGC J174540.0-290005/Swift J174540.2-290005. It is first clearly seen during a 1-ks pointing performed on March 6 and continued to be detected over the past 10 days. \nThe source is detected at a roughly constant count rate of ~1E-2 c/s and we therefore extracted an average spectrum from the 10 XRT/PC-mode observations of March 6-16. This spectral data can be described by an absorbed power-law model with a hydrogen column density of N_H=(2.5+/-1.2)E23 cm-2, and an index of 3.3+/-1.3. The inferred unabsorbed 2-10 keV flux is (1.9+/-1.5)E-11 erg/cm2/s, which translates into a luminosity of (1.5+/-1.1)E35 erg/s at a distance of 8 kpc. \nCXOGC J174540.0-290005 exhibited at least two previous outbursts; in 2003 (Muno et al. 2005, ApJ 622, L113) and in 2006 (ATel #920). In 2003, the source was found active during a single Chandra observation, when it was detected at a 2-10 keV luminosity of ~3E34 erg/s. During its 2006 outburst, the Galactic center was monitored daily with Swift/XRT and this showed that the source remained active for ~2 weeks, reaching a peak luminosity of ~2E35 erg/s (Degenaar & Wijnands 2009, A&A 495, 547). Its current level of activity is thus similar to that observed with Swift/XRT during its 2006 outburst. \nThe results of our daily Swift/XRT monitoring campaign of the Galactic center can be found at http://www.swift-sgra.com", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Neutron star, Binary system", "Repeater, Neutron star, Binary system", "Black hole, Quasar, Binary system", "Black hole, Star and stellar system, Binary system" ] }, "answerKey": "A" }, { "id": "atel_10275", "message": "Title: ePESSTO spectroscopic classification of optical transients\nAuthors: R. Cartier, C. P. Gutierrez (Southampton), J. Anderson (ESO), K. Maguire (QUB), C. Inserra (Southampton), E. Kankare (QUB), S. J. Smartt (QUB), K. W. Smith (QUB), M. Sullivan (Southampton), S. Valenti (UC Davis), O. Yaron (Weizmann), D. Young (QUB), I. Manulis (Weizmann), J. Tonry, B. Stalder, L. Denneau., A. Heinze, H. Weiland (IfA, Univ. of Hawaii), A. Rest (STScI)\nDate: 17 Apr 2017; 19:09 UT\nProvenance: Regis Cartier (rgcartier@gmail.com)\nSubjects: Optical, Supernovae\nDescription: ePESSTO, the extended Public ESO Spectroscopic Survey for Transient Objects (see Smartt et al. 2015, A&A, 579, 40 http://www.pessto.org ), reports the following supernova classification. The target was supplied by the ATLAS survey, see Tonry et al. (2011, PASP, 123, 58) and Tonry et al. (ATel #8680). The observation was performed on the ESO New Technology Telescope at La Silla on 2017 April 15, using EFOSC2 and Grism 13 (3985-9315A, 18A resolution). The classification was done with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). Classification spectrum and additional details can be obtained from http://www.pessto.org (via WISeREP) and the IAU Transient Name Server. \n \n \n Survey Name | IAU Name | RA (J2000) | Dec (J2000) | Disc. Date | Source | Disc Mag | z | Type | Phase | Notes \n ATLAS17dkw | SN2017cuh | 05:34:52.24 |-20:02:48.1 | 20170327 | ATLAS | 18.76 | 0.053 | Ia | +4 to +7 |", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Exoplanet", "Supernova", "Black hole", "Globular cluster" ] }, "answerKey": "B" }, { "id": "atel_10350", "message": "Title: Spectroscopic classification of AT 2017byx as a Type Ia Supernova\nAuthors: J. Vinko (Konkoly Obs., U Szeged, UT Austin), J. C. Wheeler (UT Austin), K. Sarneczky, R. Szakats (Konkoly Obs.), T. Szalai, P. Szekely (U Szeged) and the HETDEX collaboration\nDate: 5 May 2017; 15:32 UT\nProvenance: Jozsef Vinko (vinko@astro.as.utexas.edu)\nSubjects: Optical, Supernovae\nDescription: During the commissioning phase of the Hobby-Eberly Telescope Dark Energy Experiment (HETDEX) survey we observed AT 2017byx (ATLAS17bla, PS17bve) at R.A.=14:17:48.36 Dec.=+52:41:54.6 with the Visible Integral-field Replicable Unit Spectrograph (VIRUS) at McDonald Observatory on 2017-04-28.2 UT. \nThe spectrum (range between 3500 and 5500 Angstroms) indicates that AT 2017byx is a Type Ia supernova. The Supernova Identification (SNID) code (Blondin & Tonry 2007, ApJ, 666, 1024) gives good match with many Type Ia supernovae around z ~ 0.067 which agrees with the spectroscopic redshift of the presumed host galaxy (SDSS J141747.64+524143.2, z = 0.068). SNID estimates the age of the supernova as between 1 and 3 months after maximum light which is consistent with the date of discovery (2017-03-06).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar, Interstellar medium", "Active galactic nucleus, Interstellar medium", "Supernova, Quasar", "Supernova, Interstellar medium" ] }, "answerKey": "D" }, { "id": "atel_10410", "message": "Title: FLOYDS Classification of ASASSN-17gi/AT 2017ecp as a Type Ibn Supernova\nAuthors: G. Hosseinzadeh, I. Arcavi, C. McCully, D. A. Howell (Las Cumbres Obs./UCSB), S. Valenti (UC Davis)\nDate: 22 May 2017; 05:02 UT\nProvenance: Iair Arcavi (iarcavi@lcogt.net)\nSubjects: Optical, Supernovae\nDescription: We obtained a spectrum of ASASSN-17gi/AT 2017ecp (ATel #10398) on 2017 May 20.7 UT with the robotic FLOYDS instrument mounted on the Las Cumbres Observatory 2-meter telescope in Siding Spring, Australia. Using Superfit (Howell et al. 2005, ApJ, 634, 1190), we find a good fit to the Type Ibn SN 2006jc 25 days after maximum light at redshift z=0.02. The spectrum is available on the Transient Name Server.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Repeater", "Supernova", "Globular cluster" ] }, "answerKey": "C" }, { "id": "atel_10530", "message": "Title: A New Highest Historical 0.3-10 keV Brightness State of TeV-detected Blazar 1ES 1959+650\nAuthors: Bidzina Kapanadze (Abastumani Astrophysical Observatory at Ilia State University, Tbilisi, Georgia)\nDate: 25 Jun 2017; 08:32 UT\nProvenance: Bidzina Kapanadze (bidzina_kapanadze@iliauni.edu.ge)\nSubjects: X-ray, Blazar\nDescription: In Atel#10430 and Atel#10514, posted on 2017 May 27 and June 20, respectively, we reported the gradually enhancing X-ray flaring activity of the nearby TeV-detected blazar 1ES 1959+650 (z=0.048). Afterwards, the source has been observed seven times with the X-Ray Telescope (XRT) onboard the satellite Swift, and it underwent an extreme X-ray flux variability (see http://www.swift.psu.edu/monitoring/source.php?source=1ES1959+650 ). Namely, the 0.3-10 keV count rate initially declined by 40% to 10.70+/-0.18 cts/s in 0.6 d (June 20), then a gradual increase of the brightness by a factor of 3.2 in 3.2 d was observed. The count rate attained the value of 34.0+/-0.20 cts/s (June 24) which is by 36% higher then its highest historical value recorded on 2016 July 2. Afterwards, the X-ray brightness has declined to 19.10+/-015 cts/s in 0.95 d, although the latter value is by a factor of 2.4 higher than the weighted mean rate from all XRT observations of this source. In the framework of one-zone SSC models, a flaring activity of our target is also expected in the UV-radio and gamma-ray parts of the spectrum, and intensive multiwavelength observations of 1ES 1959+650 are strongly encouraged to study instable processes and emission mechanisms in this source. Nevertheless, it's familiar to this object to re-flare after some brightness drop during the high X-ray states (see Kapanadze et al. 2016a, MNRAS, 461, L26). XRT is one of the Swift instruments along with Burst Alert Telescope (BAT) and UV/Optical Telescope (UVOT). It is a JET-X Wolter I type telescope, developed jointly by Pennsylvania State University, Brera Astronomical Observatory (OAB) and University of Leicester. Thanks to the unique characteristics, good photon statistics and low background counts of this instrument (in combination with EEV CCD2 detector), we can investigate a flux variability on different time-scales from minutes to years, obtain high-quality spectra for the majority of the observations, derive different spectral parameters, and study their timing behaviour in the 0.3-10 keV range of the electromagnetic spectrum. The Swift Satellite is operated by Pennsylvania State University.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Black hole", "Active galactic nucleus", "Exoplanet" ] }, "answerKey": "B" }, { "id": "atel_10600", "message": "Title: S-CUBED detection of SXP 15.3 in outburst\nAuthors: J. A. Kennea (PSU), P. A. Evans (Leicester), M. J. Coe (Southhampton), A. Udalski (Warsaw University)\nDate: 27 Jul 2017; 05:12 UT\nProvenance: Jamie A. Kennea (kennea@astro.psu.edu)\nSubjects: X-ray, Transient\nDescription: Referred to by ATel #: 11030\nThe Swift SMC Survey (S-CUBED) is a wide field shallow survey of the SMC in X-rays performed weekly by NASA's Swift Mission. S-CUBED consists of approximately 150 pointings with an exposure of 60s each, which cover the SMC to search for new and recurrent X-ray transients. \nDuring an S-CUBED observation on July 25th, 2017 at 16:32UT, a source consistent with the localization of the Be/X-ray binary SXP 15.3 was detected at a brightness of 0.6 +/- 0.1 XRT count/s. Previously the source has been frequently detected in S-CUBED observations, but at a much lower count rates of between 0.05-0.15 XRT count/s. Swift performed a 2ks follow-up observations of the source starting at 14:34UT on July 26th, 2017. The source is detected in this observation at RA/Dec(J2000): 13.0558, -73.3218, which is equivalent to: \n \nRA(J2000) = 00h 52m 13.38s, \nDec(J2000) = -73d 19' 18.4'', \n \nwith an estimated uncertainty of 3.5 arc-seconds radius (90% confidence). This position is 2.6 arc-seconds from the Simbad catalogued position of SXP 15.3, and is consistent within errors. Period analysis of the data show evidence of periodicity around 15.3s. However, by coincidence, the source was located inside the field of view of other Swift observations taken on July 25th and July 26th, and by combining those data, we find a strongly detected period in the data at 15.253s, confirming that this is indeed a new outburst of SXP 15.3. Over July 25th and 26th, the source maintains an average brightness of 0.73 +/- 0.02 XRT count/s, with no evidence of fading or brightening over that time period. \nThe spectrum is well fit by an absorbed power-law model with a photon index of 1.3 +/- 0.1. The absorption corrected flux is 5.5 x 10-11 erg/s/cm-2 (0.5 - 10 keV), which at an assumed SMC distance of 61kpc, corresponds to a 0.5-10 keV luminosity of 2.4 x 1037 erg/s. \nOGLE IV monitoring of the optical counterpart to SXP 15.3, [MA 93] 552, show the I band flux to be at its brightest for several years with I=14.2 on 26 July 2017. This is 0.7 magnitudes brighter than the lowest state seen in OGLE IV some 5-6 years ago.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star, Globular cluster", "Variable star, Supernova", "Nova, Accreting object", "Variable star, Accreting object" ] }, "answerKey": "D" }, { "id": "atel_10750", "message": "Title: FLOYDS Classification of ASASSN-17lz/AT 2017grw as a Young Type Ia Supernova\nAuthors: G. Hosseinzadeh, I. Arcavi, D. A. Howell, C. McCully (Las Cumbres Obs./UCSB), S. Valenti (UC Davis)\nDate: 14 Sep 2017; 21:46 UT\nProvenance: Griffin Hosseinzadeh (griffin@lco.global)\nSubjects: Optical, Supernovae\nDescription: We obtained a spectrum of ASASSN-17lz/AT 2017grw on 2017 September 14.3 UT with the robotic FLOYDS instrument mounted on the Las Cumbres Observatory 2-meter telescope on Haleakala, Hawai'i. Using SNID (Blondin & Tonry 2007, ApJ, 666, 1024), we find good fits to several normal Type Ia supernovae in the week before maximum light at redshifts consistent with that of the proposed host galaxy (z=0.017; Barmby & Huchra 1998, AJ, 115, 6 via NED). The supernova is highly extinguished by its host galaxy, making a more precise phase estimate difficult. The spectrum is available on the Transient Name Server.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Pulsar", "Accreting object", "Globular cluster" ] }, "answerKey": "A" }, { "id": "atel_10850", "message": "Title: ASAS-SN Discovery of a Very Young Galactic Nova Candidate ASASSN-17nj\nAuthors: K. Z. Stanek, C. S. Kochanek, J. V. Shields, T. A. Thompson (OSU), L. Chomiuk, J. Strader (MSU), B. J. Shappee (IfA, Hawaii), T. W.-S. Holoien (Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), Subo Dong (KIAA-PKU)\nDate: 14 Oct 2017; 17:07 UT\nProvenance: Krzysztof Stanek (stanek.32@osu.edu)\nSubjects: Optical, Nova\nDescription: Referred to by ATel #: 10852, 10857, 10862\nDuring the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014), using data from the quadruple 14-cm \"Cassius\" telescope in CTIO, Chile, we detect a new transient source, possibly a classical nova (could also be a bright CV), close to the Galactic center\n \n \n Object RA (J2000) DEC (J2000) Gal l (deg) Gal b (deg) Disc. UT Date Disc. V mag \n ASASSN-17nj 17:30:34.18 -31:06:06.80 356.424 1.586 2017-10-14.01 14.0 \n \nASASSN-17nj was discovered in images obtained on UT 2017-10-14.01 at V~14.0. We do not detect (V>17.4) this object in subtracted images taken on UT 2017-10-13.10, so this transient was less than 1-day old at the discovery epoch. \nUsing ASAS-SN Sky Patrol public all-sky light curve interface (Kochanek et al. 2017), we have retrieved aperture photometry time series at the location of ASASSN-17nj, and the resulting light curve can be seen at this link. No previous outbursts or variability are detected at the position of ASASSN-17nj since ASAS-SN started observing this location in March 2016.\nFollow-up observations, especially multi-band photometry and spectroscopy, are strongly encouraged. If ASASSN-17nj is a classical nova, its color should be significantly affected by the large amount of interstellar extinction expected in this direction (A_V~12, Schlafly & Finkbeiner 2011). \nWe thank Las Cumbres Observatory and its staff for their continued support of ASAS-SN. ASAS-SN is funded in part by the Gordon and Betty Moore Foundation through grant GBMF5490 to the Ohio State University, NSF grant AST-1515927, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, and the Chinese Academy of Sciences South America Center for Astronomy (CASSACA).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Globular cluster", "Nova", "Minor body", "Neutron star" ] }, "answerKey": "B" }, { "id": "atel_10975", "message": "Title: Spectroscopic Observations of PNV J17184504-2454221 (Nova Oph 2017) as a Classical Nova in the Iron Curtain Phase\nAuthors: Paul Luckas, International Centre for Radio Astronomy Research, University of Western Australia \nDate: 16 Nov 2017; 01:35 UT\nProvenance: S. N. Shore (shore@df.unipi.it)\nSubjects: Nova\nDescription: PNV J17184504-2454221 (ATel #10959) has recently been announced as a nova candidate. We obtained a medium resolution spectrum (0.82A/px) using an Alpy600 spectrograph (two exposure, 600 sec, S/N of about 50 in the continuum from 4000-7000A) on 2017 Nov. 14.5 UT that confirm this identification and show that the ejecta are quite optically thick and at high expansion velocity. The wings of the Balmer alpha extend to greater than +/-3000 km/s with a narrower (FWHM ~ 2800 km/s) profile with two additional emission enhancements at about -360 km/s and +570 km/s, the latter being weaker by about 30 percent). The low ionization metal lines are all broad, Fe II 5018 and 5169A lines have maximum absorption (P Cyg) radial velocities of -1800+/-100 km/s with red wings extending to +2000 km/s. The Balmer lines do not show absorption (Halpha-Hepsilon) but show similar profiles with lower maximum emission velocity in the wings for the higher series members and asymmetric profiles with the blue core stronger than the red, suggesting possible asymmetric ejecta . Notably, Na I D displays a P Cyg profile with the emission being similar in form to the Balmer lines and the maximum absorption (depth of about 30 percent) at - 1500 km/slow velocity. Si II 6347,6374A are present with weaker absorption (no terminal edge is seen on any P Cyg profile) with a similar velocity to Na I, about -1500 km/s. Mg I 5173A is also present, with a HWZI of 2000 km/s and FWHM of 2600 km/s with similar structure on the emission as Na I. The [O I] lines are absent as are the He I lines. No strong forbidden metal ion lines were detected, and no lines have been seen from C I or C II. The spectrum is too weak below 4000A to say whether Ca II might be present. The spectrum is therefore typical of the opaque (Fe curtain) stage of the ejecta around or a bit after optical maximum and after the maximum of the recombination wave following the initial fireball. The strong neutral emission spectrum is, however, unusual and may indicate a more massive ejection. Unfortunately, the nova is likely to be unobservable from here on but it would be worth the effort to obtain a few more spectra before it is no longer visible. \nARAS Nova Spectroscopic Database", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Supernova", "Active galactic nucleus", "Variable star" ] }, "answerKey": "A" }, { "id": "atel_11025", "message": "Title: The largest glitch of the Crab pulsar detected at the X-ray band\nAuthors: Liangwei Huang (Qian Xuesen Laboratory of Space Technology), Xinyuan Zhang (Qian Xuesen Laboratory of Space Technology), Yuanjie Du (Qian Xuesen Laboratory of Space Technology), Ping Shuai (Qian Xuesen Laboratory of Space Technology) and Shaolong Chen (Qian Xuesen Laboratory of Space Technology)\nDate: 30 Nov 2017; 03:31 UT\nProvenance: Y. J. Du (duyuanjie@qxslab.cn)\nSubjects: X-ray, Neutron Star, Pulsar\nDescription: The X-ray pulsar navigation 1 (XPNAV-1) satellite is a small soft X-ray (0.5-10 keV band) telescope launched on 10 November 2016, which continues to do X-ray timing studies for pulsars. The time-resolved soft X-ray spectrometer (TSXS) is the major scientific payload onboard XPNAV-1 which monitors the Crab pulsar (PSR B0531+21) every day. Detailed information about the XPNAV-1 and the TSXS was given in the published paper as follows http://downloads.hindawi.com/journals/ijae/2017/8561830.pdf. During the time span of the largest glitch of the Crab pulsar recently reported in the radio band (ATel #10939), totally 111 TSXS observations of the Crab pulsar were carried out, of which 15 were executed during the 6 days shortly after this glitch. These X-ray observations confirm the recent glitch. Our preliminary analysis indicates a fractional rotational spin-up of \\delta(F0)/F0 = (0.470+/-0.002)E-6 (3-sigma) and the glitch epoch of MJD 58064.55+/-0.01(3 sigma), which is consistent with the values as reported by Shaw et al. (ATel #10939). The phase connected residuals with the pre-glitch solutions can be seen at the link below. Continuous follow-up XPNAV-1 observations of the Crab pulsar will be operated to obtain more detailed glitch physical information. \nPhase connected residuals with the prefit residuals", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Near-Earth object", "Neutron star, Globular cluster", "Neutron star, Pulsar", "Neutron star, Galaxy" ] }, "answerKey": "C" }, { "id": "atel_11100", "message": "Title: MAGIC detection of an unprecedented activity from S50716+714 at very-high-energy gamma rays\nAuthors: Razmik Mirzoyan (Max-Planck-Institute for Physics, Munich), on behalf of the MAGIC collaboration\nDate: 28 Dec 2017; 19:28 UT\nProvenance: Razmik Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de)\nSubjects: Gamma Ray, >GeV, TeV, VHE, AGN, Blazar\nDescription: Referred to by ATel #: 11107, 11339, 11676, 12298\nThe MAGIC telescopes have observed a strong increase in the very-high-energy (VHE; >100 GeV) gamma-ray flux from S50716+714 (RA: 7:21:53.45, Dec: 71:20:36.36, J2000.0). MAGIC observed the source for ~2 hours on 2017/12/28. The preliminary analysis of the MAGIC data indicates increasing flux reaching up to 1.5 times the flux of the Crab nebula above 150 GeV, which is ~6 times higher than the VHE flux from this source during the 2015 flare (ATel #6999). \n \nS50716+714 is an intermediate Synchrotron peaked blazar (IBL, Giommi et al. 1999, A&A, 351, 59; Ackermann et al. 2011, ApJ, 743, 171) located at the redshift of ~0.3 (Nilsson et al., 2008, A&A, 487, L29; Danforth et al., 2013, ApJ, 764, 57). VHE gamma-ray emission from S50716+714 was first reported by the MAGIC collaboration during high optical state of the source (Anderhub et al. 2009, ApJ, 704, L129). \n \nObservations of MAGIC were triggered by the hard spectrum of the source (spectral index = -1.86 +/- 0.14, Flux (100MeV-300 GeV) = 0.58 +/- 0.12 e-06 ph cm^-2.) found in the Fermi-LAT data in the 24 hour period started on 2017-12-25 at 18:00:00 UTC. \n \nMAGIC observations on S50716+714 will continue during the next two nights and possibly after the moon break and multi-wavelength observations are encouraged. The MAGIC contact person for these observations is R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) \n \nMAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located on the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Interstellar medium", "Supernova", "Star and stellar system" ] }, "answerKey": "B" }, { "id": "atel_11190", "message": "Title: REM observations of the gamma-ray flaring blazar 3C 279\nAuthors: F. D'Ammando (INAF-IRA Bologna), D. Fugazza (INAF-OA Brera), S. Covino (INAF-OA Brera)\nDate: 17 Jan 2018; 17:25 UT\nProvenance: Filippo D'Ammando (dammando@ira.inaf.it)\nSubjects: Infra-Red, Optical, Gamma Ray, >GeV, AGN, Black Hole, Blazar, Quasar\nDescription: Referred to by ATel #: 11196, 11200, 11202, 11239, 11246, 11354, 11464\nFollowing the increase of gamma-ray activity of the flat spectrum radio quasar 3C 279 recently observed by Fermi-LAT (ATel #11189), we have activated follow-up observations with the REM telescope (La Silla, Chile).\nObservations were carried out with REM on 2018 January 17 between 06:32 UT and 06:50 UT, obtaining three 300 s integration images in the optical g', r', i' bands, and fourteen 15 s integration images in the NIR J, H, and K bands.\nWe obtained for the target the following optical and NIR magnitudes:\nV = 14.39+/-0.05, R = 13.96+/-0.14, I = 13.37+/-0.08 \nJ = 12.10+/-0.02, H = 11.27+/-0.04, K = 10.27+/-0.04 \nThe NIR magnitudes were calibrated against the 2MASS catalog; optical calibration was performed against the APASS catalog.\nAccording to our photometry, 3C 279 shows a brightening of about 1 mag in NIR and 0.6-0.8 mag in optical with respect to the mean values observed by REM during 2005-2012 (see Sandrinelli, et al. 2016, ApJ, 151, 54), in agreement with the increase of gamma-ray activity observed by Fermi-LAT.\nREM will continue to monitor 3C 279 in the following weeks.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Globular cluster", "Quasar, Active galactic nucleus", "Black hole, Active galactic nucleus", "Pulsar, Active galactic nucleus" ] }, "answerKey": "C" }, { "id": "atel_11280", "message": "Title: Fermi/GBM Update on the Orbital Ephemeris of Swift J0243.6+6124\nAuthors: P. jenke (UAH-SPA/CSPAR), C. A. Wilson-Hodge (NASA/MSFC), C. Malacaria (NASA/MSFC-USRA)\nDate: 9 Feb 2018; 17:47 UT\nProvenance: Peter Jenke (peter.a.jenke@nasa.gov)\nSubjects: X-ray, Binary, Neutron Star, Transient, Pulsar\nDescription: Using Fermi/GBM data between MJD 58098 and 58154 (2017 December 11 to 2018 February 5) in the 12-50 keV range, we determine a new orbital ephemeris for the newly discovered (ATEL #10809) Be X-ray binary Swift J0243.6+6124. Pulsed searches using the ephemeris from M. Ge et al. (ATEL #10907) and V. Doroshenko et al. 2017 resulted in superfluous structure to the torque model that was correlated with the orbital period likely related to a residual orbital signature. This new orbital ephemeris results in orbit corrected frequency derivatives that correlate well with corrected Swift/BAT rates and Fermi/GBM pulsed flux. The Fermi/GBM pulsed flux and frequency history may be viewed at: https://gammaray.msfc.nasa.gov/gbm/science/pulsars/lightcurves/swiftj0243.html. \nWe obtain the following orbital parameters: orbital period ~ (27.587 +/- 0.017) days, semi-major axis ~ (115.84 +/- 0.32) light-seconds, eccentricity ~ (0.09848 +/- 0.00042), longitude of periastron ~ (-73.56 +/- 0.16) degrees, and periastron epoch (JD) ~ (2458103.629 +/- 0.017). \nFermi/GBM Accreting Pulsar Histories", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star, Binary system, Neutron star", "Magnetar, Binary system, Neutron star", "Accreting object, Binary system, Neutron star", "Accreting object, Binary system, Magnetar" ] }, "answerKey": "C" }, { "id": "atel_11350", "message": "Title: GMRT observations of Type Ic supernova SN 2018ec\nAuthors: A. J. Nayana (NCRA-TIFR) and Poonam Chandra (NCRA-TIFR and Stockholm University)\nDate: 24 Feb 2018; 20:54 UT\nProvenance: Poonam Chandra (poonam@ncra.tifr.res.in)\nSubjects: Radio, Supernovae\nDescription: We observed the Type Ic supernova SN 2018ec (Kankare et al. ATel# 11156), with the Giant Metrewave Radio Telescope (GMRT) on 2018 Jan 20.91 UT in the 1390 MHz band. We do not detect any radio emission at the supernova position RA, Decl (J2000): 10:27:50.77 -43:54:06.3. The 3-sigma upper limit of the flux density at the supernova position is 2.1 mJy. The large upper-limits are due to the emission from the host galaxy NGC 3256 (~ 0.5 Jy at 1.4 GHz). We thank the GMRT staff for scheduling these observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Magnetar", "Neutron star", "Repeater" ] }, "answerKey": "A" }, { "id": "atel_11430", "message": "Title: Optical polarimetry of TXS 0506+056 (possible counterpart of IceCube-170922A)\nAuthors: I. A. Steele, H. Jermak, C. Copperwheat (Liverpool JMU)\nDate: 16 Mar 2018; 10:08 UT\nProvenance: Iain Steele (iainsteele@mac.com)\nSubjects: Optical, Gamma Ray, Neutrinos, Quasar\nDescription: Referred to by ATel #: 11489\nATel #11419 reports enhanced Gamma Ray Activity of TXS 0506+056 detected by Fermi-LAT on 2018 March 13. A previous Fermi-LAT high state of this source in the period 2017 Sept 15-27 was potentially associated with the Ice Cube Neutrino detection 170922A (ATel #10791). TXS 0506+056 is a BL Lac object (e.g. ATel #10799) with redshift z=0.34 (Paiano et al, 2018, ApJ, 854, L32). \nWe obtained optical polarimetry of the BL Lac object on the night of 2018 March 14 using the RINGO3 polarimeter of the 2.0 metre Liverpool Telescope, La Palma. We find the polarisation is moderately strong (P~14%) at wavelengths roughly corresponding to the R and I bands. This is an increase from the R band polarisation P~8% reported in ATel #10844 from the Katana telescope at the time of the previous high state on 2017 Sept 30, although it is within the typical range of BL Lac optical polarisation values of 0-30% (see e.g. Figure 4 of Jermak et al, 2016, MNRAS, 462, 4267). \nLiverpool Telescope", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Neutron star", "Variable star", "Black hole" ] }, "answerKey": "D" }, { "id": "atel_11520", "message": "Title: X-ray re-brightening of the accreting millisecond X-ray pulsar IGR J17379-3747\nAuthors: J. van den Eijnden, N. Degenaar, T. Russell, R. Wijnands, J. V. Hernandez Santisteban (University of Amsterdam), D. M. Russell, A. AlMannaei (NYU Abu Dhabi), D. Maitra (Wheaton College), A. W. Shaw, C. O. Heinke, G. R. Sivakoff (University of Alberta), T. Maccarone (Texas Tech University), J. Miller-Jones (ICRAR-Curtin), M. Armas Padilla (Instituto de Astrofisica de Canarias), A. Bahramian (Michigan State University)\nDate: 9 Apr 2018; 18:56 UT\nProvenance: Jakob Van den Eijnden (a.j.vandeneijnden@uva.nl)\nSubjects: X-ray, Neutron Star, Transient, Pulsar\nDescription: IGR J17379-3747 is a neutron star low-mass X-ray binary, identified as an accreting millisecond X-ray pulsar by the detection of 468 Hz pulsations by NICER (Atel #11507). On 19 March 2018, MAXI/GSC reported renewed X-ray activity of this source (ATel #11447). This outburst reached a peak 2-10 keV X-ray luminosity of 9E35 (D/8 kpc)2 erg s-1 on 23 March 2018 (Atel #11487), after which it started to decay in X-rays. On 4 April 2018, the source was no longer detected in a 645 second monitoring observation using the Swift X-ray Telescope (XRT). \nHere, we report the X-ray re-brightening of IGR J17379-3747 in the latest XRT monitoring observation taken on 8 April 2018 00:59 UT. We extract the PC-mode spectrum using the Swift XRT online pipeline (Evans et al. 2009, MNRAS, 397, 1177) and fit it in the 0.5 to 10 keV energy range with an absorbed power law model (TBABS*PO in XSPEC). The spectrum is well-described with an NH = (1.05 +/- 0.17) E22 cm-2, a power law index 2.6 +/- 0.2 and a reduced chi-squared of 222/351. The unabsorbed 0.5-10 keV and 2-10 keV X-ray fluxes are (4.3 +/- 0.3)E-11 erg s-1 cm-2 and (1.4 +/- 0.2)E-11 erg s-1 cm-2, respectively. These fluxes correspond to X-ray luminosities of (3.3 +/- 0.2) (D/8 kpc)2 E35 erg s-1 and (1.1 +/- 0.1) (D/8 kpc)2 E35 erg s-1, respectively. \nFurther Swift XRT monitoring observations are planned every other day. Optical observations are planned with Las Cumbres Observatory and VLA radio monitoring is ongoing (Atel #11487). Further multi-wavelength observations are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Globular cluster", "Neutron star, Pulsar", "Neutron star, Magnetar", "Neutron star, Circumstellar disk" ] }, "answerKey": "B" }, { "id": "atel_11610", "message": "Title: ASAS-SN 18jj is a classical nova in the LMC\nAuthors: L. Chomiuk, J. Strader, L. Shishkovsky, S. Swihart (MSU), K. Z. Stanek, C. S. Kochanek, J. V. Shields, T. A. Thompson (OSU), B. J. Shappee (IfA-Hawaii), T. W.-S. Holoien (Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), Subo Dong (KIAA-PKU), M. Stritzinger (Aarhus)\nDate: 5 May 2018; 00:38 UT\nProvenance: Laura Chomiuk (chomiuk@pa.msu.edu)\nSubjects: Optical, Nova\nDescription: Referred to by ATel #: 13545\nAT 2018bej/ASAS-SN 18jj was discovered on 2018 May 3 23:02 UT by the ASAS-SN survey, at a brightness g' = 12.1 mag. Its J2000 coordinates are RA = 06:26:20.76, Dec = -69:45:46.30, implying that it is likely in the LMC. We obtained spectroscopic observations of ASAS-SN 18jj with the Goodman spectrograph on the 4-m SOAR telescope on 2018 May 5.0 UT, with a low-resolution spectrum (R~1200) covering 3850--7850 A. The spectrum indicates that ASAS-SN 18jj is a young classical nova, with strong hydrogen Balmer emission lines and additional strong lines of [O I] and Fe II. The Balmer lines show P Cygni profiles; the FWHM of the H alpha emission component is 2210 km/s, and the absorption trough extends to -2960 km/s.\nCheck on the light curve as it evolves with the ASAS-SN Sky Patrol", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Nova", "Pulsar", "Exoplanet" ] }, "answerKey": "B" }, { "id": "atel_11700", "message": "Title: Fermi/GBM detects renewed activity from XTE J1946+274\nAuthors: P. Jenke (UAH-SPA/CSPAR), C. A. Wilson-Hodge (NASA/MSFC), C. Malacaria (NASA/MSFC-USRA)\nDate: 8 Jun 2018; 15:44 UT\nProvenance: Colleen A. Wilson (Colleen.Wilson@nasa.gov)\nSubjects: X-ray, Binary, Neutron Star, Transient, Pulsar\nDescription: Pulsations from the transient Be/X-ray pulsar XTE J1946+274 are currently being detected with Fermi/GBM. The pulsations were first detected in the data of June 5.0-6.0 at a frequency of 63.463(9) mHz, with a pulsed flux of 0.17 +/- 0.02 cnts cm^-2 s^-1 in the 12-50 keV band. The last outburst of this source detected with Fermi/GBM began on April 30 2011 (ATel #2677, ATel #2663).\nFermi/GBM Accreting Pulsar Histories", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy, Pulsar", "Variable star, Pulsar", "Neutron star, Pulsar", "Exoplanet, Pulsar" ] }, "answerKey": "C" }, { "id": "atel_11775", "message": "Title: NuSTAR observations of AT2018cow reveal a hard X-ray component of emission above 15 keV\nAuthors: R. Margutti (Northwestern University), R. Chornock (Ohio University), T. Laskar (NRAO/Berkeley), W. Fong (Northwestern University), B. Grefenstette (Caltech), G. Risaliti (UniFi) on behalf of a larger collaboration\nDate: 24 Jun 2018; 18:58 UT\nProvenance: Raffaella Margutti (rmargutti@cfa.harvard.edu)\nSubjects: X-ray, Supernovae\nDescription: Referred to by ATel #: 11776, 11782, 11788, 11792, 11793, 11808, 11813, 11843\nNuSTAR started observing the transient AT2018cow (ATel #11727) on June 23 17:31:09 UT under Director Discretionary Time (DDT, PI Margutti). From the analysis of 28 ks of data, we find the following preliminary results: \nAT2018cow is very well detected with signal in excess of the background up to 60 keV. NuSTAR data in the 3-60 keV range can be fit with a simple power-law spectral model with best fitting photon index Gamma=1.20 +\\\\- 0.03 (1 sigma c.l.). This is significantly harder than inferred from Swift-XRT observations (Gamma~1.6; 0.3-10 keV) obtained around the same time. From our analysis of Swift-XRT observations of AT2018cow obtained so far (Swift ID 10724, segments 2-14), we find no evidence for statistically significant spectral evolution of the source. The combined 0.3-10 keV spectrum is well described by a simple power-law with Gamma=1.62 +\\\\- 0.03 (1 sigma c.l.) and no evidence for intrinsic neutral hydrogen absorption in excess to the Galactic component along the line of sight (NH_gal=4.95E+20 cm-2; Kalberla et al., 2005). The temporal evolution of the 0.3-10 keV flux is consistent with a ~t^-1 decay, assuming t0 to be near the initial optical detection (ATel #11727). These results are in broad agreement with results from previous Swift-XRT analysis ( ATels #11739 and 11761). We do not confirm the soft photon index (Gamma~2.2; 0.5-10.0 keV) and intrinsic absorption NH~1d21 cm-2 inferred from NICER data (ATel #11773). Fitting the NuSTAR data with a broken power-law model we find a low-energy photon index Gamma1=1.53 +\\\\- 0.03 (1 sigma c.l.), with break energy E~15 keV, consistent with the results from the Swift-XRT data at 0.3-10 keV. Above 15 keV NuSTAR data show evidence for an additional hard X-ray component with index Gamma2=0.50 +\\\\- 0.05 (1 sigma c.l.). The inferred flux of the hard X-ray component between 15-79 keV is ~3e-11 ergs/cm^2/s. Further investigation is needed to constrain the physical origin of this hard X-ray component. We thank the entire NuSTAR team for arranging these observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Supernova", "Quasar", "Globular cluster" ] }, "answerKey": "B" }, { "id": "atel_11875", "message": "Title: Photometry and spectroscopy of the continuing rise in brightness of ASASSN-18pe\nAuthors: U. Munari and L. Zampieri (INAF Padova), S. Moretti, A. Maitan and S. Tomaselli (ANS Collaboration)\nDate: 20 Jul 2018; 11:19 UT\nProvenance: U. Munari (ulisse.munari@oapd.inaf.it)\nSubjects: Optical, Cataclysmic Variable, Transient\nDescription: Referred to by ATel #: 11878\nWe have obtained UBVRI photometry (Landolt system) and optical spectroscopy of recently discovered ASASSN-18pe currently undergoing a large amplitude outburst (Atel #11867). Photometry was obtained on UT July 19.888 with the ANS Collaboration telescope 1205 (42cm) providing B=13.961, V=13.895, R=13.801, and I=13.678, with total error budgets (including transformation from the instantaneous local photometric system to the reference Landolt equatorial standards) less than 0.01 mag in all bands. We also obtain U=13.27, but with a larger uncertainty considering the sea level altitude of the observing site. This indicates a continuing (and slow) rise in brightness of ASASSN-18pe, that was reported in Atel #11867 at V=14.3 two days earlier. The overall color seems somewhat bluer that the SLOAN griz values listed for quiescence in the Pan-STARRS release 1 (PS1) Survey\nAbsolute optical spectrophotometry was obtained with the Asiago 1.22m telescope at 2.31 Ang/pix over the 3250-7950 Ang range on UT Jul 19.853. The spectrum rises steeply toward the short wavelengths in agreement with the blue photometric colors. Hbeta, gamma, delta, epsilon lines stands in clear absorption although with a minimal equivalent width, H9 being the highest Hydrogen line before those further up merge into the Balmer continuum in absorption. NaI 5890, 5896 doublet is also in clear absorption. Only an emission component is visible in Halpha with an integrated flux of 6.6 (+/- 0.6) x 10(-15) erg/cm2 sec. The strongest emission line is HeII 4686, radiating an integrated flux of 1.34 (+/-0.11) x 10(-14) erg/cm2 sec, twice larger than Halpha (both lines single peaked). No evident emission line from HeI is visible, with the possible exception of a feeble 5876 Ang. The radial velocity for all observable lines is pretty low within the limited sensitivity of the adopted spectral dispersion.\nOverall, the photometric and spectral appearances are compatible with a CV eruption. Worth noticing are the slow rising time (commented upon also in Atel #11867), the unusual strength of HeII emission and the possibly bluer colors compared to quiescence.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star, Black hole", "Circumstellar disk, Accreting object", "Variable star, Supernova", "Variable star, Accreting object" ] }, "answerKey": "D" }, { "id": "atel_11950", "message": "Title: Low frequency detection of AT2018cow with the GMRT\nAuthors: A. J. Nayana (NCRA-TIFR), Poonam Chandra (NCRA-TIFR)\nDate: 14 Aug 2018; 11:17 UT\nProvenance: Poonam Chandra (poonam@ncra.tifr.res.in)\nSubjects: Supernovae, Transient\nDescription: Referred to by ATel #: 12067\nA. J. Nayana (NCRA-TIFR) and Poonam Chandra (NCRA-TIFR) report on behalf of a larger collaboration: We observed broad lined Type Ic supernova AT2018cow (Smartt et al. ATel# 11727) with the Giant Metrewave Radio Telescope (GMRT) on 2018 Aug 12.71 UT in the 1390 MHz band. We clearly detect radio emission at the supernova position. The flux density of the supernova in this band is 438+/-82 uJy. More observations are planned. We thank GMRT staff for carrying out the observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy", "Black hole", "Supernova", "Exoplanet" ] }, "answerKey": "C" }, { "id": "atel_12025", "message": "Title: Unprecedented optical outburst of FSRQ 1633+38 (4C +38.41)\nAuthors: V. Larionov, S. Savchenko, I. Troitsky, Yu. Troitskaya, T. Grishina, A. Vasilyev and M. Makarova (St. Petersburg University)\nDate: 10 Sep 2018; 14:11 UT\nProvenance: V. Larionov (vlar@astro.spbu.ru)\nSubjects: Optical, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 12026, 12027, 12034, 12037\nWe perform optical photometric and polarimetric monitoring of a sample of gamma-bright blazars using 0.4-m LX-200 telescope (St.Petersburg) and 0.7-m AZT-8 telescope (Crimean Astrophysical Observatory), as a part of WEBT/GASP project. We report that the blazar 1633+38 reached R=15.00 in the night of 2018 September 9, TJD 58371.29. This is a brightest value during the whole time interval of our observations since 2006. R band light curve for 1633+38 can be seen on our web-page. The polarization degree is on the level of 15%. We mention that this fast brightening seems to have occurred with a noticeable (~1 weak) delay after gamma-ray outburst reported by the AGILE team (see ATel#12005). Current high activity state of this blazar deserves close attention in all wavelengths.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Neutron star", "Star and stellar system", "Active galactic nucleus" ] }, "answerKey": "A" }, { "id": "atel_12100", "message": "Title: Independent Discovery of a Probable Nova in M31\nAuthors: K. Hornoch, P. Fatka, H. Kucakova (Astronomical Institute, Ondrejov, Czech Republic)\nDate: 11 Oct 2018; 07:51 UT\nProvenance: Matt Darnley (M.J.Darnley@ljmu.ac.uk)\nSubjects: Optical, Nova, Transient\nDescription: We report the independent discovery of a probable nova in M31 on a co-added 720-s R-band CCD frame taken on 2018 Oct. 11.162 UT with the 0.65-m telescope at Ondrejov. \nThe object was independently discovered also by Q. Yin and X. Gao (designated as AT2018hfs; see here). The object was designated by us as PNV J00424990+4123348 and is located at R.A. = 0h42m49s.90, Decl. = +41o23'34\".8 (equinox 2000.0), which is 62.8\" east and 446.3\" north of the center of M31 (see link to discovery image below). \nThe following R-band magnitudes were obtained using the 0.65-m telescope at Ondrejov: \n2018 Oct. 9.738 UT, [20.5; 11.162, 17.9 ± 0.1. \nDiscovery image", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Globular cluster", "Magnetar", "Nova" ] }, "answerKey": "D" }, { "id": "atel_12180", "message": "Title: Optical observations of the rapidly varying newly discovered transient Swift J1858.6-0814\nAuthors: Maria Cristina Baglio, David M. Russell, Saarah Pirbhoy (NYU Abu Dhabi), Arash Bahramian (Curtin Uni.), Craig O. Heinke (University of Alberta), Paul Roche (Faulkes Telescope Project), Fraser Lewis (Faulkes Telescope Project & Astrophysics Research Institute, LJMU)\nDate: 7 Nov 2018; 07:24 UT\nProvenance: Maria Cristina Baglio (cristina.baglio@brera.inaf.it)\nSubjects: Optical, X-ray, Black Hole, Neutron Star, Transient\nDescription: Referred to by ATel #: 12186, 12197, 12220, 12499, 12512, 12881, 13719\nWe report on optical observations of the newly discovered transient source Swift J1858.6-0814 (first detected by the BAT instrument of the Swift satellite on October 25th, 2018; ATel#12151). \nThe source was observed in the r'-band using the the 2-metre Faulkes Telescope North on November 6th, 2018. We obtained a series of 50 30-seconds integration images. The target is well detected in all images at a position consistent with the Pan-STARRS position of a previous known object (ID 98112846453925483), as also reported in Vasilopoulos et al. 2018 (ATel#12164). \nThe source is found to be highly variable in our ~40 mins observation, with a fractional rms of 21 +/- 1 % on a ~45 seconds time resolution; in particular, we detect a maximum and minimum r'-band magnitude (which corresponds to a minimum and maximum flux) of 17.58 +/- 0.03 and 16.71 +/- 0.02, with a mean magnitude of 17.071 +/- 0.020 (from the fit of the light curve with a constant). This indicates that the target has slightly brightened in the optical with respect to previous observations (ATel#12164).\nFinally, we considered the nH estimate given in ATel #12158, which is reported to vary in the range 1.5E21 - 3E21 cm^-2 (from NICER observations). Using the relation of Foight et al. 2016 (ApJ, 826, 66), from the nH we obtained an estimate of the absorption coefficient Av (~ 0.78 +/- 0.26) and of the E(B-V) (0.168-0.335). From Green et al. 2018 (MNRAS, 478, 651; see http://argonaut.skymaps.info/query?lon=113.14⪫=-57.61&coordsys=gal&mapname=bayestar2017 ), for an E(B-V) ~ 0.168 - 0.335 we could obtain an estimate of the distance of the target from the reddening-distance relation, which is found to be in the range ~ 0.6 - 6 kpc (but we caution that reddening is not constrained beyond 6 kpc). \nWith this estimate of the distance, we constructed the optical-X-ray correlation plot to identify the nature of the compact object of the system. For the X-rays luminosity, we considered a 2-10 keV unabsorbed flux in the range of 7.3(+/-2)e-11 - 1.47(+/-0.2)e-10 erg/s/cm2 (from observations obtained with the Swift satellite on 2018 November 4th and 2nd, respectively). For the optical luminosity, we considered the r'-band magnitudes reported in ATel#12164, which were taken on November 3rd, contemporaneous with the X-ray data. From the optical - X-ray correlation plot that we could build, considering trial values of distance (1, 3, 6, 8, 24 kpc), we conclude that the compact object of the system might be either a neutron star or a black hole, depending on the actual value of the distance. In particular, if the distance is low (~1 kpc), it it is more likely to be a neutron star; instead, if the distance turns out to be higher (>3 kpc), the compact object will more likely be a black hole. \nWe encourage multiwavelength observations, especially radio, and coordinated rapid timing data, e.g. simultaneous optical/infrared and X-ray observations.\nThe Las Cumbres Observatory (LCO) observations are part of an on-going monitoring campaign of ~ 40 low-mass X-ray binaries (Lewis et al. 2008) with LCO and the Faulkes Telescopes. This work makes use of observations from the Las Cumbres Observatory.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Globular cluster, Neutron star", "Black hole, Active galactic nucleus", "Black hole, Neutron star", "Repeater, Neutron star" ] }, "answerKey": "C" }, { "id": "atel_12250", "message": "Title: Variable quasar behind the M31 disk\nAuthors: P. Nedialkov (U Washington/U Sofia), B. F. Williams (U Washington), V. D. Ivanov (ESO), A. Valcheva (U Sofia)\nDate: 29 Nov 2018; 20:25 UT\nProvenance: Petko Nedialkov (japet@phys.uni-sofia.bg)\nSubjects: Optical, Quasar\nDescription: We report spectroscopic confirmation of quasar nature of Gaia DR2 369276756923364224 behind the disk of M31, located at RA(2000) = 00h45m28s.24, Dec(2000) = +41o29'43\".9 and z=0.203. It is a PHAT (Williams et al. 2014) optical counterpart of a color-selected mid-infrared point-like source from the Spitzer catalog of Khan (2017). Four 1800s exposures were taken with the Dual Imaging Spectrograph (DIS) on 3.5 m telescope at APO on 2018 October 7.260 UT. Photometry from images obtained with the 50/70cm Schmidt telescope at Rozhen NAO, Bulgaria yields: R=18.96 +/- 0.06 (2018 October 06.812 UT) and V=19.38 +/- 0.07 (2018 October 06.850 UT). Only 3'.17 apart, both Gaia DR2 369276756923364224 and another quasar Gaia DR2 369288714109887744 at similar redshift z=0.215 (Dorn-Wallenstein et al. 2017) were misclassified as eclipsing binaries in M31 with similar periods of ~80d by Vilardell et al (2006). Zwicky Transient Facility (ZTF) observations showed that Gaia DR2 369276756923364224 had a short single outburst lasting ~1d on August 2018, 29.453 UT (JD=2458359.95) when it was at 1.1 mag brighter than its quiescent state (r=19.3 +/- 0.1). This work was supported by short-term scholar Fulbright grant for the academic year 2018-2019 by the US Department of States program number G-1-00005 and in part, by the Bulgarian NSF grant DN18/2017.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Quasar", "Black hole, Quasar", "Active galactic nucleus, Repeater", "Active galactic nucleus, Active galactic nucleus" ] }, "answerKey": "A" }, { "id": "atel_12375", "message": "Title: Spectroscopic Classification of AT2019np with Faulkes-North/FLOYDS\nAuthors: C. D. Kilpatrick, R. J. Foley (UCSC)\nDate: 10 Jan 2019; 20:17 UT\nProvenance: Charles Kilpatrick (cdkilpat@ucsc.edu)\nSubjects: Optical, Supernovae, Transient\nDescription: Referred to by ATel #: 12378\nWe report spectroscopic observations of AT2019np, discovered by Koichi Itagaki on UT 2019 Jan 9.66 in NGC 3254. The observations were performed using the FLOYDS spectrograph on Faulkes-North on UT 2018 Jan 10.44. Classification was performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). \n \n \n Name | RA (J2000) | Dec (J2000) | z | Type | Phase | Notes \n AT2019np | 10:29:21.96 | +29:30:38.40 | 0.00452 | Ia | -15 | (1) \n \nNotes: When the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. \n \n(1) Given the rise observed from ZTF and photometry on 2019 Jan 10.44 of m_r = 17 mag, which places the source at -15.5 mag assuming a Tully-Fisher distance to NGC 3254 of 31 Mpc (Tully et al. 2016, AJ, 152, 50), we infer this source is very young. We measure a Si II 6355 velocity of -15,600 km/s. We also note the presence of strong C II 6580 absorption with a velocity of -14,700 km/s. This confirms similar findings in Wu et al. (ATel #12374).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Exoplanet", "Pulsar", "Interstellar medium", "Near-Earth object" ] }, "answerKey": "C" }, { "id": "atel_12450", "message": "Title: Continued Activity of (6478) Gault\nAuthors: Quanzhi Ye (Caltech/IPAC), Michael S. P. Kelley (UMD), Dennis Bodewits (Auburn), Bryce Bolin (UW), Chan-Kao Chang (NCU), Zhong-Yi Lin (NCU) on behalf of the ZTF and GROWTH collaborations\nDate: 29 Jan 2019; 20:09 UT\nProvenance: Quanzhi Ye (qye@caltech.edu)\nSubjects: Optical, Asteroid, Comet\nDescription: We report the development of a new tail of the recently-identified active asteroid (6478) Gault, detected by the Zwicky Transient Facility (ZTF) on approximately UT 2019 Jan 28.25. Activity of Gault was first reported by ATLAS (CBET 4594, 4597) on 2019 Jan. 8, based on images taken by ATLAS from 2018 Dec. 8. Archival ZTF images show that significant brightening of Gault started before UT 2018 Oct. 31.50. The event peaked near 2018 Nov. 7, ?r=2.5 mag above the nominal asteroid brightness, and a tail first appeared on 2018 Nov. 16. The nuclear activity had seemingly subsided around mid-December 2018.\nZTF survey photometry shows another increase in brightness starting between UT 2018 Dec. 24.51 and 28.46. This second event peaked near 2019 Jan. 4, with ?r=2.0 mag above the nominal brightness. A new tail was first observed on the ZTF images taken on UT 2019 Jan. 28.51. Follow-up images obtained by the Lulin 1.0-m telescope (UT 2019 Jan. 28.88) and the Astrophysical Research Consortium 3.5-m telescope (UT 2019 Jan. 29.29) confirmed the new tail. Follow-up observations are encouraged.\nThis work is based on observations obtained with the Samuel Oschin Telescope 48-inch at the Palomar Observatory as part of the Zwicky Transient Facility project (see ATel #11266). Major funding has been provided by the U.S. National Science Foundation under Grant No. AST-1440341 and by the ZTF partner institutions: the California Institute of Technology, the Oskar Klein Centre, the Weizmann Institute of Science, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron, the University of Wisconsin-Milwaukee, and the TANGO Program of the University System of Taiwan. The GROWTH project is supported by the U.S. National Science Foundation under PIRE Grant 1545949.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater", "Variable star", "Minor body", "Galaxy" ] }, "answerKey": "C" }, { "id": "atel_12510", "message": "Title: Cygnus X-3 entered in the quenched radio and hard X-ray state\nAuthors: S. A. Trushkin, N. A. Nizhelskij, P. G. Tsybulev, A. V. Shevchenko (SAO RAS, Russia)\nDate: 17 Feb 2019; 13:04 UT\nProvenance: Sergei Trushkin (satr@sao.ru)\nSubjects: Radio, Millimeter, X-ray, Gamma Ray, Binary, Black Hole\nDescription: Referred to by ATel #: 12668, 12677, 12701, 12741\nWe continue the RATAN-600 radio telescope daily monitoring of Cyg X-3 since the giant flares in 2016-2018. During last some days we have observed that the radio fluxes from microquasar Cygnus X-3 do gradually decrease from the quiescent level 100-300 mJy to almost the quenched level 10-50 mJy at 4.6, 8.2 and 11.2 GHz on 17 February 2019 (MJD 58531.332). The dramatic quenching of the hard X-ray fluxes were detected with the Swift/BAT Hard X-ray Transient Monitor at 15-50 keV (see http://swift.gsfc.nasa.gov/results/transients/CygX-3/ and Krimm et al., 2013) also. Similar radio behaviour was detected yet by Waltman et al. (1996), as an indicator of a soon coming giant radio flare. Many times (MacCollough et al. 1997, Koljonen et al., 2010, 2018, ATel #9416, Trushkin et al., 2017) it was showed that Cyg X-3 run through a so-called \"hypersoft X-rays state\" before the powerful ejections or radio jets. Thus again we are right to expect a new giant flare during next 10-30 days. The last such events were detected in August 2018 (MJD 58337-350) although these giant flares were not record (comparing with the flare in September 2016, see ATel #9501), less 3.5 Jy at 8-11 GHz. We plotted the RATAN radio data and Swift hard X-ray data during last 60 days together (see http://www.sao.ru/hq/lran/XB/CygX-3/CygX-3_lc_rat_sw_2019f.png ). The spectrum on 17 Feb 2019 was extremely inverted with the spectral index of power-law fitting of +1.57 that could be related with a compact optically thick radio jets. We continue the RATAN daily observations and any radio, X-rays, of Gamma-rays observations will be very useful. \nThe quenched radio spectrum of Cyg X-3 on 17 February 2019", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk, Black hole", "Binary system, Active galactic nucleus", "Binary system, Repeater", "Binary system, Black hole" ] }, "answerKey": "D" }, { "id": "atel_12575", "message": "Title: Optical follow-up of the flaring blazar TXS 1515-273\nAuthors: Nibedita Kalita, Ram Kesh Yadav, Utane Sawangwit (NARIT, Thailand)\nDate: 13 Mar 2019; 23:52 UT\nProvenance: Nibedita Kalita (nibeditaklt1@gmail.com)\nSubjects: Optical, AGN, Blazar\nDescription: Following the announcement of gamma-ray flaring activity of the blazar TXS 1515-273 in ATel #12532 by S. Cutini, we performed photometric follow up observations of the source during 2019/02/28 – 2019/03/07 with a 4K x 4K CCD camera mounted on the 0.7m Thai Robotic Telescope at Springbrook Observatory (TRT-SBO), Queensland, Australia. The source has shown enhanced activity at other wavelengths as well (ATels #: 12537, #12538, #12552, #12565, #12570). \n \nOur observations consist of 50 x 200s exposures in Johnson V filter, taken under good observing conditions. After bias, flat field, and cosmic ray corrections, aperture photometry was performed on each image frame with DAOPHOT package of IRAF. For zero point correction reference star was taken from the Tycho catalogue (Hog et al., 2000) located in the same field of view. During the observing period, the brightness varied by a maximum value of 0.42 magnitude. Photometric errors from individual images range from 0.03 to 0.08 magnitudes. The resultant magnitudes corrected for Galactic extinction (Schlafly & Finkbeiner 2011) for different nights are listed in the table below: \n \nUT Date | MJD | V \n---|---|--- \n2019-02-28 | 58542.6 | 15.17 \n2019-03-01 | 58543.6 | 15.21 \n2019-03-03 | 58545.6 | 15.08 \n2019-03-04 | 58546.6 | 15.16 \n2019-03-05 | 58547.6 | 15.11 \n2019-03-07 | 58549.6 | 15.14", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Binary system", "Black hole", "Active galactic nucleus" ] }, "answerKey": "C" }, { "id": "atel_12660", "message": "Title: The symbiotic star AX Per is going into strong outburst\nAuthors: J. Merc (UPJS in Kosice, Charles University), R. Galis (UPJS in Kosice), F. Teyssier, D. Boyd, W. Sims, C. Boussin, F. Campos (ARAS)\nDate: 13 Apr 2019; 11:21 UT\nProvenance: Jaroslav Merc (jaroslav.merc@student.upjs.sk)\nSubjects: Optical, Request for Observations, Cataclysmic Variable, Transient, Variables\nDescription: AX Per is a well-known eclipsing symbiotic binary consisting of a giant of type M4.5 III (Muerset & Schmid 1999, A&AS, 137, 473) and probably a white dwarf. The orbital period of the binary system is around 680 days (Mikolajewska & Kenyon 1992, AJ, 103, 579). The light curve of AX Per is characterized by the wave-like variations whose shape is changing from cycle to cycle. After major outbursts of the system in 1988-1992, a new activity stage has begun in 2007, with minor outbursts observed in 2009, 2010, 2012 and 2014 (Munari & Siviero 2009, CBET, No. 1757; Munari , Siviero, et al. 2010, CBET, No. 2555; ATel #4265, ATel #6382). All recent outbursts were significantly lower in magnitude (maximal V around 10) than the major outbursts in 90s (with V < 9). In this Astronomer's Telegram, we report the beginning of a new outburst of AX Per with a strong increase in brightness. In the previous orbital cycle, the brightness of the symbiotic system reached the maximum of B=11.589 and V=10.873 (October 15, 2017; JD 2458042.319). During the binary eclipse in August/September 2018, the magnitudes decreased to the minimum of B=13.387 and V=12.355 on August 21, 2018 (JD 2458352.375). Since then, the brightness of AX Per has started to increase and the March 2019 measurements have shown that it has reached a similar level or was higher than the previous maximum of B=11.516 and V=10.652 (March 24, 2019; JD 2458567.330). Our observation obtained on April 10, 2019 (JD 2458584.337) indicate that the AX Per brightness continues to rise (B=11.109 and V=10.330) in what looks like a promising major outburst of this symbiotic binary. The low resolution spectroscopic observations (R < 1000) obtained during March and April 2019 showed significant changes in the prominent emission lines and in the continuum compared to the spectra acquired at the end of 2018. We note the disappearance of the highly ionized lines (e. g. [Fe VII]) or the change of the He I singlet/triplet ratio. Several emission lines of the He I which were not observable are fairly strong in the recent spectra, and similar behavior is observed in the case of Fe II lines. The Balmer lines equivalent widths have also increased significantly (1.3 times since December 2018). Nebular-to-auroral line ratio of [OIII] 5007/4363 has increased from 0.7 to 1.6. This behavior points to a classical symbiotic outburst during which a accreting layer on white dwarf expands and cools down. We will continue the photometric and spectroscopic monitoring of the AX Per current outburst. It will be interesting to see if the outburst is another of a series of minor outbursts, or we will finally observe a major outburst of this symbiotic system. Recent spectroscopic observations could be found in the ARAS Spectral Database (link to the database below). \nARAS Spectral Database", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body, Variable star", "Star and stellar system, Variable star", "Near-Earth object, Variable star", "Circumstellar disk, Variable star" ] }, "answerKey": "B" }, { "id": "atel_12725", "message": "Title: A New NIR Flare of the Blazar PKS1510-089\nAuthors: L. Carrasco, A. Porras, G. Escobedo, E. Recillas, V. Chavushyan (INAOE, Mexico)\nDate: 4 May 2019; 00:33 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Infra-Red, Optical, Gamma Ray, AGN, Blazar, Quasar\nDescription: We report on an going NIR Flare of the intermediate redshift QSO BZQJ1512-0905 (z=0.36), also known as PKS1510-089 associated with the gamma-ray source 2FGLJ1512.8-0906. Our most recent NIR photometry for this source shows that on April 30th,2019 (JD2458603.9027), the object brightness corresponded to J = 13.088 +/- 0.03, H = 12.221 +/- 0.03 and Ks = 11.421 +/- 0.04. The NIR fluxes in the JHK bands had an increase, since our previously observed fluxes were: J = 13.864 +/- 0.05, H = 13.021 +/- 0.05 and Ks = 12.421 +/- 0.04, on JD2458597.9201. Hence, the object has increased its luminosity by a factor of about 2 in this very short lapse. The object has shown flaring activity in different wavelength bands in the past. (see ATEL # 5416 #5422 #7587 #7799 #7805 #9160). Our observations are carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We strongly encourage further multiwavelength coverage.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Star and stellar system", "Supernova", "Quasar" ] }, "answerKey": "D" }, { "id": "atel_12825", "message": "Title: NICER X-ray observations of the young tidal disruption flare candidate AT2019dsg\nAuthors: Dheeraj Pasham (MIT), Ronald Remillard (MIT), Michael Loewenstein (NASA/GSFC), Keith Gendreau (NASA/GSFC), Zaven Arzoumanian (NASA/GSFC), Jon M. Miller (U. Michigan), Erin Kara (UMD/MIT), James F. Steiner (SAO) on behalf of NICER team\nDate: 31 May 2019; 15:26 UT\nProvenance: Dheeraj Pasham (drreddy@mit.edu)\nSubjects: X-ray, Transient, Tidal Disruption Event\nDescription: Referred to by ATel #: 12960\nFollowing the detection of X-rays with Swift/XRT (ATel #12777), NICER made several exposures of the tidal disruption flare (TDF) candidate AT2019dsg between 2019 May 21 (MJD 58624) and May 28 (MJD 58630), yielding a total exposure near 11 ks. We investigated the average energy spectrum derived from good time intervals with particularly low background (roughly 9.5 ks of exposure) with a variety of spectral models that included thermal and Comptonization components typically used for accreting black holes. \nThe X-ray source is extremely soft, with significant detection limited to the range 0.3-1.0 keV. Fits with a simple accretion disk model (\"ezdisk\") modified by interstellar absorption, i.e., tbabs*zashift(ezdisk) in XSPEC, produce very good results (i.e., no Comptonization term is needed), with reduced chi squared values close to unity. The spectral fits yield an absorption column density of 8.8(+-0.7)e20 cm**-2. This value is slightly higher than the Galactic column of 6.5e20 cm**-2 along the line of sight of AT2019dsg. The inner disk temperature was 0.072+-0.002 keV, and is similar to the best-fit value of 0.06+-0.01 keV from an earlier, lower signal-to-noise, spectrum obtained with Swift/XRT (ATel #12777). The implied unabsorbed X-ray (0.3-1.0 keV) flux is 5.3(+0.5,-0.4)E-12 erg/s/cm**2 which translates to a luminosity of 3(+-0.3)e44 erg/s in 0.1-10 keV band in source frame. Using models with zero torque at the inner boundary for the disk, i.e., the ezdiskbb (Zimmerman et al. 2005) and the diskpn models (Gierlinski et al. 1999) with inner disk radius fixed at 6 gravitational radii, resulted in similar absorbing column and disk temperatures. The best-fit normalization value for diskpn was 1.28(+0.4, -0.3). \nWith a pure blackbody model (tbabs*zashift(bbodyrad) in XSPEC) we obtain fits of equally good quality. The best-fit absorbing column, temperature of the blackbody, and the size of the X-ray photosphere are 7.5(+-0.7)e20 cm**-2, 0.066(+0.001,-0.002) keV, and 6.8(+0.9,-0.7)e11 cm, respectively. The best-fit unabsorbed flux in the 0.3-1.0 keV band and the 0.1-10 keV luminosity are 4.4(+0.4,-0.4)e-12 erg/s/cm**2 and 1(+0.16,-0.12)e44, respectively. The best-fit photospheric radius corresponds to the innermost stable circular orbit of a 8e5 solar mass non-spinning black hole. \nThe X-ray detections and extremely soft spectra with a luminosity of ~1e44 erg/sec are consistent with the TDF classification that is favored for this source. \nWe have requested additional Swift (XRT+UVOT) monitoring and more NICER observations are planned. We encourage follow-up observations of this rare X-ray (and also radio; ATel #12798) bright TDF candidate. \nNICER is a 0.2-12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Globular cluster", "Active galactic nucleus", "Star and stellar system" ] }, "answerKey": "A" }, { "id": "atel_12930", "message": "Title: MASTER OT J191229.11+595229.0 second historical outburst\nAuthors: A. Pozdnyakov, V. Lipunov (Lomonosov MSU), R. Rebolo, M. Serra (IAC), E. Gorbovskoy, V. Kornilov, N. Tiurina, T. Pogrosheva, A. Kuznetsov, O. Gress, I. Gorbunov, P. Balanutsa, V. Vladimirov, D. Zimnukhov, F. Balakin, V. Senik (Lomonosov MSU), N. M. Budnev, O. Ershova (API ISU), A. Tlatov, D. Dormidontov (KSS of the Pulkovo Observatory), D. Buckley (SAAO), R. Podesta, C. Lopez, C. Francile, F. Podesta (OAFA, SJNU), H. Levato (ICATE, SJNU),V. Yurkov, A. Gabovich, Yu. Sergienko, (BSPU), V. Shumkov\nDate: 12 Jul 2019; 15:43 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Request for Observations, Cataclysmic Variable, Transient, Variables\nDescription: MASTER OT J191229.11+595229.0 - outburst with ampl>4.9 \nMASTER-IAC auto-detection system ( Lipunov et al., \"MASTER Global Robotic Net\", Advances in Astronomy, 2010, 30L ) \nfound OT source at (RA, Dec) = 19h 12m 29.11s +59d 52m 29.0s on 2019-07-12.11793 UT. \nThe OT unfiltered magnitude is 17.1m (limit 19.4m). The OT is seen in 2 survey images. There is no minor planet at this place. \nPrevious outburst was in Feb 2012 (MASTER-Kislovodsk discovery) and no OT detection during surveys in MASTER-IAC, -Kislovodsk, -Tunka, -Amur , -Tavrida during 7 last years and in 2009-2012 \nThe nearest in time image without OT was on 2019-06-15 03:16:01UT with mlim=19.4. \nThis outburst is second historical, ampl>4.9m (22m POSS limit in past) \nSpectral observations are required. \nThe discovery and reference images are available at: \nhttp://master.sai.msu.ru/static/OT/MASTEROTJ191229.11+595229.0.png \nMASTER Global Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Black hole", "Galaxy", "Globular cluster" ] }, "answerKey": "A" }, { "id": "atel_12990", "message": "Title: Continuing spectroscopic observations of the SMC classical nova ASASSN-19qv\nAuthors: Terry C. Bohlsen (ARAS group; Mirranook, Armidale, NSW Australia)\nDate: 5 Aug 2019; 21:03 UT\nProvenance: S. N. Shore (shore@df.unipi.it)\nSubjects: Optical, Nova\nDescription: We report the results of our continuing optical low resolution spectroscopic monitoring of the SMC nova ASASSN-19qv (see ATel #12917, #12938). All spectra were flux calibrated with exposure times of 3100 to 3670 sec and S/N ranging from a low of about 10 to 30 (peak line fluxes). Spectra were obtained from 2019 Jul 13.5 - Aug. 3.5 UT. Integrated fluxes (1E-11 erg/s/cm^2; no reddening correction; 4000-7000A) were Jul 13.5, 9.8; 14,5, 8.4; 17.5, 6.8; 19.5, 5.0; 25.5, 3.5;28.5, 2.4, Aug 3.5, 3.6 (uncertainties approx. 0.2). It appears that the last observation caught a brightening of the nova, consistent with our simultaneous photometric monitoring. Absorption was present on all Balmer lines until Jul 28, when it disappeared; the emission wings extended to 2000 km/s (HWZI), while during the transition to optically thin the absorption radial velocity varied slightly, from -2400 km/s to -2000 km/s. Fe II was dominant in the emission lines (although always far weaker than the Balmer lines), with e.g., Fe II 4921, 5018, and 5169, 4549, 4629 A being detectable; Fe II 4630 A -- that first appeared on Jul 19, -- was about half the integrated flux of Hbeta in the last spectrum. He I 5876A may have been present (based on coincidence of high velocity absorption with Hbeta, -2200 km/s) on Jul. 14 and Jul 19 but the S/N is too low to say much about its persistence; He I 6678 was not detected at all, and the spectra ae generally too noisy to reveal other transitions such as Si II 6347. No [O I] 6300A was detected. The nova, despite its high expansion velocities, seems to still be very opaque. Its brightness is now below the limit of our monitoring. \nARAS Nova Database", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova, Galaxy", "Nova, Magnetar", "Galaxy, Variable star", "Nova, Variable star" ] }, "answerKey": "D" }, { "id": "atel_13050", "message": "Title: Swift X-ray detection during the optical peak of the recurrent nova V3890 Sgr\nAuthors: K. V. Sokolovsky (MSU), M. Orio (INAF Padova and University of Wisconsin-Madison), K. L. Page, A. Beardmore, J. P. Osborne (U. Leicester), P. Kuin (MSSL/UCL), J. Leahy-McGregor, E. Aydi, L. Chomiuk, A. Kawash, J. Strader (MSU), J. D. Linford (NRAO), M. Rupen (NRC HAA)\nDate: 29 Aug 2019; 18:12 UT\nProvenance: Kirill Sokolovsky (kirx@scan.sai.msu.ru)\nSubjects: Optical, Ultra-Violet, X-ray, Nova\nDescription: Referred to by ATel #: 13060, 13062, 13069, 13081, 13083, 13084, 13088, 13099, 13114, 13137, 13185\nThe 2019 eruption of the symbiotic recurrent nova V3890 Sgr was discovered by A. Pereira on 2019-08-27.87 UT and confirmed by many observers (ATel #13047; previous eruptions: 1962-06-02 and 1990-04-27, Schaefer 2010, ApJS, 187, 275). The latest pre-outburst observation was performed by R. Stubbings on 2019-08-27.521, who visually estimated the object brightness as 15.2mag (vsnet-alert 23507, AAVSO Alert Notice 677). \nSwift observed V3890 Sgr for 2 ks on 2019-08-28.438. Swift/XRT detected an X-ray source with the net count rate of 1.85 +/-0.03 cts/s (grade 0 events) at the position of the nova. The XRT was operating in Windowed Timing mode to avoid optical loading. The nova spectrum can be fitted with a heavily absorbed thermal plasma with kT = 7.9 +2.3/-1.6 keV and n_HI = (3.4 +/-0.3) x10^22 cm^-2. The Fe emission feature with EW ~ 1 keV is clearly visible at 6.67 +0.07/-0.06 keV. The feature can be reproduced by the APEC plasma emission model if the Fe abundance (by number) is increased by a factor of 3 with respect to the solar value. The unabsorbed 0.3-10 keV flux is 1.8x10^-10 ergs/cm^2/s. The ultraviolet count rate is too high for Swift/UVOT allowing us to place only a lower limit on the nova brightness: UVW1 < 8.6. \nOptical photometry of the nova was performed with the 0.6m telescope of the MSU Campus Observatory (MPC code 766). \n \n \n JD(UT) Band mag err \n 2458723.5492 V 7.36 0.01 \n 2458723.5514 B 7.99 0.01 \n 2458723.5528 I 6.68 0.02 \n 2458723.5536 R 6.76 0.01 \n 2458723.6188 V 7.17 0.01 \n 2458723.6204 B 7.78 0.01 \n 2458723.6216 R 6.58 0.01 \n 2458723.6222 I 6.44 0.01 \n 2458723.6516 V 7.28 0.01 \n 2458723.6529 B 7.91 0.01 \n 2458723.6540 R 6.65 0.02 \n 2458723.6546 I 6.51 0.02 \n 2458723.6734 V 7.41 0.01 \n 2458723.6746 B 8.01 0.01 \n 2458723.6758 R 6.76 0.03 \n 2458723.6764 I 6.60 0.02 \n \nThe lightcurve suggests that the nova had peaked at V=7.17 on 2019-08-28.1188. We adopted the following magnitudes for the comparison star HD 170434 B=8.566, V=8.255, R=8.070, I=8.312 (taken or color-transformed from APASS). \nV3890 Sgr is one of 4 known symbiotic (red giant donor) recurrent novae, along with T CrB, RS Oph, and V745 Sco. The 2014 eruption of V745 Sco (Page et al. 2015, MNRAS, 454, 3108) and the 2006 eruption of RS Oph (Bode et al. 2006, ApJ, 652, 629) were followed with Swift providing a direct comparison. In both novae, the hard thermal X-ray emission was detected in the first days of the outburst. The emission was attributed to the shock-heated plasma produced by the nova blast wave propagating in the red giant wind. \nWe encourage a continued high cadence monitoring of V3890 Sgr at all wavelengths. \nWe thank the Neil Gehrels Swift Observatory team and PI, Brad Cenko, for rapid scheduling of this ToO observation.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium, Binary system", "Nova, Stellar evolution", "Nova, Binary system", "Pulsar, Binary system" ] }, "answerKey": "C" }, { "id": "atel_13125", "message": "Title: A candidate supernova coincident with IceCube-190922B from ZTF\nAuthors: Robert Stein (DESY), Anna Franckowiak (DESY), Marek Kowalski (DESY), Mansi Kasliwal (Caltech)\nDate: 23 Sep 2019; 20:34 UT\nProvenance: Anna Franckowiak (anna.franckowiak@desy.de)\nSubjects: Optical, Neutrinos, Request for Observations, Supernovae, Transient\nDescription: Referred to by ATel #: 13133\nOn behalf of the Zwicky Transient Facility (ZTF) and Global Relay of Observatories Watching Transients Happen (GROWTH) collaborations: \n \nWe observed the localization region of the neutrino event IceCube-190922B (Blaufuss et. al, GCN #25806) with the Palomar 48-inch telescope, equipped with the 47 square degree ZTF camera (Bellm et al. 2019, Graham et al. 2019). We started obtaining target-of-opportunity observations in the g-band and r-band beginning at 2019-09-23 07:03:11.900 UTC, approximately 8.0 hours after event time. Excluding chip gaps, we covered the entire reported 90.0% probability region. Each exposure was 300s with a typical depth of 21.0 mag. \n \nThe images were processed in real-time through the ZTF reduction and image subtraction pipelines at IPAC to search for potential counterparts (Masci et al. 2019). AMPEL (Nordin et al. 2019) was used to search the alerts database for candidates. We rejected stellar sources (Tachibana and Miller 2018) and moving objects, applied machine learning algorithms (Mahabal et al. 2019) and rejected candidates with a history of variability. We were left with one candidate identified by our pipeline in spatial coincidence with the neutrino localisation. \n \nZTF Name | IAU Name | RA (deg) | DEC (deg) | Filter | Mag | MagErr \n---|---|---|---|---|---|--- \nZTF19abxtupj | AT2019pqh | 6.617881 | -1.131493 | r | 21.07 | 0.15 \n \nZTF19abxtupj, previously reported to the TNS as AT 2019pqh, was first detected by ZTF on 2019-09-04. It appears to have peaked on 2019-09-07 and subsequently declined. Given the host spectroscopic redshift of z=0.1334 as reported to the TNS, the absolute magnitude at peak was approximately -18.7 mag in r-band, consistent with expectations for a supernova. The arrival of a neutrino roughly 16 days after peak is also consistent with a supernova CSM-interaction model for neutrino production. \n \nWe strongly encourage spectroscopic observations to discern the nature of ZTF19abxtupj/AT2019pqh, and to rule out a classification as a type-Ia supernova. \n \nAdditional target-of-opportunity observations of the localisation region of IceCube-190922B will continue, in addition to serendipitous observations as part of the regular survey operations. \n \nZTF and GROWTH are worldwide collaborations comprising Caltech, USA; IPAC, USA, WIS, Israel; OKC, Sweden; JSI/UMd, USA; U Washington, USA; DESY, Germany; MOST, Taiwan; UW Milwaukee, USA; LANL USA; Tokyo Tech, Japan; IITB, India; IIA, India; LJMU, UK; TTU, USA; SDSU, USA and USyd, Australia.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy", "Neutron star", "Supernova", "Star and stellar system" ] }, "answerKey": "C" }, { "id": "atel_13225", "message": "Title: ASASSN-19xw is a large amplitude dwarf nova now showing superhumps\nAuthors: Christopher Lloyd (University of Sussex), Tonny Vanmunster (CBA Belgium Observatory)\nDate: 24 Oct 2019; 10:23 UT\nProvenance: Christopher Lloyd (c.lloyd@sussex.ac.uk)\nSubjects: Optical, Nova, Transient\nDescription: We report further photometry of the large-amplitude optical transient AT 2019rki = ASASSN-19xw which now shows a modulation with a full amplitude of 0.m28 and a period of 0.d057\\. \nThe transient was first reported by Stanek and Kochanek, 2019 on behalf of the ASAS-SN team (see Shappee et al., 2014) at Sloan-g magnitude 14.9 on 2019-09-29.2 UT (JD=2458755.7). For the following 14 days until 2019-10-13 it declined smoothly in the manner of a classical nova with no significant modulation (see Lloyd and Vanmunster, 2019, ATel #13180). \nNew unfiltered time series runs were made on three nights with the 0.40-m telescopes of the CBA Belgium and Extremadura (Spain) Observatories on 2019-10-17/18, 18/19 and 20/21. The new time-series data show that the slow decline seen previously has become more erratic. They also show a clear modulation with a full amplitude of 0.m28 and a period of 0.d057±0.02, which are interpreted as superhumps. \nThe outburst amplitude is at least 8 magnitudes (ATel #13180) and a recent spectrum shows that the system is not a nova but a dwarf nova in outburst (Kawash, 2019). With the photometric modulation the object can now be confirmed as a new large-amplitude SU UMa or WZ Sge-type system. \nFurther observations are encouraged particularly monitoring for possible rebrightenings. As of 2019-10-21 the system has g ~ 17.0.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Variable star", "Active galactic nucleus", "Galaxy" ] }, "answerKey": "B" }, { "id": "atel_13275", "message": "Title: ATCA radio detection of the new X-ray transient MAXI J0637-430\nAuthors: T. D. Russell (UvA), J. C. A. Miller-Jones (ICRAR/Curtin), G. R. Sivakoff (UAlberta), A. J. Tetarenko (EAO)\nDate: 7 Nov 2019; 03:11 UT\nProvenance: Thomas Russell (t.d.russell@uva.nl)\nSubjects: Radio, Black Hole, Neutron Star, Transient\nDescription: Referred to by ATel #: 13296\nFollowing the discovery of the new X-ray transient MAXI J0637-430 (ATels #13256, #13257, #13260) we observed the field with the Australia Telescope Compact Array (ATCA) on 2019-11-06 between 17:23 UT and 19:55 UT (MJD 58793.78 +/- 0.05). Observations were recorded simultaneously at central frequencies of 5.5 and 9 GHz, with 2 GHz of bandwidth at each frequency. Primary bandpass and flux calibration was done using PKS 0823-500, while PKS 0629-418 was used for secondary phase calibration. The telescope was in its 750m configuration, although its isolated 6km antenna was used for this analysis. Data were edited for RFI, calibrated, and imaged following standard procedures within CASA (v5.1; McMullin et al. 2007). Imaging was carried out with a Briggs robust parameter of 0 to balance sensitivity and resolution, which provided synthesised beams of 9\"x1\" and 6\"x0.6\" at 5.5 and 9 GHz, respectively, with a position angle of 10 degrees E of N for both frequencies. \nWe detected a radio source coincident with the Swift/XRT position (ATel #13257). Fitting for a point source in the image plane, we measure flux densities of 66 +/- 15 μJy at 5.5 GHz and 60 +/- 10 μJy at 9 GHz. The radio emission implies a spectral index of α = -0.2 +/- 0.8 (where Sν ∝ να). Therefore, our radio detection does not discriminate between emission from a compact jet (where α ≥0), or from a discrete ejection event in a transient jet (where α ∼ -0.7). \nWe measure a 9 GHz radio position of: R.A. (J2000): 06:36:23.7 +/- 0.2\" Dec. (J2000): -42:52:04.1 +/- 0.7\", where the R.A. and Dec. errors are statistical and systematic errors added in quadrature. While our radio source position is within the errors of the reported Swift/XRT position (1.2\" away), due to the uncertain nature of the radio emission, our measured position may not indicate the true source position as transient ejecta can be detected several arcseconds away from their origin. \nOur radio flux densities translate to a 5 GHz radio luminosity of ∼7E27 (D/4kpc)2 erg s-1 (Lr = 4 π d2 ν Sν). The closest in-time reported X-ray observation of MAXI J0637-430 was taken by NuSTAR on 2019-11-05 between about 14:30 and 17:30 UT, providing a 2-10 keV X-ray luminosity of ∼3.6E36 (D/4kpc)2 erg s-1 (ATel #13270). The X-ray spectrum at this time (about 1 day prior to our radio observation) is soft and the rough X-ray timing characteristics are consistent with soft-state accretion around a black hole (ATel #13270). While we are unable to determine the nature of the radio jet and, therefore, cannot use the radio/X-ray plane to classify the source, from the brightness of the radio and X-ray emission MAXI J0637-430 may either be a black hole X-ray binary in a soft state (where the radio emission arises from a discrete ejection event), or a relatively radio-faint (X-ray bright) neutron star system. However, the soft X-ray state indicated by the earlier X-ray observations (ATel #13256, #13257) favour the former. \nWe thank Jamie Stevens and ATCA staff for rapidly scheduling these observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova, Black hole", "Binary system, Black hole", "Accreting object, Black hole", "Accreting object, Star and stellar system" ] }, "answerKey": "C" }, { "id": "atel_13375", "message": "Title: Spectroscopic Observations of AT 2019yvr with SOAR\nAuthors: G. Dimitriadis, R. J. Foley, M. R. Siebert, C. D. Kilpatrick (UCSC), H. T. Corbett (UNC)\nDate: 29 Dec 2019; 10:38 UT\nProvenance: Georgios Dimitriadis (gdimitri@ucsc.edu)\nSubjects: Optical, Supernovae\nDescription: We report the classification of AT 2019yvr (ATLAS19benc) from spectroscopic observations with the Goodman spectrograph on the Southern Astrophysical Research (SOAR) telescope. The target was supplied by ATLAS. The observation was made on 2019 December 29 UT. The classification was performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). \n \n \n Name | IAU Name | RA (J2000) | Dec (J2000) | z | Type | Phase | Notes \n \n ATLAS19benc | AT2019yvr | 12:45:08.13 | -00:27:32.66 | 0.005 | Ib | -5 d | (1) \n \nNotes: When the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. (1) Good fits with many SNe Ib spectra, particularly with SN 2005bf, a few days before maximum light. \nWe thank the SOAR staff and the director, Jay Elias, for helping with this target-of-opportunity observation.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Circumstellar disk", "Minor body", "Accreting object" ] }, "answerKey": "A" }, { "id": "atel_13425", "message": "Title: Independent Discovery of a Probable Nova in M31\nAuthors: H. Kucakova, K. Hornoch (Astronomical Institute, Ondrejov, Czech Republic)\nDate: 28 Jan 2020; 22:20 UT\nProvenance: Allen W. Shafter (ashafter@sdsu.edu)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 13430\nWe report the independent discovery of a probable nova in M31 on a co-added 1530-s R-band CCD frame taken on 2020 Jan. 28.706 UT with the 0.65-m telescope at Ondrejov. \nThe object was independently discovered and first announced by M. Zhang and X. Gao and designated as PNV J00425232+4116128 = AT 2020ber. The object was designated by us as M31N 2020-01b and is located at R.A. = 0h42m52s.36, Decl. = +41o16'13\".0 (equinox 2000.0), which is 90.6\" east and 4.5\" north of the center of M31 (see link to discovery image below). \nThe following R-band magnitudes were obtained using the 0.65-m telescope at Ondrejov: \n2020 Jan. 27.725 UT, [19.2; 28.706, 17.5 ± 0.15; 28.734, 17.4 ± 0.15; 28.750, 17.5 ± 0.15. \nDiscovery image", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Nova", "Quasar", "Active galactic nucleus" ] }, "answerKey": "B" }, { "id": "atel_13475", "message": "Title: Monitoring of the giant flare of Cygnus X-3 with the Sardinia Radio Telescope\nAuthors: E. Egron, A. Pellizzoni, D. Perrodin, M. Pilia, M. Bachetti, M. Pili, L. Schirru (INAF-OAC), N. Iacolina (ASI)\nDate: 13 Feb 2020; 22:48 UT\nProvenance: Elise Egron (elise.egron@inaf.it)\nSubjects: Radio, Binary, Black Hole, Transient\nDescription: The daily monitoring performed with the RATAN-600 detected a new quenched radio state (< 5 mJy 4.7 GHz) of the microquasar Cyg X-3 on 16 January 2020 (MJD 58864). The very low radio emission was associated with an hyper-soft X-ray state (< 0.006 counts/cm^2/s from Swift/BAT, 15-50 keV). \n \nAfter a small rise of flux (< 1 Jy) during two events, the radio flux suddenly increased in a significantly way on MJD 58886 (7 February 2020) from 1 Jy to 10 Jy at 4.7 GHz within a day. This intense and quick increase marked the beginning of a new giant radio flare (Trushkin et al. in ATel #13461), which is also associated with a gamma-flare detected by AGILE on MJD 58884-58886 (Piano et al. in ATel #13458). \n \nWe triggered a daily monitoring program with the Sardinia Radio Telescope (SRT; 64-m dish) at 7.2 GHz and 24.7 GHz in order to follow the evolution of the giant flare. A first peak (11.0+/-0.5 Jy at 7.2 GHz and 8.7 +/-0.9 Jy at 24.7 GHz) was reached on MJD 58888 (9 February), then an even brighter second peak (15.0+/-0.7 Jy at 7.2 GHz and 8.7 +/-0.9 Jy at 24.7 GHz) two days later, on MJD 58890. \n \nThe radio flux is now slowly decreasing (10.8+/-0.5 Jy at 7.2 GHz and 5.5 +/-0.6 Jy at 24.7 GHz) while the hard X-ray flux (Swift/BAT) is increasing (0.024 counts/cm^2/s on MJD 58891: http://swift.gsfc.nasa.gov/results/transients/CygX-3/ ). \n \nWe thank E. Molinari and S. Poppi for allowing us to promptly trigger the observations.\nSRT light curves of Cyg X-3 at 7.2 GHz and 24.7 GHz", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Accreting object", "Minor body", "Binary system" ] }, "answerKey": "C" }, { "id": "atel_13550", "message": "Title: LJT Spectroscopic Classification of AT2020ekk as a young Type II Supernova\nAuthors: Jujia Zhang(YNAO) and Xiaofeng Wang(THU)\nDate: 13 Mar 2020; 03:52 UT\nProvenance: Ju-Jia Zhang (jujia@ynao.ac.cn)\nSubjects: Optical, Supernovae\nDescription: We report an optical spectrum (range 350-870nm) of AT2020ekk, discovered by Koichi Itagaki, that was obtained on UT Mar. 12.85 2020 with the 2.4-m telescope (+YFOSC) at LiJiang Observatory of Yunnan Observatories. This spectrum is quite blue and nearly featureless. A broad emission around 464 nm might be contributed by the NV 461 nm and He II 468.6 nm. A series of narrow and weak H Balmer lines are seen also. These features consistent with a young type II supernova at the flash spectroscopic phase.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Magnetar", "Supernova", "Minor body" ] }, "answerKey": "C" }, { "id": "atel_13600", "message": "Title: Ground-based spectroscopic monitoring of the 2020 periastron in eta Carinae\nAuthors: Felipe Navarete (IAG/USP), Augusto Damineli (IAG/USP), Noel Richardson (ERAU), Nour Ibrahim (ERAU), Bernard Heathcote (SASER), Giorgio Di Scala (SASER), Ken Harrison (SASER), Lidia Di Scala (SASER), Mark Johnston (SASER), Padric McGee (SASER/Adelaide Uni.), Paulo Cacella (SASER), Terry Bohlsen (SASER), Markus Rabus (LCOGT), Tim Brown (LCOGT)\nDate: 30 Mar 2020; 16:17 UT\nProvenance: Felipe Navarete (navarete@usp.br)\nSubjects: Optical, Binary, Star, Variables\nDescription: Referred to by ATel #: 13639\nBased on a high signal-to-noise and high plus intermediate resolution (R=100,000 and R>6,000) ground-based monitoring of eta Carinae periastron (ATEL #13508), we report the following results:\nRepresentative lines of the extended primary's photosphere, (H-δ and SiIIλ6347A) indicate no significant changes as compared to the 2014.5 (Teodoro et al. 2016, ApJ 819, 131). \nThe HeIIλ4686A light curve, produced by the wind-wind collision and the borehole, exhibited an increase in the main peak (P2), similar to what was reported by Teodoro et al. (2016) for the 2014.5 periastron. Major changes occurred in the P3 peak, which was shifted to 9 days earlier (centered on JD=2458916.672) than expected. \nSpectacular changes occurred in the narrow absorption features in the lines H-α (5 times fainter than in 2014.5) and NaD1λ5895.9A (equivalent width reached almost zero levels). These features are centered at RV= -150 km/s, probably in the Little Homunculus. Our guess is that this was caused by the dissipation of the natural coronagraph in front of eta Car, as described in Damineli et al. (2019, MNRAS, 484, 1325). \nThis strongly supports the scenario that the primary star is not evolving significantly in scales of decades, as opposed to dramatic changes in the circumstellar ejecta. \nWe encourage spectroscopic monitoring of these specific spectral lines over the next several months to quantify these expected variations, especially considering that all professional facilities are closed because of the COVID-19 pandemic. This work is sponsored by FAPESP Foundation under projects 2019/02029-2 (AD) and 2017/18191-8 (FN).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system, Repeater", "Star and stellar system, Nova", "Black hole, Variable star", "Star and stellar system, Variable star" ] }, "answerKey": "D" }, { "id": "atel_13675", "message": "Title: A Forest of Bursts from SGR 1935+2154\nAuthors: David M Palmer (LANL) on behalf of the Swift/BAT Team\nDate: 28 Apr 2020; 03:24 UT\nProvenance: David M. Palmer (palmer@lanl.gov)\nSubjects: Soft Gamma-ray Repeater, Magnetar\nDescription: Referred to by ATel #: 13679, 13681, 13682, 13685, 13689, 13713, 13720, 13721, 13723, 13748, 13769, 13773, 13777, 13778, 13783, 13786, 13799, 13816\nAt 18:26:20 of 2020-04-27 UT, the Swift Burst Alert Telescope (BAT) triggered and located a burst from the Soft Gamma Repeater SGR 1935+2154 (Trigger #968211). (GCN #27657; Barthelmy et al.) This burst, and many subsequent bursts described below, continuing to at least T+7 hours (the time of this writing) were also seen by Fermi/GBM (GCN #27659; Fletcher et al.) \nThis initial burst was followed by an intense sequence of bursts starting at ~T+300s after the first trigger time. This includes two separate time segments, 3 seconds and 15 seconds long, made up of rapid sequences of multiple bursts during which the count rate never returns to baseline on the 64 ms timescale (the highest time-resolution data that has been downlinked so far). \nDuring those time intervals, the peak count rate reaches up to 130k counts/s on a 64 ms timescale over the 15-350 keV band, and 350k counts/s on a 1 second timescale over the full detector sensitivity range. (The majority of these additional counts would be below the 15 keV calibrated energy bin but above the Low-Level-Discriminator level. This LLD level varies from detector-to-detector in BAT's 32k-element array, but is typically 12-14 keV. This indicates that the emission spectrum is very steep around those energies.) \nDuring the first 24 minutes of the episode, there were at least 35 clearly-distinguishable bursts outside of the piled-up time intervals. \nThis is similar to the forests of bursts seen 2006-03-29 from SGR 1900+14 (Israel et al, 2008, ApJ 685:1114) and 2008-05-28 from SGR 1627-41. (GCN #7777; Palmer et al.). \nSGR 1935+2154's recent activation was first detected with a burst 5 days earlier, which was seen by multiple spacecraft, providing timing information that identified the location to be this source (GCN #27625; Hurley et al.). The previous BAT detection was 9 bursts in ~24 hours in November 2019. \nNote: a preliminary draft of this ATel was accidentally distributed as GCN #27660. This ATel is the official publication of record.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Interstellar medium", "Nova", "Black hole" ] }, "answerKey": "A" }, { "id": "atel_13725", "message": "Title: Quiescent X-ray observations of Swift J1858.6-0814\nAuthors: A. S. Parikh, R. Wijnands, D. Altamirano\nDate: 10 May 2020; 19:12 UT\nProvenance: Aastha Parikh (A.S.Parikh@uva.nl)\nSubjects: X-ray, Neutron Star, Transient\nDescription: The low-mass X-ray binary Swift J1858.6-0814 has been in outburst since October 2018 (ATel #12151). Observations of type-I X-ray bursts from the source showed that this low-mass X-ray binary hosts a neutron star (ATel #13563).\nWe have been monitoring this source using the X-ray telescope (XRT) on board the Neil Gehrels Swift Observatory since late March 2020. Recent observations demonstrate that the source has been transiting to quiescence. This has also been seen using optical observations obtained by the Las Cumbres Observatory (ATel #13719).\nOur XRT coverage of Swift J1858.6-0814 shows that the source exhibited a count rate of ~0.06 c/s around 8 April 2020, which is a strong decrease as compared to its outburst count rate of ~0.9 c/s on 27 March 2020. Since then the source has continued exhibiting a low flux level.\nOur four most recent XRT observations of Swift J1858.6-0814 (obtained over a time span of ~2 weeks, with the last one obtained on 6 May 2020) exhibited a similar count of ~0.01 c/s. We have extracted a combined spectrum from these observations (obsID: 00010970056-00010970059). Fitting this spectrum with an absorbed power-law model, we find a photon index of Gamma ~2.8+/-0.7 (and the equivalent hydrogen column density was found to be Nh~0.7E22 cm^(-2)). Alternatively, the source spectrum can be fitted with an absorbed black-body or neutron star atmosphere model with temperatures of ~520 eV and ~152 eV, respectively (and corresponding Nh of ~0.1E22 cm^(-2) and ~1.0E22 cm^(-2)). These spectral fits show that the source currently has an X-ray luminosity of ~(2-5)E34 erg/s (0.5-10 keV, unabsorbed, assuming d = 15 kpc; ATel #13563). \nWe have additional XRT coverage approved to monitor the further evolution of the source. In addition, Swift J1858.6-0814 is a promising candidate to probe dense matter physics in neutron star crusts by potentially observing and monitoring the cooling evolution and an accretion-heated neutron star crust. Thus, we have triggered our approved crust cooling proposal (PI Wijnands) and we will obtain our first Chandra observation in the week of 18 May 2020.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy, Accreting object", "Neutron star, Accreting object", "Globular cluster, Accreting object", "Neutron star, Nova" ] }, "answerKey": "B" }, { "id": "atel_13800", "message": "Title: MAXI J0637-430 Not Detected by Swift in X-rays\nAuthors: John A. Tomsick (UCB/SSL) & Hadar Lazar (UCB/SSL)\nDate: 11 Jun 2020; 19:27 UT\nProvenance: John A. Tomsick (jtomsick@ssl.berkeley.edu)\nSubjects: X-ray, Black Hole, Transient\nDescription: Following the report of a decline in the optical bandpass for the black hole candidate X-ray transient MAXI J0637-430 (Johar et al., ATEL#13779), we triggered a Swift X-ray Telescope (XRT) observation, which was carried out on 2020 June 10th. The XRT observation started at 16.0 h UT, and an exposure of 2040 seconds was obtained. The source was not detected, and the 90% confidence upper limit on the 0.5-10 keV flux is <1x10^-13 erg/cm2/s. \nThe previous Swift/XRT observation took place on April 16th, and the energy spectrum is well-described by a power-law. Assuming the low column density of ~3x10^20 cm-2 previously reported for MAXI J0637-430 (Thomas et al., ATEL#13296), we find a power-law photon index of Gamma = 1.7+/-0.3 and a 0.5-10 keV flux of (2.0+0.6-0.4)x10^-12 erg/cm2/s on April 16th (90% confidence errors are given). Thus, like the optical flux, the X-ray flux has dropped dramatically. Specifically, the X-ray flux has dropped by at least a factor of 15-20 in the past 2 months, and MAXI J0637-430 may be at or approaching its quiescent level. We thank the Swift operations teams for support with the execution of these observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Globular cluster", "Black hole", "Repeater", "Stellar evolution" ] }, "answerKey": "B" }, { "id": "atel_13890", "message": "Title: The Disintegration of Comet 249P/LINEAR \nAuthors: Zhong-Yi Lin (IANCU), Wing-Huen Ip (IANCU), Michael S. P. Kelley (U. Maryland), Chi-Sheng Lin (IANCU), Hsiang-Yao Hsiao (IANCU), Wei-Jir Hou(IANCU), Hung-Chin Lin(IANCU)\nDate: 23 Jul 2020; 16:03 UT\nProvenance: Zhong-Yi Lin (zylin@astro.ncu.edu.tw)\nSubjects: Optical, Comet\nDescription: Short period comet 249P/LINEAR might have disintegrated in mid July, 2020, about three weeks after perihelion passage. Comet 249P passed its perihelion on June 29, 2020 and showed a clear condensation (nucleus) on July 5, 2020 as reported by M. Jager. http://www.aerith.net/comet/catalog/0249P/2020-pictures.html However, the images on July 21 and 22 taken by the Lulin 40 cm telescope (SLT) showed that there was no point source at the center according to the ephemeris predicted by MPEC while a tail structure remained. Additionally, the brightness was about 15 magnitude which is several magnitudes fainter than the expected value (S. Yoshida). Unlike comet C/2019 Y4 (ATLAS) (Lin et al. 2020, Atel#13629), no peculiar feature was observed (no fragments), indicating that the nucleus might have possibly completely disintegrated. The SLT images of comet 249P/LINEAR can be found at http://www.astro.ncu.edu.tw/people/zylin/249P.html (North is up, and east is left. FOV is 9.6 x 12.6 arcmin. ) Follow-up observations of comet 249P/LINEAR, both imaging and spectroscopy, are highly recommended to investigate the cause of this cometary splitting event. This work is based on observations made with 40cm telescope at Lulin observatory (MPC code: D35), operated by Institute of Astronomy, NCU, Taiwan. \n249P/LINEAR", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Star and stellar system", "Active galactic nucleus", "Minor body" ] }, "answerKey": "D" }, { "id": "atel_13975", "message": "Title: Spectroscopic identification of ASASSN-20kw = AT 2020scy as a dwarf nova\nAuthors: Kenta Taguchi, Kosuke Namekata, Soshi Okamoto, Naoto Kojiguchi, Keisuke Isogai (Kyoto University), Hiroyuki Maehara (National Astronomical Observatory of Japan)\nDate: 28 Aug 2020; 02:50 UT\nProvenance: Keisuke Isogai (isogai@kusastro.kyoto-u.ac.jp)\nSubjects: Optical, Cataclysmic Variable, Transient, Variables\nDescription: We report on a spectrum of the bright optical transient ASASSN-20kw = AT 2020scy. We obtained the spectrum on 2020-08-27.83 UT by using a fiber-fed integral field spectrograph (KOOLS-IFU; Matsubayashi et al. 2019) mounted on the 3.8-m telescope Seimei at Okayama Observatory of Kyoto University. \n \nAs reported to TNS, this object was discovered at 14.9 mag on 2020-8-27.57 UT by ASAS-SN (Shappee et al. 2014). There is a possible counterpart in the PS1 image but is no photometry data (the limiting magnitude is ~23). \n \nOur spectrum shows weak Balmer absorption lines. Through our performed plain flux calibration, we found that the continuum of this object is blue. These features suggest that this object is a dwarf nova in outburst, not a classical nova. The large amplitude suggests that the object is WZ Sge-type dwarf nova.\nSpectrum", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Variable star", "Magnetar", "Galaxy" ] }, "answerKey": "B" }, { "id": "atel_14100", "message": "Title: INTEGRAL, Swift and SRG/ART-XC joint observation of SRGA J043520.9+552226/AT2019wey\nAuthors: I. Mereminskiy, A. Lutovinov, A. Semena, S. Molkov, (IKI RAS, Russia), E. Kuulkers (ESA/ESTEC, Netherlands), I. Caballero (ESA/ESAC, Spain), I. Lapshov, A. Tkachenko, R. Krivonos, V. Arefiev (IKI RAS, Russia)\nDate: 16 Oct 2020; 14:38 UT\nProvenance: Ilya Mereminskiy (i.a.mereminskiy@gmail.com)\nSubjects: X-ray\nDescription: Referred to by ATel #: 14168, 16418\nOn Oct. 04-06 we performed joint INTEGRAL, SRG/ART-XC and Swift/XRT observations of the X-ray transient source SRGA J043520.9+552226, discovered by SRG/ART-XC as an X-ray counterpart of the AT2019wey source (see ATels #13571, #13932, #13948, #13957, #13976) which is now thought to be the Galactic X-ray binary in the outburst (ATels #13932, #14000, #14003). \nThanks to the long exposure (about 180ks) INTEGRAL/IBIS was able to securely detect the source up to ~120 keV, with a tentative 3-sigma detection in the higher 120-150 keV energy band. The broadband 0.3-150 keV X-ray spectrum could be described with a combination of the multicolor blackbody disk component (kT~0.4 keV) and exponentially cut-off power law (index~1.75, Ecut~200 keV) subject to a mild absorption NH≈2x1021 cm-2. The total flux is 1.4x10-9 ergs/cm2/s in the 0.3-150 keV energy band. \nWe also went through all available data looking for any prominent variability on short timescales, such as eclipses or Type-I bursts. No signs of either were observed. \nThe ART-XC team is grateful for the INTEGRAL ISOC team and the Neil Gehrels Swift Observatory team for scheduling and performing these observations. \nART-XC is an X-ray telescope on board the SRG observatory. The telescope is designed and built by IKI (Russian Academy of Sciences) and RFNC, with the participation from MSFC/NASA. The SRG observatory was launched from the Baikonur cosmodrome on 13 July 2019 by a Proton rocket, now ART-XC performing its second all-sky survey.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Minor body", "Galaxy", "Exoplanet" ] }, "answerKey": "C" }, { "id": "atel_14200", "message": "Title: Fermi-LAT evidence for VHE emission from NVSS J065844+063711\nAuthors: S. Buson (Univ. Wuerzburg), S. Garrappa (DESY-Zeuthen) and C. C. Cheung (Naval Research Laboratory) on behalf of the Fermi Large Area Telescope Collaboration\nDate: 19 Nov 2020; 13:36 UT\nProvenance: Sara Buson (sara.buson@gmail.com)\nSubjects: Gamma Ray, >GeV, VHE, Neutrinos, Request for Observations, Blazar\nDescription: The Fermi-Large Area Telescope (LAT) collaboration reports possible detection of very-high-energy (VHE; E>100 GeV) gamma-ray emission from the active galaxy of uncertain type NVSS J065844+063711 with coordinates R.A. = 104.687375 deg, Decl. = 6.619861 deg (J2000; Condon et al 1998, AJ, 115, 1693). This object is associated with the Fermi-LAT catalogued source 4FGL J0658.6+0636 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), also designated 3FHL J0658.3+0636 (Ajello et al. 2017, ApJS, 232, 18). \nA preliminary analysis of more than 12 years of LAT data (2008-08-04 to 2020-11-14 UTC) has identified several high-energy (HE, >10 GeV) photons positionally consistent with the source and with high probability of being associated with it (>90% probability). On average, the Fermi-LAT has detected one HE photon per year associated with this source. Among those, a 155 GeV photon (>95% probability) was detected on 2018-01-28 07:14:07.976 UTC, providing first evidence of VHE emission from this object. The detection of the VHE event was accompanied by three other HE photons within a ~1-year period. \nThe object NVSS J065844+063711 is listed in the third high-synchrotron peak catalog (3HSP J065845.0+063711; Chang et al. 2019 A&A 632, A77). Its broadband properties resemble those of a high-synchrotron peaked blazar, hence it is a promising VHE emitter. It is the second VHE object found within the 90% confidence region of a well-reconstructed, high-energy IceCube neutrino (i.e., IC201114A; GCN 28887, ATel #14188, GCN 28918). \nBecause Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact persons are S. Buson (sara.buson@gmail.com) and S. Garrappa (simone.garrappa at desy.de). \nThe Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Exoplanet", "Active galactic nucleus", "Quasar", "Circumstellar disk" ] }, "answerKey": "B" }, { "id": "atel_14310", "message": "Title: Enhanced optical activity of the blazar 3C279\nAuthors: S. S.Savchenko, E. G. Larionova, T. G. Grishina, D. A. Morozova\nDate: 11 Jan 2021; 10:35 UT\nProvenance: Sergey Savchenko (savchenko.s.s@gmail.com)\nSubjects: AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 14353\nThe quasar 3C279 shows significant activity at optical wavelengths. According to our observations with the 0.4-m LX-200 with FLI ML4710 (St. Petersburg, Russia) on January 9th, R band magnitude of the quasar reached 13.504 ± 0.005, which appears to be the object's highest state since the middle of 2018 as can be seen at the light curve here. We plan to continue to monitor this object and update the light curve.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar, Neutron star", "Quasar, Circumstellar disk", "Star and stellar system, Active galactic nucleus", "Quasar, Active galactic nucleus" ] }, "answerKey": "D" }, { "id": "atel_14400", "message": "Title: Follow up observations of GX 339-4 with AstroSat\nAuthors: Nazma Husain(Jamia Millia Islamia), Sneha Prakash Mudambi(CHRIST (Deemed to be University)), Akash Garg(Jamia Millia Islamia), Ranjeev Misra(IUCAA), Somasri Sen(Jamia Millia Islamia), Bari Maqbool (Islamic University of Science and Technology)\nDate: 18 Feb 2021; 10:12 UT\nProvenance: Bari Maqbool (bari@iucaa.in)\nSubjects: X-ray, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 14419, 14440, 14455, 14484, 14490, 14493, 14494, 14504, 15615\nA ToO observation was undertaken of the low mass black hole X-ray binary GX 339-4 with AstroSat on 2021-02-13(MJD59258) starting from 00:54:22 to 20:06:01 for about 30 ksecs. This was a follow up to the reports by NICER(Atel#14384), SWIFT(ATel #14351, #14352), MAXI(ATel #14351,#14367), NuSTAR(ATel #14352), INTEGRAL(ATel #14354) and MeerKAT(ATel #14336) indicating an onset of an outburst. The spectra were modeled with disk and Comptonization components along with Gaussian Iron line emission in the energy range 0.5-50.0 keV. The unabsorbed flux was found to vary within 5.64e-9 to 6.52e-9 erg s-1cm-2, while the power-law index changed from 1.53 to 1.59. The inner disc temperature was found to be around KTin ~ 0.25 keV and the absorption column density was estimated to be ~ 0.46e22cm-2. We carried out timing analysis in the energy range 3.0-80.0 keV. The power spectrum showed the presence of a low frequency QPO with r.m.s ~ 6.4% and having a centroid frequency 0.11+0.01-0.01 Hz with width 0.063+0.022-0.033 Hz. Further follow up observations are encouraged. We thank the AstroSat Time Allocation team and operations team for the quick response to the ToO proposal.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Variable star", "Black hole", "Accreting object" ] }, "answerKey": "C" }, { "id": "atel_14500", "message": "Title: Spectroscopic Classification of AT 2021hiz with SOAR\nAuthors: G. Dimitriadis, M. R. Siebert, C. Rojas-Bravo, R. J. Foley (UC Santa Cruz)\nDate: 31 Mar 2021; 21:49 UT\nProvenance: Ryan Foley (foley@ucsc.edu)\nSubjects: Optical, Supernovae\nDescription: Referred to by ATel #: 14595\nWe report the classification of AT 2020hiz from spectroscopic observations with the Goodman spectrograph on the Southern Astrophysical Research (SOAR) telescope, made on 2021 Mar 31 UT. The target was supplied by ALeRCE using the ZTF data stream. The classification was performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). \n \n \n Name | IAU Name | RA (J2000) | Dec (J2000) | z | Type | Phase | Notes \n \n ZTF21aaqytjr | AT2021hiz | 12:25:41.675 | +07:13:42.26 | 0.0033 | Ia | -15d | (1) \n \n \nNotes: \nWhen the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. (1) We measure a Si II velocity of -15,400 km/s and C II velocity of -13,450 km/s. Assuming a distance modulus of 32.07 mag for the host galaxy, IC 3322A (et al., 2013, AJ, 146, 86), Milky Way extinction, and no host extinction, the SN was discovered at M_g ~ -14.4 mag. Young Supernova Experiment observations indicate it rose by 1.2 mag in the g band in the day since discovery. All observations are consistent with a very young Type Ia supernova. \nWe thank the SOAR staff, and in particular Cesar Briceno, for their help with this target-of-opportunity observation.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy", "Magnetar", "Supernova", "Binary system" ] }, "answerKey": "C" }, { "id": "atel_14580", "message": "Title: X-ray detection of the SLSN-I 2020tcw \nAuthors: D. Matthews, R. Margutti, D. Coppejans, G. Terreran, A. Hajela, A. Baldeschi, P. Blanchard, M. Stroh, R. Chornock, W. Jacobson-Galan (Northwestern U.), E. Berger, T. Eftekhari (Harvard U.), M. Nicholl (U. of Birmingham), D. Milisavljevic (Purdue U.), C. Guidorzi (U. degli Studi di Ferrara), B. Metzger (Columbia U.), L. Herzog (Ohio U.), B. Zauderer (NSF), A. MacFadyen (New York U.) \nDate: 27 Apr 2021; 20:52 UT\nProvenance: Raffaella Margutti (rafmargutti@gmail.com)\nSubjects: X-ray, Supernovae\nDescription: We report the first X-ray detection of SN2020tcw with the Chandra X-ray Observatory (CXO) at 60 days post-discovery (program #21500443, PI Margutti). SN2020tcw was discovered on September 12th 2020 (Tonry et al., TNS Astronomical Transient Report No. 81951) and classified as a hydrogen-poor super-luminous supernova (Perley et al., AstroNote 2020-192) at a redshift of z~0.0645 (d~291 Mpc). \nWe observed SN2020tcw on November 10th and 11th 2020 and detected significant X-ray emission at the location of the optical counterpart of the transient. A preliminary reduction yields a 0.3-10 keV absorbed flux of 5.1E-15 erg/s/cm^2 (1 sigma c.l. between 3.5E-15 - 6.9E-15 erg/s/cm^2) assuming a power law spectral model with a photon index of 2. This corresponds to a 0.3-10 keV luminosity of 5.2E+40 erg/s (1 sigma c.l. between 3.5E+40 - 7.0E+40 erg/s). The Galactic neutral hydrogen column density along the line of sight of the transient is 1.57E+20 cm^-2 (Kalberla+ 2005). SN2020tcw was also detected by the VLA on November 15th 2020 with a flux density of 0.2 mJy at 6 GHz (Coppejans et al., AstroNote 2021-73). Extrapolating this result with an optically-thin synchrotron spectrum (assuming a spectral index of beta=1, where Fnu ~ nu^-beta) predicts an X-ray synchrotron component of 4E-17 erg/s/cm^2 (0.3-10 keV). The X-ray emission detected by CXO is in significant excess of this prediction by a factor of ~100 and we thus suggest that, similar to other SNe, the X-ray emission might be powered by bremsstrahlung radiation. Subsequent observations of SN2020tcw in December 2020 revealed no significant X-ray emission to a 0.3-10 keV luminosity upper limit of 1.5E+40 erg/s (3 sigma c.l.). This shows that the X-ray emission has faded, supporting a physical association of the detected X-ray emission with SN2020tcw. Further multi-wavelength observations are planned. We thank the entire CXO team for making these observations possible.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Supernova", "Globular cluster", "Star and stellar system" ] }, "answerKey": "B" }, { "id": "atel_14640", "message": "Title: P200+WaSP observations of Chandra Fast X-ray Transient XRT 210423\nAuthors: Igor Andreoni (Caltech), Kishalay De (Caltech), Mansi Kasliwal (Caltech), Anastasios Tzanidakis (Caltech)\nDate: 18 May 2021; 20:55 UT\nProvenance: Igor Andreoni (igor.andreoni@gmail.com)\nSubjects: Optical, Neutron Star, Transient, Magnetar\nDescription: Referred to by ATel #: 14735\nWe observed the Chandra fast transient XRT 210423 (Lin et al., ATel #14599) with the Wafer-Scale Imager for Prime (WaSP) instrument mounted on the 200-inch Hale Telescope at Palomar Observatory. Observations started on 2021 May 6 at 07:10 UT. We acquired two sets of 6 x 300s exposures, one set in i-band and one in r-band. The data were reduced using the pipeline described in De et al. (2020), PASP, 132, 025001. \nPreliminary analysis does not reveal any high-confidence transient within 1'' radius from the Chandra coordinates. Upper limits (5 sigma) are i>24.8 mag and r>25.2 mag.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Magnetar", "Supernova, Magnetar", "Quasar, Magnetar", "Black hole, Magnetar" ] }, "answerKey": "A" }, { "id": "atel_14700", "message": "Title: Fermi-LAT detection of renewed gamma-ray activity from the FSRQ PKS 1454-354\nAuthors: S. Garrappa (DESY Zeuthen) on behalf of the Fermi Large Area Telescope Collaboration\nDate: 11 Jun 2021; 22:44 UT\nProvenance: Simone Garrappa (simone.garrappa@gmail.com)\nSubjects: Gamma Ray, >GeV, Request for Observations, AGN, Blazar\nDescription: Referred to by ATel #: 14712\nThe Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed renewed gamma-ray flaring activity from a source positionally consistent with the flat-spectrum radio quasar PKS 1454-354, also known as 4FGL J1457.4-3539 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 224.361299 deg, Decl. = -35.652770 deg (J2000; Fey et al. 2006, AJ, 132, 1944), and redshift z=1.424 (Jackson et al. 2002, A&A, 386, 97). \nPreliminary analysis indicates that this source was in an elevated gamma-ray emission state on 10 June 2021, with a daily averaged gamma-ray flux (E>100MeV) of (3.6+/-0.7) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 75 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL-DR2; Ballet et al. 2020, arXiv:2005.11208). The corresponding photon index is 2.04+/-0.14, and is significantly smaller compared to the average value recorded in the 4FGL-DR2 catalog, i.e., 2.32+/-0.02. The current flux is comparable with the one recorded by the LAT during a previous flaring episode in September 2008 (ATel #1701). This source is one of the \"LAT Monitored Sources\" and consequently a preliminary estimation of the daily gamma-ray flux observed by Fermi LAT is publicly available (https://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/PKS_1454-354). \nBecause Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. A Swift ToO proposal has been submitted. We encourage further multifrequency observations of this source. For this source, the Fermi-LAT contact person is M. Marelli (martino.marelli at inaf.it). \nThe Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Star and stellar system", "Minor body, Black hole", "Exoplanet, Black hole", "Active galactic nucleus, Black hole" ] }, "answerKey": "D" }, { "id": "atel_14790", "message": "Title: Possible new LBV eruption of an Ofpe/WN9 star in M33\nAuthors: Andrew Sevrinsky, Nathan Smith (U. Arizona), Jennifer Andrews (Gemini Obs.), Tom Matheson (NOIR Lab), Monika Soraisam (NCSA/UIUC)\nDate: 16 Jul 2021; 01:18 UT\nProvenance: Nathan Smith (nathans@as.arizona.edu)\nSubjects: Optical, Star, Transient, Variables\nDescription: Photometry from ZTF over the past three years shows that the luminous blue variable (LBV) candidate star LGGS J013416.07+303642.1 is brightening slowly, possibly indicating the start of a new LBV-like eruption. If this is an LBV eruption, it would shift this star from a candidate LBV to be the sixth confirmed LBV in M33 (after Var B, Var C, Var 83, Var 2, and MCA-1B). \n \nPrior to 2019, this star had a relatively constant apparent R magnitude of around 17.6-17.8 mag, and like many LBV candidates, was previously classified with a spectral type of Ofpe/WN9 (Neugent & Massey 2011). Available ZTF photometry shows that it has brightened slowly but continuously, by about 0.4 mag in recent years at red wavelengths, from r=17.9 mag in late 2018 to r=17.5 mag in early 2021. This was flagged automatically as a possible transient/variable source (i.e. ZTF20abduida, AT2020aafy) but the transient had not yet been classified or identified as a potential LBV eruption. \n \nM33 is now observable again from the northern hemisphere and we encourage spectroscopic and multicolor photometric observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus", "Magnetar", "Interstellar medium", "Variable star" ] }, "answerKey": "D" }, { "id": "atel_14880", "message": "Title: SOAR spectroscopic classification of Gaia21dyi as a highly reddened classical nova\nAuthors: E. Aydi, K. V. Sokolovsky, A. Kawash, J. Strader, L. Chomiuk (MSU)\nDate: 28 Aug 2021; 09:03 UT\nProvenance: Kirill Sokolovsky (kirx@scan.sai.msu.ru)\nSubjects: Optical, Nova, Transient\nDescription: We report on spectroscopic follow up of the optical transient Gaia21dyi discovered on 2021-08-22.42 UT at a magnitude G = 14.86. Gaia21dyi was suggested to be a reddened classical nova by Taichi Kato [vsnet-alert 26177]. There is also a potential detection of the transient by the All-Sky Automated Survey for SNe (ASAS-SN, Shappee et al. 2014, ApJ, 788, 48) on 2021-08-23.9 at g = 16.93. \nOn 2021-08-28.1 we obtained low- and medium-resolution spectra with the Goodman spectrograph (Clemens et al. 2004, SPIE, 5492, 331) on the 4.1 m SOAR telescope. The spectra show a red continuum with emission lines of Balmer, O I, Na I, N II, He I, and [NII]. Halpha is characterized by a double peaked emission and a P Cygni profile with absorption trough at a blueshifted velocity of around 2300 km/s relative to the line center. The spectrum is that of a highly reddened classical nova, possibly after optical peak. \nWe constrain the coordinates of the nova based on the SOAR images to RA = 17:26:19.382 and Dec = -33:27:10.66 (ICRS), consistent with the Gaia reported position. \nThis ATel is based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministerio da Ciencia, Tecnologia, Inovacoes e Comunicacoes do Brasil (MCTIC/LNA), the U.S. National Science Foundation's National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Pulsar", "Circumstellar disk", "Supernova", "Nova" ] }, "answerKey": "D" }, { "id": "atel_14970", "message": "Title: Spectroscopic classification of AT2021aasl/ZTF21acgumnf\nAuthors: Stephanie Figuereo, Kevin McKinnon, Rafael Nunez, Puragra Guhathakurta (UCSC), Monika Soraisam (NOIRLab), Chien-Hsiu Lee (NOIRLab)\nDate: 14 Oct 2021; 01:51 UT\nProvenance: Monika Soraisam (soraisam@illinois.edu)\nSubjects: Optical, Supernovae, Transient\nDescription: We report the spectroscopic observation of the following transient from the SALVATION project (ATel #13952). It was flagged from the ZTF public alert stream by the ANTARES alert-broker. The spectrum was obtained on 2021 October 13 UT with the Kast double spectrograph on the Shane 3-m telescope at Lick Observatory. \n \n \n Name | IAU Name | RA (J2000) | Dec (J2000) | z | Type | Phase \n ZTF21acgumnf | AT2021aasl | 09h16m21s | +17d43m40s | 0.026 | Ia-91T | post-peak \n Note: \n Classification for the supernova was performed with DASH (Muthukrishna et al. 2019, arXiv:1903.02557). \n Light curve can be accessed at https://antares.noirlab.edu/loci/ANT20215blf2 (ZTF21acgumnf).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Exoplanet", "Supernova", "Black hole", "Binary system" ] }, "answerKey": "B" }, { "id": "atel_15050", "message": "Title: Recurrent nova M31N 2008-12a: Swift/XRT detection of the 2021 eruption\nAuthors: M. J. Darnley (LJMU), K. L. Page (Leicester) on behalf of the 12a Collaboration\nDate: 19 Nov 2021; 14:08 UT\nProvenance: Matt Darnley (M.J.Darnley@ljmu.ac.uk)\nSubjects: X-ray, Nova, Transient\nDescription: Referred to by ATel #: 15068\nThe discovery of the 2021 eruption of the annually recurring recurrent nova M31N 2008-12a was reported in ATel #15034, with spectroscopic confirmation reported in ATel #15036. Upon discovery, we triggered our pre-approved GI programme on the Neil Gehrels Swift Observatory, reporting the Swift/UVOT uvw2 detection in ATel #15040. Follow-up observations have also been reported in ATels #15037, #15038, #15039, and #15045, with observations on-going at many facilities. \nHere we report the emergence of the supersoft X-ray source (SSS) phase of M31N 2008-12a. A faint X-ray counterpart was detected in a 5.6-ks Swift observation between 2021-11-19.064 UT (MJD 59537.064) and 19.277 (MJD 59537.277). \nWe measured the preliminary XRT count rate to be (3.7 ± 1.2) × 10-3 ct/s. Although this detection is only fractionally above 3σ, there is a clear source in the XRT image at the location of M31N 2008-12a, with all detected X-ray photons below 1.5 keV. \nNo X-ray source was detected at a significant level in the preceding 1.9-ks Swift observation on 2021-11-18.5 UT with a 3σ upper limit of 4.9 × 10-3 ct/s (nor in any of the previous daily observations since the detection of this eruption). \nIf we assume an eruption date of 2021-11-14.2 ± 0.2 UT (see ATels #15034 and #15037), then the SSS counterpart appeared around day 5.0 ± 0.2 post-eruption. This preliminary estimate is broadly consistent with the 5.9 ± 0.5 days measured in 2014 (ATel #6558, Henze et al. 2015), the 5.7 ± 0.5 days seen in 2015 (ATel #7984, Darnley et al. 2016), and the 5.8 days observed for the peculiar 2016 eruption (ATel #9872, Henze et al. 2018). However, given the faintness of the detection, this may be the earliest detection yet of SSS emission from this system. \nThe X-ray spectrum at this time is consistent with SSS emission. \nWe wish to thank the Swift Team for the excellent scheduling of the observations, in particular the duty scientists, and the science planners.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Circumstellar disk", "Stellar evolution", "Nova" ] }, "answerKey": "D" }, { "id": "atel_15175", "message": "Title: Spectroscopic classification of SN 2021aau with Gemini-South/GMOS\nAuthors: M. R. Siebert, R. J. Foley (UC Santa Cruz)\nDate: 21 Jan 2022; 19:28 UT\nProvenance: Matthew Siebert (msiebert@ucsc.edu)\nSubjects: Optical, Supernovae, Transient\nDescription: Referred to by ATel #: 15176\nWe report the classification of SN 2021aau with the GMOS spectrograph on the Gemini-South Telescope with GMOS on UT 2022 Jan 21. The target was supplied by DLT40. The classification was performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). \n \n \n Name | IAU Name | RA (J2000) | Dec (J2000) | z | Type | Phase | Notes \n \n DLT22b | AT2021aau | 04:45:41.83 | -59:14:43.87 | 0.004440 | II | peak | (1) \n \n \nNotes: \nWhen the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. \n(1) The red spectrum is consistent with a SN II that suffered significant host-galaxy reddening.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Variable star", "Active galactic nucleus", "Nova" ] }, "answerKey": "A" }, { "id": "atel_15250", "message": "Title: Correction to ATEL #15249 : Filter's name corrected\t\t\t\t \nAuthors: Judhajeet Basu (IIA), Harsh Kumar (IITB), G. C. Anupama (IIA), Sudhanshu Barway (IIA), Vishwajeet Swain (IITB), Varun Balerao (IITB), Jigmat Tstenzin (IIA), Rigzin Norbu (IIA) (on behalf of the GIT team)\nDate: 1 Mar 2022; 05:26 UT\nProvenance: Sudhanshu Barway (sudhanshu.barway@iiap.res.in)\nSubjects: Optical, Nova\nDescription: We report the preliminary magnitudes of the nova AT2022cpe ( https://www.wis-tns.org/object/2022cpe ) in M31 based on observations with the 0.7m GROWTH-India Telescope (GIT). AT2022cpe was serendipitously observed on 16 February while monitoring novae in M31. Luckily, the nova was seen in the field of view (~42 X 42 arcmin) of our observations, and this allowed us to obtain data on AT2022cpe as early as an hour from the time of discovery. AT2022cpe was observed on two more nights. The observations indicate the nova faded at a rate of ~0.5 mag/day in the g' band and ~0.33 mag/day in the r' band. The estimated magnitudes are as below: JD | Filter | Magnitude (AB) +/- Error 2459627.079 | g' | 16.11 +/- 0.02 2459627.097 | r' | 16.01 +/- 0.02 2459627.088 | i' | 16.02 +/- 0.02 2459629.056 | g' | 18.21 +/- 0.07 2459629.060 | r' | 17.34 +/- 0.03 2459629.105 | i' | 17.36 +/- 0.06 2459634.083 | g' | 19.72 +/- 0.12 2459634.091 | r' | 18.33 +/- 0.06 The magnitudes are calibrated against PanSTARRS (Flewelling et al., 2018) and not corrected for Galactic extinction. The GROWTH India Telescope (GIT) is a 70-cm telescope with a 0.7-degree field of view, set up by the Indian Institute of Astrophysics (IIA) and the Indian Institute of Technology Bombay (IITB) with funding from DST-SERB and IUSSTF. It is located at the Indian Astronomical Observatory (Hanle), operated by IIA. We acknowledge funding by the IITB alumni batch of 1994, which partially supports operations of the telescope. Telescope technical details are available at https://sites.google.com/view/growthindia/.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova, Variable star, Magnetar", "Nova, Galaxy, Star and stellar system", "Nova, Variable star, Star and stellar system", "Nova, Variable star, Neutron star" ] }, "answerKey": "C" }, { "id": "atel_15330", "message": "Title: Re-appearance of optical flickering from RS Oph\nAuthors: R. Zamanov, V. Marchev (Bulgarian Academy of Sciences), D. Marchev, T. Atanasova, N. Pavlova (Shumen University)\nDate: 14 Apr 2022; 09:55 UT\nProvenance: R. K. Zamanov (rkz@astro.bas.bg)\nSubjects: Cataclysmic Variable, Nova\nDescription: Referred to by ATel #: 15339, 15387\nWe observed intra-night variability of RS Oph in Sloan g' and r' bands with the 40 cm telescope of the Shumen University \"Episkop Konstantin Preslavski\", Bulgaria (Kjurkchieva et al. 2020, BlgAJ, 32, 113) on 2022 April 14. The field of view was 30x30 arcmin and the resolution was 0.61 arcsec/pixel. For 142 minutes continuous observations, we obtained 152 exposures of 15 sec in g' band, and 160 of 10 sec in r' band. We performed standard aperture photometry with aperture size 3.5 arcsec using 4 comparison stars around RS Oph. \n \nWe do detect optical flickering on minute-to-hour time scale with peak-to-peak amplitude 0.21 mag in g' band and 0.17 mag in r' band (see Fig. 1). \n \nThe latest outburst of the recurrent nova RS Oph occurred in August 2022. The time of the eruption is estimated to be at JD2459435.0 = 2021 Aug 08.50 (Munari & Valisa, 2021, arXiv:2109.01101). The flickering variability disappeared after the 2021 outburst, as a result of the destruction of the accretion disc by nova outburst. The flickering was missing on 24 March 2022 (day 227 of the 2021 outburst; ATel #15296) and is present on 14 April 2022 (day 248). \n \nThese observations indicate re-establishment of accretion between 227 and 248 days after the onset of the 2021 outburst. \n \nAcknowledgements: projects KP-06-H28/2 and RD-08-100/2022. \nOptical flickering of RS Oph observed on 14 April 2022.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Accreting object", "Interstellar medium", "Pulsar" ] }, "answerKey": "A" }, { "id": "atel_15420", "message": "Title: Follow-up Spectroscopy of U Scorpii by the Kyoto-U Seimei Telescope\nAuthors: Kenta Taguchi, Masayuki Yamanaka, Keisuke Isogai (Kyoto University)\nDate: 7 Jun 2022; 16:24 UT\nProvenance: Keisuke Isogai (isogai@kusastro.kyoto-u.ac.jp)\nSubjects: Optical, Cataclysmic Variable, Nova, Transient\nDescription: Referred to by ATel #: 15422, 15423, 15436, 15502, 15508, 15513\nWe performed a follow-up observation of the 2022 outburst of the recurrent nova U Sco discovered by Masayuki Moriyama (vsnet-alert 26798, ATel #15417). We obtained a low-resolution spectrum (R ∼ 500, the wavelength coverage is 4100 -- 8500 Å) from 2022-06-07.4751 UT to 2022-06-07.4802 UT using the fiber-fed integral field spectrograph (KOOLS-IFU; Matsubayashi et al. 2019) mounted on the 3.8 m Seimei telescope (Kurita et al. 2020) at Okayama Observatory of Kyoto University. \nThe Hα emission profile has three peaks around 6503, 6556, and 6634 Å, among which the central one is the brightest. The Hβ emission profile also has three peaks, among which the central and the redder ones are brighter than the bluer one. These profiles are in good agreement with those shown in Figure 2 of Yamanaka et al. (2010). Follow-up observations are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Pulsar", "Star and stellar system", "Nova" ] }, "answerKey": "D" }, { "id": "atel_15480", "message": "Title: ATLAS photometry of 1308+326 shows continued brightening\nAuthors: E. K. Urbach and C. W. Stubbs (Harvard University), L. Denneau, J. Tonry, A. Lawrence. R. Siverd, H. Weiland (IfA, University of Hawaii), K. W. Smith, D. R. Young, S. J. Smartt, (Queen’s University Belfast), L. Shingles (GSI/QUB) N. Erasmus, W. Koorts (South African Astronomical Observatory), J. Anderson (ESO), A. Clocchiatti (PUC), F. Forster (CMM), G. Pignata (MAS), A. Rest (STScI)\nDate: 28 Jun 2022; 19:19 UT\nProvenance: Elana Urbach (eurbach@g.harvard.edu)\nSubjects: Optical, AGN, Blazar\nDescription: Referred to by ATel #: 15483, 15492, 16360\nMultiple reports show an outburst of 1308+326 as recently reaching a record optical brightness (see ATel #15476, ATel #15474, ATel #15459, ATel #15447). Here we present the recent light curve of this object from the ATLAS survey's public photometry server[1]. ATLAS images the sky ~nightly in the custom visible c (420-650 nm) and o (560-820 nm) bands[2], and has imaged 1308+326 over more than 5 years. Data are made immediately available and can be accessed at the link provided below, for both regular and frame-subtraction photometry[1]. \n \nWe compare the magnitude of 1308+326 to reference star C from Smith et al[3], and present evidence of the increase in brightness consistent with previous observations. Comparison star C has mean c-band and o-band AB magnitudes of C_c=13.96 and C_o=13.58, respectively. \n \nTables 1 and 2 present delta-c = c-mag(1380+326) minus C_c and o-mag(1380+326) minus C_o. Prior and subsequent data can be obtained from the ATLAS photometry server[1]. Typical photometric uncertainties per measurement are 0.07 mag. The source continues to increase in brightness. \n \nTable 1: c-band magnitude differences 1380+326 minus star C. MJD| delta-c \n---|--- \n59750.2770| 0.986 \n59750.2989| 1.042 \n59750.3025| 0.974 \n59750.3188| 0.999 \n59753.3208| 0.24 \n59753.3263| 0.265 \n59753.3304| 0.267 \n59753.3442| 0.227 \n59754.3227| -0.167 \n59754.3328| -0.341 \n59754.3383| 0.107 \n59754.3397| 0.091 \n59754.3415| 0.123 \n59754.3429| 0.122 \n59754.3484| 0.116 \n59754.3585| 0.078 \n59757.3376| -0.485 \n59757.3412| -0.600 \n59757.3526| -0.172 \n59757.3590| -0.225 \n59757.3594| -0.179 \n59757.3695| -0.183 \nTable 2: o-band magnitude differences 1380+326 minus star C. MJD| delta-o \n---|--- \n59751.2833| 0.756 \n59751.2888| 0.696 \n59751.3054| 0.728 \n59751.3211| 0.724 \n59752.3156| 0.655 \n59752.3188| 0.623 \n59752.3257| 0.65 \n59752.3377| 0.645 \n59755.3448| 0.03 \n59755.3480| 0.036 \n59755.3535| -0.023 \n59755.3711| 0.009 \n59756.3240| -0.106 \n59756.3277| -0.108 \n59756.3341| -0.097 \n59756.3480| -0.089 \n \n[1] Shingles L. et al. Astronote 2021-7, https://fallingstar-data.com/forcedphot/. \n[2] Tonry J. et al. 2018, PASP, 130:064505. \n[3] Smith et al. 1985, AJ, 90, 1184. \n \nThe Asteroid Terrestrial-impact Last Alert System (ATLAS) project is primarily funded to search for Near-Earth asteroids through NASA grants NN12AR55G, 80NSSC18K0284, and 80NSSC18K1575; byproducts of the NEO search include images and catalogs from the survey area. This work was partially funded by Kepler/K2 grant J1944/80NSSC19K0112 and HST GO-15889, and STFC grants ST/T000198/1 and ST/S006109/1. The ATLAS science products have been made possible through the contributions of the University of Hawaii Institute for Astronomy, the Queen's University Belfast, the Space Telescope Science Institute, the South African Astronomical Observatory, and The Millennium Institute of Astrophysics (MAS), Chile. \nATLAS Public Photometry Server", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Exoplanet, Black hole", "Active galactic nucleus, Black hole", "Magnetar, Black hole", "Active galactic nucleus, Nova" ] }, "answerKey": "B" }, { "id": "atel_15550", "message": "Title: A descriptive title\nAuthors: Amar Deo Chandra (IISER Kolkata)\nDate: 15 Aug 2022; 12:25 UT\nProvenance: Amar Deo Chandra (amar.deo.chandra@gmail.com)\nSubjects: X-ray, Request for Observations, Binary, Neutron Star, Transient, Pulsar\nDescription: The 7.8 s X-ray pulsar XTE J1829-098 (ATel #317) is currently undergoing an X-ray activity having daily averaged 2-20 keV flux from MAXI/GSC data of 0.078 +- 0.015 photons/s/cm^2 (21 +- 4 mCrab) on 2022-08-14 (MJD 59805). The latest daily averaged 15-50 keV flux from Swift/BAT monitoring observations of the source is 0.008 +- 0.002 count/cm^2/s (36 +- 11 mCrab) on 2022-08-14 (MJD 59805). Previous outbursts of the source have been detected in 2004 July-August (ATel #317), 2008 August (ATel #2007), 2009 August (ATel #11927), 2018 August (ATel #11927) and 2021 April (ATel #14521, #14554). The source was found to be active on 2003 March 27 using archival XMM-Newton Galactic Plane Survey observations (ATel #319). The source was also found to be active in 2019 December and 2020 August from MAXI/GSC archival observations (ATel #14554). \n \nThe time duration between successive outbursts was suggested to be ~246 days with outbursts lasting about 7 days (ATel #2007). Using a new ephemeris derived from the MAXI/GSC data spanning a duration of about 11 years (ATel #14554), the beginning of X-ray outbursts can be predicted using T_outburst = MJD 58341.73 + n * (243.66 +- 3.07), where n is the number of orbit since the outburst in 2018 August (ATel #14554). The onset of the current X-ray brightening of XTE J1829-098 around MJD 59794 nicely matches with the prediction of MJD 59803.69 +- 18.42. This suggests that the orbital period of the X-ray binary is indeed about 246 days as suggested earlier (ATel #2007, #14554). \n \nThere are known optical/NIR counterparts for the source (ATel #344; Halpern and Gotthelf, 2007, ApJ, 669, 579), but further IR/optical observations are required to ascertain the type and the class of the companion star. \n \nThe MAXI and Swift light curves of XTE J1829-098 are available at the URLs: http://maxi.riken.jp/star_data/J1829-098/J1829-098.html, https://swift.gsfc.nasa.gov/results/transients/weak/XTEJ1829-098/. \n \nFurther multiwavelength observations of the source are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova, Pulsar", "Star and stellar system, Pulsar", "Neutron star, Interstellar medium", "Neutron star, Pulsar" ] }, "answerKey": "D" }, { "id": "atel_15690", "message": "Title: NICER and NuSTAR observations of SGR 1935+2154 bracketing the time of the bright radio burst\nAuthors: Teruaki Enoto (RIKEN), Chin-Ping Hu (NCUE), Tolga Guver (Istanbul Univ.), George Younes (NASA GSFC/GWU), Keith C. Gendreau, Z. Arzoumanian (NASA GSFC), Zorawar Wadiasingh (UMD, NASA/GSFC), Walid A. Majid (JPL, Caltech), Aaron B. Pearlman (McGill Univ., McGill Space Institute, Caltech), and S. Guillot (IRAP/CNRS)\nDate: 18 Oct 2022; 06:35 UT\nProvenance: Teruaki Enoto (teruaki.enoto@gmail.com)\nSubjects: X-ray, Neutron Star, Soft Gamma-ray Repeater, Magnetar\nDescription: Referred to by ATel #: 15698\nMagnetar SGR 1935+2154, the only known Galactic emitter of fast radio bursts (FRB), entered a burst active state on 2022 October 10 (ATel #15667, GCN 32698, 32706, and 32708). We have continued our high-cadence monitoring campaign of the source with NICER (ATel #15674). We also performed ToO observations with NuSTAR starting from 2022-10-14 02:00 UTC with an exposure totalling 50 ks (NICER Proposal 5076). \nNuSTAR was observing SGR 1935+2154 during the radio burst which occurred on 2022-10-14 at 19:21:47 UTC as reported by the CHIME/FRB collaboration (ATel #15681). Unfortunately, at the arrival time of the burst, the source was Earth-occulted for NuSTAR. The closest on-target good time interval (GTI) ended approximately 12 minutes prior to the radio burst. During the NuSTAR observation, SGR 1935+2154 exhibited a high bursting rate, most notably during the two GTIs prior to the radio burst, starting at 2022-10-14 16:53 and ending on 2022-10-14 19:10. During the span of about 4 ks of livetime, we detect over a hundred bursts, sitting on a bed of enhanced baseline emission. We extracted the NuSTAR hard X-ray persistent spectrum from a few GTIs at the end of the observation which showed the lowest level of bursting activity, after eliminating the burst intervals. The background-subtracted source count rate was 0.3 cps in the 3-70 keV band. We also extracted a burst-free NICER spectrum from data that were simultaneous to NuSTAR. A preliminary analysis of the 1-70 keV broad-band spectrum indicates that it is best fit with an absorbed 2 blackbody and power-law model, \"tbabs * (bbodyrad + bbodyrad + powerlaw)\" in Xspec terminology. We derive an absorption-corrected flux of about 2.0e-11 erg/s/cm2 and 1.0e-11 erg/s/cm2 in the 0.5-10 keV and 10-70 keV ranges, respectively. Through our continued NICER monitoring, we report that SGR 1935+2154 bursting activity has decreased. From the time of the radio burst and up to 2022-10-17, we detected 14 burst candidates with significance above 7 sigma, corresponding to an occurrence rate of 0.7 bursts/ks. Further NICER monitoring is planned, and the schedule can be found on the website (https://heasarc.gsfc.nasa.gov/docs/nicer/schedule/nicer_sts_current.html). Another NuSTAR observation is also planned. Detailed analysis of these observations, including the persistent temporal and spectral evolution of the source, is ongoing. We encourage contemporaneous multiwavelength observations. We are grateful to the NuSTAR and NICER teams for the rapid scheduling of our observations. The Neutron star Interior Composition Explorer (NICER) is a 0.2-12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system", "Quasar", "Magnetar", "Active galactic nucleus" ] }, "answerKey": "C" }, { "id": "atel_15800", "message": "Title: RW Cephei great dimming\nAuthors: Wolfgang Vollmann (AAVSO/BAV, Vienna) and Costantino Sigismondi (ICRANet/AAVSO, ITIS G. Ferraris, Rome)\nDate: 9 Dec 2022; 12:54 UT\nProvenance: Costantino Sigismondi (sigismondi@icra.it)\nSubjects: Optical, Variables\nDescription: RW Cephei is a red hypergiant normally ranging between magnitudes 6.0 and 7.3. From the AAVSO light curves of the star are evident semi-regular fluctuations within the above range, but since 2022 the star is significantly dimming, instead of rebrightening, and reaching already the magnitude V=7.6. The comparison star of the DSLR series of measures from 2020 is HD211982 which is V=7.298. The V magnitude observations of the Kiso/Kyoto Wide Field Survey (KWS) confirm the quick fade in 2022 like AAVSO visual (since 1977, VOL observer code) and DSLR measures made in Vienna with 75 mm lens. This phenomenon undergoing on RW Cep might be similar to the one occurred to the red supergiant Betelgeuse at the end of 2019 (ATel #13341, ATel #13601). (for KWS see Maehara, H. (2014) Automated Wide-Field Survey for Transient Objects with a Small Telescope. Journal of Space Science Informatics Japan, 3, 119-127)\nRW Cephei light curves from 2009 till 2022", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Star and stellar system", "Globular cluster", "Binary system" ] }, "answerKey": "B" }, { "id": "atel_15850", "message": "Title: ZTF detection of the probable nova in M31 2023ax (ZTF23aaaairl)\nAuthors: D. Galan, G. Aznar Menargues, Y. Calatayud-Borras, A. Casasbuenas, M. Cervera Cortes, I. Cortes-Perez, J. del Socorro Prieto, M. Delgado Mancheno, A. Ferrer I Burjachs, R. Flores le Roux, S. Geraldia Gonzalez, P. Grebol-Tomas, S. Navarro Umpierrez, A. Pelaez-Torres, E. Reyes Rodriguez, P. Sosa-Guillen, A. Vielba Trillo (ULL), E. Esparza-Borges, F. Poidevin, and I. Perez-Fournon (IAC and ULL)\nDate: 7 Jan 2023; 17:47 UT\nProvenance: Ismael Perez-Fournon (ipf@iac.es)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 15867\nWe report the ZTF detection (ZTF23aaaairl) of the probable nova in M31 AT 2023ax (XM94MZ, PNV J00430924+4117022), that was discovered and reported to TNS by Zhang et al. (XOSS, http://xjltp.china-vo.org/xm94mz.html ). ZTF detected this source on 2023-01-07 03:18:17 UTC (g = 17.478 +/- 0.040) and 2023-01-07 06:20:25 UTC (r = 17.250 +/- 0.046). The last ZTF non detection was on 2022-12-23 04:43:28 UTC (r > 20.548). The ZTF position based on the first two detections is R.A. = 00:43:09.223, Decl. = 41:17:02.21, that is 53.51\" N, 280.41\" E (1.0 kpc) from the M31 galaxy centre. We encourage photometric and spectroscopic follow-up observations. Based on Zwicky Transient Facility (ZTF, Bellm et al. 2019) observations processed through the Lasair (Smith, Williams, Young et al. 2019), ALeRCE (Forster et al. 2020) and ANTARES (Matheson et al. 2021) brokers. ZTF light curve: https://lasair-ztf.lsst.ac.uk/object/ZTF23aaaairl/ https://alerce.online/object/ZTF23aaaairl https://antares.noirlab.edu/loci/ANT2023hk7fwwy2r59d \nZTF light curve", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Stellar evolution", "Nova", "Galaxy" ] }, "answerKey": "C" }, { "id": "atel_15925", "message": "Title: Fermi-LAT detection of enhanced gamma-ray activity from the blazar PMN J1830-4441\nAuthors: Adithiya Dinesh (UC Madrid), Janeth Valverde (UMBC / NASA GSFC), Simone Garrappa (Ruhr-Universitaet Bochum), on behalf of the Fermi Large Area Telescope Collaboration\nDate: 3 Mar 2023; 17:01 UT\nProvenance: Janeth Valverde (valverde@llr.in2p3.fr)\nSubjects: Gamma Ray, >GeV, Request for Observations, AGN, Blazar\nDescription: The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed enhanced gamma-ray activity from a source positionally consistent with the blazar PMN J1830–4441 (also known as 4FGL J1830.2-4443), with coordinates R.A. = 277.503500 deg, Decl. = -44.686583 deg (J2000; Healey et al. 2007, ApJS, 171, 61). \nPreliminary analysis indicates that this source was in an elevated gamma-ray emission state on 2023 March 1, with a daily averaged gamma-ray flux (E>100MeV) of (0.5+/-0.1) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 20 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL-DR3, Abdollahi, S., et al. for the Fermi-LAT collaboration 2022, ApJS, 260, 53). This is the highest LAT daily flux ever observed for this source. The photon index of 2.1+/-0.2 corresponds to a harder spectrum than the 4FGL-DR3 value of 2.57 +/- 0.04. \nBecause Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. Preliminary Fermi-LAT light curves can be accessed via the Fermi-LAT Light-Curve Repository at https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/source.html?source_name=4FGL_J1830.2-4443. We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is Adithiya Dinesh (adinesh@ucm.es). \nThe Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Circumstellar disk", "Binary system", "Repeater" ] }, "answerKey": "A" }, { "id": "atel_15975", "message": "Title: MAXI/GSC observation of brightest outburst of the Be/X-ray binary pulsar 4U 0115+63 in 27 years\nAuthors: M. Nakajima, H. Negoro (Nihon U.), W. Iwakiri (Chiba U.), K. Kobayashi, M. Tanaka, Y. Soejima (Nihon U.), T. Mihara, T. Kawamuro, S. Yamada, T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, M. Serino, S. Sugita, H. Hiramatsu, H. Nishikawa, A. Yoshida (AGU), Y. Tsuboi, J. Kohara, S. Urabe, S. Nawa, N. Nemoto (Chuo U.), M. Shidatsu, M. Iwasaki (Ehime U.), N. Kawai, M. Niwano, R. Hosokawa, Y. Imai, N. Ito, Y. Takamatsu (Tokyo Tech), S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, T. Kurihara (JAXA), Y. Ueda, S. Ogawa, K. Setoguchi, T. Yoshitake, K. Inaba, Y. Nakatani (Kyoto U.), M. Yamauchi, T. Sato, R. Hatsuda, R. Fukuoka, Y. Hagiwara, Y. Umeki (Miyazaki U.), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC)\nDate: 3 Apr 2023; 14:28 UT\nProvenance: Motoki Nakajima (nakajima.motoki@nihon-u.ac.jp)\nSubjects: X-ray, Binary, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 15978, 15989\nWe report on the latest observation of the ongoing giant outburst source, the Be/X-ray binary pulsar 4U 0115+63 (ATel#15967). The day-averaged 5-12 keV flux has been increasing, and reached 0.673 ± 0.040 photons/s/cm2 (715 ± 43 mCrab) on 2023 April 3 (MJD 60037). This is the brightest state observed by RXTE/ASM and MAXI/GSC in 27 years. In addition, the average flux increase rate between March 31 and April 3 records 130 mCrab/day which is the highest value observed in the 5-12 keV band so far. Further brightening might be expected from the latest scans observed by MAXI/GSC. We strongly encourage multi-wavelength observations to monitor this source. \n \nThe latest X-ray light-curve can be checked at the following pages; \nMAXI ( http://maxi.riken.jp/pubdata/v7lrkn/J0118+637/index.html ), \nSwift/BAT ( https://swift.gsfc.nasa.gov/results/transients/weak/4U0115p634/ ), \nFermi/GBM ( https://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/4u0115.html ), and \nthe BeXRB monitor page ( http://integral.esac.esa.int/bexrbmonitor/Plots/sim_plot_4U0115+63.html ).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus", "Near-Earth object", "Quasar", "Neutron star" ] }, "answerKey": "D" }, { "id": "atel_16025", "message": "Title: MeerKAT radio detection of MAXI J1820-222 following its hard state\nAuthors: Thomas Russell (INAF-IASF Palermo), Andrew Hughes (U. Alberta), Francesco Carotenuto, Rob Fender, Katie Savard (Oxford), Patrick Woudt (U. Cape Town), James Miller-Jones Curtin), on behalf of the ThunderKAT collaboration\nDate: 3 May 2023; 13:54 UT\nProvenance: Thomas Russell (thomas.russell@inaf.it)\nSubjects: Radio, Black Hole, Transient\nDescription: Referred to by ATel #: 16026, 16129\nMAXI J1810-222 is a black hole candidate X-ray binary that has been in outburst since 2018 November (ATel #12254), during which it has shown a number of transitions between the hard and soft X-ray state (Russell et al. 2022). Following recent reports of the source within the hard X-ray spectral state (ATel #16016), we observed MAXI J1810-222 with the MeerKAT radio telescope as part of the ThunderKAT Large Survey Programme (Fender et al. 2017). Observations were carried out at a central frequency of 1.28 GHz, with a total bandwidth of 860 MHz. We used PKS J1939-6342 for flux and bandpass calibration, and J1833-2103 for complex gain calibration. \nMAXI J1810-222 was observed for 15 minutes on 2023-04-30 between 02:37:15 and 02:52:19 UTC (MJD 60064.114 +/- 0.005). We detect radio emission coincident with the known source position. Fitting for a point source in the image plane, we measure a flux density of 330 +/- 20 μJy (at 1.28 GHz). This radio flux density is consistent with previous observations of this source in its hard X-ray state (Russell et al. 2022). \nFurther radio monitoring is planned. Multiwavelength follow-up is encouraged. \nThunderKAT will run for 5 years and targets X-ray binaries, Cataclysmic Variables, Supernovae and Gamma-Ray Bursts. As part of this programme, we perform weekly monitoring observations of all bright, active, southern hemisphere X-ray binaries in the radio band. For further information on this programme please contact Rob Fender and/or Patrick Woudt. \nReferences: Fender et al. 2017, arXiv:1711.04132 Russell et al. 2022, MNRAS, 513, 6196, arXiv:2205.05721", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Repeater", "Stellar evolution", "Black hole" ] }, "answerKey": "D" }, { "id": "atel_16100", "message": "Title: Swift XRT confirms outburst of GRS 1739-278\nAuthors: J. A. Kennea (PSU), A. Bahramian (Curtin) and H. Negoro (Nihon U)\nDate: 28 Jun 2023; 11:57 UT\nProvenance: Jamie A. Kennea (kennea@astro.psu.edu)\nSubjects: X-ray, Black Hole\nDescription: Referred to by ATel #: 16102, 16116\nNegoro et al. (ATEL #16097) report the MAXI detection of a possible new transient, MAXI J1741-276, or new outburst of GRS 1739-278. In response, we performed a Swift Target-of-Opportunity observation of the MAXI error circle, consisting of 4 pointings of 250-300s each, beginning at 18:02UT on June 27, 2023. We find a bright, piled up source at the following UVOT enhanced localization: RA/Dec(J2000) = 265.66723, -27.74793, which is equivalent to: \n \nRA(J2000) = 17h 42m 40.13s, \nDec(J2000) = 27d 44m 52.5s, \nwith an error radius 2.6 arc-seconds (90% confidence). This position is consistent is the source GRS 1739-278, AKA V2606 Oph, lying 1.4 arc-seconds from the catalog position. \nGRS 1739-278 is in outburst, with a Swift/XRT count rate of 56.0 +/- 2.3 count/s. The spectrum is well fit by an absorbed disk blackbody (XSPEC diskbb) model with N_H = (2.3 +/- 0.4) x 10^22 cm^-2, and kT = 0.92 +/- 0.1 keV. Additional power-law component is not required, and the power-law only fit is soft (photon index = 3.4).\nTherefore we report that GRS 1739-278 is source of the MAXI outburst, and that this BH appears to be outbursting in a soft state.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus", "Black hole", "Interstellar medium", "Exoplanet" ] }, "answerKey": "B" }, { "id": "atel_16150", "message": "Title: X-ray brightening of V1716 Sco\nAuthors: K. L. Page (U. Leicester) \nDate: 25 Jul 2023; 13:36 UT\nProvenance: Kim Page (kpa@star.le.ac.uk)\nSubjects: X-ray, Nova\nDescription: Referred to by ATel #: 16155\nThe Neil Gehrels Swift Observatory has been monitoring V1716 Sco (PNV J17224490-4137160; Nova Sco 2023) since the day after its discovery by Pearce on 2023-April-20.678 UT (CBET #5245). \nIn ATel #16069 we reported the appearance of a new, weak soft X-ray component on 2023-05-31, on day 41 after the initial optical discovery. After this time, the X-ray count rate remained close to constant, around 0.037 +/- 0.003 count s-1, until 2023-July-18. The next observation, on 21/22 July, showed a notably stronger soft component, with the X-ray count rate increasing to 0.46 +/- 0.02 count s-1; on 24 July, this has increased further, to 1.59 +/- 0.06 count s-1. All count rates are over 0.3-10 keV, and consider grade 0 (single pixel) events only. Using an atmosphere grid to approximate the temperature of the soft component, we find a consistent temperature for both of these most recent observations, with kT = (7.3 +0.1/-0.2)x10 K (63 +1/-2 eV). \nFurther monitoring by Swift is planned to follow this brightening component. We thank the Swift PI for approving these observations, and the Swift operations team for implementing them.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Nova", "Variable star", "Exoplanet" ] }, "answerKey": "B" }, { "id": "atel_16225", "message": "Title: Near-infrared counterpart and optical evolution of the outburst of Swift J1727.8-1613\nAuthors: M. Cristina Baglio (INAF-OAB), Piergiorgio Casella, Vincenzo Testa, Isabella Mariani (INAF-OAR), David M. Russell (NYU Abu Dhabi), Thomas J. Maccarone (TTU) and Tomaso Belloni (INAF-OAB)\nDate: 2 Sep 2023; 17:46 UT\nProvenance: Maria Cristina Baglio (cristina.baglio@brera.inaf.it)\nSubjects: Infra-Red, Optical, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 16230, 16231, 16237, 16238, 16243, 16245\nSwift J1727.8-1613 (originally GRB 230824A: GCN #34536, #34537) is a recently discovered candidate black hole X-ray binary. The source is undergoing a bright outburst at all wavebands, from X-rays (ATel #16205, #16206, #16207, #16210, #16215, #16217) up to optical (ATel #16208, #16209) frequencies, and also showed bright detections in the radio thanks to VLA observations (ATel #16211). \nWe are monitoring the system daily with the Rapid Eye Mount Telescope (REM; La Silla, Chile) at optical (griz) and near-infrared (H) frequencies. The source is well detected; we performed aperture photometry on the target and we calibrated the fluxes against a group of stars in the field of view with magnitudes tabulated in the APASS (optical gri) and 2MASS (NIR) catalogs. \nHere we report the results of the first observation, performed on 2023 August 29 (MJD 60185.01). We obtain the following optical-NIR calibrated magnitudes: g=12.92+/-0.03 mag (AB), r=12.71 +/- 0.03 (AB), i=12.69+/-0.03 mag (AB), H=11.35+/-0.05 mag (Vega). \nThe optical magnitudes show that the source has brightened with respect to the observations reported in ATel #16208; moreover, the brightening is stronger at lower frequencies (delta_i~0.7 mag, delta_r~0.6 mag, delta_g~0.5 mag), suggesting that the source is becoming redder, possibly due to the onset of a compact jet (also suggested by the recent radio detections, ATel #16211). \nThe monitoring with REM is ongoing. \nFurther multiwavelength observations are strongly encouraged during the current outburst of the source. \nWe remember our colleague and friend Tomaso Belloni, who sadly passed away on 2023 August 26, who made invaluable contributions in the past years to the studies of X-ray transients.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova, Binary system", "Black hole, Interstellar medium", "Black hole, Binary system", "Black hole, Nova" ] }, "answerKey": "C" }, { "id": "atel_16290", "message": "Title: Follow-up of AT2023uri, a probable Nova in M31\nAuthors: Roberto Nesci (INAF/IAPS)\nDate: 14 Oct 2023; 21:29 UT\nProvenance: Roberto Nesci (roberto.nesci@inaf.it)\nSubjects: Optical, Nova\nDescription: Referred to by ATel #: 16293\nPrompted by the ATel #16285, regarding the discovery of a new Nova in M31, I observed the star with the 30cm telescope of the Foligno Observatory (K56) equipped with a QHY174M cooled camera and R_Cousins filter. 15 nearby stars were taken from the UCAC4 catalog as comparisons, using their r_Sloan magnitudes; aperture photometry was made with iraf/apphot. The star was found at r_Sloan=16.67 +/-0.6 on 2023-10-13T22:31 and 16.96 +/-0.07 on 2023-10-14T20:25, suggesting that it has already past the maximum light. Bad weather is predicted for the next days, so further follow-up is unlikely for our Observatory.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Near-Earth object", "Quasar", "Nova" ] }, "answerKey": "D" }, { "id": "atel_16375", "message": "Title: Multi-wavelength follow up observations of SN 2023xrs\nAuthors: Luca Izzo (INAF-OACn & DARK/NBI), James Leung (U. Toronto), Ziteng Wang (ICRAR/Curtin), Katie Auchettl (U. Melbourne), Fabio De Colle (UNAM), Aprajita Hajela (DARK/NBI), Keiichi Maeda (Kyoto U.), Tara Murphy (U. Sydney)\nDate: 11 Dec 2023; 20:40 UT\nProvenance: Luca Izzo (luca.izzo@gmail.com)\nSubjects: Radio, Optical, X-ray, Supernovae\nDescription: We report radio observations of SN 2023xrs (AN 2023-312) conducted with the Australia Telescope Compact Array (ATCA), project code C3448. The observations were conducted from 12:30 to 18:30 UT on 2023 November 23, centered on frequencies 5.5, 9.0, and 16.7 GHz. From preliminary analysis, we report non-detections in all observed bands, with the following 3-sigma upper limits: < 138 micro-Jy/beam at 5.5 GHz, < 165 micro-Jy/beam at 9 GHz, < 582 micro-Jy/beam at 16.7 GHz. \n \nWe have also observed SN 2023xrs with the X-ray Telescope on board the Neil Gehrels Swift observatory (GI prop. 1922064). The observations were conducted along five different epochs, ranging from 2023 November 19 to November 27, with a total exposure time on-source of 9.35 ks. From a preliminary analysis of the stacked X-ray image, we report no X-ray source at the position of SN 2023xrs, with a one-sigma upper limit of 0.0013 ctg/s. Assuming a power-law spectrum with photon index gamma=2, and a Galactic column density of NH = 1.59x10^22 cm^-2 (Kalberla et al. 2005 A&A, 440, 775), we obtain an unabsorbed flux (0.3-10.0 keV) limit of 1.6x10^-13 erg/cm^2/s. \n \nAn optical spectrum of SN 2023xrs has also been obtained with the WiFES spectrograph at the Australian National University 2.3-meter telescope located at Siding Spring (AU). The spectrum consists of a single exposure of 750s in both grisms B3000 and R3000. Observations started on December 8, at 11:14 UT. The spectrum shows typical absorption lines observed in type-Ic SNe, including Fe II, Si II, O I, and Ca II NIR, at an expanding velocity of ~ 12,000 km/s, as measured from Ca II NIR and O I 7775 Ang. Using SNID (Blondin & Tonry 2007 ApJ, 666, 1024), we find a best match with the type-Ic SN 2004aw at 5 days from its peak brightness. \n \nWe thank CSIRO staff for rapidly scheduling, supporting, and executing these observations. We also thank the Neil Gehrels Swift Observatory team for the rapid scheduling of these ToO observations. K.A. would also like to acknowledge Ian Price and Chris Lidman with the ANU 2.3-metre telescope. The automation of the ANU 2.3-meter telescope was made possible through funding provided by the Centre of Gravitational Astrophysics at the Australian National University.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Exoplanet", "Nova", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_16425", "message": "Title: NuSTAR Observation of GX 339-4 in a Bright Hard State\nAuthors: O. K. Adegoke (Caltech), G. Mastroserio (University of Milan), J. A. Garcia (NASA/GSFC & Caltech), J. A. Tomsick (UC Berkeley, SSL), R. M. T. Connors (Villanova), F. Harrison (Caltech)\nDate: 30 Jan 2024; 22:30 UT\nProvenance: Oluwashina Adegoke (oadegoke@caltech.edu)\nSubjects: X-ray, Black Hole, Transient\nDescription: GX 339-4 is a black hole X-ray binary that undergoes an outburst every 1-2 years on average. For the past several weeks, it has showed a steady increase in X-ray activity since the onset of the current outburst (ATel #16260, #16302). Over this time, the radio brightness of GX 339-4 has also been observed to steadily increase based on data from MeerKAT (ATel #16421). Here, we report results from a recent NuSTAR observation of the source, carried out on 2024 January 19 for a duration of ~19 ks. \nAn absorbed (N_H fixed to 6e21 cm^-2) cutoff-powerlaw fit to its 3-79 keV spectra reveals strong relativistic reflection features including the iron K alpha line at ~6.4keV and the Compton hump that peaks around 25keV. The spectrum can be approximated by a model including a Comptonized-disk continuum, relativistic and distant reflection. The powerlaw photon index is 1.71+/-0.01 and the diskbb temperature kT_in is 0.29^{+0.01}_{-0.02} keV. The unabsorbed 3-79 keV flux is ~9 E-9 erg/cm2/s (about 400 mCrab). The power density computed from the timing analysis of the NuSTAR light curve shows a strong QPO at 0.46+/-0.01 Hz and the presence of broadband noise at lower frequencies. The total rms noise level in the 0.01-50 Hz band is 30%. The source appears to be in the bright hard state during this observation.\nSince the 19th of January when this observation was made, the 2-20 keV MAXI light curve of the source has more than doubled and it has been confirmed to have transitioned from the hard state a few days after the NuSTAR observation (ATel #16424). Further multi-wavelength observations are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution, Accreting object", "Black hole, Variable star", "Black hole, Accreting object", "Black hole, Pulsar" ] }, "answerKey": "C" }, { "id": "atel_75", "message": "Title: Infrared Observations of the Neutron Star X-ray Transient KS 1731-260\nAuthors: Jerome A. Orosz (Utrecht University), Charles D. Bailyn and Katie Whitman (Yale University)\nDate: 6 Sep 2001; 14:54 UT\nProvenance: Jerome A. Orosz (J.A.Orosz@astro.uu.nl)\nSubjects: Infra-Red, Binary, Neutron Star, Transient\nDescription: We have obtained J-band images of the field of the neutron star X-ray transient KS 1731-260 on July 13, 2001 using the YALO 1m telescope at Cerro Tololo Interamerican Observatory and the ANDICAM optical/IR camera. We compared our image with the J-band image obtained June 1, 1996 with the Canada-France-Hawaii Telescope (Barret, Motch, & Predehl, 1998, A&A, 329, 965). The counterpart suggested by Wijnands et al. (ATEL #72) is the only star in the ROSAT error circle that is significantly variable between the two images. Using the programs DAOPHOT and ALLSTAR (Stetson, 1987, PASP, 99, 191) to compute instrumental magnitudes and the J magnitudes of several field stars given in Barret et al. (1998) to calibrate the zero point, we find J = 17.18 +/- 0.14 for the counterpart in the CFHT image and J = 18.62 +/- 0.21 in the YALO image. Using a distance of 8.3 +/- 0.3 kpc (Smith, Morgan, & Bradt, 1997, ApJ, L137) and a J-band extinction of A_J = 2.0 +/- 0.3 (Barret et al. 1998), we find an absolute J-magnitude of 2.0 +/- 0.4. This is significantly brighter than the absolute J-magnitude of a K or M dwarf (e.g. a K0V star has M_J = 4.5, Allen's Astrophysical Quantities, 4th ed.). We therefore conclude that the companion star is either significantly evolved or that its spectral type is much earlier than K, assuming the accretion disk is faint in the infrared and that there are no other sources of light such as an unresolved field star (which is the case for Aql X-1, Callanan, Filippenko, & Garcia, 1999, IAU Circular #7086; Chevalier et al., 1999, A&A, 347, L51). \nWe thank Christian Motch for providing the archival CFHT data.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Near-Earth object", "Circumstellar disk", "Globular cluster" ] }, "answerKey": "A" }, { "id": "atel_175", "message": "Title: Further radio observations of V4641 Sgr (= SAX J1819.3-2525)\nAuthors: M. P. Rupen, V. Dhawan, & A. J. Mioduszewski\nDate: 9 Aug 2003; 06:23 UT\nProvenance: Michael P. Rupen (mrupen@nrao.edu)\nSubjects: Radio, Request for Observations, Binary, Black Hole, Transient, Variables\nDescription: We report further radio observations of the X-ray transient and likely black hole binary V4641 Sgr (ATEL #170, #171, #172, #173, #174). Observations with the Very Large Array (VLA) August 8 and 9, 2003 gave flux densities of 4.08+/-0.08 and 3.07+/-0.11 mJy, respectively, at 4.86 GHz; and 2.84+/-0.05 and 2.16+/-0.09 mJy at 8.46 GHz. The corresponding spectral index on both days is about -0.6, indicating optically-thin synchrotron emission. \nThis represents a very marked decline from the 545-665 mJy seen on August 6 (ATEL #172). Comparing the data from August 8 and 9 however suggests a much slower decay at both frequencies, which can be fit, for example, by an exponential with a time constant of 3.6 days. This could be a long-lived remnant as seen following the major flare in 1999 (cf. Hjellming et al. 2000, ApJ 544, 977-992), or the beginning of a series of rapid and chaotic events as in 2002 (e.g., IAUCs 7906 , 7908 , and 7928 ; ATEL #105). \nFurther VLA and VLBA observations are planned, and we urgently request complementary observations at other wavelengths. Simultaneous observations at radio, X-ray, and optical/infrared wavelengths are particularly valuable. To this end we have created a Web site summarizing the planned observations of which we are aware, particularly at X-ray and radio wavelengths: \nhttp://www.aoc.nrao.edu/~mrupen/XRT/V4641Sgr/v4641sgr.shtml \nObservations at other wavelengths during these intervals will be invaluable in deciphering the physical mechanism(s) behind the emission. \nPlanned Observations of V4641 Sgr", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Stellar evolution", "Active galactic nucleus", "Variable star" ] }, "answerKey": "A" }, { "id": "atel_250", "message": "Title: Planned Observation Schedule on PSR 1259-63 by the H.E.S.S. experiment in March, 2004\nAuthors: M. Beilicke, Universitaet Hamburg; M. Ouchrif, Laboratoire de Physique Nucleaire de Haute Energie, Universite Paris VI and VII; G. Rowell, Max-Planck-Institut fuer Kernphysik; and S. Schlenker, Humboldt-Universitaet, Berlin; on behalf of the H. E.S. S. (High Energy Stereoscopic System) Collaboration\nDate: 13 Mar 2004; 18:28 UT\nProvenance: Michael Punch (punch@in2p3.fr)\nSubjects: Gamma Ray, >GeV, Request for Observations, Binary, Pulsar\nDescription: Further to our preceding telegram (ATEL #249) on the discovery of very-high-energy gamma-ray emission from the binary millisecond pulsar PSR 1259-63 by the H.E.S.S. experiment above a threshold of about 200 GeV, we present here our planned programme for observations for March, 2004, in order to facilitate simultaneous observations. Periastron passage of the pulsar was expected on Mar. 7.43 UT, and the pulsar is now leaving periastron. It will traverse the the inclined Be disk for the second time on Mar. 20-25, and phenomona on time-scales of hours or days may be expected preceding and during this phase. Simultaneous or quasi-simultaneous observations in other wavelengths are important for understanding of the source. The next periastron passage will not take place for another 3.4 years. \nOur planned observing schedule on this source in the coming days is: \n * Mar. 14.90-14.97 \n * Mar. 15.90-16.01 \n * Mar. 16.90-17.06 \n * Mar. 17.90-18.09 \n * Mar. 18.90-19.09 \n\nFor the following nights, the times below are planned: \n * Mar. 20.00-20.09 \n * Mar. 21.00-21.09 \n * Mar. 22.00-22.09 \n * Mar. 23.00-23.09 \n\n\nThese nights' times may be modified to begin 0.1 day earlier if the preliminary analysis of the preceding nights' data shows a high flaring state. \nObservations on subsequent nights will be determined by the preliminary results of the preceding nights of this period, and may be the object of a further follow-up telegram. Observations in this dark-moon period may continue up to Mar. 27 (as a multiwavelength campaign on another source will preclude further observations). \nAn INTEGRAL Target of Opportunity observation has been obtained on this source. Observations in other wavelengths (radio, X-ray) are strongly encouraged. \nH.E.S.S. experiment Homepage", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Pulsar, Binary system", "Black hole, Binary system", "Pulsar, Magnetar", "Pulsar, Star and stellar system" ] }, "answerKey": "A" }, { "id": "atel_325", "message": "Title: SGR 1806-20\nAuthors: S. Molkov (IKI, Moscow), K. Hurley (USB), A. Lutovinov (IKI, Moscow), R. Sunyaev (IKI, Moscow and MPA, Garching)\nDate: 30 Aug 2004; 18:28 UT\nProvenance: A.Lutovinov (aal@hea.iki.rssi.ru)\nSubjects: X-ray, Gamma Ray, Soft Gamma-ray Repeater\nDescription: The Soft Gamma-Ray Repeater SGR 1806-20 was observed with INTEGRAL during the campaign of the Galactic Center monitoring on 21-24 Aug, 2004. These observations were preceded by the INTEGRAL Galactic Plan Scan in which the source exhibited bursting activity (ATEL#324). \nThe source was in the field of view of the IBIS telescope FOR ~120 ks and more than sixty bursts were detected IN the ISGRI/IBIS low energy detection plane (18-70 keV). A few of them were unusually long (>1s) and some were extremely powerful (mean flux up to 4 10^{-6} erg/s/cm2 in the 18-70 keV energy band). In addition, the mean persistent flux of SGR 1806-20 was AT A level of ~5 mCrab in the energy range 18-60 keV, which is approximately a factor of 2 higher than it was during autumn 2003 INTEGRAL observations. \nThe next observations of the region of SGR 1806-20 with INTEGRAL are scheduled for the period 18:30 Sept. 1, 2004 to 02:10 Sept. 2, 2004 (UT). Simultaneous observations, especially in soft X-rays, are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Near-Earth object", "Repeater", "Neutron star" ] }, "answerKey": "C" }, { "id": "atel_390", "message": "Title: RXTE PCA Observations of XTE J1118+480\nAuthors: Jean Swank (GSFC), Craig Markwardt (GSFC/UMD)\nDate: 14 Jan 2005; 23:50 UT\nProvenance: Jean Swank (swank@milkyway.gsfc.nasa.gov)\nSubjects: X-ray, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 420\nRXTE had pointed observations of XTE J1118+480 for 660 and 960 seconds, respectively, on Jan. 13, 2005 at 6:31 UT and Jan 14, 3:17 UT. The average spectra were well fit with a power law of photon index 1.8 and an iron line with 42 eV equivalent width. The fluxes were equivalent to 20 and 21 mCrab 2-10 keV. With as much flux again above 10 keV, the X-ray luminosity above 2.5 keV is 3.7E35 ergs/s. The power density spectra indicate variability below 0.1 Hz of 25-30%, with possible quasiperiodic oscillations near 0.02 Hz. These observations, in which the spectrum is very similar to that observed in 2000, are much earlier in the outburst. Further observations are planned.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Binary system", "Star and stellar system, Binary system", "Black hole, Stellar evolution", "Black hole, Circumstellar disk" ] }, "answerKey": "A" }, { "id": "atel_450", "message": "Title: Aql X-1 optical/IR outburst\nAuthors: Dipankar Maitra and Charles Bailyn (Yale)\nDate: 3 Apr 2005; 01:40 UT\nProvenance: Dipankar Maitra (maitra@astro.yale.edu)\nSubjects: Infra-Red, Optical, Request for Observations, Binary, Neutron Star, Transient\nDescription: Referred to by ATel #: 452, 464, 491\nOngoing SMARTS consortium observations of Aql X-1 with the 1.3m telescope at CTIO + ANDICAM instrument show evidence for a new outburst from this source. Data obtained starting 3/29/05 showed significant flux above the quiescent level - as of April 2.381 (UT) we find R=17.1 (quiescent brightness of ~18.8) and J=15.5 (quiescent brightness of ~16.4). We note that these measurements include light from the near neighbor star (Chevalier et al., 1999, A&A, 347,L51). It is likely that the source is still in the canonical low/hard state and a transition to high/soft state might occur soon. Multiwavelength observations of the source are encouraged. Attached is the OIR lightcurve. \nOIR lightcurve of Aql X-1", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system, Neutron star", "Neutron star, Neutron star", "Interstellar medium, Neutron star", "Binary system, Interstellar medium" ] }, "answerKey": "A" }, { "id": "atel_510", "message": "Title: Radio emission from X-ray pulsar PSR J1852+0040\nAuthors: Alexander A. Ershov (PRAO ACS LPI, Pushchino)\nDate: 6 Jun 2005; 02:16 UT\nProvenance: Alexander A. Ershov (ershov@prao.psn.ru)\nSubjects: Radio, X-ray, Neutron Star, Supernova Remnant, Transient, Pulsar\nDescription: Malofeev et. al. (ATEL #501) reported the detection of radio pulses from X-ray pulsar J1852+0040 at the frequency of 111.23 MHz. I also made observations of this object using the same telescope. \nObservations were performed from April to May 2005 with the Large Phase Array (BSA) Radio Telescope at Pushchino Radio Astronomy Observatory of Lebedev Physical Institute at a frequency of 111 MHz. BSA is a transit telescope with an effective area of about 15,000 square meters. One linear polarization was received. I used a 128-channel receiver with channel bandwidth 20 kHz. The sampling interval was 2.56 ms and the receiver time constant was tau = 3 ms. The duration of each observation session was about 3 min (1600 pulsar periods). A total of 27 observations were carried out in the mode of recording single pulses. \nFolding of all 27 observation sessions using parameters of Malofeev et. al. (ATEL #501) gives negative result for each observation session - there are no pulses with S/N > 5 at the dispesion measure of 110 pc/cm(3). Unfortunately, I can't confirm the detection of radio emission from X-ray pulsar PSR J1852+0040.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Accreting object", "Neutron star, Exoplanet", "Neutron star, Pulsar", "Neutron star, Stellar evolution" ] }, "answerKey": "C" }, { "id": "atel_570", "message": "Title: Classification of SN2005db, a Type IIn Supernova\nAuthors: The Nearby Supernova Factory: N. Blanc, S. Bongard, Y. Copin, E. Gangler, L. Sauge, G. Smadja (Institut de Physique Nucleaire de Lyon), P. Antilogus, G. Garavini, S. Gilles, R. Pain (Laboratoire de Physique Nucleaire et de Haute Energies de Paris), G. Aldering, S. Bailey B. C. Lee, S. Loken, P. Nugent, S. Perlmutter, R. Scalzo, R. C. Thomas, L. Wang, B. Weaver (Lawrence Berkeley National Laboratory, Berkeley, CA), C. Bonnaud, E. Pecontal (Centre de Recherche Astronomique de Lyon), R. Kessler (Kavli Institute for Cosmological Physics, Chicago, IL), C. Baltay, D. Rabinowitz, A. Bauer (Yale)\nDate: 20 Jul 2005; 22:30 UT\nProvenance: Peter Nugent (penugent@lbl.gov)\nSubjects: Optical, Supernovae\nDescription: The Nearby Supernova Factory reports that a spectrum (range 320-1000 nm) of SN 2005db (CBET # 182), obtained July 20.6 UT with the Supernova Integral Field Spectrograph on the University of Hawaii 2.2-m telescope, shows it to be a Type IIn supernova. Adopting the NED recession velocity of 4534 km/s for the host galaxy, the spectrum is blue and featureless save for narrow emission lines of H-alpha and H-beta of approximately 400 km/s (FWHM). The narrow H-alpha emission line sits on top of a broader component that is approximately 1600 km/s (FWHM).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Supernova", "Exoplanet", "Nova" ] }, "answerKey": "B" }, { "id": "atel_675", "message": "Title: Likely Start of X-Ray Outburst from 4U 1630-47\nAuthors: John A. Tomsick (UC San Diego)\nDate: 14 Dec 2005; 20:14 UT\nProvenance: John A. Tomsick (jtomsick@ucsd.edu)\nSubjects: Radio, X-ray, Request for Observations, Black Hole, Transient\nDescription: Referred to by ATel #: 685\nRecent measurements of the recurrent black hole transient and microquasar 4U 1630-47 with the Rossi X-ray Timing Explorer All-Sky Monitor indicate that a new outburst from this source may be beginning. On Dec. 8, a single ASM dwell gave a count rate of 10.6 +/- 3.7 counts/s (151 +/- 48 millicrab, 1.5-12 keV). Four measurements on Dec. 14 confirm this detection with an average count rate of 12.6 +/- 1.1 counts/s (168 +/- 15 millicrab). 4U 1630-47 was very active between 2002 and 2004, but has been below detection in the ASM since the middle of December, 2004 (Tomsick et al. 2005, ApJ, 630, 413). Although sun-angle constraints make pointed X-ray observations impossible at the present time, the source will be observable in the coming weeks and months, and X-ray and radio observations would be useful if further ASM measurements confirm the new outburst. A list of X-ray observatories and start dates for the next observing window follow: RXTE -- 2005 December 22; Swift -- 2006 January 13; Chandra -- 2006 January 13; INTEGRAL -- 2006 February 3; Suzaku -- 2006 February 5; XMM-Newton -- 2006 Feburary 14. We anticipate triggering a target of opportunity observation with INTEGRAL in 2006 February.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Nova", "Accreting object", "Exoplanet" ] }, "answerKey": "A" }, { "id": "atel_750", "message": "Title: Radio Observations of RS Oph: Past the First Peak?\nAuthors: G. G. Pooley (MRAO Cambridge), J. L. Sokoloski (CfA), M. P. Rupen, A. J. Mioduszewski (NRAO)\nDate: 27 Feb 2006; 15:50 UT\nProvenance: Michael P. Rupen (mrupen@nrao.edu)\nSubjects: Radio, Binary, Cataclysmic Variable, Nova, Star, Transient, Variables\nDescription: Radio observations of the symbiotic recurrent nova RS Oph made with the Ryle Telescope at Cambridge at 15.2 GHz give the following: \n * Feb 24, 06:30 - 08:40 UT: 37.4 mJy\n * Feb 26, 09:54 - 11:40 UT: 33.9 mJy\n * Feb 27, 09:20 - 10:31 UT: 30.3 mJy\n\n\nThis is a low elevation source for the Ryle Telescope, and these flux densities are correspondingly uncertain, at about the 15% level. Still it seems clear that RS Oph has brightened considerably since the VLA measurement on Feb. 17.5 (23.2 +/- 0.6 mJy at 15 GHz; Eyres et al., IAU Circular 8678), consistent with the 6 GHz rise seen with MERLIN (ibid). The source is clearly not continuing to brighten at the same rate, and may be past its first peak. Further observations are on-going. \nThe National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova, Supernova", "Exoplanet, Binary system", "Interstellar medium, Binary system", "Nova, Binary system" ] }, "answerKey": "D" }, { "id": "atel_875", "message": "Title: Swift XRT observation of an X-ray burst of 1A 1246-588\nAuthors: A. K.H. Kong (MIT)\nDate: 12 Aug 2006; 22:29 UT\nProvenance: Albert Kong (akong@cfa.harvard.edu)\nSubjects: X-ray, Binary, Neutron Star\nDescription: Referred to by ATel #: 3482, 13305\nWe further analyzed the outburst of the X-ray burster 1A 1246-588 recently detected with Swift on 2006 August 11 (GCN #5436, Romano et al. 2006). Swift XRT began observation 193s after the BAT trigger; the X-ray light curve was clearly fading during the first ~500s and after that, the source count rate remained constant. We extracted time-resolved energy spectra for the first 400s. The spectra can be fitted with an absorbed blackbody model with temperature decreasing from 0.82 keV for the first 50s to 0.65 keV for the last 100s. The typical 90% error is about 0.03 keV. This suggests that the object is cooling during the decay. Excluding the first 2000s, we also fitted the spectrum of the persistent emission. The X-ray spectrum is consistent with an absorbed power-law model with a column density of 4.3+/-0.1 E21 cm^-2 and a photon index of 2.02+/-0.03 plus a Gaussian line at 0.65+/-0.02 keV. The absorbed 0.1-2.4 keV and 0.5-10 keV fluxes are 2E-10 and 5.8E-10 erg s^-1 cm^-2, consistent with previous ROSAT observation (IAUC # 6546 , Boller et al. 1997). We therefore suggest that the \"outburst\" detected with Swift is in fact a long Type-I X-ray burst with duration of at least 10 minutes.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Pulsar", "Neutron star", "Exoplanet" ] }, "answerKey": "C" }, { "id": "atel_950", "message": "Title: M31 Nova Candidate\nAuthors: WeCAPP: A. Riffeser, S. Geier (University Observatory Munich)\nDate: 20 Nov 2006; 13:12 UT\nProvenance: Arno Riffeser (arri@usm.uni-muenchen.de)\nSubjects: Optical, Nova\nDescription: The WeCAPP team discovered a M31 nova (coordinates RA 00:42:44.05 DEC +41:15:02.2 J2000.0) on three 300-sec R-filtered CCD images obtained with the 0.8-m Ritchey-Chretien f/12.4 telescope at Wendelstein Observatory, Germany, using the MONochromatic Image CAmera with a Tektronix (SITe) TK1024 1kx1k chip. Positional uncertainty given as 0\".2. A previous image from 2006 Nov. 16.9903 UT shows no object at the position of the nova (limiting magnitude 19.6 in R). \nWeCAPP M31 Novae", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Galaxy", "Supernova", "Globular cluster" ] }, "answerKey": "A" }, { "id": "atel_1020", "message": "Title: Swift Observations of SN 2007af\nAuthors: S. Immler (NASA/USRA/GSFC), P. J. Brown (PSU), and P. Milne (U of Arizona) on behalf of the Swift satellite team\nDate: 3 Mar 2007; 17:06 UT\nProvenance: Stefan Immler (immler@milkyway.gsfc.nasa.gov)\nSubjects: Optical, Ultra-Violet, X-ray, Supernovae\nDescription: Swift Ultraviolet/Optical Telescope (UVOT) and X-Ray Telescope (XRT) observed SN 2007af (CBET #863) on 2007-03-02.80 UT. The following UVOT magnitudes were measured: V = 15.0 (410 s exposure time), B = 15.1 (410 s), U = 15.4 (410 s), UVW1 [181-321nm] = 17.2 (820 s), UVM2 [166-268 nm] = 18.8 (1160 s), and UVW2 [112-264 nm] = 18.4 (1640 s). The magnitudes have not been corrected for extinction. Statistical and systematic errors are estimated to be 0.1 mag each. \nThe UV and optical colors are most similar to those of young type Ia SNe observed by Swift UVOT and well separated from young type II SNe. \nNo X-ray source is detected at the position of the SN in the 4.9 ks Swift XRT observation obtained simultaneously with the UVOT observations. The 3-sigma upper limit to the XRT net count rate is 4.0 E-03 cts/s, corresponding to an unabsorbed (0.2-10 keV band) X-ray flux of <2.0 E-13 ergs/cm/cm/s and a luminosity of <1.3 E40 ergs/s for an adopted thermal plasma spectrum with a temperature of kT = 10 keV, a Galactic foreground column density of N_H = 3.09E+20 (Dickey & Lockman, 1990, ARAA 28) and a distance of 23.2 Mpc (z=0.005464, NED; H_o = 71 km/s/Mpc, Omega_M = 1/3, Omega_L = 2/3).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Nova", "Active galactic nucleus", "Neutron star" ] }, "answerKey": "A" }, { "id": "atel_1080", "message": "Title: Optical/IR Confirmation of Outburst of Aql X-1\nAuthors: D. Maitra (Univ. of Amsterdam), C. Bailyn (Yale Univ.)\nDate: 22 May 2007; 16:43 UT\nProvenance: Dipankar Maitra (maitra@astro.yale.edu)\nSubjects: Infra-Red, Optical, Binary, Neutron Star, Transient\nDescription: Referred to by ATel #: 1087, 1218, 1219, 1557, 1970\nOngoing optical/IR monitoring of Aql X-1 with the SMARTS 1.3m telescope and ANDICAM instrument at CTIO show a steady rise over the past week. This confirms the INTEGRAL detection of the beginning of a new outburst of the source as reported by Rodriguez et al. (ATEL #1079). Our most recent data show that on May 22, 7.8h UTC (mid-exposure) the source was at R=17.2, J=15.8, compared to mean quiescent values of R=18.8, J=16.7. These magnitudes include the unrelated star 0.5\" away (Chevalier et al. 1999 A&A 347, L51). SMARTS light curves can be seen at http://www.astro.yale.edu/maitra/AqlX-1/AqlX-1.lc.jpg . Multiwavelength observations are highly encouraged. \nOIR light curve of Aql X-1", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system, Neutron star", "Pulsar, Neutron star", "Binary system, Interstellar medium", "Star and stellar system, Neutron star" ] }, "answerKey": "A" }, { "id": "atel_1225", "message": "Title: Observations of Nova M33 2007 No. 01\nAuthors: A. W. Shafter (SDSU), M. F. Bode, M. J. Darnley (Liverpool JMU), K. A. Misselt (U. Arizona), R. Quimby (Caltech), and F. Yuan (U. Mich.)\nDate: 27 Sep 2007; 18:04 UT\nProvenance: Allen W. Shafter (aws@nova.sdsu.edu)\nSubjects: Optical, Cataclysmic Variable, Nova, Transient\nDescription: As part of an ongoing study of novae in nearby galaxies, we report optical photometric and spectroscopic observations of the extragalactic nova M33 2007 No. 01 (CBET #1074, CBET #1080). Our spectroscopic observations (4280à – 7260à , at ~ 4.5à resolution), which were obtained on 22 Sep 2007 UT (four days after discovery) with the Marcario Low Resolution Spectrograph on the Hobby-Eberly Telescope, confirm that the nova is a member of the He/N spectroscopic class of Williams (1992). Specifically, the spectrum shows extremely strong and broad [EW (Hα) ~ 800à , FWHM (Hα) ~ 5500 km/s] Balmer, N II,III, and He I,II emission lines. Photometric observations obtained with the ROTSE IIIb telescope at McDonald Observatory show that the nova has faded approximately two magnitudes (unfiltered) in the first six days after discovery. Such a rapid fade rate is consistent with that expected for a He/N nova. The observed magnitude at maximum light (~16.5) allows us to place a conservative lower limit on the luminosity of the nova, M < − 8.2, at the distance of M33 (taken to be μ = 24.7). Given that maximum light could have been missed by up to a day, and that we have not made any correction for extinction, the nova is likely to be somewhat more luminous. \nThis material is based upon work supported by the National Science Foundation under Grant No. 0607682 (to AWS), and on observations obtained with the Marcario Low Resolution Spectrograph on the Hobby - Eberly Telescope, which is operated by McDonald Observatory on behalf of the University of Texas at Austin, the Pennsylvania State University, Stanford University, the Ludwig-Maximillians-Universitaet, Munich, and the George-August-Universitaet, Goettingen. Public Access time is available on the Hobby-Eberly Telescope through an agreement with the National Science Foundation.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Pulsar", "Nova", "Black hole", "Repeater" ] }, "answerKey": "B" }, { "id": "atel_1300", "message": "Title: AGILE detection of day-to-day gamma-ray variability from Blazar 3C 454.3\nAuthors: G. Pucella, M. Tavani, F. D'Ammando, V. Vittorini, E. Costa, M. Feroci, I. Donnarumma, L. Pacciani, E. Del Monte, F. Lazzarotto, P. Soffitta, Y. Evangelista, I. Lapshov, M. Rapisarda, A. Argan, A. Trois , G. De Paris (INAF/IASF Roma), S. Vercellone, A. Chen, A. Giuliani, S. Mereghetti, A. Pellizzoni, F. Perotti, F. Fornari, M. Fiorini, P. Caraveo, A. Zambra (INAF/IASF Milano), A. Bulgarelli, F. Gianotti, M. Trifoglio, G. Di Cocco, C. Labanti, F. Fuschino, M. Marisaldi, M. Galli, (INAF/IASF Bologna), G. Barbiellini, F. Longo (INFN Trieste), P. Picozza, A. Morselli (INFN Roma-2), M. Prest, E. Vallazza (Universita` dell'Insubria), P. Lipari, D. Zanello (INFN Roma-1), F. Mauri (INFN Pavia) and P. Giommi, C. Pittori, L. A. Antonelli, D. Gasparrini, S. Cutini, F. Verrecchia (ASDC) and L. Salotti (ASI)\nDate: 22 Nov 2007; 18:33 UT\nProvenance: Andrew Chen (chen@iasf-milano.inaf.it)\nSubjects: Gamma Ray, >GeV, AGN, Quasar\nDescription: Referred to by ATel #: 1545, 1581, 1592, 2322\nThe AGILE satellite, currently in its Science Verification Phase, during the Observing Block that started on 2007-11-02 12:00 UT, detected significant gamma-ray emission from a source coincident with the blazar 3C 454.3, as reported in ATEL #1278. The source continues to be active in > 100 MeV gamma rays, showing variability on day-to-day time scales, with particular activity within the last two days. We strongly encourage continued multi-frequency observations of the field of the gamma-ray source detected by AGILE.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar, Quasar", "Active galactic nucleus, Galaxy", "Active galactic nucleus, Quasar", "Magnetar, Quasar" ] }, "answerKey": "C" }, { "id": "atel_1410", "message": "Title: VLA radio upper limit on Type IIn Supernova 2008X\nAuthors: Poonam Chandra, Alicia Soderberg\nDate: 4 Mar 2008; 14:27 UT\nProvenance: Poonam Chandra (pc8s@virginia.edu)\nSubjects: Radio, Supernovae\nDescription: We observed a Type IIn supernova SN 2008X (CBET 1239) in NGC 4141 with the VLA in 8.46 GHz frequency band on 2008 Feb 19.39 UT. We do not detect any radio source at the supernova position (CBET 1239). The peak flux density at the supernova position is 8 +/- 38 uJy. We thank VLA staff for making this observation possible. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Nova", "Binary system", "Repeater" ] }, "answerKey": "A" }, { "id": "atel_1475", "message": "Title: Optical observations of the fast nova V2491 Cyg\nAuthors: T. Tomov, M. Mikolajewski, E. Ragan, E. Swierczynski, P. Wychudzki (Uniwersytet Mikolaja Kopernika, Torun, Poland)\nDate: 14 Apr 2008; 22:27 UT\nProvenance: M. Mikolajewski (mamiko@astri.uni.torun.pl)\nSubjects: Optical, Binary, Cataclysmic Variable, Nova, Star\nDescription: Referred to by ATel #: 1478, 1480, 1485, 1504, 1514, 1561\nWe report on optical spectral observations and UBVRI brightness estimations obtained with 60/90 cm Schmidt and 60 cm Cassegrain telescopes of the Nicolaus Copernicus University Observatory (Torun, Poland). The nova V2491 Cyg was discovered on Apr. 10.728 UT with about 7.7 mag on unfiltered CCD frames (IAUC# 8934 ). Additionally, the X-ray emission was detected for the prenova several months ago (ATel#1473). The magnitudes estimated on Apr. 13.957 UT were U=9.02, B=9.21, V=9.03, R=8.04, I=7.72 using HD 331150 as the comparison star and assuming 10.30, 10.254, 10.25, 10.26 and 10.27 for its UBVRI magnitudes, respectively. The accuracy of our photometry is about 0.01 magnitude. A comparison with the data from IAUC# 8934 shows that our photometry was obtained about 2.2-2.3 days after the maximum when the star reached about 7.1-7.4 magnitude in the V light. Prismatic optical spectra (4000-9500 AA), with a resolution ~18 A around H-alpha and ~6 A around H-beta, were obtained on Apr. 11.99 UT and Apr. 13.95 UT. In both spectra the Balmer lines from H-alpha to H-delta are seen in emission. The FWHM of H-alpha is ~4800 km/s on Apr. 11.99 and ~4600 km/s on Apr. 13.95. The H-beta FWHM is ~4860 km/s and ~4220 km/s, respectively. The equivalent width of H-alpha increased twice, from ~380 A on Apr. 11.99 to ~760 A on Apr. 13.95. In the same time the H-beta equivalent width changed from ~140 A on Apr. 11.99 to ~180 A on Apr. 13.95. The FWHM and equivalent width of H-alpha observed on Apr. 11.99 are very close to those observed near the maximum (CBET#1334). P Cyg absorptions with a velocity about -3900 km/s on Apr. 11.99 and about -4000 km/s on Apr. 13.95 are well visible in H-beta and H-gamma profiles. It is possible that a second P Cyg absorption component, with velocity of about -6400 km/s, appeared in H-beta on Apr. 13.95 UT. An additional emission component with a velocity about +2300 km/s presents in the H-beta and H-gamma profiles on both dates. A strong asymmetry of the red H-alpha wing is most probably caused by a similar emission component. In addition to the Balmer lines in the spectrum of V2491 Cyg, relatively strong lines of Fe II multiplets 37, 38, 42 and 49 and OI 8446 A are present as well. Both, the expansion velocities and rapid fading of the brightness, indicate that V2491 Cyg belongs to the group of the extremely fast novae.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Near-Earth object", "Nova", "Quasar" ] }, "answerKey": "C" }, { "id": "atel_1575", "message": "Title: The faint neutron star and probable ultra-compact transient AX J1754.2-2754: quiescent after a (long) outburst\nAuthors: C. Bassa (SRON & Nijmegen), P. G. Jonker (SRON & CfA), G. Nelemans (Nijmegen), D. Steeghs (Warwick), M. A.P. Torres (CfA), L. Kuiper (SRON), J. J.M. In 't Zand (SRON), N. Rea (UvA), T. Maccarone (Southampton), E. Kuulkers (ESA/ESAC), J. Grindlay (CfA), R. Wijnands (UvA), M. Mendez (Groningen)\nDate: 13 Jun 2008; 08:05 UT\nProvenance: P.G. Jonker (pjonker@cfa.harvard.edu)\nSubjects: Optical, X-ray, Request for Observations, Neutron Star, Transient\nDescription: Referred to by ATel #: 1643, 4109, 10195\nWe report on multi-epoch Chandra and optical observations of the faint, bursting (Chelovekov & Grebenev 2007, Atel #1094) neutron star transient AX J1754.2-2754. The source has been detected every time since 1999 (Sakano et al. 1999) when an X-ray satellite observed the source. However, we do not detect the source in Chandra Galactic Bulge Survey observations obtained in May 2008. The Galactic Bulge Survey is an optical and X-ray survey of two strips each 6 by 1 degrees centered 1.5 degrees above and below the Galactic plane towards the Galactic center. \n \nWe derive an accurate source position for AX J1754.2-2754 using a 1.18 ks Chandra HRC-I observation that we obtained on Aug. 14, 2007. The source position is: R.A.: 17h54m14.5s Dec: -27d54m35.6s (J2000.0). The positional uncertainty is dominated by the Chandra aspect offset which, for the HRC-I, has a 90% confidence radius of 0.45 arcsec. This location is inside the Swift error circle of the source (Del Santo et al. 2007; Atel #1143). Using the spectral parameters found by Del Santo et al. (2007) and the source distance given by Chelovekov & Grebenev (2007; 6.6/9.2 kpc) we get a source 0.5-10 keV luminosity of 1.6-3.2E35 erg/s. \n \nIn the Chandra X-ray Galactic Bulge Survey observations obtained in May 2008, we detect more than a 1000 sources. However, AX J1754.2-2754 is not one of them. The Chandra ACIS-I observation of the field of AX J1754.2-2754 took place on May, 14, 2008 and lasted 2.19 ks. We do not find X-ray photons in a circular region with radius of 2 arcsec centered on the source position. Using the formulation of Gehrels (1989) this yields a 95% confidence upper limit to the source 0.5-10 keV luminosity of 3.0-5.8E32 erg/s for a power-law spectrum with photon index 2 and an extinction as found by ASCA and Swift observations of the source in outburst (N_H=2.3E22 cm-2). Similar limits are derived assuming a blackbody spectrum with temperature of 0.35 keV. \n \nAs part of our Galactic Bulge Survey we have also obtained optical images with the Blanco 4m telescope in June 2006 of the area covered by the X-ray observations. We do not detect a source in the Chandra error circle. This provides an upper limit to the outburst SDSS i-band magnitude of i>23.5. Using the distance and the fact that the interstellar extinction found in outburst X-ray spectra corresponds to A_i~7 we calculate an upper limit to the outburst absolute i-band magnitude of 2.4/1.7 for a distance of 6.6/9.2 kpc. The low outburst luminosity, the burst properties (cf. In't Zand, Jonker & Markwardt 2007) together with the low absolute magnitude suggest that AX J1754.2-2754 is an ultra-compact X-ray binary. \n \nDue to the faintness of the source in outburst the historic light curve of the source is sketchy, but probably the source has been in outburst at least since the discovery by ASCA in October 1999. Depending on the exact date that the source went to quiescence (some time between Aug. 14, 2007 and May 15, 2008) deep follow-up observations could find the cooling neutron star.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Accreting object", "Neutron star", "Supernova" ] }, "answerKey": "C" }, { "id": "atel_1700", "message": "Title: Improved position of the new X-ray transient XTE J1637-498\nAuthors: R. Wijnands, M. Linares, N. Degenaar (UvA), C. B. Markwardt (CRESST/U. Md./NASA/GSFC) \nDate: 5 Sep 2008; 21:23 UT\nProvenance: Rudy Wijnands (rudy@space.mit.edu)\nSubjects: X-ray, Request for Observations, Binary, Black Hole, Neutron Star, Transient\nDescription: Referred to by ATel #: 1704\nFollowing the discovery of the new X-ray transient XTE J1637-498 (Atel #1699), we obtained a short (nearly 1 ksec) observation using the Swift/XRT in PC mode on 2008-09-04 at 18:15 UT. We detected one relatively bright source within the ~6 arcminutes PCA error circle at a position of RA=16:37:02.995, Dec=-49:51:37 (J2000), with an estimated uncertainty of 3.8 arcseconds radius (90% confidence). \nThe X-ray spectrum of the source can be adequately (a reduced chi^2 of 0.7) described by an absorbed power-law with a column density of 2.3+/-0.9E22 cmE-2 and a photon index of 1.5+/-0.4 and an absorbed 2-10 keV flux of ~2.7E-11 erg/s/cm^2. The X-ray spectrum is consistent with the source being a low-mass X-ray binary, but due to the large errors on the spectral parameters other types of system cannot be excluded (i.e., high-mass X-ray binaries). We urge follow-up observations in optical and near-IR to try to find the counterpart of the transient at these wavelengths. \nWe thank the Swift team for approving and scheduling our observation.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object, Binary system", "Repeater, Binary system", "Accreting object, Neutron star", "Accreting object, Globular cluster" ] }, "answerKey": "A" }, { "id": "atel_1775", "message": "Title: SuperAGILE detects an X-ray burst from SAX J1750.8-2900\nAuthors: L. Pacciani, E. Costa, E. Del Monte, I. Donnarumma, Y. Evangelista, M. Feroci, I. Lapshov, F. Lazzarotto, M. Rapisarda, P. Soffitta, A. Argan, A. Trois , M. Tavani, G. Piano, G. Pucella, F. D'Ammando, V. Vittorini (INAF/IASF Roma), A. Bulgarelli, F. Gianotti, M. Trifoglio, G. Di Cocco, C. Labanti, F. Fuschino, M. Marisaldi, M. Galli, (INAF/IASF Bologna), A. Chen, S. Vercellone, A. Giuliani, S. Mereghetti, F. Perotti, F. Fornari, M. Fiorini, P. Caraveo (INAF/IASF Milano), A. Pellizzoni (OAC/INAF Cagliari), G. Barbiellini, F. Longo, E. Vallazza (INFN Trieste), P. Picozza, A. Morselli (INFN Roma-2), M. Prest (Universita` dell'Insubria), P. Lipari, D. Zanello (INFN Roma-1), A. Rappoldi (INFN Pavia) and C. Pittori, F. Verrecchia, P. Santolamazza, B. Preger, P. Giommi (ASDC) and L. Salotti (ASI)\nDate: 10 Oct 2008; 13:33 UT\nProvenance: Marco Feroci (marco.feroci@iasf-roma.inaf.it)\nSubjects: Binary, Neutron Star, Transient\nDescription: Referred to by ATel #: 1777\nWhile pointing at the Galactic Center region, SuperAGILE detected an X-ray burst from a position consistent with the neutron star transient SAX J1750.8-2900. This source was recently reported by Linares et al. (ATel #1662) as returning to a quiescent state, based on a Swift/XRT observation on August 14th 2008 (ATel #1662), after a long outburst started on March 2008 (Markwardt & Swank, ATel #1425), during which also SuperAGILE detected the source at hard X-rays at a flux level of about 80 mCrab (Pacciani et al., ATel #1428). The observed X-ray burst lasted approximately 60 sec, starting on 9 October 2008 at 21:26:04 UT. The average flux in the 17-25 keV energy range was about 2.3 Crab, while no significant signal is detected above 25 keV. A search in the SuperAGILE data in the 60 and 600 sec preceding and following the burst provided no evidence of prolonged source activity. The source is currently not detected by SuperAGILE in the standard 20-60 keV energy range, on a daily timescale, with a 3-sigma upper limit of about 20 mCrab.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium, Binary system", "Circumstellar disk, Binary system", "Neutron star, Binary system", "Near-Earth object, Binary system" ] }, "answerKey": "C" }, { "id": "atel_1890", "message": "Title: Optical flaring of a probable blazar seen in the Catalina Sky Survey \nAuthors: A. A. Mahabal, A. J. Drake, S. G. Djorgovski, M. Graham, R. Williams (Caltech), E. Beshore, S. M. Larson, A. Boattini (UA/LPL), E. Christiansen (Gemin Obs.) \nDate: 5 Jan 2009; 01:31 UT\nProvenance: Ashish Mahabal (aam@astro.caltech.edu)\nSubjects: Radio, Optical, Request for Observations, Quasar, Variables\nDescription: Referred to by ATel #: 1952\nWe have detected the optical brightening by over 2 mags (V ~ 17.5) of a previously known radio source (CRATES J112402+233643; 709 mJy at 6 cm; Spectral Index 1 of 0.227) in the Catalina Sky Survey (CSS) on 3 Jan 2009 UT. The source is also detected in FIRST, NVSS etc. The SDSS object ID is 587742189362741377 and the mags are u=20.69, g=20.40, r=20.13, i=19.77, z=19.57. \nCSS090102:112403+233646 | 2009-01-02 UT 11:08:48 | 11:24:02.69 | 23:36:46.2| 901021230574116817 \n---|---|---|---|--- \nThe discovery data, CSS lightcurve and finding chart are posted at the VOEventNet webpage: http://voeventnet.caltech.edu/feeds/ATEL/CRTS/901021230574116817.atel.html We encourage multicolor/multiepoch imaging and spectroscopy.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus", "Supernova", "Globular cluster", "Exoplanet" ] }, "answerKey": "A" }, { "id": "atel_1975", "message": "Title: SAX J1753.5.-2349 is back to quiescence\nAuthors: Melania Del Santo (INAF/IASF-Roma), Patrizia Romano (INAF/IASF-Palermo), Lara Sidoli (INAF/IASF-Milano)\nDate: 17 Mar 2009; 19:46 UT\nProvenance: Melania Del Santo (melania.delsanto@iasf-roma.inaf.it)\nSubjects: X-ray, Binary, Neutron Star, Transient\nDescription: Referred to by ATel #: 2505\nOn 2009 March 13th Swift/XRT observed the field of the Very Faint X-ray Transient (VFXT) SAX J1753.5-2349. In the ~2.2 ks (net exposure) photon counting mode observation, no sources are detected in the XRT error box for SAX J1753.5-2349. A 3-sigma upper limit can be measured at about 6E-3 counts/s. Adopting a spectral model with Nh=2.1E22 cm-2 and a photon index of 2.2, we obtain an unabsorbed flux as 6.0E-14 erg cm-2 s-1 (2-10 keV), corresponding to a luminosity level of about 5E32 erg s-1 (at 8 kpc). \nSAX J1753.5-2349 is a neutron star X-ray binary discovered by BeppoSAX in 1996 during a type-I burst event without any persistent emission detected (in't Zand et al. 1996), i. e. at a luminosity level below the WFC sensitivity. Thereafter it was no longer detected until 2008 October 11th, when PCA/RXTE reported an outburst at 8 mCrab flux level (ATel #1799), corresponding to a peak luminosity of about 1E36 erg s-1 (d=8kpc). \nThe flux decreasing phase has been reported by the IBIS telescope on-board INTEGRAL in the middle of October (ATel #1810) and by Swift/XRT (2008 October 24th) when SAX J1753.5-2349 was about 3.5E35 erg s-1 (ATel #1809). \nDue to the sensitivities, hard X-ray detectors (i. e. IBIS and BAT), cannot follow the complete evolution of outbursts of the Very Faint X-ray Transients (i. e. outburst luminosities of 1E34-1E36 erg s-1). However, from the end of October 2008 until March 3009 SAX J1753.5-2349 was no longer observed with Swift/XRT. \nIt should be noted that on 2008 February 12th, SAX J1753.5-2349 was quiescent (ATel #1809). This allow us to estimate the lower limit on the outburst duration as 5 months, while the upper limit is one year. \nWe would like to thank the Swift Team for performing these observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater", "Star and stellar system", "Circumstellar disk", "Neutron star" ] }, "answerKey": "D" }, { "id": "atel_2040", "message": "Title: Addition to ATel #2306, \"Light curve oscillations and flux decline in the Be/X-ray binary Swift J1626.6-5156\" \nAuthors: M. E. DeCesar (University of Maryland), K. Pottschmidt (CRESST/GSFC/UMBC), T. Belloni (INAF - Brera Observatory), P. Reig (U. Crete/FORTH), J. Wilms (Dr. Karl Remeis-Observatory, Bamberg/ECAP, Erlangen) \nDate: 29 Apr 2009; 18:20 UT\nProvenance: Katja Pottschmidt (katja@milkyway.gsfc.nasa.gov)\nSubjects: X-ray, Binary, Transient, Pulsar\nDescription: As an addition to and clarification of ATel #2036, we point out that the oscillations with period ~45d were first presented and discussed by Reig et al. (2008, A&A 485, 797). At the time of publication, the source had not yet clearly transitioned into the ~72d period oscillatory stage. The intent of ATel #2036 was to present the changing periodicity, and not the discovery of oscillations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy, Pulsar", "Pulsar, Pulsar", "Binary system, Pulsar", "Quasar, Pulsar" ] }, "answerKey": "C" }, { "id": "atel_2100", "message": "Title: SN candidate in NGC 3106\nAuthors: A. J. Drake, S. G. Djorgovski, A. A. Mahabal, M. J. Graham, R. Williams (Caltech); M. Catelan (PUC); E. C. Beshore, S. M. Larson, A. Gibbs (LPL/UA); E. Christensen (Gemini Observatory); \nDate: 25 Jun 2009; 08:05 UT\nProvenance: Andrew J. Drake (ajd@cacr.caltech.edu)\nSubjects: Supernovae, Transient\nDescription: We report the discovery of a SN candidate found by the Catalina Real-time Transient Survey (CRTS) in NGC 3106. \n\nID| Date| RA| Dec| Mag| Mag host| z host \n---|---|---|---|---|---|--- \nCSS090625:100407+311229| 2009-06-25 UT 04:03:46 | 10:04:06.78 | 31:12:29.0 | 16.1| 12.7 | 0.021 \n \n\nFor finding charts, discovery images, lightcurves, etc., please see: http://voeventnet.cacr.caltech.edu/feeds/ATEL/CRTS. \nCurrent candidate and confirmed SNe can be found here. \nWe request follow-up.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Quasar", "Circumstellar disk", "Pulsar" ] }, "answerKey": "A" }, { "id": "atel_2175", "message": "Title: Fermi LAT detection of GeV flare from blazar PKS 2023-07\nAuthors: D. Gasparrini (ASDC) on behalf of the Fermi Large Area Telescope Collaboration\nDate: 27 Aug 2009; 13:38 UT\nProvenance: Dario Gasparrini (dario.gasparrini@asdc.asi.it)\nSubjects: Gamma Ray, >GeV, AGN, Quasar\nDescription: Referred to by ATel #: 2179, 8879, 8932\nThe Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, detected on August 23, 2009 increasing gamma-ray activity from a source positionally consistent with the EGRET flat spectrum radio quasar PKS 2023-07 also known as 3EG J2025-0744, 0FGL J2025.6-0736 (RA: 160h 25m 40.6604s -07d 35m 52.688s, J2000.0, ref. Beasley, A. J. et l 2002, ApJS, 141, 13B; redshift 1.388, ref. Drinkwater, M. J. et al. 1997, MNRAS, 284, 85D). \nPreliminary analysis indicates that on August 23, 2009, PKS 2023-07 appeared in a high state with a gamma-ray flux (E>100MeV) of 1.42+/-0.28 x 10^-6 photons cm^-2 s^-1 (statistical only), which represents an increase of a factor of 3 with respect to the source flux level indicated in Abdo et al. 2009, ApJ, 700, 597A. \nBecause Fermi operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. In consideration of the ongoing gamma-ray activity, we strongly encourage multiwavelength observations. For the source the Fermi LAT contact person is D. Bastieri (bastieri@pd.infn.it). \nThe Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Active galactic nucleus", "Accreting object", "Minor body" ] }, "answerKey": "B" }, { "id": "atel_2250", "message": "Title: Orbital Modulation and Long Term Spin-up Rate of SWIFT J1626.6-5156\nAuthors: A. Baykal (METU), S. C. Inam (Baskent), E. Gogus (Sabanci), T. M. Belloni (INAF)\nDate: 21 Oct 2009; 15:00 UT\nProvenance: Sitki Cagdas Inam (inam@baskent.edu.tr)\nSubjects: X-ray, Binary, Neutron Star, Transient, Pulsar\nDescription: We report on the long-term pulse period history of the ~15.35s X-ray pulsar SWIFT J1626.6-5156 obtained from pulse timing analysis of RXTE-PCA observations between MJD ~53724 and MJD ~54379. A preliminary circular orbit fit to the pulse period history between MJD ~53924 (200 days after the first observation) and MJD ~54379 reveals an orbital period of ~132.9 days.\nFrom this preliminary fit to the pulse period history, we obtain an (a/c)sini value of ~405sec which corresponds to a mass function value of ~4.2 Solar mass. The source is also found to have a secular spin-up between MJD ~53924 and MJD ~54379 with a rate of ~1.37x10^{-12} Hz/sec.\nWork on pulse arrival time history to obtain a more accurate orbital model of the source is in progress.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Exoplanet, Pulsar", "Neutron star, Binary system, Pulsar", "Neutron star, Circumstellar disk, Pulsar", "Stellar evolution, Binary system, Pulsar" ] }, "answerKey": "B" }, { "id": "atel_2310", "message": "Title: AGILE confirms high gamma-ray state of GB6 B1310+4844\nAuthors: A. Bulgarelli, F. Gianotti, M. Trifoglio (INAF/IASF-Bo), S. Vercellone (INAF/IASF-Pa), M. Tavani (INAF/IASF-Rm), E. Striani (Univ. Roma Tor Vergata and INFN Roma), F. Verrecchia, C. Pittori, P. Santolamazza (ASDC), F. D'Ammando (Univ. Roma Tor Vergata and INAF/IASF-Rm), I. Donnarumma (INAF/IASF-Rm), V. Vittorini, E. Del Monte, Y. Evangelista, M. Feroci, F. Lazzarotto, L. Pacciani, P. Soffitta, E. Costa, I. Lapshov, M. Rapisarda, A. Argan, G. Piano, G. Pucella, S. Sabatini, A. Trois (INAF/IASF-Rm), F. Fuschino, M. Galli, C. Labanti, M. Marisaldi, G. Di Cocco (INAF/IASF-Bo), A. Chen, A. Giuliani, S. Mereghetti, P. Caraveo, F. Perotti (INAF/IASF-Mi), A. Pellizzoni, M. Pilia (INAF/OA-Cagliari), G. Barbiellini, F. Longo, E. Moretti, E. Vallazza (INFN Trieste), A. Morselli, P. Picozza (INFN and Univ. Roma Tor Vergata), M. Prest (Universita` dell'Insubria), P. Lipari, D. Zanello (INFN and Univ. Roma Sapienza), P. W. Cattaneo, A. Rappoldi (INFN Pavia), S. Colafrancesco, P. Giommi,(ASDC), L. Salotti (ASI)\nDate: 23 Nov 2009; 13:04 UT\nProvenance: Stefano Vercellone (stefano@iasf-milano.inaf.it)\nSubjects: Gamma Ray, >GeV, AGN, Quasar\nDescription: Referred to by ATel #: 2316\nThe AGILE Gamma-Ray Imaging Detector (GRID) detected significant gamma-ray emission above 100 MeV from a source consistent with the blazar GB6 B1310+4844, recently reported in a high gamma-ray state by Fermi/LAT on Nov. 18 2009 (Sokolovsky et al., ATel #2306). \nIntegrating from 2009-11-20 17:00 UT to 2009-11-22 17:00 UT, a maximum likelihood analysis shows a detection at a significance level above 4.7 sigma, with a source flux above 100 e-8 ph/cm2/sec (E > 100 MeV), confirming the current high gamma-ray state of the source. \nA maximum likelihood analysis from 2009-11-18 17:00 UT to 2009-11-22 17:00 UT shows an AGILE detection at a significance level above 6 sigma. \nThe AGILE/GRID detection was obtained while AGILE is observing in spinning mode, surveying a large fraction of the sky each day.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Nova", "Black hole", "Stellar evolution" ] }, "answerKey": "C" }, { "id": "atel_2375", "message": "Title: Swift/BAT Detects an Outburst from XTE J1901+014 \nAuthors: H. A. Krimm (CRESST/GSFC/USRA), P. Romano, S. Vercellone (INAF-IASF Palermo), S. D. Barthelmy (GSFC), W. Baumgartner (CRESST/GSFC/UMBC), J. Cummings (CRESST/GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC), C. B. Markwardt (CRESST/GSFC/UMD), D. Palmer (LANL), T. Sakamoto (CRESTT/GSFC/UMBC), G. Skinner (CRESST/GSFC/UMD), M. Stamatikos (OSU/GSFC), J. Tueller (GSFC), T. Ukwatta (GSFC/GWU) \nDate: 8 Jan 2010; 15:15 UT\nProvenance: Hans A. Krimm (Hans.Krimm@nasa.gov)\nSubjects: X-ray, Request for Observations, Binary, Black Hole, Neutron Star, Transient\nDescription: Referred to by ATel #: 13328, 15904\nAt 00:58:50.58 UT on 2010-Jan-08 (MJD 55204), Swift/BAT triggered on a rapid outburst from XTE J1901+014. The trigger was a 128-second image trigger and detectable emission lasted from T-150 sec to at least T+250 sec, when the spacecraft moved away from the field due to a pre-planned slew. The time-averaged spectrum from T-137.5 to T+263.9 sec is best fit by a simple power-law model. The photon power law index of the time-averaged spectrum is 5.22 +- 0.51. The fluence in the 15-150 keV band is 1.5 +- 0.2 x 10-6 erg/cm2. This corresponds to 0.056 ± 0.010 ct/s/cm2 or 250 mCrab in the 15-50 keV band. Due to an observing constraint (proximity to the sun), no Swift XRT or UVOT observations will be possible until 2010-Feb-16. \nThis is the second time Swift/BAT has triggered on XTE J1901+014. The first was on 2006-June-06 at 10:17:18.76 for a weaker flare. The time-averaged spectrum of the 2006 flare from T+0.0 to T+33.1 sec was best fit by a simple power-law model. The photon power law index of the time-averaged spectrum was 4.32 +- 1.94 and the fluence in the 15-150 keV band was 1.1 +- 0.7 x 10-7 erg/cm2. The flux in a 1984-second observation beginning at 10:17:18 averaged 0.068 ± 0.048 ct/s/cm2 (31 mCrab, 15-50 keV). \nXTE J1901+014 is normally barely detectable in the BAT hard X-ray transient monitor at ~2.5 mCrab. It has shown signs of increased, but variable, activity since about 2009-Dec-03. \nThis source was discovered in 2002 (Remillard and Smith, ATel #88) and is known for having rapid, intense variations in its X-ray flux (e.g. Smith et al, ATel #1268). The true nature of the source is still in question. Optical photometry of the field suggests a low mass companion and the source may be the first low-mass fast X-ray transient (Karasev, Lutovinov & Burenin, 2008, Astron. Lett., 34, 753). This recent trigger tells us that XTE J1901+014 has again become active, so further observations are encouraged. \nSwift/BAT Hard X-ray Transient light curve for XTE J1901+014", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Circumstellar disk", "Black hole, Neutron star", "Quasar, Neutron star", "Neutron star, Neutron star" ] }, "answerKey": "B" }, { "id": "atel_2475", "message": "Title: Near-IR observations of the Supergiant Fast X-ray Transient (SFXT) IGR J17544-2619\nAuthors: Sachindra Naik, Vishal Joshi, S. V. Vadawale, N. M. Ashok (Physical Research Laboratory, Ahmedabad, India)\nDate: 12 Mar 2010; 04:09 UT\nProvenance: Sachindra Naik (snaik@prl.res.in)\nSubjects: Infra-Red, Binary, Transient, Variables\nDescription: Referred to by ATel #: 2820\nThe Supergiant Fast X-ray Transient (SFXT) IGR J17544-2619 which went to outburst on 2010 March 04 (ATel #2463) was observed in the near-infrared J-band on March 6 and in J, H, and K-band on March 7 with the 1.2m telescope (+ NICS with HAWAII-1 infrared array) at Gurushikhar, Mt Abu, operated by Physical Research Laboratory, Ahmedabad, India. The photometric observations were carried out in very clear and photometric sky conditions. Several frames in each of the three J, H, and K-bands were obtained in three dithered positions, offset by typically 30 arcsec from each other. The sky frames were generated by median combining the dithered frames and subtracted from the source frames followed by aperture photometry. On March 6, the J-band magnitude of the source was found to be 8.76 (+/- 0.03), whereas the J, H, and K-band magnitudes of the object, on March 7, were found to be 8.76 (+/- 0.05), 8.27 (+/- 0.04) and 8.20 (+/- 0.04), respectively. Spectroscopic observations were difficult because of the limited visibility of the object from the observatory. Further monitoring of the source will be carried out from Mt. Abu observatory.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system", "Active galactic nucleus", "Binary system", "Galaxy" ] }, "answerKey": "C" }, { "id": "atel_2575", "message": "Title: Spectroscopic Identification of CSS100409:154258+021653\nAuthors: J. M. Silverman, I. K. W. Kleiser, C. V. Griffith, and A. V. Filippenko (University of California, Berkeley)\nDate: 19 Apr 2010; 16:36 UT\nProvenance: Alexei V. Filippenko (alex@astro.berkeley.edu)\nSubjects: Optical, Supernovae\nDescription: We report that inspection of a low signal-to-noise ratio CCD spectrum (range 350-1000 nm) of CSS100409:154258+021653, obtained on Apr. 15 UT with the 3-m Shane reflector (+Kast) at Lick Observatory, shows that CSS100409:154258+021653 (ATEL #2555) is a normal type-Ia supernova. Cross-correlation with a library of supernova spectra using the \"SuperNova IDentification\" code (SNID; Blondin and Tonry 2007, Ap.J., 666, 1024) indicates that it is within a few days of maximum brightness and has a redshift of 0.039.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Exoplanet", "Accreting object", "Magnetar" ] }, "answerKey": "A" }, { "id": "atel_2625", "message": "Title: NIR Flaring of S4 1030+61.\nAuthors: L. Carrasco, A. Carramiñana ,E. Recillas, A. Porras, D. Y. Mayya (INAOE. Mexico)\nDate: 19 May 2010; 09:40 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Infra-Red, Gamma Ray, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 2628, 3062, 3287, 8715, 11361, 12648\nWe call attention on our recent observation of the Gamma Ray source 1FGL J1033.8+6048 with the CANICA NIR camera on the 2.1m telescope at the Observatorio Astrofísico Guillermo Haro, located in Cananea, Mexico. We found this blazar to be in outburst. It shows fluxes about 2.7 magnitudes brighter than previous NIR photometry listed in the 2MASS catalog of point sources. Our photometric results in the H Band for the date JD2455335.6830, yield a value of H=13.298 +/- 0.05. Our observations were prompted by ATELs #2622 and #2623. They provide further support for the identification of the gamma ray source 1FGL J1033.8+6048 with the optical source SDSS J103351.42+605107.3. Multiwavelength observations would be very valuable.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Exoplanet", "Galaxy", "Pulsar", "Black hole" ] }, "answerKey": "D" }, { "id": "atel_2730", "message": "Title: Detection of new outbursts of the recurrent X-ray transient CXOM31J004217.0+411508\nAuthors: W. Pietsch (Max-Planck-Institut fuer extraterrestrische Physik, MPE), M. Henze (MPE), F. Haberl (MPE)\nDate: 10 Jul 2010; 19:30 UT\nProvenance: Wolfgang Pietsch (wnp@mpe.mpg.de)\nSubjects: X-ray, Transient\nDescription: We report the discovery of a new outburst of the recurrent X-ray transient CXOM31J004217.0+411508 (r3-46) in a 4.4 ks Swift XRT observation (ObsID 00035336022) starting on 2010-07-09.95 UT. The source was not yet active in the preceding 3.9 ks observation of the XRT monitoring campaign (00035336021) starting on 2010-07-07.07 UT. We find count rates of 10.6+-1.9 ct/ks and <2.0 ct/ks, respectively, which correspond to luminosities (0.2-10 keV) of 3.5e37 erg/s and <0.7e37 erg/s (assuming an absorbed power-law model with photon index = 1.7 and NH = 6.6e20 cm-2 at a distance of 780 kpc). The object is identified as a hard source. \n \nPrevious outbursts with similar brightness have been reported for August 2000, October 2001, January 2004, May 2006, and November 2007 (see Henze et al. 2007, ATel #1307 and references therein). Henze et al. proposed a recurrence time of the outbursts of the transient of about 1.2 years. While there was no X-ray coverage at the expected times of outburst in 2003 and 2005, we detected the start of an additional outburst of CXOM31J004217.0+411508 in Chandra HRC-I observations on 2009-02-16.89 UT (ObsID 10683, exposure 19.9 ks) and 2009-02-26.17 UT (10684, 18.7 ks) with count rates of 2.28+-0.47 ct/ks and 6.70+-0.78 ct/ks. Assuming a spectrum as above, these count rates correspond to luminosities (0.2-10 keV) of 0.34e37 erg/s and 1.0e37 erg/s, respectively. \n \nThe outbursts in 2009 and 2010 further confirm a recurrence time of the outbursts of about 1.2 years. As already Henze et al mentioned, transients with similar recurrence times have been identified as neutron star systems (e.g. Aql X-1) or black hole systems (e.g. 4U 1630-472) in the Galaxy. \n \nWe would like to thank the Swift team for the scheduling of the observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Black hole", "Nova, Black hole", "Neutron star, Neutron star", "Neutron star, Magnetar" ] }, "answerKey": "A" }, { "id": "atel_2820", "message": "Title: INTEGRAL sees IGR J17544-2619 active again\nAuthors: E. Kuulkers (ESA/ESAC, Spain), J. Chenevez (DNSC, Denmark), J. Alfonso-Garzon (LAEX-CAB/INTA-CSIC, Spain), V. Beckmann (ISDC, Switzerland), T. Bird (Southampton, UK), S. Brandt (DNSC, Denmark), T. Courvoisier (ISDC, Switzerland), A. Domingo (LAEX-CAB/INTA-CSIC, Spain), K. Ebisawa (ISAS, Japan), P. Jonker (SRON, The Netherlands), P. Kretschmar (ESA/ESAC, Spain), C. Markwardt (GSFC, USA), T. Oosterbroek (ESA/ESTEC, The Netherlands), A. Paizis (INAF-IASF, Italy), C. Sanchez-Fernandez (ESA/ESAC, Spain), R. Wijnands (UvA, The Netherlands)\nDate: 30 Aug 2010; 13:25 UT\nProvenance: Erik Kuulkers (ekuulker@rssd.esa.int)\nSubjects: X-ray, Request for Observations, Binary, Neutron Star, Transient, Variables\nDescription: INTEGRAL Galactic bulge monitoring observations (see, e.g., ATels #438 and #1266) between UT 29 Aug 2010 22:54 and 30 Aug 2010 02:35 revealed X-ray flaring from the Supergiant Fast X-ray Transient (SFXT) IGR J17544-2619. Its last activity was reported about 180 days ago, in March 2010 (ATel #2463). \nIGR J17544-2619 flared on time scales of about half an hour, from around a peak IBIS/ISGRI count rate of 60 +/- 10 mCrab (18-40 keV) during an 1800-sec pointing down to about 10 mCrab, i.e., near the half-an-hour detection limit. The average IBIS/ISGRI detection significance over the 12.6 ksec observation is about 19 sigma (18-40 keV). The behaviour is similar to that seen during its previous detected activity by INTEGRAL (e.g., ATel #1266, #1697). \nJEM-X detects IGR J17544-2619 too, at 22 +/- 12 mCrab (3-10 keV, 3 sigma), and 40 +/- 22 mCrab (10-25 keV, 4 sigma), over the course of the observation. \nSince activity at other wavelengths is expected (see, e.g., ATel #2475) we encourage follow-up observations. The next INTEGRAL Galactic bulge monitoring observation is expected to start at UT 4 Sep 2010 11:26. \nThe INTEGRAL Galactic bulge monitoring results (JEM-X and IBIS/ISGRI light curves and mosaic images) are publicly available at http://isdc.unige.ch/Science/BULGE/.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Magnetar", "Black hole", "Neutron star" ] }, "answerKey": "D" }, { "id": "atel_2910", "message": "Title: Discovery of Very High Energy Gamma-Ray Emission from B3 2247+381 by MAGIC\nAuthors: Mose Mariotti (INFN and Univ. of Padova) on behalf of the MAGIC Collaboration\nDate: 7 Oct 2010; 13:02 UT\nProvenance: Mosè Mariotti (mariotti@pd.infn.it)\nSubjects: Optical, X-ray, >GeV, TeV, VHE, AGN, Blazar\nDescription: Referred to by ATel #: 2923\nThe MAGIC Collaboration reports the discovery of Very High Energy (VHE; >100 GeV) gamma-ray emission from the High Frequency peaking BL Lac object B3 2247+381 with z=0.1187. The source is positionally consistent with the Fermi-LAT gamma-ray source 1FGL J2250.1+3825 (RA 22 50 06.6 dec +38 25 58, J2000), which was flagged as a promising VHE source candidate by the Fermi-LAT collaboration, information which was shared with the MAGIC collaboration (as well as other IACTs) back in October 2009. The MAGIC observations were triggered by an optical high-state of the source, reported by the Tuorla blazar monitoring program (http://users.utu.fi/kani/1m/B3_2247+381.html). The VHE detection is based on a 9.3 hour-long observation performed on 2010 September 30th, October 1st, 2nd, 4th, 5th and 6th in stereoscopic mode with the two 17m diameter imaging Cherenkov telescopes on La Palma, Canary Islands, Spain. The preliminary analysis of the MAGIC data using standard cuts yields a detection of 64 gamma-rays above 150 GeV, corresponding to a pre-trial statistical significance of 5 standard deviations. The observed flux is estimated to be ~2% of the Crab nebula flux above 150 GeV. Target of Opportunity Observations with Swift have also been performed on this source location. A preliminary analysis of the Swift/XRT data shows that the X-ray flux from the source is ~4 times higher than during last observation (spring 2010). Further Swift observations are expected until October 15. We thank the Swift team for accepting and promptly scheduling the X-ray observations. MAGIC will continue observations of B3 2247+381. Observations at other wavelengths are encouraged. Questions regarding the MAGIC observations should be directed to Mose Mariotti (mose.mariotti@pd.infn.it).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Black hole", "Globular cluster", "Active galactic nucleus" ] }, "answerKey": "B" }, { "id": "atel_2970", "message": "Title: MAXI/GSC detects a new activity from Be pulsar A0535+262 \nAuthors: T. Mihara (RIKEN), M. Nakajima (Nihon U.), T. Yamamoto, M. Sugizaki, M. Suzuki, Y. E. Nakagawa, T. Sootome, M. Matsuoka (RIKEN), N. Kawai, M. Morii, K. Sugimori, R. Usui (Tokyo Tech), K. Kawasaki, S. Ueno, H. Tomida, M. Kohama, M. Ishikawa (JAXA), A. Yoshida, K. Yamaoka, S. Nakahira (AGU), H. Tsunemi, M. Kimura (Osaka U.), H. Negoro, H. Ozawa, F. Suwa (Nihon U.), Y. Ueda, N. Isobe, S. Eguchi, K. Hiroi (Kyoto U.), A. Daikyuji (Miyazaki U.), A. Uzawa, T. Matsumura, K. Yamazaki (Chuo U.) report on behalf of the MAXI team\nDate: 25 Oct 2010; 21:33 UT\nProvenance: Motoki Nakajima (nakajima.motoki@nihon-u.ac.jp)\nSubjects: X-ray, Binary, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 3020, 3075, 3166, 14157, 14392\nAn increase of X-ray flux of the Be/X-ray binary pulsar A0535+26 has been observed with MAXI/GSC since 2010 October 14. The current activity is clearly out of the outburst phase (only 0.7 x ~110-day orbital period since the last outburst peak), and probably is a precursor activity. Assuming that it is a precursor, this is the fifth detection of the consecutive activities following the ~110-day orbital cycle (Moritani+ 2010), although the average interval of the last four outbursts has been significantly longer at about 115 days. Assuming this 115-day outburst period, the series of outbursts and precursor events observed by MAXI took place at same phases, ~0.2 and ~0.95 respectively, where the phase zero is taken at MJD 55153.5, the periastron passage prior to the previous giant outburst (Atel #2324, #2336, #2337, #2343). This change in outburst period may indicate a secular change in the size, density, or orientation (possibly precession) of the circumstellar disk of the companion Be star. The latest light curve and folded light curve are available at the following URL: http://maxi.riken.jp/top/index.php?cid=1&jname=J0538+263 and also in the news page URL:http://maxi.riken.jp/news/.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Stellar evolution", "Pulsar", "Minor body" ] }, "answerKey": "A" }, { "id": "atel_3075", "message": "Title: MAXI/GSC detects a renewed activity from binary X-ray pulsar GX304-1\nAuthors: M. Nakajima (Nihon-U), T. Yamamoto, T. Mihara, M. Sugizaki, M. Serino, Y. E. Nakagawa, T. Sootome, M. Matsuoka (RIKEN), N. Kawai, M. Morii, K. Sugimori, R. Usui (Tokyo Tech), K. Kawasaki, S. Ueno, H. Tomida, M. Kohama, M. Ishikawa (JAXA), A. Yoshida, K. Yamaoka, S. Nakahira (AGU), H. Tsunemi, M. Kimura (Osaka U.), H. Negoro, H. Ozawa, F. Suwa (Nihon U.), M. Shidatsu, Y. Ueda, N. Isobe, S. Eguchi, K. Hiroi (Kyoto U.), A. Daikyuji (Miyazaki U.), A. Uzawa, T. Matsumura, K. Yamazaki (Chuo U.) on behalf of the MAXI team\nDate: 9 Dec 2010; 23:46 UT\nProvenance: Motoki Nakajima (nakajima.motoki@nihon-u.ac.jp)\nSubjects: X-ray, Binary, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 3087, 3309, 4420\nThe MAXI/GSC auto transient-alert system has detected a new activity from a binary X-ray pulsar, GX 304-1 on 2010-12-08. The current source activity is the fourth event since the MAXI/GSC observation started on 2009 August. The source flux started to increase on 2010-12-05 (MJD 55535.5) and reached 20 mCrab (2-20 keV) on 2010-12-08 (MJD 55538.5). Comparing with the previous outburst (Atel#2779), the current flux increase is about 1-week earlier than that of the previous one within the orbital cycle of 132.5-day period. Thus, the current activity may be a precursor, or an onset of an anomalous giant outburst that occurs out of regular recurrent phase. In case of A0535+26 (Atel#2970), precursor events are seen in large outbursts (Atel#2970). Among the previous three outbursts from GX 304-1, only the last one, which developed into the giant outburst, had a precursor. Applying this relation, the incoming outburst is supposed to become giant. The latest light curve and folded light curve are available at the following URL:@ http://maxi.riken.jp/top/index.php?cid=1&jname=J1301-616 and also in the news page URL: http://maxi.riken.jp/news/.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system, Magnetar", "Binary system, Supernova", "Binary system, Pulsar", "Binary system, Galaxy" ] }, "answerKey": "C" }, { "id": "atel_3200", "message": "Title: New Swift observations of the SFXT IGR J11215-5952 in outburst\nAuthors: P. Romano (INAF-IASFPA), P. Esposito (INAF-OAC), S. Vercellone (INAF-IASFPA), V. Mangano (INAF-IASFPA), D. N. Burrows (PSU), G. Cusumano (INAF-IASFPA), R. Farinelli (INAF-IASFPA, U. Ferrara), J. A. Kennea (PSU), V. La Parola (INAF-IASFPA), N. Gehrels (GSFC)\nDate: 2 Mar 2011; 09:44 UT\nProvenance: Pat Romano (romano@ifc.inaf.it)\nSubjects: X-ray, Binary, Transient, Pulsar\nDescription: The supergiant fast X-ray transient (SFXT) IGR J11215-5952 (Lubinski et al. 2005, Atel #469) undergoes periodic outbursts separated by about 165 days (Sidoli et al. 2007, A&A 476, 1307), which most likely correspond to the orbital period of the binary system. Based on the ephemeris of Romano et al. (2009, ApJ, 696, 2068), that predicted the peak of the new outburst on 2011 March 1 at about 9.30 UT, we observed the source with Swift. \nThe Swift/XRT observations started on 2011 March 1 at 12:16:46 (effective exposure 2.4 ks). IGR J11215-5952 was detected with a mean count rate of (1.1+/-0.1)E-01 counts/s (1-10 keV). The average XRT/PC spectrum can be fit with an absorbed powerlaw model with a photon index of Gamma=1.0-0.5+0.6 and an absorbing column density of NH=(2.2-1.0+1.3)E+22 cm-2 (Cash statistics C-stat=542.6; 51% of 1E4 Monte Carlo realizations with statistic < C-stat). The mean observed (unabsorbed) 1-10 keV flux is 1.2E-11 erg/cm2/s (1.5E-11 erg/cm2/s), which translates into a luminosity of about 0.7E35 erg/s (assuming the optical counterpart HD 306414 at a distance of 6.2 kpc, Masetti et al. 2006 A&A, 449, 1139). These findings are consistent with those of previous outbursts (Romano et al. 2007, A&A, 469, L5; Sidoli et al 2007, A&A, 476, 1307; Romano et al. 2009, ApJ, 696, 2068; Atel #2257). \nWe thank the Swift Team for making these observations possible, in particular the duty scientists and the science planners. \nSFXT Project web page", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Pulsar", "Binary system, Pulsar", "Binary system, Neutron star", "Active galactic nucleus, Pulsar" ] }, "answerKey": "B" }, { "id": "atel_3300", "message": "Title: SWIFT J1626.6-5156 is a Be/X-ray binary\nAuthors: E. Nespoli (Valencian International University, Univ. of Valencia), P. Reig (FORTH, Univ. of Crete), J. Fabregat (Univ. of Valencia), R. E. Mennickent (Univ. of Concepcion) \nDate: 21 Apr 2011; 12:46 UT\nProvenance: Elisa Nespoli (elisa.nespoli@uv.es)\nSubjects: Infra-Red, X-ray, Binary, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 3362\nWe report results from NIR spectroscopy of the optical counterpart to the hard X-ray transient SWIFT J1626.6-5156 (ATel #678, #679). The proposed infrared counterpart (2MASS J16263652-5156305, ATel #688, #713, #739) was observed in visiting mode at the European Southern Observatory on 2010 July 23 with the SofI spectrograph on the 3.5m NTT in La Silla, Chile (ESO proposal 085.D-0297A). The sky had thin cirri, the seeing averaged between 0.9'' and 1.3'' and the target was observed at airmass 1.12. Data were taken in the Short Wavelength - Low Resolution mode, with a resolution of R=588, covering the 1.53-2.52 micron spectral range. The retrieved S/N averaged 100.\nOurs is the first available IR spectrum of the proposed counterpart to the X-ray source.\nThe low-resolution K spectrum is almost featureless, except for presence of both HeI 20581 Å and HI 21660 Å (Brackett-gamma) in strong emission (EW = -9.9 and -8.8 Å, respectively). Both transitions are typical of Be-stars and confine the spectral type of the companion to be earlier than B2.5 (see Clark and Steele, 2000, A&AS, 141, 65). The H-band spectrum shows much more complexity, with the evidence of the HI Br-18-11 recombination series in emission. No FeII lines (1.534, 1.600 and 1.620 micron respectively) are observed. As for the K band, all the observed features are typical of Be stars, while they are absent, or observed in absorption in normal (non-emission) OB stars.\nBy comparison with spectral atlases (Clark and Steele, 2000, A&AS, 141, 65, Steele and Clark, 2001, 2001, A&A, 371, 643), the optical counterpart to SWIFT J1626.6-5156 can be classified as a B0-2Ve star, and the system is definitely a Be/X-ray binary.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system", "Stellar evolution", "Circumstellar disk", "Nova" ] }, "answerKey": "A" }, { "id": "atel_3390", "message": "Title: Swift J2058+0516: GROND detection of candidate optical counterpart\nAuthors: Arne Rau, Jochen Greiner, Felipe Olivares E. (all MPE Garching)\nDate: 30 May 2011; 13:31 UT\nProvenance: Arne Rau (arau@mpe.mpg.de)\nSubjects: Optical, Transient\nDescription: Referred to by ATel #: 3425, 3426\nStarting May 29, 2011 at 8:56 UT we continued observations of the new transient Swift J2058.4+0516 (Krimm et al. 2011, ATEL #3384; Greiner et al. 2011, ATEL #3385) with GROND (Greiner et al. 2008, PASP 120, 405), the 7-channel imager mounted at the 2.2m MPI/ESO telescope at La Silla Observatory (Chile). \n \nIn a 60min exposure we detected a single, unresolved source within the 1.7 arcsec Swift/XRT error circle (Krimm et al. 2011, ATEL #3384) at \n \nRA = 20:58:19.90 (314.58292 deg) \nDec = +05:13:32.2 (5.22562 deg) \n \nThe uncertainty in both coordinates is ~0.3 arcsec rms. \n \nWe measured the following magnitudes (all in AB system): \n \ng = 23.5 +/- 0.1 \nr = 23.6 +/- 0.1 \ni = 23.6 +/- 0.2 \nz > 22.5 \nJ > 21.2 \nH > 20.6 \nK > 18.2 \n \nThese magnitudes were derived by calibrating the images against SDSS and 2MASS field stars and are not corrected for Galactic foreground reddening of E(B-V)~0.1mag (Schlegel et al. 1998). Upper limits are 3 sigma. \n \nA GROND r'-band image is available at http://www.mpe.mpg.de/~jcg/xrt/Swift2058p0516.html \n \nIf the soft X-ray flux remained at the same level as reported by Krimm et al. (2011, ATEL #3384) the X-ray to optical flux ratio would be 3x10^4. This is challenging for both, an AGN, and a LMXB/CV interpretation. The blue color hints towards an accretion disk origin of the optical emission. In case of a Galactic source (D<10kpc) the donor would have to be of M-type or later and the X-ray luminosity would be ~5x10^35 (D/10kpc)^2 erg/s. Optical spectroscopic observations will be important to reveal the true nature of this source. \n \nNo cataloged radio source has been found within <3arcmin from the GROND position.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Near-Earth object", "Stellar evolution", "Galaxy" ] }, "answerKey": "A" }, { "id": "atel_3450", "message": "Title: Spectroscopy of PSN J19583553+0236163 \nAuthors: D. C. Leonard (San Diego State University), J. Moustakas (U. C. San Diego), B. J. Swift (U. Arizona), D. McCarthy (U. Arizona), V. Bailey, E. Carrico, A. Carter, E. Chui, E. Douglas, E. Eggeman, R. Goldberg, R. Grant, K. Hartman, J. Hellerstein, E. Hooper, C. Horlick-Cruz, L. Hunter, T. Jiles, E. D. Johnson, K. Kumar, L. Lappe, J. Lee, W. Lee, F. Marsh, G. Mehta, P. Miller, R. Rampalli, J. Reed, K. Rice, H. Saldivar, M. Salgado-Flores, A. Schlingman, W. F. Schlingman, W. M. Schlingman, S. Scibelli, K. Sinclair, I. Steincamp, N. Stock, N. Todd, L. L. Aizpuru Vargas, S. Yamanaka, E. Zachary (2011 Advanced Teen Astronomy Camp) \nDate: 23 Jun 2011; 19:04 UT\nProvenance: D. C. Leonard (leonard@astro.caltech.edu)\nSubjects: Optical, Supernovae\nDescription: As part of the 2011 Advanced Teen Astronomy Camp (http://www.astronomycamp.org), we obtained a low dispersion optical spectrum (range 370-690 nm) of PSN J19583553+0236163 in UGC 11501 with the 2.3m Bok telescope (+ Boller & Chivens spectrograph) at Steward Observatory, on 2011 June 23 UT. Cross-correlation with a library of supernova spectra using the Supernova Identification code (SNID; Blondin and Tonry 2007, Ap.J. 666, 1024) shows it to be a type-Ia supernova of the 91T-like sub-class several days before maximum light; good matches are obtained with pre-maximum (-6.4 +/- 2.7 days) template spectra of SN 1991T, SN 1997br, and SN 1999aa. Using the NED redshift of z=0.025 for UGC 11501, the velocity of the (weak) Si II 635.5-nm feature is approximately 10,100 km/s.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Globular cluster", "Variable star", "Active galactic nucleus", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_3525", "message": "Title: Chandra Localization of the Galactic Center X-ray Transient Swift J174535.5-285921\nAuthors: Deepto Chakrabarty (MIT), Manuel Linares (MIT), Peter G. Jonker (SRON), Craig B. Markwardt (NASA/GSFC)\nDate: 2 Aug 2011; 18:45 UT\nProvenance: Deepto Chakrabarty (deepto@space.mit.edu)\nSubjects: X-ray, Black Hole, Neutron Star, Transient\nDescription: Referred to by ATel #: 3529, 9236, 13839\nAs part of an ongoing Chandra program for precise localization of X-ray transients in low-mass X-ray binaries, we obtained a short Chandra/ACIS-I observation of the X-ray transient Swift J174535.5-285921 during its 2011 July discovery outburst (ATEL #3472, #3476, #3481, #3508). The exposure time was 966 s, using a (1/8)-subarray of the I3 chip with 0.5 s readout time. Our observation was made on 2011 July 21, 06:35 TT. This was at least one week after the transient is inferred to have returned to X-ray quiescence based on Swift observations, but it is also the same date that Swift observed marginal evidence for residual enhanced emission from the source (ATEL #3508). \nOur Chandra observation weakly detected the source at an intensity of 0.023(5) count/s. The best-fit X-ray source position is: \nRA(J2000) = 17h 45m 35.746s \nDec(J2000) = -28d 59' 29.06\" \nwith an error radius of 0.6 arcsec (90% confidence). This position is inconsistent with the reported Swift XRT-UVOT enhanced position (3.3 arcsec error radius; ATEL #3472), lying 8.2 arcsec away. However, our Chandra position is consistent with the unenhanced Swift XRT position (3.8 arcsec error radius; ATEL #3472), lying 3.5 arcsec away. It is also consistent with the previously reported faint Chandra point source CXOUGC J174535.6-285928 (source 1680 in Table 2 of Muno et al. 2009, ApJS, 181, 110), lying 0.6 arcsec away. Given the number density of sources from the Muno et al. catalog in this field, the chance coincidence probability is 2.2 percent. We note that recent infrared counterpart searches during the X-ray outburst were evidently analyzing the wrong source position (ATEL #3476, #3481). \nAssuming the average X-ray spectrum measured by Swift (an absorbed power-law spectrum with photon index 1.4 and hydrogen column density 5.7E22 cm^(-2)), the absorbed (unabsorbed) 2-10 keV flux in our Chandra observation was 8.2E-13 (1.1E-12) erg/cm^2/s, corresponding to a luminosity of 8.0E33 erg/s for a distance of 8 kpc. This is roughly consistent with the July 21 luminosity inferred from the marginal Swift detection (ATEL #3508). It is an order of magnitude fainter than the mean outburst luminosity reported by Swift (ATEL #3508), but nearly three orders of magnitude brighter than the quiescent luminosity for CXOUGC J174535.6-285928 reported by Muno et al. (2009).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk, Neutron star", "Repeater, Neutron star", "Black hole, Neutron star", "Black hole, Nova" ] }, "answerKey": "C" }, { "id": "atel_3601", "message": "Title: Refined Orbital Timing Solution for IGR J17498-2921\nAuthors: C. B. Markwardt (NASA/GSFC), T. E. Strohmayer (NASA/GSFC)\nDate: 27 Aug 2011; 22:39 UT\nProvenance: Craig B. Markwardt (Craig.Markwardt@nasa.gov)\nSubjects: X-ray, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 3606, 3622, 3638, 3643, 15996\nWe report a refined solution for the accreting millisecond X-ray pulsar IGR J17498-2921 (ATels #3551, #3555, #3556, #3558, #3559, #3560, #3561, #3562, #3563, #3568). \nAnalysis is based on RXTE PCA data in the energy band 2-30 keV between 2011-08-13 and 2011-08-23, for total exposure of 121 ksec. A coherent orbit solution was found using the Z^2 technique (Bucheri et al 1983). We caution that this solution is preliminary in the sense that definitive RXTE orbit and fine clock correction data are not yet used. \nThe best-fit orbital solution has a barycentered pulsar frequency of 400.990187287(4) Hz, a projected pulsar semi-major axis of 0.365108(3) lt-sec, and an orbital period of 13835.615(1) s. There is no detectable orbital eccentricity or long-term pulse frequency change. The mass function is 0.002042(1) solar masses, implying a minimum companion mass of approximately 0.17-0.22 solar masses, depending on the neutron star mass. The epoch of the ascending node is JD 2455786.5608963(4) referred to the TDB time system. Numbers in parentheses are formal 1-sigma errors in the final digits. These quantities are substantially consistent with the earlier preliminary results reported by Papitto et al. (ATEL #3563). \nThe pulse profile semi-amplitude is between 10% and 30%, depending on the amount of contamination due to other point-like and diffuse sources in the PCA collimator field of view. \nThe X-ray light curve has varied somewhat in the 30-40 mCrab range, but does not show clear signs of rapid decline. This increases the chances that it will be detectable by other observatories.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy", "Circumstellar disk", "Magnetar", "Nova" ] }, "answerKey": "C" }, { "id": "atel_3675", "message": "Title: Fermi LAT detection of a GeV flare from 3C 446\nAuthors: K. V. Sokolovsky (ASC Lebedev/SAI MSU) and F. K. Schinzel (MPIfR) on behalf of the Fermi Large Area Telescope Collaboration\nDate: 10 Oct 2011; 17:56 UT\nProvenance: Kirill Sokolovsky (kirx@scan.sai.msu.ru)\nSubjects: Gamma Ray, >GeV, Request for Observations, AGN, Blazar, Quasar\nDescription: The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed a short gamma-ray flare from a source positionally consistent with 3C 446 (22:25:47.2593 -04:57:01.391, J2000, Fey et al. 2004, AJ, 127, 3587) a flat spectrum radio quasar at z=1.404 (Perez, Penston & Moles 1989, MNRAS, 239, 55). \nPreliminary analysis indicates that the source on 2011 October 08 was in a high state with a gamma-ray flux (E>100MeV) of (1.5 +/-0.4)x10^-6 photons cm^-2 s^-1 (statistical uncertainty only). This is about 30 times higher than the average flux level observed during the first two years of Fermi mission (2FGL J2225.6-0454, Abdo et al. 2011, submitted to ApJ, arXiv:11081435). On October 09, the source was again below the detection limit in a 24h integration. \nBecause Fermi operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. We encourage multiwavelength observations to confirm the identification of the flaring GeV source and study its activity in detail. For this source the Fermi LAT contact person is David Thompson (David.J.Thompson@nasa.gov). \nThe Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater", "Quasar", "Binary system", "Black hole" ] }, "answerKey": "B" }, { "id": "atel_3780", "message": "Title: Swift/BAT reports increased activity from IGR J18483-0311\nAuthors: H. A. Krimm (CRESST/GSFC/USRA), P. Romano (INAF-IASF Palermo), S. D. Barthelmy (GSFC), W. Baumgartner (CRESST/GSFC/UMBC), J. Cummings (CRESST/GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC), C. B. Markwardt (GSFC), D. Palmer (LANL), T. Sakamoto (CRESTT/GSFC/UMBC), G. Skinner (CRESST/GSFC/UMD), M. Stamatikos (OSU/GSFC), J. Tueller (GSFC), T. Ukwatta (GSFC/MSU)\nDate: 24 Nov 2011; 12:08 UT\nProvenance: Hans A. Krimm (Hans.Krimm@nasa.gov)\nSubjects: Binary, Neutron Star, Transient\nDescription: The Swift/BAT hard X-ray transient monitor reports renewed activity in the 15-50 keV band from the supergiant fast X-ray transient and HMXB neutron star system IGR J18483-0311. The source has increased in intensity from its normal level of approximately 0.001 cts/cm^2/sec (~4 mCrab) on 2011 Nov. 18 to a level of 0.013 +/- 0.003 (~60 mCrab) on 2011 Nov. 23 (MJD 55888). This is the highest level seen since August 2008. An earlier peak of ~30 mCrab was seen one orbital period ago on 2001 Nov. 5. \nSwift/BAT Hard X-ray Transient light curve for IGR J18483-0311", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Binary system", "Magnetar, Binary system", "Neutron star, Circumstellar disk", "Black hole, Binary system" ] }, "answerKey": "A" }, { "id": "atel_3925", "message": "Title: Swift observation of PS1-12fo (=CSS120121)\nAuthors: R. Margutti, A. Soderberg, L. Chomiuk, E. Berger, D. Milisavljevic, N. Sanders (Harvard University)\nDate: 14 Feb 2012; 23:52 UT\nProvenance: Raffaella Margutti (rmargutti@cfa.harvard.edu)\nSubjects: Optical, Ultra-Violet, X-ray, Supernovae\nDescription: PS1-12fo is a spectroscopically confirmed, very luminous supernova with similarities to SN2010gx, lying at redshift z=0.175 (Valenti et al. ATels #2668, #3351; Smartt et al. Atel #3918). A Swift ToO was executed starting from 2012-02-13T16:55:19 UT. Swift-UVOT observations have been obtained in the 6 optical/UV filters. A source is marginally detected at the SN position in the v, b, u and m2 filters, while it is seen faintly in the w1 and w2 filters. Including possible contamination from the underlying host galaxy, we measure the following preliminary magnitudes (UVOT photometric system Breeveld et al. 2011, arXiv:1102.4717): v= 19.0 +/- 0.2; b= 19.8 +/- 0.2; u= 19.5 +/- 0.2; m2= 20.4 +/- 0.2. Magnitudes are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.068 in the direction of the transient (Schlegel et al. 1998). Contemporary Swift-XRT observations have been performed (total exposure of 5 ks). No X-ray source is detected at the optical position of the transient, with a 3 sigma upper limit of ~3.2d-3 c/s in the 0.3-10 keV energy band. The Galactic neutral hydrogen column density in the direction of the event is 2.38d20 1/cm2 (Kalberla 2005). Assuming a spectral photon index ~2, this translates into an absorbed flux of ~1.6d-13 erg/s/cm2 (corresponding to a luminosity of ~1d43 erg/s. A luminosity distance of 836 Mpc has been used). We thank the Swift team for scheduling these ToO observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Star and stellar system", "Supernova", "Galaxy" ] }, "answerKey": "C" }, { "id": "atel_4020", "message": "Title: DETECTION OF HIGH OPTICAL ACTIVITY OF BLAZAR OJ287\nAuthors: M. M.M. Santangelo (O. A.C.)\nDate: 6 Apr 2012; 14:00 UT\nProvenance: Filippo Mannucci (filippo@arcetri.astro.it)\nSubjects: Optical, Blazar\nDescription: Referred to by ATel #: 4021, 4026, 4057\nM.M.M. Santangelo, Astronomical Observatory of Capannori (OAC) Italy, recently performed optical CCD photometric monitoring of the blazar OJ287. This monitoring is part of the CATS (Capannori Astronomical Transient Survey) project. This CCD photometry of OJ287 was obtained with OAC's 0.30-m f/10 telescope equipped with a SBIG ST-9XE CCD camera + BVRI (Johnson/Cousins) filters in the nights of March 28th, March 29th, and April 1st. Bias images, master darks and master flats (both twilight sky and dome flats) were obtained each night. The photometric calibration was performed on every night on the secondary UBVRI standards around the so-called \"dipper asterism\" in M67. Our V and R magnitudes are as follows: 2012 March 28.91UT R = 13.78 +/-0.01 and V = 14.34 +/- 0.02; 2012 March 29.86UT R = 13.84 +/-0.01 and V = 14.29 +/-0.02; 2012 April 1.84UT R = 13.95 +/-0.03 and V = 14.30 +/-0.04. This photometry shows that OJ287 is at the brightest photometric levels of the last two years. OJ287 is now only 0.3 magnitudes fainter than the outburst of the late 2005, and about an half magnitude fainter than that of the outburst of 1994, but by far fainter than the great outbursts of 1983 and 1972. This high optical activity of OJ287 apparently contradicts some of the predictions made by Sundelius et al.(ApJ 484,180,1997); their fig.6 with a prediction for a small outburst by 2014-2015 and not in 2012. Apparently this recent activity is not in agreement with the ~12 years cycle discovered by Sillanpaa et al.(A&A 315, L13, 1996). The high optical activity of OJ287 observed at OAC was not predicted by Valtonen (2007, ApJ 659, 1074) based on the precessing binary black hole model. Infact in tables 1,2,3 in Valtonen's paper there are no predicted outbursts between late 2007 and late 2015 (or early 2016). Smaller outbursts, flickering and synchrotron flares (Dultzin-Hacyan et al., 1997, Rev.Mex.A&A 33, 17) are not uncommon in blazars. But the recent fairly high photometric activity of OJ287 can be classified at an intermediate level between the smaller flares and the biggest outbursts.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Interstellar medium", "Globular cluster", "Black hole" ] }, "answerKey": "D" }, { "id": "atel_4100", "message": "Title: Near-IR photometric observations of nova V5588 Sagittarii\nAuthors: W. P. Varricatt, T. Wold and J. Ehle (Joint Astronomy Centre, Hilo, HI, USA)\nDate: 7 May 2012; 19:43 UT\nProvenance: Watson Varricatt (w.varricatt@jach.hawaii.edu)\nSubjects: Infra-Red, Nova\nDescription: We report near-IR photometry of Nova V5588 Sgr (Nova Sagittarii 2011 no. 2). Observations were performed with the 3.8-m United Kingdom Infrared Telescope (UKIRT) and the UKIRT Wide Field Camera (WFCAM) using the near-IR filters Z, Y, J, H and K (effective wavelengths: 0.8717, 1.0305, 1.2483, 1.6313 and 2.2010 microns respectively). In our images, the source is located at RA=18:10:21.344, Dec=-23:05:30.05 (J2000). The epochs of our observations, filters used and the magnitudes derived (in the UKIRT photometric system) are given in the table below. The near-IR brightness of V5588 Sgr decreased during the period of our observations reported here. \nThe nova was discovered in outburst on 27.837 March 2011 UT (Arai et al. CBET #2679; Nishiyama et al. IAUC# 9203 ). We inspected pre-outburst K-band images from the UK Infrared Deep Sky Survey (UKIDSS; GPS DR7+; observed on 20070331 UT) and the 2MASS JHK images; the object is not detected in these images showing that V5588 Sgr is currently several magnitudes brighter in the near-IR compared to its pre-outburst brightness. \n \n \n ----------------------------------------------------------- \n UTDATE | UT | Heliocentric | Filt.|mag. | error \n yyyymmdd | hh:mm:ss | Julian Date \n ----------------------------------------------------------- \n 20110807 | 05:42:07.0 | 2455780.741882 | H | 10.909 | 0.010 \n 20110807 | 05:44:53.0 | 2455780.743804 | K | 10.152 | 0.010 \n 20110807 | 05:47:38.5 | 2455780.745719 | J | 11.227 | 0.010 \n \n 20110821 | 06:11:45.5 | 2455794.761451 | K | 10.420 | 0.020 \n 20110821 | 06:25:54.5 | 2455794.771277 | Z | 12.595 | 0.010 \n 20110821 | 06:28:32.5 | 2455794.773106 | Z | 12.579 | 0.025 \n \n 20110929 | 05:44:20.5 | 2455833.738804 | K | 10.293 | 0.010 \n 20110929 | 05:46:52.5 | 2455833.740563 | H | 11.105 | 0.010 \n 20110929 | 05:49:56.5 | 2455833.742692 | J | 11.370 | 0.020 \n 20110929 | 05:52:57.5 | 2455833.744787 | Y | 11.722 | 0.010 \n 20110929 | 05:55:59.5 | 2455833.746893 | Z | 12.783 | 0.010 \n 20110929 | 05:58:38.5 | 2455833.748733 | Z | 12.764 | 0.030 \n \n 20111001 | 05:18:02.5 | 2455835.720344 | K | 10.342 | 0.010 \n 20111001 | 05:20:41.0 | 2455835.722178 | H | 11.199 | 0.020 \n 20111001 | 05:23:42.5 | 2455835.724279 | J | 11.475 | 0.010 \n 20111001 | 05:26:49.5 | 2455835.726443 | Y | 11.810 | 0.025 \n 20111001 | 05:29:55.5 | 2455835.728595 | Z | 12.828 | 0.015 \n 20111001 | 05:32:44.5 | 2455835.730551 | Z | 12.838 | 0.010 \n \n 20111005 | 05:12:25.5 | 2455839.716050 | K | 10.380 | 0.010 \n 20111005 | 05:15:05.0 | 2455839.717896 | H | 11.244 | 0.010 \n 20111005 | 05:18:05.5 | 2455839.719985 | J | 11.509 | 0.010 \n 20111005 | 05:21:06.0 | 2455839.722074 | Y | 11.854 | 0.010 \n 20111005 | 05:24:06.5 | 2455839.724163 | Z | 12.914 | 0.010 \n 20111005 | 05:26:46.5 | 2455839.726015 | Z | 12.903 | 0.010 \n ----------------------------------------------------------- \n \nUKIRT is funded by the UK-STFC. The data reduction and distribution are performed by the CASU and WFAU respectively.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Circumstellar disk", "Magnetar", "Repeater" ] }, "answerKey": "A" }, { "id": "atel_4175", "message": "Title: MAXI/GSC detection of a new soft X-ray transient MAXI J1647-227\nAuthors: H. Negoro (Nihon U.), S. Nakahira (JAXA), Y. Tsuboi, M. Higa (Chuo U.) M. Morii (Tokyo Tech), T. Yamamoto (RIKEN), S. Ueno, H. Tomida, M. Ishikawa (JAXA), T. Mihara, M. Serino, M. Sugizaki, J. Sugimoto, M. Matsuoka (RIKEN), N. Kawai, R. Usui, K. Ishikawa (Tokyo Tech), M. Nakajima, M. Asada, H. Sakakibara, N. Serita (Nihon U.), A. Yoshida (AGU), H. Tsunemi, M. Kimura (Osaka U.), Y. Ueda, K. Hiroi, M. Shidatsu, R. Sato (Kyoto U.), M. Yamauchi, Y. Nishimura, T. Hanayama, K. Yoshidome (Miyazaki U.), K. Yamaoka (Waseda U.) report on behalf of the MAXI team\nDate: 15 Jun 2012; 12:57 UT\nProvenance: Hitoshi Negoro (negoro@phys.cst.nihon-u.ac.jp)\nSubjects: X-ray, Binary, Black Hole, Cataclysmic Variable, Neutron Star, Star, Transient, Variables\nDescription: Referred to by ATel #: 4178, 4179, 4192, 4204\nOn 14 June 2012, the MAXI/GSC detects enhanced soft X-ray emission at a posittion:\n(R.A., Dec) = (+251.96 deg, -22.75 deg) = (16 47 50, -22 44 59) (J2000)\nwith a statistical uncertainty of 0.54 deg at the 90% confidence limit and an additional systematic uncertainty of 0.1 deg (90% containment radius). There is no bright known X-ray source within the error circle, and we tentatively name the source MAXI J1647-227.\nThe enhanced emission has been recognized since 12 June 2012 from daily images, and the one-day averaged fluxes on 14 June are 23+-6 mCrab in the 2-4 keV band and 33+-7 mCrab in the 4-10 keV band.\nWe note that there is a nearby star forming region Rho Oph dark cloud, separated by about 1 degree from the source. It is also possible that the source is a new black hole candidate or neutron star in the soft state. Followup observations are encouraged to reveal the nature of the source.\nThe latest light curves and images of MAXI J1647-227 by MAXI/GSC will be placed at the following URL: http://maxi.riken.jp/top/index.php?cid=1&jname=J1647-227 \nMAXI home page", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Exoplanet", "Galaxy, Neutron star", "Variable star, Neutron star", "Black hole, Neutron star" ] }, "answerKey": "D" }, { "id": "atel_4375", "message": "Title: Detection of new X-ray transient in M 31\nAuthors: F. Hofmann, W. Pietsch, R. Sturm, J. Greiner, F. Haberl, M. Henze (Max-Planck-Institut fuer extraterrestrische Physik, MPE)\nDate: 14 Sep 2012; 16:12 UT\nProvenance: Wolfgang Pietsch (wnp@mpe.mpg.de)\nSubjects: X-ray, Transient\nDescription: In an observation of the M 31 central region with the X-ray telescope (XRT) on board the Swift satellite (ObsId 0035336069, start time 2012-09-13.16 UT, exposure 2.64 ks), we detect about 60 counts from a new X-ray transient at position RA = 00h42m47.21 Dec = +41d14'05.5\" (± 3.0\", J2000, 90% confidence) after correcting systematic offsets (Kaaret 2002, ApJ, 578, 114), which we name SWIFT J004247.2+411405. About half the counts are detected above 1 keV excluding a super-soft spectrum. However, a power law fit proposes a rather soft spectrum (photon index of >4). This is confirmed by the best fitting bremsstrahlung (kT = 0.42 keV, NH = 2.0 × 1021 cm-2) or disk black body models (kT = 0.27 keV, NH = 1.1 × 1021 cm-2). The unabsorbed luminosity in the 0.2-10 keV band is 4 × 1037 erg s-1. \n \nIn earlier observations with XMM-Newton EPIC, Chandra HRC I, and Swift XRT, the transient is not visible. The 3σ upper limit for a source at the transient position derived for the last Swift observation seven days before (ObsId 0035336068) is 6× 10-3 cts s-1. After this Swift observation, the source brightened at least by a factor of 4, compared to the last Chandra HRC I observation (ObsID 13281, starting on 2012-06-01.90 UT) by at least a factor of 40 (assuming the Swift spectrum above). \n \nSwift observation 0035336069 was split in 5 slots spread over 19 hours. There is no indication of strong time variability between the slots, excluding the possibility of a flaring Galactic star in the foreground. The timing and spectral behavior suggests that SWIFT J004247.2+411405 is a transient low mass X-ray binary system (likely a black hole system) detected in the soft state. \n \nWe would like to thank the Swift Team for making these observations possible, in particular N. Gehrels, the duty scientists as well as the science planners.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system", "Neutron star", "Black hole", "Nova" ] }, "answerKey": "C" }, { "id": "atel_4425", "message": "Title: Re-brightening of SN2009ip in the UV\nAuthors: R. Margutti, A. Soderberg, R. Chornock, R. Foley (Harvard University)\nDate: 26 Sep 2012; 13:56 UT\nProvenance: Raffaella Margutti (rmargutti@cfa.harvard.edu)\nSubjects: Ultra-Violet, X-ray, Supernovae\nDescription: Referred to by ATel #: 4430, 4431, 4435, 4439, 4479\nSN2009ip has been recently suggested to have transitioned from LBV-like eruption episodes to a real type-IIn supernova explosion (Smith, Atel#4412). We performed a Swift/UVOT follow-up observation on Sept 22, and found no clear evidence for a re-brightening (Margutti et al., Atel #4414), in agreement with the results reported by Martin et al., (Atel #4416). Further observations were planned and executed starting from 2012-09-26T05:32:41 UT. We obtained Swift-UVOT observations in the 6 optical/UV filters. SN2009ip is well detected in all the 6 filters with preliminary magnitudes (UVOT photometric system Breeveld et al. 2011, arXiv:1102.4717): v= 14.90 +/- 0.04; b= 14.78 +/- 0.04; u=13.43 +\\\\- 0.04; w1= 13.00 +/- 0.05; m2= 12.82 +\\\\- 0.06; w2= 12.85 +\\\\- 0.07 . The magnitudes listed include possible contamination from the underlying host galaxy and are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.03 in the direction of the transient (Schlegel et al. 1998). These observations indicated that SN2009ip has re-brightened by ~3 mag in ~3.5 days (v-band), in agreement with the findings by Brimacombe in the I-band (Atel # 4423). The re-brightening is even more extreme in the UV, with the w1 flux increasing by ~6 mag in ~3.5 days. This corresponds to a drastic change in the optical to UV colors (w1-v= 1.1 on Sept 22nd; w1-v=-1.9 on Sept. 26th). Contemporaneous Swift-XRT observations revealed no source at the optical position of the transient, with a 3 sigma upper limit of 3.5d-3 cps in the 0.3-10 keV energy band (total exposure of 4.3 ks). The Galactic neutral hydrogen column density in the direction of the event is 1.2d20 /cm2 (Kalberla 2005). Assuming a spectral photon index ~2, this translates into an absorbed flux of ~2d-13 erg/s/cm2 (corresponding to a luminosity of ~1d40 erg/s. A luminosity distance of 24 Mpc has been used). We thank the Swift team for scheduling these ToO observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Minor body", "Nova", "Globular cluster" ] }, "answerKey": "A" }, { "id": "atel_4525", "message": "Title: PSN J03333599-3607377 in NGC 1365 is a Young Type Ia Supernova\nAuthors: M. Childress, G. Zhou, B. Tucker, D. Bayliss, R. Scalzo, F. Yuan, B. Schmidt (Australian National University)\nDate: 28 Oct 2012; 22:08 UT\nProvenance: Michael Childress (mjc@mso.anu.edu.au)\nSubjects: Optical, Supernovae\nDescription: We obtained a spectrum of PSN J03333599-3607377 in NGC 1365 (see Klotz & Conseil ATel #4523) on 2012 October 28.53 with the Wide Field Spectrograph (WiFeS - Dopita et al., 2007, ApSS, 310, 255) on the ANU 2.3m telescope at Siding Spring Observatory, NSW Australia, using the B3000/R3000 gratings (3600-10000 A, 1 A resolution). The object displays clear signatures of a young Type Ia Supernova, including the Si 6355 line observed at 5910 (22,000 km/s), and broad high velocity Ca IR triplet observed at 7700. The object spectrum was compared to supernova spectral templates using SNID (Blondin & Tonry, 2007, ApJ, 666, 1024) and the best SN Ia match was SN 2001W at -11 days and redshift z=0.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Active galactic nucleus", "Nova", "Star and stellar system" ] }, "answerKey": "A" }, { "id": "atel_4620", "message": "Title: PESSTO spectroscopic classification of optical transients\nAuthors: L. Le Guillou, S. Baumont (LPNHE), K. Maguire, Y. Pan (Oxford), M. Sullivan (Southampton), S. Taubenberger (MPA Garching), S. Valenti (UCSB/LCOGT), A. Pastorello, S. Benetti (INAF - Padova Astronomical Observatory), S. J. Smartt, K. Smith, D. Young (Queen's University Belfast), A. Gal-Yam, O. Yaron (Weizmann Institute for Science), C. Baltay, N. Ellman, E. Hadjiyska, R. McKinnon, D. Rabinowitz, E. S. Walker (Yale University), U. Feindt, M. Kowalski (Universitat Bonn), P. Nugent (LBL Berkeley)\nDate: 5 Dec 2012; 14:54 UT\nProvenance: Sylvain Baumont (baumont@lpnhe.in2p3.fr)\nSubjects: Optical, Supernovae\nDescription: PESSTO, the Public ESO Spectroscopic Survey for Transient The Objects (see Valenti et al., ATel #4037; http://www.pessto.org ), reports the following supernova classifications. Targets were supplied by the La Silla-Quest survey (see Hadjiyska et al., ATel #3812) and the Catalina Real-time Transient Survey (http://crts.caltech.edu/). All observations were performed on the ESO New Technology Telescope at La Silla on 2012 December 04, using EFOSC2 and Grism 13 (3985-9315A, 18A resolution). Classifications were done with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024) and GELATO (Harutyunyan et al., 2008, A&A, 488, 383). Classification spectra can be obtained from http://www.pessto.org (via WISeREP). \n \n \n Name | RA (J2000) | Dec (J2000) | Disc. Date | Disc. Source | Disc Mag | z | Type | Phase | Notes \n \n LSQ12gwy | 10 43 32 | -13 17 20 | 20121201 | LSQ | 15.4 | 0.018 | Ia | +14d |", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Variable star", "Near-Earth object", "Stellar evolution" ] }, "answerKey": "A" }, { "id": "atel_4700", "message": "Title: MASTER prediscovery observations of SSS130101:122222-311525\nAuthors: H. Levato, C. Saffe (ICATE), C. Mallamaci, C. Lopez and F. Podest (Observatorio Astronomico Felix Aguilar; OAFA), D. Denisenko, V. Lipunov, E. Gorbovskoy, P. Balanutsa, V. Yecheistov, N. Tiurina, V. Kornilov, A. Belinski, N. Shatskiy, V. Chazov, A. Kuznetsov, D. Zimnukhov (Moscow State University, SAI), V. Krushinsky, I. Zalozhnih, A. Popov, A. Bourdanov, A. Punanova (Ural Federal University), K. Ivanov, S. Yazev, N. Budnev, E. Konstantinov, O. Chuvalaev, V. Poleshchuk, O. Gress (Irkutsk State University), A. Parkhomenko, A. Tlatov, D. Dormidontov, V. Senik (Kislovodsk solar station of the Pulkovo observatory RAS), V. Yurkov, Y. Sergienko, D. Varda, E. Sinyakov (Blagoveshchensk Educational University), V. Shumkov, S. Shurpakov, P. Podvorotny (MASTER team members), \nDate: 4 Jan 2013; 14:31 UT\nProvenance: Vladimir Lipunov (lipunov2007@gmail.com)\nSubjects: Optical, Cataclysmic Variable, Transient\nDescription: Referred to by ATel #: 4716, 4744, 4785\nFollowing the announcement of a bright transient SSS130101:122222-311525 detected by CRTS (Drake et al., ATel #4699) we have checked the archival observations of this field by MASTER-ICATE very wide field camera (72-mm f/1.2 lens + 11 Mpx CCD, FOV=24x16 sq. deg.) located at OAFA near San Juan, Argentina. The object is present on two combined images obtained on 2012 Dec. 16.357 UT (total exposure time 122 sec) and 2012 Dec. 17.248 UT (292 sec). The magnitude on both dates is 11.8+/-0.2m (unfiltered with Tycho-2 V zero point). \nOn Dec. 16 image the OT was located at 102 pixels from the edge of 4008x2672 CCD field of view. 200x200 crop of Dec. 16 MASTER-WFC image (zoomed at 200%) is posted at http://master.sai.msu.ru/static/OT/J122222-311525-MASTER-Arg-Dec16.jpg \nMASTER-ICATE observations are showing that this OT was already in outburst at least 10 days before the Kyoto/Kiso Wide-field Survey images reported by H. Maehara in [vsnet-alert 15240] and 16 days before Siding Spring Survey detection. The last MASTER-WFC image of this area of sky without OT was taken on 2012 July 11.946 UT (combined exposure 280 sec, limiting mag 12.6). \nList of optical transients discovered by MASTER\nGlobal MASTER Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk, Supernova", "Active galactic nucleus, Supernova", "Nova, Supernova", "Nova, Interstellar medium" ] }, "answerKey": "C" }, { "id": "atel_4770", "message": "Title: Swift detection of increased X-ray activity from gamma-ray flaring blazar PKS 1424-41\nAuthors: Stefano Ciprini (ASI ASDC & INAF OAR Rome), Sara Cutini (ASI ASDC & INAF OAR Rome) on behalf of the Fermi Large Area Telescope Collaboration\nDate: 30 Jan 2013; 17:25 UT\nProvenance: Stefano Ciprini (stefano.ciprini@asdc.asi.it)\nSubjects: X-ray, Gamma Ray, >GeV, Request for Observations, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 4775, 4819\nFollowing enduring gamma-ray flaring activity of the flat spectrum radio quasar PKS 1424-41 (also known as 2FGL J1428.0-4206, Nolan et al. 2012, ApJS, 199, 31) detected by Fermi LAT during January 2013, two Swift target of opportunity observations were performed on January 24 and 27, 2013. Recent gamma-ray and X-ray flaring activity from the source was observed on January 6 and January 7 (ATel#4714 and ATel #4717). Gamma-ray flaring activity was observed in the period January 13 - 27 when Fermi LAT detected daily-averaged gamma-ray fluxes (E>100MeV) ranging from about 2.0x 10^-6 to 2.6x 10^-6 photons cm^-2 s^-1. PKS 1424-41 is one of the \"LAT Monitored Sources\", and consequently, a preliminary, uncalibrated estimation of the daily gamma-ray flux observed by Fermi LAT is publicly available at: http://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/PKS_1424-41. \nSwift XRT data were taken in Photon Counting mode in two pointings of total exposure of about 2 ksec each. Preliminary analysis indicates that the X-ray spectrum (0.3-10 keV) of PKS 1424-41 can be fit by an absorbed power law model with an HI column density consistent with the Galactic value in the direction of the source (n_H = 7.7 x 10^20 cm^-2, Kalberla et al. 2005, A&A, 440, 775) and a photon index of 1.4+/-0.2 and 1.5+/-0.2 for the observation performed on January 24 and January 27, respectively. The corresponding observed 0.3-10 keV fluxes are (6.5+/-0.3) x10^-12 erg cm^-2 s^-1 and (6.2+/-0.3) x10^-12 erg cm^-2 s^-1 respectively, higher than the flux observed by Swift XRT on January 7 that was (5.5+/- 0.4)x10^-12 erg cm^-2 s^-1. Swift UVOT observed PKS 1424-41 in UV bands on January 24 and 27 detecting U band (350.1 nm) filter magnitudes of 15.03+/-0.01 and 14.98+/-0.01 respectively, and W1 band (263.9 nm) filter magnitude of 15.57+/-0.01 on January 27. \nFurther multiwavelength observations are encouraged. For this source the Fermi LAT contact person is F. Longo (francesco.longo@ts.infn.it). \nWe would like to thank the Swift Team for making these observations possible, in particular B. Sbarufatti and D. Malesani as Swift Observatory Duty Scientists.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Minor body", "Active galactic nucleus, Nova", "Active galactic nucleus, Black hole", "Active galactic nucleus, Galaxy" ] }, "answerKey": "C" }, { "id": "atel_4850", "message": "Title: Disappearance of the Supergiant Progenitor of SN 2011dh in M51\nAuthors: Schuyler D. Van Dyk (IPAC/Caltech), Alexei V. Filippenko, Ori Fox, Patrick Kelly (UC Berkeley), and Nathan Smith (University of Arizona)\nDate: 2 Mar 2013; 22:28 UT\nProvenance: Schuyler D. Van Dyk (vandyk@ipac.caltech.edu)\nSubjects: Optical, Supernovae\nDescription: Referred to by ATel #: 4912\nWe report that in Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3) observations at F555W and F814W with the UVIS channel, conducted on 2013 March 2 UT as part of our Cycle 20 Snapshot program GO-13029 (PI: A. Filippenko), we have discovered that the yellow supergiant star, identified by Van Dyk et al. (2011, ApJ, 741, L28) and Maund et al. (2011, MNRAS, 739, L37) at the position of the Type IIb SN 2011dh in M51, has vanished. From preliminary photometry extracted from the 2013 images using Dolphot v2.0 (Dolphin 2000, PASP, 112, 1383), the HST flight-system magnitudes of the object seen at the position of the supergiant and SN are F555W = 23.20 +/- 0.02 and F814W = 22.51 +/- 0.02 mag. The brightness of the supergiant in, e.g., Van Dyk et al. (2011) was F555W = 21.86 +/- 0.01 and F814W = 21.22 +/- 0.01 mag. It is therefore evident that the yellow supergiant has disappeared, making it highly likely that it was the star that actually exploded (in agreement with the theoretical analyses by Bersten et al. 2012, ApJ, 757, 31 and Benvenuto, Bersten, & Nomoto 2013, ApJ, 762, 74, and the conclusions of Maund et al. 2011). Additionally, there is no obvious presence of a light echo around the SN in the 2013 images. Further analysis is ongoing.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system", "Variable star", "Neutron star", "Stellar evolution" ] }, "answerKey": "A" }, { "id": "atel_4925", "message": "Title: IGR J18245-2452: a new hard X-ray transient discovered by INTEGRAL\nAuthors: D. Eckert (ISDC, Switzerland), M. Del Santo, A. Bazzano (INAF/IAPS Rome, Italy), K. Watanabe (FGCU, USA), A. Paizis (INAF-Milano, Italy), E. Bozzo, C. Ferrigno (ISDC, Switzerland), I. Caballero (CEA, France), L Sidoli (INAF-IASF Milano, Italy), L. Kuiper (SRON, Netherlands)\nDate: 29 Mar 2013; 11:18 UT\nProvenance: E. Bozzo (enrico.bozzo@unige.ch)\nSubjects: X-ray, Gamma Ray, Request for Observations, Black Hole, Neutron Star, Transient\nDescription: Referred to by ATel #: 4927, 4929, 4934, 4959, 4960, 4961, 4964, 4981, 5003, 5031, 5045, 5068, 5069, 5086\nDuring the observations of the Galactic Center performed on 2013 March 28 from 2:56 to 17:38 (UTC), the hard X-ray imager IBIS on-board INTEGRAL detected a new transient source, dubbed IGR J18245-2452, at: \nRA=276.1383 \nDEC=-24.8793 \nwith an associated uncertainty of 1.4 arcmin (all uncertainties are given at 90% c.l.).\nThe source is detected at a significance level of 21 sigma in the 20-40 keV energy band and 15 sigma in the 40-80 keV energy band. The corresponding fluxes estimated from the ISGRI mosaic are 45.8+/-2.0 mCrab and 44.0+/-2.8 mCrab, respectively.\nThe ISGRI spectrum (effective exposure time 32 ks) can be reasonably well fit with a power-law model. We estimated a photon index of 2.1+/-0.2. and a 20-100 keV X-ray flux of 9E-10 erg/cm^2/s.\nThe source was outside the JEM-X FOV during the entire observation.\nWe note that the ISGRI position of the source is compatible with that of the Globular Cluster M 28.\nFurther INTEGRAL observations of the region around IGR J18245-2452 are already scheduled for the next days. \nMulti-wavelength follow-up observations of IGR J18245-2452 are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Globular cluster", "Neutron star", "Black hole" ] }, "answerKey": "D" }, { "id": "atel_5070", "message": "Title: Search for pulsed radio emission from PSR J1745-2900 at 1 GHz with the GMRT\nAuthors: M. P. Surnis, B. C. Joshi, S. Roy (National Centre for Radio Astrophysics, Pune, India)\nDate: 17 May 2013; 17:48 UT\nProvenance: Bhal Chandra Joshi (bcj@ncra.tifr.res.in)\nSubjects: Radio, Neutron Star, Soft Gamma-ray Repeater, Pulsar\nDescription: We have observed, with the GMRT, PSR J1745-2900, which was discovered following an X-ray flare by Swift, accompanied by 35-ms flare (ATEL #5006, #5009). Pulsating high energy and radio emission with a period of 3.76 s have been subsequently reported with emission properties and estimated surface magnetic field consistent with a magnetar (ATEL #5020, #5032, #5035, #5040, #5043, #5046, #5053, #5058). The observations were carried out at the source position provided in ATEL #5032 with 14 antenna of the GMRT used as a phased array at 1041 GHz. Data from 512 channels across 33.33333 MHz band were recorded with a sampling time of 1 ms on 2013-05-09 at 22:52:19 UTC for 1.0 hours. The data were incoherently dedispersed to 476 trial DMs ranging from 0 - 2000 pc cm^-3 followed by a harmonic and single pulse search. No significant radio pulsations were detected. We estimate an upper limit on flux density of 0.4 mJy for 30% duty cycle (system temperature ~ 140 K - Treceiver 70K and Tsky 70 K). We estimate an upper limit of 37 mJy for individual bursts. Our non-detection is consistent with high scatter-broadening for the pulsar implying a large DM. Thus, the pulsar is unlikely to be detected at frequencies lower than 1 GHz. Further, we do not find any other pulsar candidate at low DM (< 100 pc cm^-3). Strong RRAT like bursts, useful to constrain scatter-broadening, may be detectable, but we do not detect such bursts in our observations. The field was imaged using 22 antennas of the GMRT simultaneously with the time-series observations. The source lies within ~1 synthesised beamwidth away from Sgr A*. Due to very high confusion from Sgr A* at its vicinity at our waveband, we cannot put an upper limit on its continuum flux density.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Pulsar", "Galaxy", "Binary system" ] }, "answerKey": "A" }, { "id": "atel_5150", "message": "Title: X-ray detection of SN 2013df\nAuthors: K. L. Li and A. K.H. Kong (National Tsing Hua University, Taiwan)\nDate: 20 Jun 2013; 10:37 UT\nProvenance: Albert Kong (akong@phys.nthu.edu.tw)\nSubjects: X-ray, Supernovae, Transient\nDescription: Referred to by ATel #: 8452\nFollowing the report of a progenitor search of the Type IIb supernova 2013df (CBET #3557), a series of Swift ToO observations have been triggered since 2013 June 13 (5.5 days after the discovery). Eight observations have been taken till 2013 June 19. From the combined 14.1 ks X-Ray Telescope (XRT) observation, a hard X-ray source is seen at RA, Dec (J2000)=12h26m29.52s, +31d13m37.5s (186.6230, 31.2271) with an uncertainty of 3.8 arcsec (radius, 90% confidence), which is just 2.1 arcsec offset from the SN position (ATel #5139). There is no significant X-ray source detected at the same position in the 1.7 ks Chandra observation taken in 2000 (ObsId: 1639; PI: Garmire). \nThe average X-ray spectrum can be described by an absorbed power law with a photon index of 1.51 (+0.23, -0.19) and a column density of N(H)=6e20 cm^-2 obtained from the Leiden/Argentine/Bonn (LAB) map (z=0.002395 is assumed). The inferred average luminosity (absorption corrected) is about 7e39erg/s (0.3-10 keV), which is similar to previous X-ray detected SNe (see Immler & Lewin (2003)). The hard X-ray spectrum also suggests that the X-ray emissions at the SN position are very unlikely the diffuse emission of the host galaxy NGC 4414. From the X-ray lightcurve, the emission decayed gradually within the first 4e5 seconds since the trigger and showed a strong variation in the later observations. \nMore multi-wavelength follow-up observations are strongly encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy", "Supernova", "Neutron star", "Variable star" ] }, "answerKey": "B" }, { "id": "atel_5275", "message": "Title: SN 2013ej is a Highly Polarized Type II-Plateau Supernova\nAuthors: Posted by D. C. Leonard (San Diego State University), G. Pignata (Universidad Andres Bello), L. Dessart (Laboratoire d'Astrophysique de Marseille), D. Hillier (University of Pittsburgh), H. G. Khandrika, A. A. Rachubo, R. D. Fahad, S. J. Hadden (San Diego State University), L. Gonzalez (University of California, San Diego)\nDate: 13 Aug 2013; 22:00 UT\nProvenance: D. C. Leonard (leonard@astro.caltech.edu)\nSubjects: Optical, Supernovae\nDescription: We report photometric and spectropolarimetric observations of the young Type II supernova SN 2013ej (PSN J01364816+1545310; CBET #3606) that establish its membership in the (photometrically defined) Type-II Plateau subclass and reveal unusually strong polarization at a very early phase. \nWe present the following optical (B, V, R_C, I_C) photometry from observations taken at Mount Laguna Observatory's 1-m reflector: \n \n \n UT | Day* | B | V | R_C | I_C \n 2013-07-31.37 | 5.99 | 12.64 | 12.65 | 12.58 | 12.47 \n 2013-08-03.37 | 8.99 | 12.59 | 12.52 | 12.44 | 12.30 \n 2013-08-06.41 | 12.03 | 12.69 | 12.53 | 12.41 | 12.28 \n 2013-08-10.44 | 16.06 | 12.83 | 12.50 | 12.34 | 12.19 \n \n*Day since discovery, 2013-07-25.38 UT (CBET #3609), which is likely within 2 days of explosion (ATEL #5237). \nThe data were calibrated against local standard stars provided by Foley et al. (2003, PASP, 115, 1220); uncertainties are estimated to be ~0.03 mag. The data demonstrate that SN 2013ej has begun a photometric plateau in the V, R_C, and I_C bands, and so we propose a Type II-Plateau (II-P) classification for this core-collapse event. From comparison with light curve templates derived from observations of SN 1999gi (Leonard et al. 2002, AJ, 124, 2490), we conclude that B-band maximum was achieved within about one day of our 2013-08-03.37 (~day 9) observation. \nWe obtained spectropolarimetry of SN 2013ej on Aug. 1.35 UT (~day 7) with the ESO Very Large Telescope (+ FORS2 in polarimetric mode; range 430-920 nm, resolution 1.2 nm). The flux spectrum resembles those of SNe II-P at similarly early epochs, presenting a smooth, blue continuum with broad P-Cyg features corresponding to H_alpha, H_beta, He I (587.6 nm), and N II (P-Cyg absorptions near 450.0 nm and 550.0 nm; see Dessart & Hillier 2006, A&A 447, 691) all evident. In addition, we note a strong absorption feature centered at 615.0 nm, in the blue wing of the H_alpha P-Cyg trough. This feature may be attributed to Si II (635.5 nm), although it is unusually strong for this early epoch. This may point to peculiar ionization conditions at the photosphere, perhaps related to a non-standard red supergiant envelope at explosion. An alternative origin for such a blue notch in the H_alpha trough is circumstellar interaction (Chugai et al. 2007, ApJ, 662, 1136). The ejecta velocity, as deduced from the minimum of H_beta, is about 10,500 km/s. \nThe observed spectropolarimetry (uncorrected for interstellar polarization -- ISP) are characterized by significant polarization that decreases from ~1.3% at 430 nm to ~1.0% at 920 nm, with marked modulations of up to ~0.6% occurring across all strong P-Cyg line features. To our knowledge, these are the earliest spectropolarimetry data yet obtained for this class of SN. Such strong early-time polarization is unusual for an SN II-P (e.g. Leonard et al. 2001, ApJ, 553, 861) but not without precedent: SN 2012aw showed moderate polarization (~0.5%) at an early phase (~day 17) that exhibited a similar wavelength dependence (ATEL #4033). While some portion of the observed continuum polarization of SN 2013ej may be due to (an as-yet unknown) ISP, the strength of the line features suggests that much of it is intrinsic to the SN. This implies substantial asymmetries in the electron-scattering atmosphere of the outer ejecta at these early times (Dessart & Hillier 2011, MNRAS, 415, 3497). \nFurther spectropolarimetry observations from VLT are planned, and we gratefully acknowledge the effort of the entire observing staff at ESO-Paranal for the prompt execution of our spectropolarimetry ToO request. D.C.L. thanks the NSF for support through grants AST-1009571 and AST-1210311, and L.D. thanks the Agence Nationale de la Recherche for support through grant ANR-11-BS56-007.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Globular cluster", "Supernova", "Nova" ] }, "answerKey": "C" }, { "id": "atel_5325", "message": "Title: Erratum to the OGLE-IV Transient Search report 24 August 2013\nAuthors: L. Wyrzykowski (Warsaw University Astronomical Observatory, Poland)\nDate: 26 Aug 2013; 12:11 UT\nProvenance: Lukasz Wyrzykowski (wyrzykow@ast.cam.ac.uk)\nSubjects: Optical, Supernovae, Transient\nDescription: This is a correction to our ATel #5321. \nThe supernova labeled OGLE-2013-SN-055 is a duplicate entry for another transient found earlier by the OGLE-IV Transient Search, OGLE-2013-SN-034 (ATel #5204). \nWe apologise for any confusion it might have caused. We thank David Bishop for his thoroughness which allowed him to spot this error. \nOGLE-IV Transient Survey light curves and finding charts.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Supernova", "Minor body", "Quasar" ] }, "answerKey": "B" }, { "id": "atel_5400", "message": "Title: FIRE near-infrared spectroscopic classifications of PSN J19590795-5555466\nAuthors: E. Y. Hsiao (LCO), G. H. Marion (UT Austin, CfA), Y. Beletsky (LCO), S. Parker (BOSS), M. M. Phillips (LCO)\nDate: 18 Sep 2013; 20:53 UT\nProvenance: Eric Hsiao (hsiao@lco.cl)\nSubjects: Infra-Red, Optical, Supernovae\nDescription: We report the spectroscopic classification of PSN J19590795-5555466 using a near-infrared spectrum (range 800-2400 nm) obtained with the FoldedPort Infrared Echellette (FIRE) spectrograph on the 6.5-m Magellan Baade Telescope at Las Campanas Observatory. The near-infrared spectrum of PSN J19590795-5555466 is most similar to that of Type Ib supernova SN 2008ax near maximum (Chornock, R. et al, 2011, ApJ, 739, 41) at an approximate redshift of 0.02. The faint host galaxy is anonymous, and its redshift is unknown. Several near-infrared He I P Cygni profiles are present at approximately 10000 km/s, assuming a redshift of 0.02.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Supernova", "Stellar evolution", "Accreting object" ] }, "answerKey": "B" }, { "id": "atel_5460", "message": "Title: ASAS-SN Discovery of a Candidate Supernova in Uncatalogued Galaxy \nAuthors: J. L. Prieto (Princeton), K. Z. Stanek, B. J. Shappee, C. S. Kochanek, T. W-S. Holoien, J. Jencson, U. Basu, J. F. Beacom (Ohio State), D. Szczygiel, G. Pojmanski (Warsaw University Observatory), M. Dubberley, M. Elphick, S. Foale, E. Hawkins, D. Mullins, W. Rosing, R. Ross, Z. Walker (Las Cumbres Observatory), J. Brimacombe (Coral Towers Observatory), D. Berssier (LJMU)\nDate: 10 Oct 2013; 23:59 UT\nProvenance: Jose L. Prieto (jose@obs.carnegiescience.edu)\nSubjects: Optical, Supernovae, Transient\nDescription: Referred to by ATel #: 5469, 5508, 5707\nDuring the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or \"Assassin\"), using data from the double 14-cm \"Brutus\" telescope in Haleakala, Hawaii, we discovered a new optical transient source, likely a supernova: \n \n \n Object RA(J2000) Dec(J2000) Disc. UT Date Disc. V Mag \n ASASSN-13dl 07:38:49.54 +58:12:43.3 2013-10-10.51 16.76 \n \nASASSN-13dl was discovered in images obtained on UT Oct 10.51, but was also present in images obtained Oct. 4.5 at V~17 mag. The source was undetected (V>17 mag) in images obtained on Sep. 29 and earlier. This figure shows the ASAS-SN discovery image and an archival DSS image. The transient is approximately 2\" from the center of an uncatalogued galaxy detected in DSS images. \nFor more information about the ASAS-SN project see the ASAS-SN Homepage and also ASAS-SN Transients page.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Globular cluster", "Quasar", "Supernova", "Accreting object" ] }, "answerKey": "C" }, { "id": "atel_5575", "message": "Title: Optically thin synchrotron emission from XTE J1908+094 observed by the ATCA\nAuthors: M. Coriat (Univ. Cape Town), Tasso Tzioumis (ATNF), S. Corbel (Univ. Paris Diderot & CEA Saclay), R. Fender (Oxford)\nDate: 12 Nov 2013; 19:34 UT\nProvenance: Mickael Coriat (mickael@coriat.eu)\nSubjects: Radio, X-ray, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 12628\nThe black hole candidate XTE J1908+094, currently in outburst (Krimm et al. ATel #5523, Atel #5529; Miller-Jones et al. Atel #5530; Rushton et al. Atel #5532), recently started a hard-to-soft state transition (Negoro et al. Atel #5549). Rushton et al. (ATel #5551) reported a significant increase of the radio flux density at 16.3 GHz from 0.93 mJy on 2013-11-04T14:22-18:19 to 7.3 mJy on 2013-11-05T14:27-20:24 UT suggesting the ejection of optically thin radio-emitting plasma as usually associated with a hard-to-soft state transition. \nWe report on ATCA observations of XTE J1908+094 conducted on 2013-11-07T04:57-08:29 at 5.5 GHz, 9 GHz, 17 GHz and 19 GHz. The source was detected at all frequency bands with the following flux densities: \n \n5.5 GHz: 1.51 +/- 0.04 mJy \n9 GHz: 1.05 +/- 0.04 mJy \n17 GHz: 0.51 +/- 0.05 mJy \n19 GHz: 0.27 +/- 0.06 mJy \n \nwhich implies a spectral index alpha = -0.92 +/- 0.13 (S = k nu^+alpha). We therefore confirm the optically thin synchrotron nature of the radio flare reported by Rushton et al. (ATel #5551) which has significantly faded compare to the 7.3 mJy detected at 16.3 GHz two days earlier. However, multiple flares can be expected while the source is transiting toward the soft X-ray state. We therefore encourage a regular monitoring of the source at multiple wavelengths. \nWe did not resolve any radio emitting structure separated from the core down to a beam size of 0.3 by 12.5 arcsec (at 19 GHz) oriented 2.8 degrees west of north. \n \nWe thank Phil Edwards for the rapid scheduling of these observations", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Globular cluster", "Black hole", "Interstellar medium" ] }, "answerKey": "C" }, { "id": "atel_5670", "message": "Title: ROTSE-III observation of a new outburst of Dwarf Nova AL Com\nAuthors: G. Dhungana, F. V. Ferrante, R. Kehoe (Southern Methodist University)\nDate: 17 Dec 2013; 10:19 UT\nProvenance: Farley Ferrante (fferrante@smu.edu)\nSubjects: Optical, Cataclysmic Variable, Nova, Transient, Variables\nDescription: Referred to by ATel #: 7235\nWe report on a new outburst of the WZ Sge-type dwarf nova AL Comae Berenices in unfiltered CCD images with the 0.45-m ROTSE-IIIb telescope at McDonald Observatory, Texas. The transient, located at RA: 12:32:25.84 Dec: +14:20:42.5 (J2000.0; uncertainty ~ 1\"), was observed at mag 13.20 on Dec. 12.47 UT, at mag 13.39 on Dec. 14.46 UT, and at mag 13.51 on Dec. 16.44 UT. The limiting mag prior to detection was 15.5.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Circumstellar disk", "Galaxy", "Minor body" ] }, "answerKey": "A" }, { "id": "atel_5760", "message": "Title: The X-ray outburst of RX J0520.5-6932 is reaching the Eddington luminosity\nAuthors: G. Vasilopoulos, R. Sturm, P. Maggi, F. Haberl (MPE)\nDate: 14 Jan 2014; 14:49 UT\nProvenance: Pierre Maggi (pmaggi@mpe.mpg.de)\nSubjects: Optical, X-ray, Binary, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 5856\nWe report on the evolution of the current X-ray outburst of the LMC Be/X-ray binary pulsar RX J0520.5-6932 (see ATel #5673) from our Swift/XRT monitoring. Since the start of the outburst (2013 Dec 28) the luminosity of the source has continued to rise to a maximum of 1.91×1038erg s-1 (0.3-10 keV band), which is close to or at the Eddington limit for a neutron star. Given the brightness and duration of the event, we classify it as a Type II outburst. \nThe current spectrum of RX J0520.5-6932 can be best fitted by a power law with a photon index of 1.03. The luminosity evolution of the source, assuming a distance of 50 kpc, is presented in the table below. Luminosities before 2013 Dec 8 were converted from count rate assuming a power-law spectrum with a photon index ~0.7 (as measured on 2013 Dec 10) and an absorption column density of 6.44×1020cm-2. All other luminosities were derived from individual spectral fits. \nThe Be-star companion to RX J0520.5-6932 is also undergoing an outburst (see OGLE-IV XROM light curve): Since 2013 Dec 23 it brightened by ~0.1 mag. We encourage optical spectroscopy to measure the Hα line profile during this extraordinary bright phase. \n \n \n Date XRT count rate Luminosity (0.3-10 keV) \n [counts s-1] [1038 erg s-1] \n 2013 Nov 28 0.034±0.007 0.00854 \n 2013 Nov 30 0.075±0.010 0.0188 \n 2013 Dec 02 0.133±0.020 0.034 \n 2013 Dec 04 0.206±0.015 0.056 \n 2013 Dec 08 0.471±0.025 0.11 \n 2013 Dec 10 0.494±0.011 0.09 \n 2013 Dec 12 0.766±0.027 0.16 \n 2013 Dec 14 1.17±0.04 0.23 \n 2013 Dec 16 1.57±0.04 0.32 \n 2013 Dec 18 3.42±0.06 0.70 \n 2013 Dec 28 3.42±0.06 0.65 \n 2013 Dec 30 3.08±0.06 0.57 \n 2014 Jan 01.0 3.04±0.08 0.62 \n 2014 Jan 01.4 7.894±0.13 1.58 \n 2014 Jan 03 8.56±0.11 1.59 \n 2014 Jan 07 9.47±0.10 1.76 \n 2014 Jan 09 10.7±0.11 1.91 \n 2014 Jan 11 9.70±0.11 1.67 \n 2014 Jan 13 11.0±0.11 1.8 \n \n \n \n \n We thank the Swift team for accepting and scheduling the target of opportunity observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Pulsar", "Binary system, Interstellar medium", "Binary system, Near-Earth object", "Binary system, Pulsar" ] }, "answerKey": "D" }, { "id": "atel_5880", "message": "Title: Upper Limits on the VHE Gamma-Ray Flux of SN2014J in M82 From Observations by MAGIC\nAuthors: Max-Planck-Institute for Physics\nDate: 12 Feb 2014; 02:24 UT\nProvenance: Razmik Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de)\nSubjects: Gamma Ray, TeV, VHE, Supernovae\nDescription: The MAGIC collaboration observed SN2014J, the nearest supernova (SN) explosion in 10 years, located in the galaxy M82. The MAGIC observations started 6 days after the first detection by the UCL Observatory (CBET #3792) and amounted to a total of 5.4 hours. This Ia-type SN is unique and follow-up observations in all wavelengths have been pursued (i.e. ATel #5835, #5809, #5812, #5851). The SN was observed with the MAGIC telescopes from January 27 to 29 under moderate moonlight conditions and on February 1 and 2 under dark-night conditions. The preliminary analysis of these data resulted in an integral flux upper limit of 1.6e-12 cm-2 s-1 above the energy 300 GeV at 95% c.l. (this corresponds to ~1.3% of the Crab Nebula flux; for energies above 700 GeV the corresponding limit is ~2%), assuming a Crab-like spectral index. The daily flux upper limits (~1h observation per day) vary from 1.8e-12 to 18.e-12 cm-2 s-1 (E>300 GeV, 95% c.l.), due to different observational conditions. The VHE flux contribution from the host galaxy M82 was previously measured by VERITAS (Nature, 462, 700) at the level of 0.9% of the Crab flux for E>700 GeV. The MAGIC observations covered the maximum of the SN brightening (on Jan 31, mag=10.5 AAVSO data: PSN J09554214+6940260). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV. Questions regarding the MAGIC observations should be directed to Razmik Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and Christian Fruck (christian.fruck@gmail.com).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater", "Supernova", "Galaxy", "Variable star" ] }, "answerKey": "B" }, { "id": "atel_6000", "message": "Title: Moderate re-brightening of the transient magnetar SGR 0501+4516\nAuthors: M. Morii (RIKEN), T. Kohmura (Kogakuin Univ.), T. Sakamoto (Aoyama Gakuin Univ.), and N. Kawai (Tokyo Institute of Technology)\nDate: 22 Mar 2014; 14:23 UT\nProvenance: Mikio Morii (morii@hp.phys.titech.ac.jp)\nSubjects: X-ray, Soft Gamma-ray Repeater\nDescription: We observed the transient magnetar SGR 0501+4516 by Swift/XRT on 2014-03-16 (ObsID: 00033199001), and then found the flux enhancement at 0.17 +- 0.01 c/s in the 0.3 - 10.0 keV band after background subtraction. The XRT count rate of a previous observation on 2013-01-29 was 0.09 +- 0.02 c/s. It is the first detection of the flux increase after the source became in a quiescent state around early 2010. Our observation might indicate a sign of re-activation of this source. SGR 0501+4516 was discovered in August 2008 by typical SGR-like spiky short X-ray bursts (GCN #8112, ATel #1676). After this episode, the source flux was monitored by Swift/XRT. The peak flux on August 2008 was about 1.2 c/s. The gradual decay of the flux was found in this monitor data. The minimum flux was 0.03 +- 0.01 c/s on 2013-01-21. Here, all the fluxes are in the 0.3 - 10.0 keV band. Further Swift/XRT observation of SGR 0501+4516 is planned.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Magnetar", "Neutron star", "Galaxy" ] }, "answerKey": "B" }, { "id": "atel_6100", "message": "Title: Swift Follow up observation of the transient source Fermi J0641-0317\nAuthors: M. Ajello (Clemson University), D. Kocevski (GSFC/NASA), R. Buehler (DESY/Zeuthen), J. Becerra (GSFC/NASA), R. Ojha (GSFC/NASA) on behalf of the Fermi Large Area Telescope Collaboration\nDate: 25 Apr 2014; 19:05 UT\nProvenance: Marco Ajello (majello@clemson.edu)\nSubjects: X-ray, Gamma Ray, >GeV, Request for Observations, Transient\nDescription: Referred to by ATel #: 6101, 6122, 6139\nOn April 24, 2014 Swift carried out a 3 ks target of opportunity observation of the transient Fermi J0641-0317 (see ATel #6098). Only one bright source is detected by the Swift X-ray telescope (XRT) at RA, Dec = 06h 41m 51.5s, -03d 20' 49.2\" (J2000) with a 90 % error radius of 4.0 arcsec. The source is spatially coincident with the bright flat-spectrum radio source PMN J0641-0320. The XRT source, well described by an absorbed power law with absorption consistent with the Galactic one, displays a hard spectrum with a photon index of 0.93 (+0.43/-0.39) and a 2-10 keV flux of 4.9 (+1.0/-0.5) 12-12 erg cm-2 s-1. \n \nFollow up observations of Fermi J0641-0317 at longer wavelengths are encouraged. \n \nWe thank the Swift team and the Swift PI for promptly accepting and scheduling the ToO observation.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Globular cluster", "Galaxy", "Pulsar" ] }, "answerKey": "C" }, { "id": "atel_6180", "message": "Title: Optical observations Swift Transient in M31\nAuthors: Velasco S., Chinchilla P., Gómez M., Martinez C., Monteagudo L. (Instituto de Astrofísica de Canarias, Dpto Astrofísica Universidad de La Laguna)\nDate: 28 May 2014; 08:15 UT\nProvenance: Sergio Velasco (svelasco@iac.es)\nSubjects: Optical, Gamma-Ray Burst\nDescription: We report our optical observations of the M31 globular cluster G108 (Bo 45), associated with the transient reported by the Swift team (Barthelmy et al., GCN 16332) using 0.82 meter IAC-80 Telescope at Teide Observatory located in Tenerife (Spain) and operated by the Instituto de Astrofísica de Canarias. We obtained B, V and I band observations of the field on 2014 May 28 at 4:55 UT. Using 300s exposure times for V and I bands and 360s for the B band. We are able to clearly detect the source in each filter. Reference was selected on the same field, due to the lack of a well-photometric determined star, we have used values for Bol 50 Globular Cluster from Galleti S. et al., (2004A&A...416..917G). FILTER MAG ERR B 16.9±0.2 B-V 1.04 V-I 0.99 There are not any remarkable changes in the optical bands. Based on observations made with the IAC80 operated on the island of Tenerife by the ISC in the Spanish Observatorio del Teide.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Globular cluster", "Minor body", "Galaxy" ] }, "answerKey": "B" }, { "id": "atel_6270", "message": "Title: Radio Detection of SN 2014bc in NGC 4258 with eMERLIN\nAuthors: M. Argo (JBCA, Manchester), M. Perez-Torres (IAA-CSIC and CEFCA, Spain), A. Alberdi (IAA-CSIC), R. Beswick (JBCA, Manchester), J. Conway (OSO, Onsala), N. Elias-Rosa (INAF, Padova), R. Herrero-Illana (IAA-CSIC, Granada), R. Kotak (Queen's Univ. Belfast), P. Lundqvist (Stockholms Observatory), S. Mattila (Univ. of Turku), J. Marcaide (Univ. de Valencia), T. Muxlow (JBCA, Manchester), I. Marti-Vidal (OSO, Onsala), N. Ramirez-Olivencia (IAA-CSIC, Granada), C. Romero-Canizales (IA-PUC/MAS, Chile), C. Stockdale (Marquette University), E. Varenius (OSO, Onsala).\nDate: 25 Jun 2014; 14:55 UT\nProvenance: Miguel A. Perez-Torres (torres@iaa.es)\nSubjects: Radio, Supernovae\nDescription: We report the first detection at radio wavelengths of the type II SN 2014bc, using the electronic Multi-Element Radio Linked Interferometer Network (eMERLIN).SN 2014bc, initially dubbed PS1-14xz (also PSN J12185771+4718113) was discovered near (~100 pc) the core of NGC4258 (Messier 106; D=7.6 Mpc) by Smartt et al. (ATel #6156). KAIT unfiltered imaging by Zheng and Fillipenko (ATel #6159) showed the light curve of PS1-14xz to be consistent with a Type II-P SN, and a spectrogram confirmed the transient to be a Type II SN (Smartt et al. and Ochner et al. CBET 3877). The discovery images were taken on 2014 May 19.25 UT with the Pan-STARRS1 telescope. Unfiltered CCD images on 2014 May 9.98 did not detect the SN down to a limiting magnitude of 18.5 (very faint, pre-discovery, CBET 3877). \nWe observed SN 2014bc at a frequency of 1.51 GHz on 2014 May 23 with eMERLIN, using a total bandwidth of 512 MHz. The resulting synthesized Gaussian beam was of (0.15 x 0.13) sq. arcseconds. We centered our observations at the position of the optical discovery (RA(J2000.0)=12:18:57.71 and DEC(J2000.0)=47:18:11.3) and imaged a (113 x 113) sq. arcsecond region. We detected SN 2014bc with a peak flux density of 1.165 mJy/b at the following position: RA(J2000.0)=12:18:57.5034; DEC(J2000.0)=47:18:11.286. The off-source r.m.s. of the image was of 0.035 mJy/b. The above radio brightness corresponds to a monochromatic 1.51 GHz luminosity of (8.00 +/- 0.25)*1e25 erg/s/Hz. This value is typical of Type II-P SNe close to its peak radio luminosity. However, since our observations were taken when the SN was less than about 13 days old, the detection at 1.51 GHz would imply a very fast evolution for SN 2014bc, if it is indeed a type II-P SN (see, e.g. Fig. 4 in Romero-Canizales et. al 2014, MNRAS, 440, 1067). \nFurther observations of this nearby SN at radio and other wavelengths are planned to shed light on the CCSN type of SN 2014bc. \nWe thank the eMERLIN staff for supporting our ToO program on nearby core-collapse supernovae (Project code CY1204; PI: Perez-Torres).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Supernova", "Galaxy", "Binary system" ] }, "answerKey": "B" }, { "id": "atel_6360", "message": "Title: ASAS-SN Discovery of A Possible Supernova in PGC 053612\nAuthors: E. Conseil (Association Francaise des Observateurs d'Etoiles Variables), T. W.-S. Holoien, K. Z. Stanek, B. J. Shappee, A. B. Davis, C. S. Kochanek, J. Jencson, U. Basu, J. F. Beacom (Ohio State), J. L. Prieto (Diego Portales), D. Bersier (LJMU), J. Brimacombe (Coral Towers Observatory), I. Cruz (Cruz Observatory), S. Kiyota (Variable Star Observers League in Japan), W. Wiethoff (Arrowhead Astronomical Society of Duluth), D. Szczygiel, G. Pojmanski (Warsaw University Observatory)\nDate: 2 Aug 2014; 00:18 UT\nProvenance: Thomas Holoien (tholoien@astronomy.ohio-state.edu)\nSubjects: Optical, Supernovae, Transient\nDescription: Referred to by ATel #: 6363\nDuring the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or \"Assassin\"), using data from the recently commissioned double 14-cm \"Cassius\" telescope in Cerro Tololo, Chile, we discovered a new transient source, possibly a supernova, near the galaxy PGC 053612: \n \n \n Object RA (J2000) DEC (J2000) Disc. UT Date Disc. V mag \n ASASSN-14eu 15:00:36.84 -03:50:48.9 2014-08-01.02 16.6 \n \nASASSN-14eu was discovered in images obtained on UT 2014-08-01.02 at V~16.6 mag. We do not detect (V>17.15) the object in images taken on UT 2014-07-26.04 and before. An image obtained on 2014-08-01.95 by E. Conseil using a 0.35m f/11 Schmidt-Cassegrain + ST-10XME (Kodak KAF-3200E CCD) from Slooh Space robotic telescope T2 at Mt. Teide, Canary Islands confirms the discovery of the transient. This figure shows the archival DSS image of the host (left) and the E. Conseil confirmation image (right). The red circle has a radius of 5\" and is centered on the position of the transient. \nThe ASAS-SN position of ASASSN-14eu is approximately 41.1\" North and 29.4\" West from the center of the galaxy PGC 053612 (z=0.022722, d=97.9 Mpc, via NED), giving a projected distance of ~24 kpc from the host nucleus. At this distance, the transient would have an absolute V-band magnitude of approximately -18.8 (m-M=34.95, A_V=0.422). \nGiven the relatively large projected distance of the transient from the potential host galaxy, this transient could also be a chance projection, though Vizier indicates no apparent stellar counterparts. Follow-up observations, especially spectroscopy, are encouraged. \nWe thank LCOGT and its staff for their continued support of ASAS-SN. For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Binary system", "Quasar", "Galaxy" ] }, "answerKey": "A" }, { "id": "atel_6540", "message": "Title: Recurrent Nova M31N 2008-12a: Liverpool Telescope SPRAT Spectrum\nAuthors: M. J. Darnley (LJMU), I. A. Steele (LJMU), R. J. Smith (LJMU), A .W. Shafter (SDSU), M. F. Bode (LJMU), A. S. Piascik (LJMU), S. C. Williams (LJMU), M. Henze (ESAC), J.-U. Ness (ESAC), R. A. Hounsell (STSCI)\nDate: 4 Oct 2014; 22:17 UT\nProvenance: Matt Darnley (M.J.Darnley@ljmu.ac.uk)\nSubjects: Nova\nDescription: Referred to by ATel #: 6543, 6546, 6703, 6704\nThe recent detection of a sixth optical eruption of the M31 recurrent nova M31N 2008-12a (ATel #6527, #6532, #6535) was spectroscopically confirmed by iPTF (ATel #6537). \n \nThe 2m fully robotic Liverpool Telescope (LT, Steele et al. 2004) observed the eruption with its new, low dispersion, high throughput spectrograph 'SPRAT' (SPectrograph for the Rapid Acquisition of Transients; Piascik et al. 2014). \n \nEach of a series of LT SPRAT spectra of M31N 2008-12a taken between 2014 Oct 3.928 UT and Oct 4.213 UT shows features that are consistent with those reported in ATel #6537. These spectra are remarkably similar to the spectrum of M31N 2008-12a following its 2012 eruption (aka M31N 2012-10a; see ATel #4503 and Darnley et al. 2014). \n \nThe SPRAT spectra are dominated by Hydrogen Balmer series emission lines (Hα, Hβ, Hγ, and Hδ). The following emission lines are also present, He I (4471, 5017, 5876, 6678, 7065), N II (5001, 5680), and N III (4641). The N I (6485) and Si II (6347, 6371) emission lines may also be present. We measure the FWHM of the Hα and Hβ emission lines to be 2,500 ± 100 km/s and 2,200 ± 100 km/s, respectively. \n \nThe spectra of the 2014 eruption of M31N 2008-12a are consistent with a He/N nova, although the emission lines are not as broad as those typically associated with this spectral class of nova.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Galaxy", "Nova", "Binary system" ] }, "answerKey": "C" }, { "id": "atel_6600", "message": "Title: Spectral ID of snASASSN-14jb\nAuthors: peter challis, Harvard-Smithsonian Center for Astrophysics\nDate: 20 Oct 2014; 20:29 UT\nProvenance: Peter Challis (pchallis@cfa.harvard.edu)\nSubjects: Optical, Supernovae, Transient\nDescription: P. Challis, Harvard-Smithsonian Center for Astrophysics (CfA), on behalf of the CfA Supernova Group, reports a spectrum (range 350-760 nm) of ASASSN-14jb was obtained on Oct 20, 2014 UT by P. Berlind with the F. L. Whipple Observatory 1.5-m telescope (+ FAST). The spectrum has a very blue continuum with emission of H Alpha, H Beta, H Gamma, H Delta and He II 4686. Cross-correlation with a library of supernova spectra using the \"Supernova Identification\" code (SNID; Blondin and Tonry 2007, Ap.J. 666, 1024) shows a reasonable match to the spectrum of type II supernova SN2005cs.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Nova", "Quasar", "Variable star" ] }, "answerKey": "A" }, { "id": "atel_6690", "message": "Title: ASASSN-14kb = OGLE-LMC529.30.114 is a New Eclipsing SU UMa-type Dwarf Nova\nAuthors: L. Wyrzykowski, P. Mroz, A. Udalski, R. Poleski, Z. Kostrzewa-Rutkowska, on behalf of the OGLE-IV team.\nDate: 12 Nov 2014; 23:08 UT\nProvenance: Lukasz Wyrzykowski (wyrzykow@ast.cam.ac.uk)\nSubjects: Optical, Cataclysmic Variable, Transient\nDescription: The transient announced by the ASAS-SN group (Prieto et al. ATEL#6688) is present in the OGLE-IV Magellanic System monitoring program under OGLE ID: OGLE-LMC529.30.114. The data collected since 2010 show multiple super-outbursts with period of about 162 days and numerous normal outbursts. Additionally, OGLE-IV data revealed periodic eclipsing behavior in the quiescence with a period of 0.0681057 days = 98 mins. This behavior fulfils the criteria of a dwarf nova of SU UMa type. The full span light curve and the phase-folded with eclipsing period is available here: http://ogle.astrouw.edu.pl/CVs/OGLE-LMC529.30.114-ASASSN-14kb.pdf \nOGLE-IV will continue the photometric monitoring of this object. Further studies including spectroscopic observations are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Interstellar medium", "Galaxy", "Supernova" ] }, "answerKey": "A" }, { "id": "atel_6825", "message": "Title: X-ray Absorption Lines in the Candidate Tidal Disruption Event ASASSN-14li\nAuthors: J. M. Miller (Michigan), J. J. Drake (SAO), J. Kaastra (SRON), F. Paerels (Columbia), R. Mushotzky (Maryland), S. Gezari (Maryland), K. Gultekin (Michigan), M. Reynolds (Michigan), A. Zoghbi (Michigan), E. Ramirez-Ruiz (UCSC), S. B. Cenko (NASA/GSFC), G. Brown (Warwick), A. Levan (Warwick)\nDate: 16 Dec 2014; 01:23 UT\nProvenance: Jon Miller (jonmm@umich.edu)\nSubjects: X-ray, Black Hole, Transient\nDescription: Referred to by ATel #: 6834\nWe report on a 94 ks observation of the TDE candidate ASASSN-14li, obtained on 8 December 2014 with XMM-Newton. \n \nThe high resolution first-order RGS spectra show a number of significant absorption features in the 20-40 Angstroms band, most notably at 24.6, 25.25, 27.9, 29.9, 31.1, and 32.9 Angstroms. It is worth noting that the features at ~25 and ~31 Angstroms correspond to the strongest line candidates in the Chandra/LETGS-HRC spectrum of ASASSN-14li (Miller et al. 2014, ATEL #6800). To our knowledge, this is the first detection of discrete X-ray spectral features in a TDE or TDE candidate. The results signal that the environment close to disruptions can be probed effectively through X-ray spectroscopy. \n \nThe RGS continuum is described adequately with a simple blackbody (kT = 53 eV), modified by interstellar absorption (1.8 E+20 /cm/cm). \n \nSome of these lines may plausibly be attributed to different charge states of N. Overall, the character of the spectrum is similar to atmospheric absorption from white dwarfs in outburst or super-soft phases (such spectra can include blends and require detailed modeling for secure line identifications; see, e.g., Rauch et al. 2010 ApJ 717 363). This may not be unexpected: if ASASSN-14li is indeed in a super-Eddington phase, common physics may cause it to resemble cataclysmic variable in a super-Eddington outburst. The spectrum does not closely resemble a typical Seyfert warm absorber. \n \nThe nature of this spectrum raises the possibility that the source is indeed a Galactic white dwarf. However, given the close proximity of this event to the center of a plausible host galaxy, given the lack of a previously known white dwarf or nova at this location, and given the emergence of a broad H-alpha line at the putative host galaxy redshift (Jose et al. 2014; ATEL #6777), a chance alignment is highly improbable. If the absorption line at 25.25 Angstroms is N VII, its redshift would be commensurate with that of the host galaxy and further exclude a Galactic object. \n \nWe thanks Norbert Schartel and the XMM-Newton team for executing this TOO program.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Nova", "Circumstellar disk", "Black hole" ] }, "answerKey": "C" }, { "id": "atel_6950", "message": "Title: ASAS-SN Discovery of A Bright Probable Supernova in the dwarf galaxy GALEXASC J025245.83-341850.6\nAuthors: J. Brimacombe (Coral Towers Observatory), Subo Dong (KIAA-PKU), S. Kiyota (Variable Star Observers League in Japan), R. A. Koff (Antelope Hills Observatory), K. Z. Stanek, T. W.-S. Holoien, C. S. Kochanek, A. B. Danilet, G. Simonian, U. Basu, N. Goss, J. F. Beacom (Ohio State), B. J. Shappee (Hubble Fellow, Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), D. Bersier (LJMU), P. R. Wozniak (LANL), D. Szczygiel, G. Pojmanski (Warsaw University Observatory)\nDate: 19 Jan 2015; 06:05 UT\nProvenance: Subo Dong (dongsubo@pku.edu.cn)\nSubjects: Optical, Supernovae\nDescription: Referred to by ATel #: 6988\nDuring the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or \"Assassin\"), using data from the quadruple 14-cm \"Cassius\" telescope in Cerro Tololo, Chile, we discovered a new, bright transient source, most likely a supernova, in the galaxy GALEXASC J025245.83-341850.6: \n \n Object RA (J2000) DEC (J2000) Disc. UT Date Disc. V mag \n ASASSN-15be 02:52:46.39 -34:18:52.52 2015-01-19.07 16.4\nASASSN-15be was discovered in images obtained on UT2015-01-19.07 at V~16.4. and it is also detected on 2015-01-15.15 at V~17.8. We do not detect (V>17.6) this object in images taken on UT 2015-01-12.10 and before. \nSee the ASAS-SN discovery image, An image obtained by J. Brimacombe on UT 2015-01-19.17 with the RCOS 51-cm telescope in New Mexico Skies Observatory confirms the discovery of the transient. This figure shows the archival DSS image of the host (left) and the J. Brimacombe's confirmation image (right). The red circle (10\" radius) indicates the position of the transient in the J. Brimacombe's image. \nThe position of ASASSN-15be is approximately 7\" from the center of the dwarf galaxy GALEXASC J025245.83-341850.6 (z=0.0219, d=88 Mpc, via NED), giving an absolute V-band magnitude of approximately -18.4 (m-M=34.7, A_V=0.054). Follow-up observations are encouraged. \nWe thank LCOGT and its staff for their continued support of ASAS-SN. ASAS-SN is supported in part by Mt. Cuba Astronomical Foundation. For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Binary system", "Variable star", "Galaxy" ] }, "answerKey": "D" }, { "id": "atel_7020", "message": "Title: Chandra position of IGR J17454-2919 and discovery of a possible NIR counterpart\nAuthors: A. Paizis, M. Nowak, S. Chaty, J. Chenevez, M. Del Santo, J. Rodriguez, A. Segreto, J. Wilms\nDate: 3 Feb 2015; 09:22 UT\nProvenance: Adamantia Paizis (ada@iasf-milano.inaf.it)\nSubjects: Radio, Infra-Red, Optical, X-ray, Binary, Black Hole, Nova, Neutron Star, Transient\nDescription: On 2014 November 3, we observed the recently discovered INTEGRAL source IGR J17454-2919 (ATels #6530, #6574 and #6602) with Chandra HETGS for 20ks. \nThe J2000.0 Chandra position we obtain is \nRA: 17 45 27.689 \nDEC: -29 19 53.83 \n(90% uncertainty of 0.6\") \n \nThis position (2.4\" away from the Swift position, ATel #6530), is consistent with the source 2MASS J17452768-2919534 (J=16.227, H=13.038+-0.06, Ks=11.365+-0.024). This candidate counterpart is also consistent with the Swift error circle of ATel #6530. \n \nWe encourage follow-up multi-wavelength observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system, Accreting object", "Magnetar, Accreting object", "Binary system, Active galactic nucleus", "Star and stellar system, Accreting object" ] }, "answerKey": "A" }, { "id": "atel_7100", "message": "Title: Optical observations of the transient 1RXS J180408.9-342058\nAuthors: M. C. Baglio (Universita` dell'Insubria, Como), S. Campana (INAF-Osservatorio Astronomico di Brera), P. D'Avanzo (INAF-Osservatorio Astronomico di Brera)\nDate: 18 Feb 2015; 14:38 UT\nProvenance: Maria Cristina Baglio (cristina.baglio@brera.inaf.it)\nSubjects: Optical, Binary, Neutron Star, Transient\nDescription: Referred to by ATel #: 7255\nWe report on optical observations of the galactic transient 1RXS J180408.9-342058, currently in outburst (Krimm et al., ATel #6997; Negoro et al., ATel #7008). Observations were carried out with the instrument EFOSC2 mounted on the ESO/NTT (La Silla, Chile) on Feb 08, 2015 between 08:35 UT and 09:01 UT. We obtained a series of eight 15s images in the optical VR filters. \nThe optical counterpart of 1RXS J180408.9-34205 is clearly detected at the following position (J2000): \nRA= 18h 04m 08.371s = 271.03488 (deg) \ndec: -34d 20' 51.38'' = -34.34767 (deg) \nwith an uncertainty of 0.5''. \nWe obtained for the source the following mean Vega magnitudes: \nV=17.1 +/- 0.1 \nR=17.0 +/- 0.1 \nThe magnitudes are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.48 in the direction of the object (Schlegel et al. 1998) and are calibrated against the GSC-II catalog. \nThe source position is consistent with the value reported in Atel #7039 (Krimm et al.).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system, Neutron star", "Neutron star, Neutron star", "Binary system, Supernova", "Nova, Neutron star" ] }, "answerKey": "A" }, { "id": "atel_7175", "message": "Title: Fermi-LAT detection of hard spectrum gamma-ray activity from the FSRQ PKS 1532+01\nAuthors: S. Ciprini (ASI Science Data Center Rome & INFN Perugia, Italy), C. C. Cheung (Naval Research Laboratory, USA) on behalf of the Fermi Large Area Telescope Collaboration\nDate: 4 Mar 2015; 18:31 UT\nProvenance: Stefano Ciprini (stefano.ciprini@asdc.asi.it)\nSubjects: Gamma Ray, >GeV, Request for Observations, AGN, Blazar, Quasar\nDescription: The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed increasing gamma-ray flux and an unusually hard gamma-ray spectrum from a source positionally consistent with the flat spectrum radio quasar (FSRQ) PKS 1532+01 (also known as 3FGL J1534.5+0128, Acero et al. 2015, arXiv:1501.02003) with radio counterpart coordinates (J2000.0), R.A. = 233.71856 deg, Dec. = 1.51784 deg (Johnston et al. 1995, AJ, 110, 880). This FSRQ has redshift z=1.425 (White et al. 1988, ApJ, 327, 561). \nPreliminary analysis indicates that on February 27, 2015, the gamma-ray source was in a high state with a daily averaged flux (E>100 MeV) of (0.3+/-0.1) x 10^-6 photons cm^-2 s^-1 (statistical uncertainty only), more than 10 times greater than the average flux reported in the third Fermi LAT source catalog (3FGL). The corresponding daily-averaged photon index (E>100 MeV) of 1.7+/-0.2 (statistical uncertainty only) is notably smaller than the average index of 2.779+/-0.114 in the 3FGL catalog. The weekly averaged flux (E>100 MeV) from February 23 - March 1, 2015 is (0.2+/-0.1) x 10^-6 photons cm^-2 s^-1, with a corresponding photon index of 2.0 +/- 0.2. \nBecause Fermi operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. In consideration of the ongoing activity of this source, we encourage multiwavelength observations. For this source the Fermi LAT contact person is S. Ciprini (stefano.ciprini@asdc.asi.it). \nThe Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Pulsar", "Quasar", "Active galactic nucleus" ] }, "answerKey": "C" }, { "id": "atel_7300", "message": "Title: Detection of Pulsed Hard X-ray Emission from 4U 0142+61 with Fermi/GBM\nAuthors: Ersin Gogus (Sabanci Univ. Istanbul), George Younes (GWU), Chryssa Kouveliotou (GWU) report on behalf of a larger collaboration:\nDate: 27 Mar 2015; 14:26 UT\nProvenance: Ersin Gogus (ersing@sabanciuniv.edu)\nSubjects: X-ray, Gamma Ray, Neutron Star, Soft Gamma-ray Repeater\nDescription: As part of our effort to monitor pulsed hard X-ray emission from magnetars with Fermi/GBM, we searched continuously recorded daily data (CTIME, 0.256 s time resolution) of 4U 0142+61 collected on March 1, 2015, soon after the onset of its latest activation (GCN #17507). We obtained the spin frequency of the magnetar using Swift XRT observations performed on the same day (Observation ID: 00030738055, ~4 ks exposure) as 0.115083(3) Hz and used it to fold the GBM data. We find that pulsed hard X-rays from 4U 0142+61 can be detected up to about 300 keV. We also find a marginal evidence of declining RMS pulsed count rates with energy: RMS pulsed count rates are 0.0061(7), 0.0040(8), 0.0046(8), and 0.0039(8) cts/s in the 11-26.5, 26.5-50.4, 50.4-101.3, and 101.3-298.6 keV ranges, respectively. Further investigations of the pulsed hard X-ray emission of this magnetar are ongoing. Energy resolved pulse profiles of the source as seen on March 1, 2015 can be seen at: https://www.dropbox.com/s/akesqy92vzql5iu/4u0142_150301_d10_pulseprof_energy.pdf?dl=0", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Interstellar medium", "Nova", "Star and stellar system" ] }, "answerKey": "A" }, { "id": "atel_7380", "message": "Title: INTEGRAL observations of SAX J1808.4-3658 currently in outburst\nAuthors: M. Del Santo (INAF/IASF-Palermo, Italy), E. Bozzo (ISDC, Switzerland), E. Kuulkers (ESA/ESAC, Spain), A. Bazzano (INAF/IAPS, Italy), V. Beckmann (APC, France), T. Bird (Univ. of Southampton, UK), A. Bodaghee (GCSU, USA), J. Chenevez (DTU Space, Denmark), A. Domingo (CAB/INTA-CSIC, Spain), P. Jonker (SRON, The Netherlands), P. Kretschmar (ESA/ESAC, Spain), C. Markwardt (GSFC, USA), A. Paizis (INAF/IASF-Milano, Italy), K. Pottschmidt (UMBC/NASA GSFC, USA), C. Sanchez-Fernandez (ESA/ESAC, Spain), R. Wijnands (UvA, The Netherlands)\nDate: 13 Apr 2015; 14:42 UT\nProvenance: Melania Del Santo (melania@ifc.inaf.it)\nSubjects: X-ray, Binary, Neutron Star, Pulsar\nDescription: Referred to by ATel #: 12964, 12993\nThe latest INTEGRAL Galactic Bulge monitoring (ATel #438) was performed during revolution 1529 on 2015 April 12 starting at 18:15 UT (57124.761 MJD) for a total of 12462 seconds. \nWe report on the IBIS/ISGRI detection of the new outburst from the millisecond X-ray pulsar SAX J1808.4-3658 (ATels #7364 #7371 #7376 #7379). The source is detected at about 23 sigma in both 18-40 keV and 40-80 keV IBIS/ISGRI maps with 8.7 ks effective exposure time, and the estimated fluxes are 60+/-3 mCrab and 78+/-3 mCrab in the two energy bands, respectively. SAX J1808.4-3658 was outside the JEM-X and OMC field of view. \nThe IBIS/ISGRI spectrum extends up to 100 keV and it is well described by a simple power-law model with a photon index of 2.0+/-0.2. The 20-100 keV X-ray flux estimated from the spectral fit is 1.4E-09 erg/cm^2/s. \nThe INTEGRAL monitoring of the Galactic bulge will also continue in the coming weeks, and the observation results from the near real time data will be made available on the WEB (http://integral.esac.esa.int/BULGE/).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Pulsar", "Interstellar medium", "Variable star", "Exoplanet" ] }, "answerKey": "A" }, { "id": "atel_7530", "message": "Title: NOT spectroscopic classification of supernova PS15aip/Gaia15aev as Type IIn\nAuthors: T. Reynolds, S. Mattila, J. Harmanen (University of Turku), N. Blagorodnova, M. Fraser (University of Cambridge), L. Wyrzykowski (Warsaw University Observatory), R. Kotak, E. Kankare (Queen's University Belfast)\nDate: 18 May 2015; 20:19 UT\nProvenance: Seppo Mattila (seppo.mattila@utu.fi)\nSubjects: Optical, Supernovae\nDescription: We report the spectroscopic classification of supernova PS15aip/Gaia15aev based on a low-resolution spectrum obtained on May 16.2 UT, with the Nordic Optical Telescope (+ ALFOSC; range 320-910nm; R = 360). \nPS15aip was discovered (Smith et al. 2015, ATel #7488) by the Pan-STARRS Survey for Transients (PSST) programme at magnitude of 17.46 on 2015 May 02.8 UT, the most recent non-detection being 30 days earlier. The object was later detected by the Gaia Photometric Science Alerts programme at magnitude of 17.92 on 2015 May. 11.6 UT. PS15aip/Gaia15aev is located 2.16 arcsec from the nucleus of the galaxy KUG 1319+356. The spectrum exhibits narrow (FWHM ~ 1150 km/s) spectral lines of the Balmer series on a featureless continuum. The H alpha line exhibits a Lorentzian profile. Adopting the host galaxy redshift z = 0.0195 from the NED and a moderate reddening of E(B-V)=0.2, we estimate an absolute magnitude for PS15aip/Gaia15aev to be -17.8 at the time of the PSST discovery. \n \n \n Name | RA (J2000) | Dec (J2000) | Disc. Date | Disc Mag | z | Type | Phase | Notes \n \n PS15aip/Gaia15aev | 13:21:55.23 | +35:21:32.0 | 20150502 | 17.46 |~0.0195| SN IIn | ~1 month past max | (1) \n \n(1) Good match found with the type IIn SN 1995G at ~1 month after the max. light, adopting a reddening of E(B-V)=0.2 \nThe classifications were done with GELATO (Harutyunyan et al. 2008, A&A,488, 383). We acknowledge ESA Gaia (http://cosmos.esa.int/gaia), and the DPAC Photometric Science Alerts Team (http://gaia.ac.uk/selected-gaia-science-alerts) (Rixon et al,2014, ATel #6593).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system", "Supernova", "Nova", "Variable star" ] }, "answerKey": "B" }, { "id": "atel_7620", "message": "Title: Optical photometry of the black hole transient GS 1354-64 (BW Cir) in outburst\nAuthors: J. Corral-Santana (U. Catolica de Chile), T. Munoz-Darias (IAC/ULL - Tenerife), J. A. Carballo-Bello (IFA-Valparaiso), F. E. Bauer (U. Catolica de Chile)\nDate: 11 Jun 2015; 13:51 UT\nProvenance: Teo Muñoz-Darias (tmd@brera.inaf.it)\nSubjects: Optical, Black Hole\nDescription: Referred to by ATel #: 7637, 7656, 7887\nFollowing the recent outburst of GS 1354-64 (BW Cir) reported in ATel#7612 and ATel#7614, we have started an optical monitoring of this dynamically confirmed black hole. We obtained images in g', r' and i' SDSS bands on UT 20150610/11 with the SOAR Optical Imager (SOI) installed on the 4.1-m SOAR telescope at Cerro Pachon, Chile. The sky conditions were not stable, with poor seeing (1.5-1.8 arcsec) and some cirrus. In order to avoid contamination by nearby stars in the field, we performed PSF photometry using DAOPHOT II/ALLSTAR (Stetson 1987). The average magnitudes obtained are: \n \ng'=19.76+-0.03 \nr'=18.49+-0.04 \ni'=18.34+-0.05 \n \nThese values were calibrated against the stars A-C published in Casares et al. (2009) using the Jester et al. (2005) transformations. In agreement with X-ray observations (ATel#7612 and ATel#7614), the system is still fainter than observed in previous outbursts: \n \nV=16.92 in 1987 (Kitamoto et al. 1990) \nV=17.40 in 1997 (Brocksopp et al. 2001). \n \n \nREFERENCES: \nBrocksopp et al. 2001, MNRAS 323, 517 \nCasares et al. 2009, ApJS 181, 238 \nJester et al. 2005, AJ, 130, 873, 895 \nKitamoto et al. 1990, ApJ 361, 590 \nStetson, 1987, PASP 99, 191 \n \nJMC-S acknowledges financial support to CONICYT through the FONDECYT project No. 3140310. Based on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministerio da Ciencia, Tecnologia, e Inovacao (MCTI) da Republica Federativa do Brasil, the U.S. National Optical Astronomy Observatory (NOAO), the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU). These observations were granted by the Chilean TAC with the proposal number: CN2015A-88.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Nova", "Active galactic nucleus", "Black hole" ] }, "answerKey": "D" }, { "id": "atel_7680", "message": "Title: PSN J11473508+5558147 is a Type Ib Supernova Near Maximum Light\nAuthors: D. C. Leonard (San Diego State University), P. Sheehan, D. McCarthy (University of Arizona), K. Follette (Stanford University), J. Moustakas (Siena College), D. Cantillo, A. Cazares-Kelly, S. Cazares-Kelly, Y. Cendes, N. Damm, A. Donati, E. Douglas, L. Ferrell, H. Fosbiner-Elkins, C. Fox, M. Greenberg, K. Hart, H. Hensley, A. Holt, E. Hooper, C. Juran, J. Keane, K. Key, L. Korus, T. Lee, K. Leidig, E. Merchak, K. Nessmann, S. Pendyala, S. Pirkl, J. Reeder, A. Roos, S. Rounseville, E. Ruddy, A. Schlingman, W. Schlingman, W. Schlingman, E. Schwartzman, V. Shanmugam, E. Silver, A. Stein, N. Stock, B. Svoboda, B. Thomas, N. Thomas, K. Thompson-Taylor, H. Walton (2015 Advanced Teen Astronomy Camp)\nDate: 21 Jun 2015; 09:26 UT\nProvenance: D. C. Leonard (leonard@astro.caltech.edu)\nSubjects: Optical, Supernovae\nDescription: We report spectroscopic classification of PSN J11473508+5558147 through inspection of a low-dispersion optical spectrum (range 370-680 nm), obtained with the 2.3-m Bok telescope (+ Boller & Chivens spectrograph) at Kitt Peak on 2015 June 21 UT. Information on this transient, discovered by P. Wiggins, was announced through the CBAT Transient Object Followup Reports (http://www.cbat.eps.harvard.edu/index.html) and is also available from the \"Bright Supernova\" website (http://www.rochesterastronomy.org/snimages/). \nPSN J11473508+5558147 is a Type Ib supernova; cross-correlation with a library of supernova spectra using the comparison tool GELATO (Harutyunyan et al. 2008, A&A, 488, 383) finds good matches with near-maximum Type-Ib supernovae at a redshift of 0.008, consistent with the NED redshift of the putative host galaxy, NGC 3888 (de Vaucouleurs et al., 1991, RC3 catalogue).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Circumstellar disk", "Quasar", "Pulsar" ] }, "answerKey": "A" }, { "id": "atel_7750", "message": "Title: A new Giant NIR Flare of the FSRQ S40954+65\nAuthors: L. Carrasco, A. Porras, E. Recillas, J. Leon-Tavares, V. Chavushyan, A. Carraminana (INAOE, Mexico)\nDate: 2 Jul 2015; 15:38 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Infra-Red, Gamma Ray, VHE, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 8445\nWe report on a new giant NIR flare of the intermediate redshift FSRQ S4 0954+658(z=0.368), also known as CGRaBSJ0958+6533 associated with the gamma-ray source 2FGL0958.6+6533. Our most recent NIR photometry for this source shows that on June 11th,2015 (JD2457184.6502), the object brightness corresponded to J = 13.300+/- 0.04, H = 12.542 +/- 0.04 and Ks = 11.657 +/- 0.04. The NIR fluxes in the JHK bands had a sudden increase since the previously observed fluxes were: J = 14.468 +/- 0.07, H = 13.509 +/- 0.04 and Ks = 12.699 +/- 0.06, on JD2457180.6762. Hence the object has increased its luminosity by a factor of about 2.5 in this very short lapse. The object has shown flaring activity in different wavelength bands in the past. (see Atels #3220, #6709, #6996, #7001, #7007, #7046). Our observations are carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We strongly encourage further multiwavelength coverage.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar, Accreting object", "Quasar, Variable star", "Binary system, Accreting object", "Magnetar, Accreting object" ] }, "answerKey": "A" }, { "id": "atel_7890", "message": "Title: Multi-frequency radio observations of S5 0836+710 after gamma-ray outburst\nAuthors: M. Giroletti (INAF/ORA, Bologna, Italy), S. Righini (INAF/ORA, Medicina, Italy), U. Bach (MPIfR, Bonn, Germany), F. D'Ammando (Univ. of Bologna, Italy), M. Orienti (INAF/ORA, Bologna, Italy), C. M. Raiteri (INAF/OATo, Torino, Italy), M. Villata (INAF/OATo, Torino, Italy)\nDate: 7 Aug 2015; 15:43 UT\nProvenance: Marcello Giroletti (giroletti@ira.inaf.it)\nSubjects: Radio, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 7898\nWe report on multi-frequency radio observations of S5 0836+710 (4C 71.07), obtained following the report of the Fermi-LAT detection of its highest-level gamma-ray outburst (ATEL #7870). The observations were carried out in the context of our Medicina-Noto radio monitoring of gamma-ray loud blazars that is part of the GLAST-AGILE Support Program (GASP) of the Whole Earth Blazar Telescope (WEBT).\nWe observed S5 0836+710 with the Medicina 32 m radio telescope at 5, 8.4, and 24 GHz on 2015 August 5.52UT, 5.59UT, and 6.33UT. From our preliminary analysis, we measured a flux density of 3.3 +/- 0.1 Jy at 5 GHz, 2.9 +/- 0.1 Jy at 8.4 GHz, and 2.5 +/- 0.3 Jy at 24 GHz. The corresponding near-simultaneous spectral index is 0.25 +/- 0.20 between 5 and 8.4 GHz and 0.14 +/- 0.11 between 8.4 and 24 GHz (defined by Sν∝ν-α).\nA comparison with earlier observations indicates that at present the source is in a high level of activity in the radio band. A further increase is expected based on the typical radio-gamma delay for blazar flares. The radio monitoring of S5 0836+710 at Medicina continues. The next observation date is provisionally scheduled for 2015 September 10.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Magnetar", "Minor body", "Supernova" ] }, "answerKey": "A" }, { "id": "atel_7975", "message": "Title: Fermi LAT detection of renewed GeV gamma-ray activity from blazar AO 0235+164\nAuthors: Stefano Ciprini (ASDC Rome & INFN Perugia, Italy), on behalf of the Fermi Large Area Telescope Collaboration.\nDate: 1 Sep 2015; 15:34 UT\nProvenance: Stefano Ciprini (stefano.ciprini@asdc.asi.it)\nSubjects: Gamma Ray, >GeV, Request for Observations, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 8044, 8429, 8802\nThe Large Area Telescope (LAT), one of two instruments on the Fermi Gamma-ray Space Telescope, has observed flaring gamma-ray emission from a source positionally consistent with the blazar AO 0235+164 (also known as OD 160, PKS 0235+164, 1ES 0235+164 and 3FGL J0238.6+1636), with radio coordinates (J2000) R.A.: 39.662209 deg, Dec.: 16.616465 deg (Johnston et al. 1995, AJ, 110, 880). This blazar has a redshift z=0.94 (Cohen et al. 1987, ApJ, 318, 577). \nPreliminary analysis indicates that on 29, 30 and 31 August 2015 AO 0235+164 was in a high-flux state, with a daily gamma-ray flux (E>100MeV) respectively of (1.2+/-0.2) X 10^-6 photons cm^-2 s^-1, (1.2+/-0.2) X 10^-6 photons cm^-2 s^-1, and (0.8+/-0.2) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). The corresponding daily spectral photon indices (E>100MeV) of respectively 2.0+/-0.1, 2.05+/-0.05 and 2.0+/-0.2 are consistent with the average index of 2.057+/-0.024 reported in the 3FGL catalog. \nA peak 6-hour integrated gamma-ray flux of (1.5+/-0.5) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only), is reached on September the 1st 2015, 00:00-06:00 UT, corresponding to about 10 times greater than the average flux reported in the third Fermi-LAT source catalog, 3FGL (Acero et al. 2015, ApJS 218, 23). \nThis is the third time that the LAT collaboration is announcing gamma-ray flaring activity from AO 0235+164 through an ATel, after those in September and October 2008 (ATel#1744 and ATel#1784) and after the 2008-2009 flaring state (Ackermann et al. 2012, ApJ, 751, 159). \nAO 0235+164 is one of the \"LAT Monitored Sources\" and consequently a preliminary estimation of the daily gamma-ray flux observed by Fermi LAT is publicly available (http://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/0235p164). \nBecause Fermi operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. In consideration of the ongoing activity of this source, we encourage multiwavelength observations. For this source the Fermi LAT contact persons are L. C. Reyes (e-mail: lreyes04@calpoly.edu) and S. Raino' (silvia.raino@ba.infn.it). \nThe Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Exoplanet", "Binary system", "Variable star", "Black hole" ] }, "answerKey": "D" }, { "id": "atel_8070", "message": "Title: FLOYDS Classification of LSQ15baf as a Post-Peak Type Ia Supernova\nAuthors: G. Hosseinzadeh, I. Arcavi, Z. C. Wong, D. A. Howell, C. McCully, S. Valenti (LCOGT/UCSB), C. Baltay, N. Ellman, D. Rabinowitz (Yale)\nDate: 19 Sep 2015; 00:06 UT\nProvenance: Iair Arcavi (iarcavi@lcogt.net)\nSubjects: Optical, Supernovae\nDescription: LSQ15baf was discovered on 2015 August 26.2 UT by the La Silla-QUEST survey (Baltay et al. 2013, PASP, 125, 683) at right ascension 23:49:43.53 and declination +18:45:17.6 (J2000), 1\" from the center of the galaxy SDSS J234943.58+184516.9 at a magnitude of V~18 (latest magnitude estimate is V~19 from 2015 September 11). We obtained a spectrum of LSQ15baf on 2015 September 17.5 UT with the robotic FLOYDS instrument mounted on the Faulkes Telescope North under our LCOGT TDE vetting program (P.I.: Arcavi). Using SNID (Blondin & Tonry 2007, ApJ, 666, 1024), we find a good fit to the normal Type Ia SN 2003cg 10 days after maximum light at redshift z=0.044.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Minor body", "Pulsar", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_8160", "message": "Title: MASTER: new short optical transient\nAuthors: O. Gress, V. Lipunov, E. Gorbovskoy, P. Balanutsa (Lomonosov MSU), D. Buckley (SAAO), V. Kornilov, N. Tiurina, A. Kuznetsov, I. Gorbunov, D. Vlasenko, V. Chazov, V. Shumkov, E. Popova (M. V. Lomonosov MSU, SAI), N. Budnev, K. Ivanov (Irkutsk State University, Applied Physics Institute), S. Potter, M. Kotze (South African Astronomical Observatory), R. Rebolo, M. Serra-Ricart, N. Lodieu, G. Israelian (The Instituto de Astrofisica de Canarias), A. Tlatov, V. Senik, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), V. Krushinskiy (Ural Federal University), Yu. Sergienko, A. Gabovich, V. Yurkov (Blagoveschensk Educational State University)\nDate: 13 Oct 2015; 23:31 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Request for Observations, Cataclysmic Variable, Gamma-Ray Burst, Transient, Variables\nDescription: MASTER OT J234149.80-465633.6 discovery - short optical transient , no VIZIER, Ampl>3m \nMASTER-SAAO auto-detection system ( Lipunov et al., Advances in Astronomy, MASTER Global Robotic Net, 2010 ) discovered OT source at (RA, Dec) = 23h 41m 49.80s -46d 56m 33.6s on 2015-10-11.81150 UT. \nThe OT unfiltered magnitude is 18.9m (the limit is 20.4m). There are 6 images with this OT at 2015-10-11 19:28:34, 19:32:16, 19:35:57(MASTER is twin telescope). There is no minor planet at this place. There is no object at 2015-10-11 19:40:33 and later, and on 2015-10-10 20:40:28 and earlier. \nWe have 1458 images of this area with m_lim_W up to 21.2, m_lim_B up to 20.8, m_lim_V up to 20.8, m_lim_R up to 20.0 without OT from 2014-12-27 19:53:19UT in MASTER-SAAO database, for ex., on 2015-08-17.98584 UT with m_lim=20.6m. \nThere is no any source in VIZIER database inside 5\" (up to 22m) \nSpectral observations are required. \nThe discovery and reference images are available at http://observ.pereplet.ru/images/MASTER234149.80-465633.6.jpg List of Optical Transients discovered by MASTER\nMASTER Global Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Circumstellar disk", "Star and stellar system", "Variable star" ] }, "answerKey": "D" }, { "id": "atel_8220", "message": "Title: NIR photometry of M31LRN 2015\nAuthors: Stefan Geier (GTC/IAC/ULL), Peter Pessev (GTC/IAC/ULL)\nDate: 28 Oct 2015; 08:31 UT\nProvenance: Peter Pessev (peter.pessev@gtc.iac.es)\nSubjects: Infra-Red, Nova, Transient\nDescription: A new epoch JHKs NIR photometry of the stellar merger candidate MASTER OT J004207.99+405501.1 / M31N 2015-01a / M31LRN 2015 (Kurtenkov et al. 2015, Williams et al. 2015, ATel #6911, ATel #7150) has been obtained. In the morning hours of September 28th we carried out observations with the 2.5m Nordic Optical Telescope (NOT) at the Observatorio Roque de Los Muchachos (ORM), La Palma, using the NOTCam instrument. We obtained 700sec, 720sec, and 700sec of total exposure time in the J-, H-, and Ks-band, respectively. As outlined in ATel #7624, five nearby 2MASS stars with accurate magnitudes (AAA quality flags) were used for the photometric calibration. The photometry data points are listed below: \n \nUT Band Mag Merr AM Seeing \n \n2015-09-28.08 J 18.89 0.12 1.03 1.04 \n \n2015-09-28.09 H 17.21 0.06 1.03 0.94 \n \n2015-09-28.11 Ks 15.34 0.08 1.05 0.78 \n \nThe observed colors of the object are summarized below: \n \nUT J-H H-Ks J-Ks \n \n2015-09-28.09 1.69 ± 0.13 1.864 ± 0.102 3.55 ± 0.15 \n \nWe observe no significant variations (within the error bars) of the colors of the transient, compared to the previous observation on 2015-09-03UT (ATel #8059), however there is a general decrease of the NIR brightness (0.27 ± 0.09 mag in H band).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Quasar", "Near-Earth object", "Nova" ] }, "answerKey": "D" }, { "id": "atel_8310", "message": "Title: A new NIR Flare of the Blazar CGRaBSJ2345-1555\nAuthors: L. Carrasco, A. Porras, E. Recillas, V. Chavushyan, A. Carraminana (INAOE, Mexico)\nDate: 20 Nov 2015; 08:39 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Infra-Red, Optical, Gamma Ray, AGN, Blazar, Quasar\nDescription: We report on the recent NIR flare of the high redshift QSO BZQJ2345-1555 (z=0.621), cross identified with the source CGRaBSJ2345-1555 and the gamma-ray source 2FGLJ2345.0-1553. On November 1st,2015 (MJD 2457327.70), we found the source with the following fluxes in the NIR: J= 13.247 +/- 0.02, H = 12.417 +/- 0.05 and Ks = 11.412 +/- 0,05. This is to be compared with our previous observation on MJD 2457297.76, when the source flux corresponded to J = 14.030 +/- 0.02, H = 13.062 +/- 0.04 and Ks = 12.375 +/- 0.09 . Hence the source has had a flux increment of a factor 2.5 in this short lapse. This source has shown flaring activity in the past (see ATEL #2977)Our observations are carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We strongly encourage further multiwavelength coverage.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Neutron star", "Magnetar, Quasar", "Nova, Quasar", "Active galactic nucleus, Quasar" ] }, "answerKey": "D" }, { "id": "atel_8375", "message": "Title: PESSTO spectroscopic classification of optical transients\nAuthors: L. Le Guillou, R. Le Breton, S. Baumont (LPNHE), J. Anderson (ESO), L. Galbany (DAS, MAS), C. Inserra (QUB), E. Kankare (QUB), K. Maguire (QUB), S. J. Smartt (QUB), K. Smith (QUB), M. Sullivan (Southampton), S. Valenti (UC Davis), D. Young (QUB), O. Yaron, I. Manulis (Weizmann), D. Wright (QUB), K. Chambers, H. Flewelling, M. Huber, E. Magnier, J. Tonry, C. Waters, R. J. Wainscoat (IfA, Univ. Hawaii)\nDate: 6 Dec 2015; 15:05 UT\nProvenance: Sylvain Baumont (baumont@lpnhe.in2p3.fr)\nSubjects: Optical, Cataclysmic Variable, Transient\nDescription: PESSTO, the Public ESO Spectroscopic Survey for Transient The Objects (see Smartt et al. 2015, A&A, 579, 40 http://www.pessto.org ), reports the following supernova classification. The target was supplied by Pan-STARRS Survey for Transients (see Huber et al., ATel #7153). All observations were performed on the ESO New Technology Telescope at La Silla on 2015 December 05, using EFOSC2 and Grism 13 (3985-9315A, 18A resolution). Classification was done with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024) and GELATO (Harutyunyan et al., 2008, A&A, 488, 383). Classification spectrum can be obtained from http://www.pessto.org (via WISeREP). \n \n \n Name | RA (J2000) | Dec (J2000) | Disc. Date | Disc. Source | Disc Mag | redshift | Type | Phase | Notes \n \n PS15dbp | 06 44 39.91 | -19 56 42.2 | 2015 12 01 | Pan-STARRS | 18.0 | M.W. | C.V. | young | (1) \n \n(1) Blue continuum, with narrow Balmer emission lines at null redshift, and no evidence of P-Cygni signature.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Stellar evolution", "Quasar", "Variable star" ] }, "answerKey": "A" }, { "id": "atel_8475", "message": "Title: INTEGRAL/Swift observations of V404 Cyg back in outburst\nAuthors: S. E. Motta (Uni. Oxford), C. Sanchez-Fernandez, J. Kajava, E. Kuulkers (ESA/ESAC), K. Page (Uni. Leicester), E. Bozzo, D. Malyshev (uni. Geneva)\nDate: 30 Dec 2015; 09:47 UT\nProvenance: Sara Elisa Motta (sara.motta@physics.ox.ac.uk)\nSubjects: X-ray, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 8482, 8489, 8494, 8499, 8500, 8501, 8507, 8510, 8512, 8516\nThe black hole candidate V404 Cyg has recently entered a new outburst phase (ATel #8453, #8454, #8455, #8457, #8462). \nINTEGRAL performed a ToO observation of V404 Cyg in spacecraft revolution 1626 (from 2015-12-26 07:59 to 2015-12-28 12:00). The total observation time was about 170 ks. \nV404 Cyg was observed by ISGRI and JEM-X instruments with the following fluxes and significances: \nisgri 20-40 keV 0.76 +/- 0.09 cts/s (4.7 +/- 0.6 mCrab) significance=8.9 \nisgri 40-80 keV 0.615 +/- 0.06 cts/s (8.0 +/- 0.8 mCrab) significance=10.5 \njmx 3-10 keV 0.24 +/- 0.03 cts/s (1.0 +/- 0.1 mCrab) significance = 16.5 \njmx 10-20 keV 0.066 +/- 0.026 cts/s ( 1.1 +/- 0.4 mCrab) \nThe IBIS/JEM-X light curve shows moderate flickering, comparable to the one seen in the Swift/XRT data. No significant flares are visible in the lightcurve. \nThe spectra of IBIS/ISGRI, JEMX-1 and Swift/XRT (Obs. taken on 2015-12-26 08:08:23, 2015-12-26T22:59:30, 2015-12-27 08:12:58, 2015-12-27 12:59:58 ) can be simultaneously fitted with and absorbed power law (Nh = 3.2 +/- 0.5 x 10^22 g/cm^2) with a photon index of 1.6 +/- 0.2, consistent with the photon index from the fits to the IBIS/ISGRI and JEM-X spectra alone (1.9 -0.3/+0.4). No soft excess nor a narrow line around 6.4 keV are visible in the joint spectrum and no high-energy cutoff is required. The addition of a reflection component does not improve the fit. The observed flux in the (0.6-200) keV energy band is 2.4x10^-10 ergs/cm^2/s \nThe multi-wavelength data obtained so far all show a much fainter outburst with respect to the one we witnessed during the summer of 2015. The current outburst is characterised by the same underlying moderate flaring activity that was observed, during the rise and decay of the June 2015 outburst (ATel #7959), although with a substantial lack of the strong flares (where the flux of the source increased of order of magnitudes in matters of minute, see e.g. ATel #7731) that characterised the previous outburst(s). It might be therefore possible that V404 Cyg is going through a standard X-ray outburst. \nINTEGRAL will continue observing the source until the end of the year, while Swift will continue the monitoring until the 6th of January. Multi-Wavelength observations are strongly encouraged. \nWe would like to sincerely thank the INTEGRAL and Swift teams for the fast re-planning of the observing schedule over the Christmas break.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Supernova", "Black hole, Binary system", "Accreting object, Binary system", "Black hole, Repeater" ] }, "answerKey": "B" }, { "id": "atel_8550", "message": "Title: jujia@ynao.ac.cn\nAuthors: Spectroscopic Classification of ASASSN-16aj (AT 2016K) as a Type Ia Supernova\nDate: 15 Jan 2016; 14:09 UT\nProvenance: Ju-Jia Zhang (jujia@ynao.ac.cn)\nSubjects: Optical, Supernovae\nDescription: Referred to by ATel #: 10722\nWe report an optical spectrum (range 350-900 nm) of ASASSN-16aj (ATEL #8542, AT 2016K) obtained on UT 2016 Jan. 15.5 with the 2.4 m telescope ( LJT + YFOSC) at Lijiang observatory of Yunnan Observatories. The spectrum is consistent with a Type Ia supernova at around maximum light. Cross-correlation with a library of supernova spectra using the \"Supernova Identification\" code (SNID; Blondin and Tonry 2007, ApJ. 666, 1024) shows that it matches with SN 2003du at t = -1 days. Adopting a redshift of 0.0307 for its host galaxy NGC 1562, an expansion velocity of about 11,500 km/s can be derived from the absorption minimum of Si II 635.5 nm.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system", "Circumstellar disk", "Supernova", "Interstellar medium" ] }, "answerKey": "C" }, { "id": "atel_8650", "message": "Title: VR Photometric Monitoring of the PNV J09553757+6900146 Nova in M81\nAuthors: Peter Pessev (Gran Telescopio Canarias, Instituto de Astrofísica de Canarias, Universidad de La Laguna, SPAIN); Galin Borisov (Armagh Observatory, Northern Ireland, UK); Yanko Nikolov (Institute of Astronomy, BAS, BG)\nDate: 8 Feb 2016; 12:35 UT\nProvenance: Peter Pessev (peter.pessev@gtc.iac.es)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 8678\nPNV J09553757+6900146 transient in M81 was observed with the 2m RCC telescope of BNAO Rozhen, equipped with the FoReRo2 instrument starting on February 07.729 (middle 07.736) and 07.745 (middle 07.752) 2016 UT in R and V bands respectively under a clear sky conditions and 1.5 arcsec seeing. There 300 seconds exposures were acquired in the V and R bands, along with short 1 second calibration exposures for a total of 900 seconds in each filter. We measured V = 21.6 +/- 0.5 and R = 20.6 +/- 0.2, using the standards of de Vaucouleurs et al. 1994, located in the M81 field. This corresponds to a V-R colour, equal to 1.0 +/- 0.5. Taking into account the R band photometry, published in ATel #8632, the nova has passed its maximum light. Further observations are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Nova", "Stellar evolution", "Interstellar medium" ] }, "answerKey": "B" }, { "id": "atel_8730", "message": "Title: MASTER-Kislovodsk: bright OT with 7mag amplitude\nAuthors: O. Gress, V. Lipunov, E. Gorbovskoy (Lomonosov MSU), N. Samus (INASAN, Lomonosov MSU), N. Tiurina, P. Balanutsa, V. Vladimirov, A. Kuznetsov, V. Kornilov, V. Shumkov, I. Gorbunov, D. Vlasenko, D. Kuvshinov (Lomonosov Moscow State University, SAI), , A. Tlatov, V. Senik, D. Dormidontov, A. Parkhomenko(Kislovodsk Solar Station, Main Pulkovo observatory)\nDate: 25 Feb 2016; 08:23 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Request for Observations, Cataclysmic Variable, Transient, Variables\nDescription: MASTER OT J073325.52+373744.9 discovery - outburst with Ampl>7m, Nova or dwarf nova?\nMASTER-Kislovodsk auto-detection system ( Lipunov et al., \"MASTER Global Robotic Net\", Advances in Astronomy, 2010 )discovered OT source at (RA, Dec) = 07h 33m 25.52s +37d 37m 44.9s on 2016-02-24.90468 UT. \nThe OT unfiltered magnitude is \n15.1m \n(limit 18.0m).The OT is seen in 3 images. There is no minor planet at this place. \nWe have the following reference images without OT: \n2015-11-20 20:16:45 19.6 (MASTER-Tunka) \n2015-09-24 20:24:29 19.1 (MASTER-Tunka) \n2015-02-18 14:46:28 19.5 (MASTER-Tunka) \n2014-10-26 01:46:21 20.4 (MASTER-Kislovodsk) \n2013-11-27 19:22:56 19.5 (MASTER-Tunka) \n2012-01-27 17:01:13 20.2 (MASTER-Tunka) \n2011-11-05 20:39:29 20.3 (MASTER-Tunka) \n2011-01-25 14:17:22 20.1 (MASTER-Tunka) \n2011-10-28 02:23:13 20.3 (MASTER-Kislovodsk) \n\nThere is SDSS star in 0.5\" with u=22.1(=-0.3),g=21.9(+-0.1),r=22.1(=-0.2),i=22.5, so we suggest the dwarf nova outburt with Ampl>7m. \nSpectral observations are required. \nThe discovery and reference images are available at http://master.sai.msu.ru/static/OT/MASTEROTJ073325.52373744.9.png \nList of Optical Transients discovered by MASTER\nMASTER Global Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Quasar", "Circumstellar disk", "Globular cluster" ] }, "answerKey": "A" }, { "id": "atel_8820", "message": "Title: ATLAS limits on explosion epoch of SN2016bau in NGC3631\nAuthors: J. Tonry, L. Denneau, B. Stalder, A. Heinze, A. Sherstyuk (IfA, University of Hawaii), A. Rest (STScI), K. W. Smith, S. J. Smartt (Queen's University Belfast)\nDate: 15 Mar 2016; 16:42 UT\nProvenance: Stephen Smartt (s.smartt@qub.ac.uk)\nSubjects: Optical, Supernovae\nDescription: Referred to by ATel #: 8911\nFollowing the discovery of SN2016bau in NGC3631 at 13Mpc by Ron Arbour (TNS Astronomical Transient Report No. 1487) and the spectroscopic confirmation of Granata et al. (ATel #8818, Asiago Transient Classification Program) as a young type Ib supernova, we report limits on the explosion epoch. \nThe ATLAS unit in Haleakala (see Tonry et al. ATel #8680) observed NGC3631 during its robotic sky operations with four 30 sec exposures on 2016-03-11 between 10:13 and 11:33 UT in the ATLAS cyan filter. (420-650nm, for more details see http://www.fallingstar.com ). Ron Arbour's discovery images are 2016-03-13 23:22 UT. SN2016bau is not visible in any of the four ATLAS images. Difference images were produced as part of standard ATLAS operations with respect to a reference sky. No object is detected and the stack of 4x30s also did not detect the SN. \nWe estimate the limiting 5-sigma magnitude in an aperture of radius equal to the measured FWHM. This is m_AB = 19.2 in the 4x30s stack, at the position of the SN. The background flux in the ATLAS pixels at this position (35\" W 15\" N of Host) is about 50% from the night sky and 50% from NGC3631. \nOur limiting mag of 19.2 compares with Ron Arbour's discovery measurement of 17.8 approximately 2.5 days later. This confirms the conclusion of Granata et al. (ATel #8818) that this was indeed a supernova discovered very young. Given the early discovery and still faint absolute magnitude pointed out by Granata et al., further multi-wavelength observations are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Supernova", "Repeater", "Pulsar" ] }, "answerKey": "B" }, { "id": "atel_8925", "message": "Title: AGILE detection of gamma-ray activity from the FSRQ S5 1039+81 region\nAuthors: A. Bulgarelli (INAF/IASF-Bo), F. Lucarelli, F. Verrecchia, C. Pittori (ASDC and INAF/OAR), G. Piano, P. Munar-Adrover (INAF/IAPS), V. Fioretti, A. Zoli (INAF/IASF-Bo), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), S. Vercellone (INAF/IASF-Pa), I. Donnarumma (INAF/IAPS), E. Striani (CIFS and INAF/IAPS), M. Cardillo (INAF/OA-Arcetri and INAF/IAPS), F. Gianotti, M. Trifoglio (INAF/IASF-Bo), A. Giuliani, S. Mereghetti, P. Caraveo, F. Perotti (INAF/IASF-Mi), A. Chen (Wits University), A. Argan, E. Costa, E. Del Monte, Y. Evangelista, M. Feroci, F. Lazzarotto, I. Lapshov, L. Pacciani, P. Soffitta, S. Sabatini, V. Vittorini (INAF/IAPS), G. Pucella, M. Rapisarda (ENEA-Frascati), G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, M. Marisaldi (INAF/IASF-Bo), A. Pellizzoni, M. Pilia, A. Trois (INAF/OA-Cagliari), G. Barbiellini, E. Vallazza (INFN Trieste), F. Longo (Univ. Trieste and INFN Trieste), A. Morselli, P. Picozza (INFN and Univ. Roma Tor Vergata), M. Prest (Univ. dell'Insubria), P. Lipari, D. Zanello (INFN and Univ. Roma Sapienza), P. W. Cattaneo, A. Rappoldi (INFN Pavia), S. Colafrancesco (INAF/OAR and Wits University), N. Parmiggiani (University of Modena and Reggio Emilia), A. Ferrari (Univ. Torino and CIFS), A. Antonelli (ASDC and INAF/OAR), P. Giommi (ASDC), L. Salotti, G. Valentini, and F. D'Amico (ASI)\nDate: 8 Apr 2016; 13:25 UT\nProvenance: Andrea Bulgarelli (bulgarelli@iasfbo.inaf.it)\nSubjects: Gamma Ray, Transient\nDescription: The AGILE satellite is detecting a bright gamma-ray source consistent with the position of the FSRQ S5 1039+81 (also known as 5BZQJ1044+8054). \nIntegrating from 2016-04-05 19:13 UT to 2016-04-07 19:13 UT, a maximum likelihood analysis of AGILE data yields the detection of a source with a flux of (1.5 +/- 0.45) x 10^-6 ph/cm2/s (E > 100 MeV) at a significance level of 5.3 sigma. \nThis measurement was obtained with AGILE observing a large portion of the sky in spinning mode. Multifrequency observations of the source are strongly encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Binary system", "Supernova", "Active galactic nucleus" ] }, "answerKey": "D" }, { "id": "atel_9025", "message": "Title: Spectroscopic Classification of SN 2016cck (=PTSS-16efw) as a Type Ia Supernova\nAuthors: Jujia Zhang, Jianguo Wang (YNAO), Xiaofeng Wang, Wenxiong Li, Zesheng Yang (Tsinghua University), Bin Li, Zhijian Xu, Haibin Zhao, Lifan Wang (PMO)\nDate: 6 May 2016; 01:08 UT\nProvenance: Ju-Jia Zhang (jujia@ynao.ac.cn)\nSubjects: Optical, Supernovae\nDescription: We obtained an optical spectrum (range 340-900 nm) of SN 2016cck (=PTSS-16efw), discovered by the PMO-Tsinghua Supernova Survey (PTSS: http://119.78.210.3/ptss2/ ), on UT May 05.8 2016 with the 2.4 m telescope ( LJT + YFOSC) at LiJiang Observatory of Yunnan Observatories (YNAO). The spectrum is consistent with a type Ia supernova at the maximum light. Cross-correlation with a library of supernova spectra using the \"Supernova Identification\" code (SNID; Blondin and Tonry 2007, ApJ, 666, 1024) shows that it matches with SN 2007af at t = +0 days from the maximum light. This is consistent with the report of ATel#9023 about this transient (i.e., SN1999cc at t = -1 days). After correcting for a redshift of 0.037 for its host galaxy (from the H alpha emission near the SN), an expansion velocity of about 11000 km/s can be derived from the absorption minimum of Si II 635.5 nm.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Supernova", "Neutron star", "Star and stellar system" ] }, "answerKey": "B" }, { "id": "atel_9090", "message": "Title: Spectroscopic classification of ASASSN-16fp with the Nordic Optical Telescope\nAuthors: N. Elias-Rosa (INAF-Padova), S. Mattila (Turku), P. Lundqvist (Stockholm), M. Stritzinger (Aarhus U), H. Kuncarayakti (MAS, DAS), J. Harmanen (Turku), A. Pastorello (INAF-Padova), S. Benetti (INAF-Padova), E. Cappellaro (INAF-Padova), N. Blagorodnova (Caltech), S. Davis (FSU), S. Dong (KIAA-PKU), M. Fraser (IoA), C. Gall (Aarhus U), D. Harrison (IoA), S. Hodgkin (IoA), E. Y. Hsiao (FSU), P. Jonker (SRON), T. Kangas (Turku), E. Kankare (QUB), Z. Kostrzewa-Rutkowska (Warsaw/SRON), M. Nielsen (Aarhus U), P. Ochner (INAF-Padova), J. L. Prieto (UDP, MAS), T. Reynolds (Turku, NOT), C. Romero-Canizales (PUC, MAS), F. Taddia (OKC), L. Tartaglia (INAF-Padova), G. Terreran (INAF-Padova/QUB), L. Tomasella (INAF-Padova), L. Wyrzykowski (Warsaw Observatory)\nDate: 28 May 2016; 12:23 UT\nProvenance: Seppo Mattila (seppo.mattila@utu.fi)\nSubjects: Optical, Supernovae\nDescription: Referred to by ATel #: 9124, 9134, 9147\nThe NOT Unbiased Transient Survey (NUTS; ATel #8992) collaboration reports the spectroscopic classifications of supernova ASASSN-16fp in UGC 11868. The candidate was discovered by the All-Sky Automated Survey for Supernovae (ASAS-SN, ATEL#9086). \nThe observations were performed with the 2.56 m Nordic Optical Telescope equipped with ALFOSC (range 350-950 nm; resolution 1.4 nm) on 2016-05-28.15 UT. \n \n \n Name | Host gx. | Redshift | Discovery (UT) | Discovery mag | Type | Phase | Notes \n \n ASASSN-16fp | UGC 11868 | 0.0036 | 2016-05-27.55 |15.7 | Ic-broad | pre-max | (1) \n \n(1) Also known as SN 2016coi. The redshift of the host galaxy (UGC 11868) is from Giovanelli and Haynes 1993, AJ, 105, 1271; via NED. Best match with the broad line Type Ic SN 2006aj a few days before the maximum brightness. \nClassifications were performed using the GELATO (Harutyunyan et al. 2008, A&A, 488, 383) and SNID (Blondin and Tonry 2007, ApJ, 666, 1024) tools, and are posted on WISeREP (Yaron & Gal-Yam 2012, PASP, 124, 668).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Globular cluster", "Neutron star", "Nova" ] }, "answerKey": "A" }, { "id": "atel_9175", "message": "Title: New nova candidate in M81\nAuthors: M. Henze (CSIC-IEEC), G. Sala, J. Jose, J. Figueira (UPC-IEEC), M. Hernanz (CSIC-IEEC)\nDate: 21 Jun 2016; 17:04 UT\nProvenance: Martin Henze (henze@ice.cat)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 9177\nWe report the discovery of a new nova candidate in the M81 galaxy on 16x200s stacked R filter CCD images, obtained with the 80 cm Ritchey-Chretien F/9.6 Joan Oro telescope at Observatori Astronomic del Montsec, owned by the Catalan Government and operated by the Institut d'Estudis Espacials de Catalunya, Spain, using a Finger Lakes PL4240-1-BI CCD Camera (with a Class 1 Basic Broadband coated 2k x 2k chip with 13.5 microns sq. pixels). \n \nThe new object is clearly detected with a magnitude of R = 19.5±0.3 mag on 2016-06-20.91 UT. Its coordinates are RA = 9h54m53.95s, Dec = +69o02'33.8\" (J2000, 1σ accuracy 0.2\"). Nothing was found at this position in our preceding observation on 2016-06-07.91 UT, with an upper limit of about R = 20.5, and no object is present within a 4\" radius in the VizieR/CDS data base. Astrometry and photometry were calibrated based on the SDSS DR7 photometry catalogue. \n \nSpectroscopic follow-up observations are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy", "Pulsar", "Interstellar medium", "Nova" ] }, "answerKey": "D" }, { "id": "atel_9240", "message": "Title: FLOYDS Classification of Gaia16ann as an AGN\nAuthors: G. Hosseinzadeh, I. Arcavi, D. A. Howell, C. McCully (LCOGT/UCSB), S. Valenti (UC Davis)\nDate: 12 Jul 2016; 12:39 UT\nProvenance: Curtis McCully (cmccully@lcogt.net)\nSubjects: Optical, AGN, Supernovae, Transient\nDescription: We obtained a spectrum of Gaia16ann on 2016 July 7.5 UT with the robotic FLOYDS instrument mounted on the LCOGT 2-meter telescope on Haleakala, Hawai'i. Using SNID (Blondin & Tonry 2007, ApJ, 666, 1024), we find a good fit to an AGN at redshift z=0.196.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Active galactic nucleus", "Quasar", "Interstellar medium" ] }, "answerKey": "B" }, { "id": "atel_9350", "message": "Title: Renewed gamma-ray activity from the blazar PKS 1510-089 detected by AGILE\nAuthors: C. Pittori (ASDC and INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), F. Lucarelli, F. Verrecchia (ASDC and INAF/OAR), G. Piano, P. Munar-Adrover (INAF/IAPS), A. Bulgarelli, V. Fioretti, A. Zoli (INAF/IASF-Bo), S. Vercellone (INAF/IASF-Pa), G. Minervini (CIFS and INAF/IAPS), E. Striani (CIFS and INAF/IAPS), M. Cardillo (INAF/OA-Arcetri and INAF/IAPS), F. Gianotti, M. Trifoglio (INAF/IASF-Bo), A. Giuliani, S. Mereghetti, P. Caraveo, F. Perotti (INAF/IASF-Mi), A. Chen (Wits University), A. Argan, E. Costa, E. Del Monte, Y. Evangelista, M. Feroci, F. Lazzarotto, I. Lapshov, L. Pacciani, P. Soffitta, S. Sabatini, V. Vittorini (INAF/IAPS), G. Pucella, M. Rapisarda (ENEA-Frascati), G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, M. Marisaldi (INAF/IASF-Bo), A. Pellizzoni, M. Pilia, A. Trois (INAF/OA-Cagliari), G. Barbiellini, E. Vallazza (INFN Trieste), F. Longo (Univ. Trieste and INFN Trieste), A. Morselli, P. Picozza (INFN and Univ. Roma Tor Vergata), M. Prest (Univ. dell'Insubria), P. Lipari, D. Zanello (INFN and Univ. Roma Sapienza), P. W. Cattaneo, A. Rappoldi (INFN Pavia), S. Colafrancesco (INAF/OAR and Wits University), N. Parmiggiani (University of Modena and Reggio Emilia), A. Ferrari (Univ. Torino and CIFS), A. Antonelli (ASDC and INAF/OAR), P. Giommi (ASDC), L. Salotti, G. Valentini, and F. D'Amico (ASI)\nDate: 9 Aug 2016; 16:48 UT\nProvenance: Carlotta Pittori (carlotta.pittori@asdc.asi.it)\nSubjects: Gamma Ray, AGN, Blazar, Transient\nDescription: Referred to by ATel #: 9450, 9520\nAGILE is now detecting transient gamma-ray emission above 100 MeV from a source positionally consistent with the blazar PKS 1510-089. \nIntegrating from 2016-08-07 09:00 UT to 2016-08-09 09:00 UT, a preliminary maximum likelihood analysis yields a detection above 100 MeV positioned at Galactic coordinates (l,b) = (350.64,40.32) +/- 0.7 (stat.) +/- 0.1 (syst.). The gamma-ray flux is F =(2.7 +/- 0.9) x 10E-6 ph/cm2/sec with a significance level above 5 sigma. \nThis measurement was obtained with AGILE observing a large portion of the sky in spinning mode. Multifrequency observations of the source are strongly encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Black hole", "Active galactic nucleus", "Globular cluster" ] }, "answerKey": "B" }, { "id": "atel_9425", "message": "Title: MASTER: OT discovered during inspection of HESE 58537957 trigger \nAuthors: N. Tyurina, V. Lipunov (Lomonosov MSU), D. Buckley (SAAO), E. Gorbovskoy, P. Balanutsa, A. Kuznetsov, V. Kornilov, D. Kuvshinov, D. Vlasenko, O. Gress, K. Ivanov, V. Shumkov (Lomonosov Moscow State University, SAI), S. Potter (South African Astronomical Observatory)\nDate: 30 Aug 2016; 00:37 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Neutrinos, Request for Observations, Transient\nDescription: Referred to by ATel #: 9456\nMASTER OT J130845.02-323254.9 - optical transient detection during inspection of HESE 58537957_128340 alert\nMASTER-SAAO auto-detection system ( Lipunov et al., \"MASTER Global Robotic Net\", Advances in Astronomy, 2010, 349171 ) discovered OT source at (RA, Dec) = 13h 08m 45.02s -32d 32m 54.9s on 2016-08-24.73811 UT during inspection of HESE alert ( 58537957 trigger number ) http://gcn.gsfc.nasa.gov/notices_amon/58537957_128340.amon . \nThe OT unfiltered magnitude is 19.6m (limit 20.5m). \nThe OT is seen in 12 images. There is no minor planet at this place. \nWe have reference image without OT on 2015-02-20.01763 UT with unfiltered magnitude limit 20.5m. \nSpectral observations are required (preliminary possible classification is dwarf nova). \nThe discovery and reference images are http://observ.pereplet.ru/images/HESE58537957MASTER.jpg List of Optical Transients discovered by MASTER\nMASTER Global Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Variable star", "Star and stellar system", "Active galactic nucleus" ] }, "answerKey": "B" }, { "id": "atel_9500", "message": "Title: Updated Transit Ephemeris for KELT-1b\nAuthors: T. Beatty (PSU)\nDate: 16 Sep 2016; 20:09 UT\nProvenance: Thomas Beatty (tgbeatty@gmail.com)\nSubjects: Optical, Exoplanet\nDescription: Using KeplerCam on the FLWO 1.2m, we observed a transit of KELT-1b on the night of UT 2013 October 18 in the SDSS i' filter. Combined with the transit center time given in Siverd et al. (2012), we find a revised transit ephemeris of: \nTc = 2456583.78435 +/- 0.0006 BJD_UTC \nP = 1.217494 +/- 0.000004", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Exoplanet", "Repeater", "Star and stellar system" ] }, "answerKey": "B" }, { "id": "atel_9625", "message": "Title: GRS 1758-258 not detected at hard X-rays\nAuthors: K. Pottschmidt (NASA-GSFC/UMBC), W. Eikmann, I. Kreykenbohm, J. Wilms, M. Hirsch, M. Kuehnel (all ECAP-FAU), B. H.G. Rodrigues (Itajuba), F. Krauss (UvA), R. Soria (ICRAR-Curtin/Sydney), V. Grinberg (MIT), D. M. Smith (UCSC), M. Cadolle Bel (MPCDF), J. A. Tomsick (UCB), A. Bodaghee (GSCU), E. Kuulkers (ESA-ESAC) on behalf of the INTEGRAL Galactic bulge monitoring team, E. Kalemci (Sabanci), J. M. Miller (Michigan)\nDate: 14 Oct 2016; 18:01 UT\nProvenance: Katja Pottschmidt (katja@milkyway.gsfc.nasa.gov)\nSubjects: X-ray, Black Hole\nDescription: Referred to by ATel #: 9890\nThe Galactic black hole candidate GRS 1758-258 is usually found in the hard state but has been known to enter soft states in which the spectrum changes from a power-law to a thermal disk without substantial changes in bolometric luminosity (Soria et al., 2011, MNRAS 415, 410). The most extended soft state to date was observed in 2000-2002 (Smith et al., 2001, ApJ 554, L41). The soft states are associated with a strong drop in flux above 3 keV (Pottschmidt et al., 2006, A&A 452, 285; Soria et al., 2011, MNRAS 415, 410). Recent observations of the source show the strongest drop in flux since the 2000-2002 episode: \nThe Swift BAT 15-50 keV light curve of GRS 1758-258 shows a rapid decline in flux over the past ~50 days and the source has not been detected during the past ~15 days ( http://swift.gsfc.nasa.gov/results/transients/GRS1758-258/ ). \nThe source has been extensively covered by the INTEGRAL Galactic bulge monitoring-, Galactic Center monitoring-, and our GRS 1758-258 TOO observation program from 2016 August 17 onward. INTEGRAL ISGRI confirms the rapid flux decline over this time range. Selected values in the 20-40 keV energy band are 69+/-3 mCrab (8.7+/-0.3 cps) on 8/17, 24+/-2 mCrab (3.0+/-0.2 cps) on 9/2, and 15+/-1 mCrab (1.9+/-0.2 cps) on 9/27. Selected values in the 40-80 keV energy band are 74+/-4 mCrab (4.8+/-0.3 cps) on 8/17 31+/-2 mCrab (2.0+/-0.2 cps) on 9/2, and 13+/-2 mCrab (0.9+/-0.1 cps) on 9/27. \nGRS 1758-258 has not been detected by ISGRI since 2016 September 30. During the most recent INTEGRAL Galactic Center observation on 2016 October 11, with an effective exposure of 4.4 ks, upper limits of 0.4 cps and 0.5 cps were obtained in the 20-40 keV and 40-80 keV energy bands, respectively. \nAdditional observations are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Binary system", "Near-Earth object", "Black hole" ] }, "answerKey": "D" }, { "id": "atel_9700", "message": "Title: Classification of DES16C2nm as a SLSN at z=1.998 \nAuthors: L. Galbany (MAS/U. de Chile/U. Pitt), C. D'Andrea (University of Pennsylvania), S. Prajs, M. Smith, M. Sullivan (University of Southampton), K. Ponder (U. Pitt), S. Gonzalez-Gaitan (MAS/CMM), F. Forster (MAS/CMM), M. Hamuy (U. de Chile/MAS), Jose Luis Prieto (U. Diego Portales/MAS), M. Schubnell (University of Michigan), R. Kessler, J. Lasker, D. Scolnic (University of Chicago), D. J. Brout, L. Gladney, M. March, M. Sako, R. C. Wolf (University of Pennsylvania), P. J. Brown, K. Krisciunas, N. Suntzeff (Texas A&M University), E. Macaulay, R. Nichol (University of Portsmouth), M. Childress (University of Southampton), R. Maartens (University of the Western Cape), E. Kovacs, S. Kuhlmann, H. Spinka (Argonne National Laboratory), E. Ahn, D. A. Finley, J. Frieman, J. Marriner, W. Wester (Fermilab), G. Aldering, R. Gupta, A. G. Kim, R. C. Thomas (Lawrence Berkeley National Laboratory), K. Barbary, J. S. Bloom, D. Goldstein, P. Nugent, S. Perlmutter (Lawrence Berkeley National Laboratory + University of California, Berkeley), R. J. Foley, Y.-C. Pan (University of California, Santa Cruz), R. Casas, F. J. Castander (ICE, IEEC/CSIC, Barcelona), A. Papadopoulos (Cyprus University), E. Morganson (University of Illinois at Urbana-Champaign), S. Desai, K. Paech (Ludwig Maximilians University, Munich), R. C. Smith (NOAO/CTIO)\nDate: 1 Nov 2016; 21:47 UT\nProvenance: Mathew Smith (matsmith2@gmail.com)\nSubjects: Optical, Supernovae, Transient\nDescription: We report the spectroscopic classification of DES16C2nm as a superluminous supernova (SLSN) discovered by the Dark Energy Survey (ATEL #4668). DES16C2nm was discovered in the first epoch of DES Y4, on 22 August 2016 at R.A. = 03:40:14.83, Decl = -29:05:53.5 with i = 23.2 mag. DES16C2nm has a non-detection in the final epoch of DES Y3 on 08 February 2016. We obtained spectra using LDSS3 on the 6.5m Clay telescope at the Las Campinas Observatory on 10 October 2016 which indicated a redshift of z = 1.998 from Mg II 2800 and FeII 2344/2383 absorption. Further observations were obtained with the X-SHOOTER instrument (wavelength range 380-950nm) on the Very Large Telescope (VLT) of the European Southern Observatory (ESO) on 23 & 24 October 2016, which confirm DES26C2nm to be a SLSN at z = 1.998 near maximum light, spectroscopically similar to iPTF13ajg. Object classification was performed using superfit (Howell et al, 2005, ApJ, 634, 119), the details of which are reported in the table below. \n \n \n Name | RA (J2000)| Dec (J2000)|Discovery |Discovery|Spectrum |Redshift| Type | Phase |Notes \n | | |Date (UT) |Mag (i) |Date (UT) | | | | \n DES16C2nm |03:40:14.83|-29:05:53.5 |2016 Aug 22| 23.2 |2016 Oct 10 (Magellan), 2016 Oct 23/24 (VLT)| 1.998 |SLSN-I |near-max| a \n \n a). Redshift from galaxy absorption features", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Near-Earth object", "Supernova", "Pulsar" ] }, "answerKey": "C" }, { "id": "atel_9810", "message": "Title: Chandra observation of Nova SMC 2016\nAuthors: M. Orio (University of Wisconsin and INAF-Padova, Italy), Ehud Behar (Department of Physics, Technion, Haifa, Israel), Thomas Rauch (Institute for Astronomy and Astrophysics, Eberhard Karls University, Tuebingen, Germany) and Polina Zemko (Dept of Physics and Astronomy, Padova University, Italy) on behalf of a larger collaboration\nDate: 30 Nov 2016; 09:59 UT\nProvenance: Marina Orio (orio@astro.wisc.edu)\nSubjects: X-ray, Nova, Transient, Variables\nDescription: Referred to by ATel #: 9970\nNova SMC 2016 (MASTER OT J010603.18-744715.8; see ATel #9621, #9733) was observed with Chandra, the High Resolution Camera (HRC-S) and the Low Energy Transmission Grating (LETG) on 2017 November 17-18 with an exposure time of approximately 8 hours and 20 minutes. A luminous supersoft X-ray source was detected with a count rate of about 8.6 and 9 counts/s in the -1 and +1 order, respectively. The spectrum shows a stellar continuum, revealing a very hot white dwarf with an effective temperature of about 650,000 K, and deep absorption features, mainly of carbon and nitrogen. We also tentatively identified several absorption features due to transitions of sulfur (S VIII, S X and S XI) that may be attributed to an Oxygen-Neon white dwarf, although more work is necessary for a correct atmospheric model. All absorption features are blue shifted by about 1700 km/s. Some emission lines appear to be superimposed on the spectrum, mostly of nitrogen (N VI), which are likely originating in the ejecta. The zero order light curve measured with the HRC-S detector shows large variability on different time scales. A more complete analysis is under way.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution, Nova", "Variable star, Minor body", "Variable star, Repeater", "Variable star, Nova" ] }, "answerKey": "D" }, { "id": "atel_9875", "message": "Title: ASASSN-16ov: Discovery of A Probable Supernova in NPM1G +01.0158\nAuthors: R. S. Post (Post Astronomy), J. Brimacombe (Coral Towers Observatory), T. W.-S. Holoien, K. Z. Stanek, C. S. Kochanek, J. S. Brown, T. A. Thompson, J. Shields (Ohio State), B. J. Shappee (Hubble Fellow, Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), D. Bersier (LJMU), Subo Dong, S. Bose, Ping Chen (KIAA-PKU), .M. Fernandez (Observatory Inmaculada del Molino), S. Kiyota (Variable Star Observers League in Japan), G. Masi (Virtual Telescope Project, Ceccano, Italy), G. Stone (Sierra Remote Observatories)\nDate: 19 Dec 2016; 02:18 UT\nProvenance: Thomas Holoien (tholoien@astronomy.ohio-state.edu)\nSubjects: Optical, Supernovae, Transient\nDescription: During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or \"Assassin\"), using data from the quadruple 14-cm \"Brutus\" telescope in Haleakala, Hawaii, we discovered a new transient source, most likely a supernova, in the galaxy NPM1G +01.0158. \nASASSN-16ov (AT 2016ixb) was discovered in images obtained on UT 2016-12-17.29 at V~17.6 mag. We do not detect (V>17.1) the object in images taken on UT 2016-12-15.42 and before. Images obtained on UT 2016-12-18 by R. S. Post and J. Brimacombe confirm the discovery of the transient. This figure shows the archival DSS image of the host (left) and the J. Brimacombe confirmation image (right). The red circle has a radius of 5\" and is centered on the position of the transient in the J. Brimacombe image. \nThe position of ASASSN-16ov is approximately 0.40\" North and 0.03\" East from the center of the galaxy NPM1G +01.0158 (z=0.028343, d=119 Mpc, via NED), giving an absolute V-band magnitude of approximately -17.9 (m-M=35.37, A_V=0.161). Properties of the new source and photometry are summarized in the tables below: \n \n \n Object RA (J2000) DEC (J2000) Disc. UT Date Disc. V mag Approx. Abs. Mag Offset from Host (\") \n ASASSN-16ov 04:53:59.79 +01:57:46.21 2016-12-17.29 17.6 -17.9 0.4 \n \n \n \n Obs. UT Date V mag \n 2016-12-15.42 >17.1 \n 2016-12-17.29 17.6 \n \nFollow-up observations are encouraged. \nWhile we are participating in the TNS system to minimize potential confusion, ASAS-SN will continue using ASASSN-16xx transient names as our primary nomenclature (including supernovae, but also other classes of transients), and we encourage others to do the same. We prefer merging the names as ASASSN-16xx (AT2016xyz) to preserve, rather than anonymize, the origin of the transient. \nWe thank Las Cumbres Observatory and its staff for their continued support of ASAS-SN. ASAS-SN is supported by NSF grant AST-1515927, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, the Chinese Academy of Sciences South America Center for Astronomy (CASSACA), and the Mt. Cuba Astronomical Foundation. For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system", "Circumstellar disk", "Supernova", "Interstellar medium" ] }, "answerKey": "C" }, { "id": "atel_10050", "message": "Title: A NIR Flare of the Blazar BZUJ1048+7143\nAuthors: L. Carrasco, R. Gonzalez, E. Recillas, A. Porras, V. Chavushyan, D. Y. Mayya (INAOE, Mexico)\nDate: 4 Feb 2017; 17:39 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Infra-Red, Optical, Gamma Ray, AGN, Blazar, Quasar, Transient\nDescription: We report on the recent NIR flare of the high redshift QSO (z=1.15) BZUJ1048+7143 also known as CGRaBSJ1048+7143, cross correlated with the radio source S51044+71 and the Gamma-ray source 2FGLJ1048.3+7144.On January 11th,2017 MJD(2457764.9797), we found the source with NIR fluxes corresponding to J = 13.900 +/- 0.05, H = 12.975 +/- 0.03 and Ks = 12.214 +/- 0.05. While, on MJD 2457498 the flux in the H band corresponded to H = 14.252 +/- 0.03. Hence, the source has tripled its flux in this lapse. Our observations are carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We encourage further multi wavelength coverage.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar, Black hole", "Repeater, Black hole", "Binary system, Black hole", "Quasar, Stellar evolution" ] }, "answerKey": "A" }, { "id": "atel_10140", "message": "Title: A Bright Supernova Candidate Detected by the VVV Survey\nAuthors: D. Minniti (Universidad Andres Bello, The Milky Way Millennium Nucleus, Center for Astrophysics and Associated Technologies, Vatican Observatory), R. K. Saito (Universidade Federal de Santa Catarina)\nDate: 3 Mar 2017; 01:27 UT\nProvenance: Roberto Saito (saito@astro.ufsc.br)\nSubjects: Infra-Red, Supernovae, Transient\nDescription: Referred to by ATel #: 10163\nWe report the discovery of a large-amplitude near-IR transient event observed by the VVV Survey (vvvsurvey.org; Minniti et al. 2010, New Astronomy, 15, 433). The light curve has a clear eruption peaking in July 2013, reaching Ks~9 mag. Previous ZYJHKs observations taken in 2010, and Ks-band observations taken during during the 2010, 2011, and 2012 seasons show no detection of the progenitor at the source position. Taking into consideration that the detection limit in the field is of Ks~18.5 mag we can infer a total amplitude of Delta_Ks>9.5 mag. There is a nearby saturated star (~90 arcsec away to the West), but it does not seem to be responsible for producing the observed variation in brightness. \nWe derived an accurate position of this object using the VVV Ks-band images. The Equatorial coordinates are RA=17h07m18.917s, DEC=-39d06m26.45s (J2000), corresponding to Galactic coordinates l=347.14539, b=+0.88522. The approximate colours are (J-Ks)=2.146, (H-Ks)=0.952, (J-H)=1.194, measured at the decline phase in 27 July 2015. The object is located in a very reddened field, and we estimate a total extinction of A_V=10-15 mag depending on the shape of the reddening law. \nThe large amplitude, and the light curve shape and decline slope are consistent with a supernova. The amplitude is larger than those of VVV-WIT-01 (ATel #4041), and VVV-WIT-05 (ATel #8869). However, there are no published neutrino detections in the area at that time. Our search for earlier data of this object shows that it had no observable counterpart (within a distance of 5\") in previous images from 2MASS, GLIMPSE, Spitzer, WISE, nor MSX. We encourage further observations of this object at other wavelengths. \nThe tables below report the Cambridge Astronomical Survey Unit (CASU) photometry for this object. \n \n \n Ks-band observations: \n \n HJD mag merr flag \n 55285.39108101 beyond detection \n 55374.18025550 beyond detection \n 55692.31379194 beyond detection \n 55695.32765782 beyond detection \n 55697.37805366 beyond detection \n 55711.32512609 beyond detection \n 55795.07494736 beyond detection \n 55810.07695970 beyond detection \n 55840.00604085 beyond detection \n 56105.05465843 beyond detection \n 56111.03293386 beyond detection \n 56112.00600012 beyond detection \n 56113.96733594 beyond detection \n 56115.05587517 beyond detection \n 56473.09881128 10.001 0.01 -9 \n 56474.04973095 9.604 0.01 -9 \n 56475.19182240 9.693 0.01 -9 \n 56484.11403293 9.300 0.01 -9 \n 56496.04942542 9.096 0.01 -9 \n 56497.13131776 9.196 0.01 -9 \n 56498.06406656 9.359 0.01 -9 \n 56498.09551678 9.499 0.01 -9 \n 56508.98402608 10.825 0.01 -9 \n 56509.10667710 10.897 0.01 -9 \n 56509.17817734 10.834 0.01 -9 \n 56510.03239554 10.862 0.01 -1 \n 56510.16380074 10.803 0.01 -9 \n 56511.05712890 10.814 0.01 -9 \n 56521.98026580 11.528 0.01 -9 \n 56522.05744970 11.544 0.01 -9 \n 56522.99287532 11.560 0.01 -1 \n 56525.03867764 11.601 0.01 -1 \n 56526.07011642 11.535 0.01 -1 \n 56534.98473180 11.516 0.01 -1 \n 56535.05776775 11.507 0.01 -9 \n 56535.99602704 11.540 0.01 -1 \n 56837.98565643 14.894 0.036 -1 \n 56850.02943426 14.938 0.041 -1 \n 56850.15113615 14.895 0.031 -1 \n 56878.03521206 15.100 0.043 -1 \n 56887.99337296 15.102 0.042 -1 \n 56888.00700966 15.142 0.045 -1 \n 56888.02052799 15.179 0.045 -1 \n 56888.04609087 15.096 0.040 -1 \n 57113.22871432 16.071 0.094 -1 \n 57162.21248616 16.251 0.123 -1 \n 57228.09581258 16.301 0.122 -1 \n 57228.10790160 16.257 0.120 -1 \n 57228.11917881 16.495 0.153 -1 \n 57231.10604126 16.165 0.079 -1 \n \n Multicolour observations: \n \n Filter Date HJD mag merr flag \n Z 20150422 57135.37095248 beyond detection \n Y 20150422 57135.36738701 19.633 0.188 -1 \n J 20150727 57231.11120670 18.311 0.111 -1 \n H 20150727 57231.10081079 17.117 0.083 -1 \n Ks 20150727 57231.10604126 16.165 0.079 -1 \n \nPhotometric flags are described in Saito et al. 2012 (A&A, 537, A107): -1 corresponds to a stellar object, whereas -9 to a saturated source.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Circumstellar disk", "Supernova", "Star and stellar system" ] }, "answerKey": "C" }, { "id": "atel_10230", "message": "Title: MASTER: bright OT discovered during Fermi trigger 512353690/GRB170328A inspection\nAuthors: E. Gorbovskoy, V. Lipunov (Lomonosov MSU), D. Buckley (SAAO), R. Rebolo, M. Serra-Ricart (IAC), O. Gress, N. Tiurina, P. Balanutsa, V. Kornilov, V. Vladimirov (Lomonosov MSU, SAI)\nDate: 31 Mar 2017; 01:41 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Gamma Ray, Request for Observations, Gamma-Ray Burst, Transient, Variables\nDescription: Referred to by ATel #: 10231\nMASTER OT J184546.55-352847.6 discovery - possibly Fermi trigger 512353690/GRB170328A counterpart detection \nMASTER-SAAO auto-detection system ( Lipunov et al., \"MASTER Global Robotic Net\", Advances in Astronomy, 2010, 30L ) discovered OT source at (RA, Dec) = 18h 45m 46.55s -35d 28m 47.6s on 2017-03-28.06645 UT during Fermi trigger 512353690(GRB170328A) inspection \nhttps://gcn.gsfc.nasa.gov/other/512353690.fermi \n(trigger time is 17/03/28 00:28:05.53UT). \nThe OT's unfiltered magnitude is 17.0m (mlim=19.0). \nThere are only 2 images of this area (large Fermi error-boxes MASTER observed in inspection mode) and OT is seen in both images on \nTstart=2017-03-28 01:35:41UT and \nTstart=2017-03-28 01:42:14UT with exposition duration 60s (each). \nThere is no minor planet at this place except (208700)_2002_JK with Vmag=20.4 and 0.6E,7.0S offset (doesn't have any connection with our OT). \nWe have reference image on 2016-05-14.93352 UT with unfiltered mlim= 19.1m, the nearest in time images of this area are in MASTER-IAC database on 2016-07-31 23:23:26 with mlim=19.4. \nThere is no any sources in VIZIER database, it means 22mag limit in history \n \nDeep photometry and Spectral observations are required. \nThe discovery and reference images are available at: \nhttp://master.sai.msu.ru/static/OT/MASTEROTJ184546.55-352847.6.jpg \n\nMASTER Global Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Supernova", "Variable star", "Minor body" ] }, "answerKey": "C" }, { "id": "atel_10290", "message": "Title: Discovery of a Probable Nova in M81\nAuthors: R. Belligoli, F. Castellani, C. Marangoni, F. Marziali (OMB-CAV), K. Hornoch (Ondrejov), M. Henze (CSIC-IEEC), G. Sala, J. Jose, J. Figueira (UPC-IEEC), M. Hernanz (CSIC-IEEC), H. Kucakova (Charles University), S. C. Williams (Lancaster), H. Meusinger (TLS), M. J. Darnley (LJMU), A. Kaur, D. H. Hartmann (Clemson), A. W. Shafter (SDSU)\nDate: 20 Apr 2017; 09:28 UT\nProvenance: Martin Henze (henze@ice.cat)\nSubjects: Optical, Nova, Transient\nDescription: The extended M81 nova monitoring collaboration reports the discovery of a probable nova in M81 on pair of co-added 3900-s and 4200-s unfiltered CCD frames taken on 2017 Apr. 18.799 UT and 18.848 UT, respectively with the 0.4-m telescope at the Monte Baldo Observatory, Verona, Italy (MBO). The probable nova is also visible on a prediscovery R-band image taken on Apr. 18.086 UT with the 0.80-m telescope Joan Oro (TJO). \nThe object designated PNV J09551279+6900093 is located at R.A. = 9h55m12s.79, Decl. = +69o00'09\".3 (equinox 2000.0), which is 109.4\" west and 225.8\" south of the center of M81 (see link to discovery image below). \nHere we list the observing dates and corresponding photometry: \n \n \n Date [UT] | Mag | Err | Filter | Telescope \n 2017-04-16.857 | <21.3 | | C | OND \n 2017-04-17.086 | <21.5 | | R | TJO \n 2017-04-18.086 | 20.0 | 0.3 | R | TJO \n 2017-04-18.801 | 19.9 | 0.3 | C | MBO \n \n \nThe MBO 0.4-m is a Ritchey-Chretien F/8 telescope at the Monte Baldo Observatory, Ferrara di Monte Baldo, Verona, Italy. It uses a Moravian Instruments G4-9000 CCD camera (with a Kodak KAF-9000 sensor). The TJO is a 80-cm Ritchey-Chretien F/9.6 telescope at the Observatori Astronomic del Montsec, owned by the Catalan Government and operated by the Institut d'Estudis Espacials de Catalunya, Spain. It uses a Finger Lakes PL4240-1-BI CCD Camera with a Class 1 Basic Broadband coated 2k x 2k chip with 13.5 microns square pixels. The OND 0.65-m is a reflecting telescope at the Ondrejov observatory operated jointly by the Astronomical Institute of ASCR and the Astronomical Institute of the Charles University of Prague, Czech Republic. It uses a Moravian Instruments G2-3200 CCD camera (with a Kodak KAF-3200ME sensor and standard BVRI photometric filters) mounted at the prime focus. The MBO photometry is based on the NOMAD catalog. The TJO photometry is based on the SDSS DR7 photometry catalogue. The unfiltered OND photometry was calibrated against R-band comparison stars from Perelmuter & Racine (1995). \nDiscovery image", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Nova", "Active galactic nucleus", "Near-Earth object" ] }, "answerKey": "B" }, { "id": "atel_10375", "message": "Title: Spectroscopic classification of SN 2017dys (= ASASSN-17gb) with Faulkes Telescope North/FLOYDS\nAuthors: Y.-C. Pan, D. A. Coulter, C. D. Kilpatrick, M. R. Siebert, R. J. Foley (UCSC), S. W. Jha, K. Dettman (Rutgers), A. Rest (STScI), D. Scolnic (Chicago/KICP)\nDate: 15 May 2017; 01:15 UT\nProvenance: Yen-Chen Pan (ypan6@ucsc.edu)\nSubjects: Optical, Supernovae\nDescription: We obtained spectroscopic observations of 2017dys (= ASASSN-17gb) with the FLOYDS spectrograph on the 2-m Faulkes Telescope North on UT 2017 May 14. The spectrum indicates that SN 2017dys is a Type-Ia supernova. Using SNID (Blondin & Tonry, 2007, ApJ, 666, 1024), we find good match to several normal SNe Ia around maximum light at the redshift of the proposed host galaxy (z = 0.029264; NED).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Star and stellar system", "Supernova", "Pulsar" ] }, "answerKey": "C" }, { "id": "atel_10425", "message": "Title: INTEGRAL detection of continued hard X-ray emission from MAXI J0911-655\nAuthors: J.-G. Victor (ISDC, Switzerland), E. Kuulkers (ESA/ESTEC, Netherlands), L. Sidoli (INAF-IASF Milano, Italy), C. Sanchez-Fernandez (ESA/ESAC, Spain), K. Watanabe (FGCU, USA), L. Pavan, E. Bozzo (ISDC, Switzerland)\nDate: 25 May 2017; 17:21 UT\nProvenance: E. Bozzo (enrico.bozzo@unige.ch)\nSubjects: X-ray, Gamma Ray, Binary, Neutron Star, Transient\nDescription: Referred to by ATel #: 16358\nDuring the observations performed in the direction of the Carina Region and IGR J11014-6103 between 2017 May 8 at 04:50 and May 24 at 17:39, INTEGRAL detected activity from the accreting millisecond X-ray pulsar (AMXP) MAXI J0911-655 (Sanna et al., 2017, A&A, 598, 34; Atel #8872, #8884, #8914, #8971, #8986, #9738, #9740).\nThe source was detected in the IBIS/ISGRI mosaic accumulated over the entire period at 18 sigma in the 20-40 keV energy band and 9 sigma in the 40-80 keV energy band. The source high energy spectrum could be well described (reduced chi^2/d.o.f. = 1.3/8) by a power law of photon index 3.0(-0.7,+1.1) and the correspondingly measured 20-100 keV X-ray flux was 1.3e-10 ergs/cm^2/s. The source was outside the JEM-X field of view for the entire observational period. MAXI J0911-655 was discovered in outburst on 2016 February 19 and the monitoring carried out with Swift/XRT suggests that it did not go back to quiescence since then. The detection in the INTEGRAL data confirms that the source is still active after more than 450 days since the onset of the event, making MAXI J0911-655 the second AMXP after XTE J1807-294 displaying peculiarly long X-ray outbursts (not counting the case of the quasi-persistent HETE J1900.1-2455). Further INTEGRAL observations in the direction of the source are planned for the coming days. Observations at softer energies are strongly encouraged to understand the origin of the long-lasting outburst.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Accreting object", "Supernova", "Star and stellar system" ] }, "answerKey": "B" }, { "id": "atel_10560", "message": "Title: Renewed gamma-ray emission from the FSRQ CTA 102 detected by AGILE\nAuthors: A. Bulgarelli, N. Parmiggiani (INAF/IASF-Bo), F. Lucarelli, F. Verrecchia, C. Pittori (ASDC and INAF/OAR), G. Piano (INAF/IAPS), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), G. Minervini (INAF/IAPS), P. Munar-Adrover (INAF/IAPS), I. Donnarumma (INAF/IAPS), V. Fioretti (INAF/IASF-Bo), S. Vercellone (INAF/OA-Brera), E. Striani (CIFS and INAF/IAPS), M. Cardillo (INAF/OA-Arcetri and INAF/IAPS), F. Gianotti, M. Trifoglio (INAF/IASF-Bo), A. Giuliani, S. Mereghetti, P. Caraveo, F. Perotti (INAF/IASF-Mi), A. Chen (Wits University), A. Argan, E. Costa, E. Del Monte, Y. Evangelista, M. Feroci, F. Lazzarotto, I. Lapshov, L. Pacciani, P. Soffitta, S. Sabatini, V. Vittorini (INAF/IAPS), G. Pucella, M. Rapisarda (ENEA-Frascati), G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, M. Marisaldi (INAF/IASF-Bo), A. Pellizzoni, M. Pilia, A. Trois (INAF/OA-Cagliari), G. Barbiellini, E. Vallazza (INFN Trieste), F. Longo (Univ. Trieste and INFN Trieste), A. Morselli, P. Picozza (INFN and Univ. Roma Tor Vergata), M. Prest (Univ. dell'Insubria), P. Lipari, D. Zanello (INFN and Univ. Roma Sapienza), P. W. Cattaneo, A. Rappoldi (INFN Pavia), S. Colafrancesco (INAF/OAR and Wits University), A. Ferrari (Univ. Torino and CIFS), Paoletti (East Windsor RSD Hightstown and INAF/IAPS), A. Antonelli (ASDC and INAF/OAR), P. Giommi (ASDC), L. Salotti, G. Valentini, and F. D'Amico (ASI)\nDate: 7 Jul 2017; 12:22 UT\nProvenance: Andrea Bulgarelli (bulgarelli@iasfbo.inaf.it)\nSubjects: Gamma Ray, >GeV, AGN, Black Hole, Blazar\nDescription: Referred to by ATel #: 11045\nAGILE is detecting increased gamma-ray emission above 100 MeV from a source positionally consistent with the FSRQ blazar CTA 102 at Galactic coordinates (l,b) = (77.29, -38.22) +/- 0.75 deg (stat. 95% c.l.) +/- 0.1 deg (syst.), (RA, Dec) = (337.82, 11.93) (J2000). \nIntegrating from 2017-07-05 05:46:44 UT to 2017-07-07 05:46:44 UT a preliminary maximum likelihood analysis yields a detection with a significance of 6.5 sigma and flux F(E>100 MeV) = ( 3.7 +/- 0.9) x 10^-6 ph cm^-2 s^-1. \nRecent activity of CTA102 was reported in ATel #10386 by AGILE, in ATel #10330 by WEBT/GASP project and in ATel #10292 by Fermi (outside the AGILE visibility). \nThis measurement was obtained with AGILE observing a large portion of the sky in spinning mode.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Star and stellar system", "Black hole", "Repeater" ] }, "answerKey": "C" }, { "id": "atel_10675", "message": "Title: FRB 121102: Detection at 4 - 8 GHz band with Breakthrough Listen backend at Green Bank\nAuthors: Gajjar, Vishal (University of California, Berkeley, USA), Andrew P. V. Siemion (University of California, Berkeley, USA), David H. E. MacMahon (University of California, Berkeley, USA), Steve Croft (University of California, Berkeley, USA), Gregory Hellbourg (University of California, Berkeley, USA), Howard Isaacson (University of California, Berkeley, USA), J. Emilio Enriquez (University of California, Berkeley, USA), Danny C. Price (University of California, Berkeley, USA), Matthew Lebofsky (University of California, Berkeley, USA), David DeBoer (University of California, Berkeley, USA), Dan Werthimer (University of California, Berkeley, USA), Jack Hickish (University of California, Berkeley, USA), Casey Brinkman (University of Vermont, Burlington, USA), Shami Chatterjee (University of Cornell, Ithaca, USA), Scott Ransom (University of Virginia, Charlottesville, USA)\nDate: 29 Aug 2017; 03:11 UT\nProvenance: Steve Croft (scroft@astro.berkeley.edu)\nSubjects: Radio, Transient, Fast Radio Burst\nDescription: Referred to by ATel #: 10693, 11376\nOn Saturday, August 26 at 13:51:44 UTC we initiated observations of the well-known repeating fast radio burst FRB 121102 [Spitler et al., Nature, 531, 7593 202-205, 2016] using the Breakthrough Listen Digital Backend with the C-band receiver at the Green Bank Telescope. We recorded baseband voltage data across 5.4375 GHz of bandwidth, completely covering the C-band receiver's nominal 4-8 GHz band [MacMahon et al. arXiv:1707.06024v2]. Observations were conducted over ten 30-minute scans, as detailed in Table 1. Immediately after observations, the baseband data were reduced to form high time resolution (300 us integration) Stokes-I products using a GPU-accelerated spectroscopy suite. These reduced products were searched for dispersed pulses consistent with the known dispersion measure of FRB 121102 (557 pc cm^-3); baseband voltage data were preserved. We detected 15 bursts above our detection threshold of 10 sigma in the first two 30-minute scans, denoted 11A-L and 12A-B in Table 2. In Table 2, we include the detection signal-to-noise ratio (SNR) of each burst, along with a very rough estimate of pulse energy density assuming a 12 Jy system equivalent flux density, 300 us pulse width, and uniform 3800 MHz bandwidth. We note the following phenomenological properties of the detected bursts: 1\\. Bursts show marked changes in spectral extent, with characteristic spectral structure in the 100 MHz - 1 GHz range. 2\\. Several bursts appear to peak in brightness at frequencies above 6 GHz. \n \n \n Table 1: \n \n Scan No. | MJD | Duration (min) | No. Bursts detected \n ----------------------------------------------------------------------- \n 11 | 57991.5776 | 30 | 12 \n 12 | 57991.5986 | 30 | 3 \n 13 | 57991.6196 | 30 | 0 \n 14 | 57991.6406 | 30 | 0 \n 15 | 57991.6616 | 30 | 0 \n 16 | 57991.6825 | 30 | 0 \n 17 | 57991.7035 | 30 | 0 \n 18 | 57991.7245 | 30 | 0 \n 19 | 57991.7454 | 30 | 0 \n 20 | 57991.7664 | 20 | 0 \n \n \n \n \n Table 2: \n \n \n Burst | SNR* | Energy Density | Time* | Sample \n | | (Jy us) | (s) | \n ------------------------------------------------------------- \n 11G | 60.6 | 144.5 | 597.612 | 1709782 \n 11A | 47.9 | 114.2 | 16.2505 | 46493 \n 11C | 47.2 | 112.5 | 323.352 | 925118 \n 11D | 25.6 | 61.0 | 344.768 | 986388 \n 11E | 24.6 | 58.7 | 356.033 | 1018619 \n 11F | 21.2 | 50.5 | 356.034 | 1018620 \n 11L | 20.8 | 49.6 | 1454.55 | 4161497 \n 12B | 20.7 | 49.4 | 743.071 | 2125942 \n 12A | 13.6 | 32.4 | 104.922 | 300184 \n 11J | 12.3 | 29.3 | 1036.42 | 2965234 \n 11I | 11.6 | 27.7 | 769.864 | 2202599 \n 11K | 11.1 | 26.5 | 1142.41 | 3268458 \n 12C | 10.8 | 25.7 | 1526.39 | 4367026 \n 11H | 10.6 | 25.3 | 691.83 | 1979341 \n 11B | 10.4 | 24.8 | 285.436 | 816640 \n \n * seconds from tstart = MJD 57991.5776 \n \n \nThese are the highest frequency and widest bandwidth detections of bursts from FRB 121102 obtained to-date. Additional fully calibrated full-Stokes analysis employing coherent dedispersion on raw voltage data is ongoing. These observations may indicate FRB 121102 is currently in a heightened activity state [Law et al. arXiv:1705.07553], and follow-on observations are encouraged, particularly at higher radio frequencies. \nPlots are available here", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Interstellar medium", "Black hole", "Circumstellar disk" ] }, "answerKey": "B" }, { "id": "atel_10770", "message": "Title: Large glitch event observed in PSR J1731-4744\nAuthors: Fabian Jankowski (Swinburne University of Technology [SUT]), Matthew Bailes (SUT), Ewan D. Barr (Max-Planck-Institut fur Radioastronomie), Timothy Bateman (The University of Sydney [USyd]), Shivani Bhandari (SUT), Manisha Caleb (University of Manchester), Adam Deller (SUT), Duncan Campbell-Wilson (USyd), Wael Farah (SUT), Chris Flynn (SUT), Anne J. Green (USyd), Richard W. Hunstead (USyd), Andrew Jameson (SUT), Evan F. Keane (SKA Organisation), Vivek Venkatraman Krishnan (SUT), Kathryn Plant (Caltech), Morgan O'Neill (SUT), Stefan Oslowski (SUT), Aditya Parthasarathy (SUT), Vikram Ravi (Caltech), Dave Temby (USyd)\nDate: 24 Sep 2017; 08:10 UT\nProvenance: Fabian Jankowski (fjankowski@swin.edu.au)\nSubjects: Radio, Neutron Star, Transient, Pulsar\nDescription: We detected a large glitch event in the timing data of the pulsar J1731-4744, which we monitor routinely as part of the pulsar timing programme at the Molonglo Observatory Synthesis Radio Telescope (UTMOST project). The UTMOST project is described by Bailes et al. 2017 (arXiv ID 1708.09619). \nOur preliminary analysis indicates a fractional glitch size of dF0/F0 = (3147.7 +/- 0.1) E-9 (3 sigma), which makes it the largest glitch reported in this pulsar so far by a large margin, based on the ATNF glitch table and Jodrell Bank glitch database. There is no indication of a significant change in spin-down rate yet. The glitch epoch is only poorly constrained, as it happened in an observing gap. Our best estimate of the glitch epoch is MJD 57984.26 -18.3 +20.9 (UTC 2017-08-19), obtained when placing it near the centre of the gap and assuming zero glitch phase change. Note that the glitch could have happened as recently as UTC 2017-09-09 07:00. \nFollow-up observations of this pulsar are encouraged to help refine the glitch characteristics.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Interstellar medium", "Magnetar", "Exoplanet" ] }, "answerKey": "A" }, { "id": "atel_10860", "message": "Title: VLT/FORS2 spectroscopic classification of nuclear transient OGLE17hil as normal Supernova Type Ia\nAuthors: N. Ihanec (University of Nova Gorica), M. Gromadzki, L. Wyrzykowski, P. Iwanek, A. Udalski (Warsaw University Astronomical Observatory)\nDate: 17 Oct 2017; 13:06 UT\nProvenance: Lukasz Wyrzykowski (wyrzykow@astrouw.edu.pl)\nSubjects: Optical, Supernovae, Transient\nDescription: We report on the spectroscopic classification of a nuclear transient discovered by the OGLE-IV Transient Search System on 2017-10-13 (http://ogle.astrouw.edu.pl/ogle4/transients/ Wyrzykowski et al. 2014, Acta Astronomica 64, 197). The spectrum was obtained on 2017-10-14, using the FOcal Reducer/low dispersion Spectrograph 2 (FORS2) on the Very Large Telescope (VLT). The spectroscopic classification was done using SNID code (Blondin & Tonry 2007, ApJ, 666, 1024) and it was matched to SN Type Ia-norm at about 7 days past maximum. We estimated redshift z=0.0612 base on host lines: H-alpha, [N II] SII, [O II] and [O III] in emission and Hdelta, Na and CaII H&K in absorption. OGLE photometric measurements do not constrain the maximum date, however at the moment of detection the observed magnitude at this redshift corresponds to the absolute magnitude of approximately -18.7 mag which is consistent with SN Type Ia. \nWe note that the archival OGLE-IV photometry of this host galaxy reveals there was another (previously undetected) supernova near its nucleus in October 2011. Its light curve resembles that of SN Ia, with the secondary bump visible in the I-band. \nName | IAU name | RA (J2000) | Dec (J2000) | Disc. Date | Disc. Mag | Obs. Date | z | Host | Type | Notes \nOGLE17hil | 2017hil | 05:57:30.04 | -62:28:44.60 | 2017-10-13 | 18.56 | 2017-10-13 | 0.0612 | OGLE-GAL-LMC605.05-897.374-1129.222 | SN Ia-norm | +7 days \n\nThe classification spectrum will be available on the IAU's Transient Name Server (TNS). The observations were carried under ToO programme 0100.B-0503(A), PI: M. Gromadzki. We thank ESO/VLT staff for their support.\nFinding chart and light curve is available here", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Exoplanet", "Supernova", "Quasar" ] }, "answerKey": "C" }, { "id": "atel_10980", "message": "Title: Spectroscopic Classification of SN 2017hqf (=PTSS-17ygv) as a Type Ia Supernova\nAuthors: Han Lin, Xiaofeng Wang, Danfeng Xiang, Wenxiong LI, Liming Rui (Tsinghua University), Hong Wu, Peng Qiu (NAOC), Zhijian Xu, Bin Li, Haibin Zhao, Lifan Wang (PMO), Jujia Zhang (YNAO), and Tianmeng Zhang (NAOC)\nDate: 17 Nov 2017; 14:09 UT\nProvenance: Xiaofeng Wang (wang_xf@mail.tsinghua.edu.cn)\nSubjects: Optical, Supernovae, Transient\nDescription: We obtained an optical spectrum (range 360-840 nm) of SN 2017hqf(PTSS-17ygv), discovered by the PMO-Tsinghua Supernova Survey (PTSS, http://www.cneost.org/ptss/ ), on UT 2017 Nov. 16.85 with the Xinglong 2.16 m telescope (BFOSC) at Xinglong Observatory of NAOC. The spectrum is consistent with that of a type Ia supernova at about two weeks after the maximum light. Cross-correlation with a library of supernova spectra using the \"Supernova Identification\" code (SNID; Blondin and Tonry 2007, ApJ, 666, 1024) shows that it matches with SN 1995D at t = +14 days from the maximum light. After correcting for a redshift of 0.047 (from SNID fit) an expansion velocity of about 9800 km/s can be derived from the absorption minimum of Si II 635.5 nm.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Pulsar", "Globular cluster", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_11040", "message": "Title: OAUNI photometry of SN2017glq/Gaia17cfi\nAuthors: A. Pereyra (Geophysical Institute of Peru - IGP, Astronomy Area), J. Ricra (National University of Engineering - UNI, Astronomy Group, Peru)\nDate: 8 Dec 2017; 00:17 UT\nProvenance: Antonio Pereyra (apereyra@igp.gob.pe)\nSubjects: Optical, Supernovae, Transient\nDescription: We report optical photometry of Type Ia SN2017glq/Gaia17cfi (TNSDR 2017-13365, TNSCR 2017-1194) on 2017-09-19.182 (UT) gathered with the OAUNI 51cm telescope at Huancayo Observatory, Peru. CCD imaging was performed using R band with seeing ~1.6\" and airmass = 1.5. A total integration time of 59x20s=1180s yielded R = (14.16 +/- 0.05) mag. NOMAD field stars were used for the zero point calibration. Following OSC (Guillochon et al. 2016, arXiv:1605.01054) light curve, our measurements are very close to the maximum. The OAUNI project is supported by UNI, TWAS, IGP and Cienciactiva (Convenio 102-2015 Fondecyt).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Galaxy", "Supernova", "Magnetar" ] }, "answerKey": "C" }, { "id": "atel_11125", "message": "Title: Recurrent Nova M31N 2008-12a: Early multi-color photometric observations of the 2017 eruption with SARA-ORM\nAuthors: Amanpreet Kaur, Dieter H. Hartmann (Clemson University), Martin Henze, Allen Shafter (SDSU), Matt Darnley (LJMU)\nDate: 4 Jan 2018; 17:20 UT\nProvenance: Amanpreet Kaur (akaur@g.clemson.edu)\nSubjects: Optical, Cataclysmic Variable, Nova\nDescription: Referred to by ATel #: 11130, 11133, 11134, 11144, 11149, 11214\nWe report optical photometric observations of the 2017 eruption (see ATels #11116, #11117, #11118, #11121) of the recurrent nova M31N 2008-12a (Henze et al. 2014, 2015a, 2015b; Darnley et al. 2014, 2015, 2016). The data were obtained using the BESSEL B, V, R, I filters between 2018 Jan 01.01 UT - 2018 Jan 02.00 UT with the 1.0 m Jacobus Kapteyn Telescope telescope (SARA-ORM) equipped with ARC CCD camera(Keel et al. 2017), located at Roque de los Muchachos, La Palma, Spain. The derived magnitudes were calibrated with the standard stars in the field of this nova. The total exposure time for each reported magnitude was 5 minutes. \nOptical Observations 2018 UT | Mag | Filter Optical Observations | UT | Mag | Filter | Jan 01.839 | 19.34± 0.12 | B | Jan 01.852 | 19.34± 0.12 | B | Jan 01.859 | 20.35± 0.29 | B | Jan 01.871 | 18.81± 0.08 | B | Jan 01.885 | 19.24± 0.10 | B | Jan 01.900 | 19.48± 0.15 | B | Jan 01.915 | 21.82± 1.32 | B | Jan 01.922 | 18.61± 0.06 | R | Jan 01.929 | 21.18± 0.74 | B | Jan 01.836 | 19.12± 0.12 | V | Jan 01.868 | 18.99± 0.09 | V | Jan 01.882 | 19.01± 0.09 | V | Jan 01.897 | 18.71± 0.07 | V | Jan 01.911 | 18.74± 0.06 | V | Jan 01.926 | 20.22± 0.28 | V | Jan 01.940 | 19.28± 0.12 | V | Jan 01.828 | 18.82± 0.10 | R | Jan 01.832 | 20.97± 0.52 | R | Jan 01.864 | 18.51± 0.05 | R | Jan 01.878 | 18.61± 0.07 | R | Jan 01.893 | 18.42± 0.05 | R | Jan 01.908 | 18.51± 0.05 | R | Jan 01.937 | 18.80± 0.07 | R | Jan 01.933 | 19.12± 0.21 | I | Jan 01.947 | 18.63± 0.13 | I | Jan 01.843 | 19.07± 0.23 | I | Jan 01.875 | 18.21± 0.10 | I | Jan 01.889 | 19.23± 0.26 | I | Jan 01.904 | 19.06± 0.22 | I | Jan 01.919 | 18.22± 0.08 | I", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Exoplanet", "Nova", "Variable star", "Neutron star" ] }, "answerKey": "B" }, { "id": "atel_11200", "message": "Title: AGILE observations of intense gamma-ray emission from the blazar 3C 279\nAuthors: F. Lucarelli (SSDC and INAF/OAR), A. Bulgarelli (INAF/IASF-Bo), F. Verrecchia, C. Pittori (SSDC and INAF/OAR), N. Parmiggiani (INAF/IASF-Bo), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, G. Piano, A. Ursi (INAF/IAPS), S. Vercellone (INAF/OA-Brera), M. Pilia (INAF/OA-Cagliari), I. Donnarumma (ASI), V. Fioretti, F. Gianotti, M. Trifoglio (INAF/IASF-Bo), A. Giuliani, S. Mereghetti, P. Caraveo, F. Perotti (INAF/IASF-Mi), A. Chen (Wits University), A. Argan, E. Costa, E. Del Monte, Y. Evangelista, M. Feroci, F. Lazzarotto, I. Lapshov, L. Pacciani, P. Soffitta, S. Sabatini, V. Vittorini (INAF/IAPS), G. Pucella, M. Rapisarda (ENEA-Frascati), G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, M. Marisaldi (INAF/IASF-Bo), A. Pellizzoni, A. Trois (INAF/OA-Cagliari), G. Barbiellini, E. Vallazza (INFN Trieste), F. Longo (Univ. Trieste and INFN Trieste), S. Colafrancesco (INAF/OAR and Wits University), A. Morselli, P. Picozza (INFN and Univ. Roma Tor Vergata), M. Prest (Univ. dell'Insubria), P. Lipari, D. Zanello (INFN and Univ. Roma Sapienza), P. W. Cattaneo, A. Rappoldi (INFN Pavia), A. Ferrari (Univ. Torino and CIFS), F. Paoletti (East Windsor RSD Hightstown and INAF/IAPS), A. Antonelli (SSDC), P. Giommi, L. Salotti, G. Valentini, and F. D'Amico (ASI)\nDate: 19 Jan 2018; 14:45 UT\nProvenance: Fabrizio Lucarelli (fabrizio.lucarelli@asdc.asi.it)\nSubjects: Gamma Ray, >GeV, Blazar, Transient\nDescription: Referred to by ATel #: 11216, 11239, 11246, 11464\nAGILE is detecting an intense gamma-ray emission above 100 MeV from a source consistent with the Flat Spectrum Radio Quasar 3C 279 (RA: 194.046527 deg, Dec: -5.789312 deg, J2000) at z=0.536. \nIntegrating from 2018-01-18 03:50 UT to 2018-01-19 03:50 UT, a maximum likelihood analysis yields a detection at a significance level above 12 sigma, and a flux F = (1.8 +/- 0.3) x 10^-5 ph/cm^2/s (E > 100 MeV). For a 12-hour integration, starting from 2018-01-18 00:00 UT, a preliminary maximum likelihood analysis yields a flux F = (2.2 +/- 0.5) x 10^-5 ph/cm^2/s (E > 100 MeV). \nThis is the highest flux above 100 MeV measured by AGILE since June 2015 (ATel #7631, #7633, Pittori et al. 2018 (submitted to ApJ)), and higher with respect to the recent detections reported by Fermi-LAT in ATel #11189 and by AGILE in ATel #11115. The source is also reported to be in optical high-state (ATel #11190, #11196). \nThe AGILE-GRID detection was obtained while AGILE is observing in spinning mode, surveying a large fraction of the sky each day. The source can be monitored with the public mobile application \"AGILEScience\" developed by the AGILE Team, available for both Android and iOS devices. \nMultifrequency observations of 3C 279 are strongly encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Pulsar", "Minor body", "Accreting object" ] }, "answerKey": "A" }, { "id": "atel_11300", "message": "Title: ASAS-SN Discovery of a Possible Galactic Nova ASASSN-18cs\nAuthors: K. Z. Stanek, C. S. Kochanek, J. V. Shields, T. A. Thompson (OSU), T. W.-S. Holoien, B. J. Shappee (Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), Subo Dong (KIAA-PKU)\nDate: 14 Feb 2018; 17:55 UT\nProvenance: Krzysztof Stanek (stanek.32@osu.edu)\nSubjects: Optical, Nova\nDescription: During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014), using data from the quadruple 14-cm \"Cassius\" telescope in CTIO, Chile, we detect a new transient source, possibly a classical nova (could also be a bright CV), near the Galactic plane\n \n \n Object RA (J2000) DEC (J2000) Gal l (deg) Gal b (deg) Disc. UT Date Disc. V mag \n ASASSN-18cs 17:34:08.84 -43:05:50.5 346.74 -5.544 2018-02-13.37 13.7 \n \nASASSN-18cs was discovered in images obtained on UT 2018-02-13.37 at V~13.7, and it is also detected in g-band data from the \"Paczynski\" telescope at UT 2018-02-14.38 at g~13.7. There was a ~120-day seasonal gap before these observations, so the nova candidate could have peaked already. We do not detect (V>17.4) this object in subtracted images taken on UT 2017-10-17.03 and before. \nWe have retrieved V-band image subtraction photometry time series at the location of ASASSN-18cs. No previous outbursts or variability are detected at the position of ASASSN-18cs since ASAS-SN started observing this location in March 2016.\nFollow-up observations, especially spectroscopy, are strongly encouraged. \nWe would like to thank Las Cumbres Observatory and its staff for their continued support of ASAS-SN. ASAS-SN is funded in part by the Gordon and Betty Moore Foundation through grant GBMF5490 to the Ohio State University, NSF grant AST-1515927, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, the Chinese Academy of Sciences South America Center for Astronomy (CASSACA), and the Villum Fonden (Denmark).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Pulsar", "Nova", "Supernova" ] }, "answerKey": "C" }, { "id": "atel_11370", "message": "Title: Spectroscopic Classification of SN 2018yo (= SNhunt353) as a Type IIP Supernova\nAuthors: Jujia Zhang (YNAO) and Xiaofeng Wang (THU)\nDate: 28 Feb 2018; 21:01 UT\nProvenance: Ju-Jia Zhang (jujia@ynao.ac.cn)\nSubjects: Optical, Supernovae\nDescription: We obtained optical spectra (range 360-870 nm) of SN 2018yo (= SNhunt353), discovered by the Catalina Real-Time Transient Survey Transient Survey and Nikolay Mishevskiy, on UT Feb.28.83 2018 with the 2.4m telescope (+YFOSC) at Lijiang Observatory of YNAO. The spectrum is consistent with that of a type IIP supernova at a few weeks after the maximum light. Cross-correlation with a library of supernova spectra using the \"Supernova Identification\" code (SNID; Blondin and Tonry 2007, Ap.J., 666, 1024) shows that it matches with SN 2006bp at t = +25 days from the maximum light. After correcting for a redshift of 0.0134 for its host galaxy UGC 7840, an expansion velocity of about 10000 km/s can be derived from the absorption minimum of Ha line.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Globular cluster", "Supernova", "Galaxy", "Pulsar" ] }, "answerKey": "B" }, { "id": "atel_11460", "message": "Title: Spectroscopic Observations of ASASSN-18fv as a Classical Nova in the Iron Curtain Phase \nAuthors: Paul Luckas (International Centre for Radio Astronomy Research, University of Western Australia)\nDate: 21 Mar 2018; 17:35 UT\nProvenance: S. N. Shore (shore@df.unipi.it)\nSubjects: Nova\nDescription: Referred to by ATel #: 11468, 11504, 11506, 11546, 11553, 11677\nObservations of ASASSN-18fv (ATel# 11454) were obtained on 2018 Mar. 21.49 (MJD 58199.0), with an Alpy600 spectrograph having a resolution of about 540 in the range 3800-7300A using a Atik414 CCD and a total exposure time 5x120 sec. The spectrum confirms that this source is a classical nova on the rise in the optically thick (Fe curtain) phase, The Fe II 5018, 5169 lines, for instance, show absorption troughs (about as strong as the emission) extending to about -800 km/s, about the same as the zero intensity width of the redshifted emission wing. The Balmer lines (H-alpha to H-gamma) show absorption with similar maximum velocities and strongly decreasing emission-to-absorption ratio with increasing line number, similar profiles and kinematics are found on Si II 6347,6371 and other metallic ion lines. Ca II H and K are mainly in absorption, as are the Na I D lines, but the absorption is displaced by about But in both cases the profiles are broad and poorly resolved, although the Na I D is centered at about vrad=0 km/s while Ca II K has a vrad ~ -400 km/s deepest absorption and a similar maximum absorption velocity, suggesting the Na I line is dominated by interstellar absorption. Neither O I nor He I are seen in this spectrum. The optical depth is quite large now and, with these absorption velocities, it would be of interest to obtain high resolution time sequences to study the appearance of multiple absorption systems and track the changes in ejecta transparency. \nARAS Nova Spectroscopic Database", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Globular cluster", "Neutron star", "Nova", "Accreting object" ] }, "answerKey": "C" }, { "id": "atel_11525", "message": "Title: Spectroscopic classification of SN 2018aql as a young type IIP supernova\nAuthors: Jujia Zhang, Yuxin Xin (YNAO); Zhijian Xu; Zhitong Li, Wenxiong Li, Xiaofeng Wang (THU) and Tianmeng Zhang (NAOC)\nDate: 11 Apr 2018; 01:35 UT\nProvenance: Ju-Jia Zhang (jujia@ynao.ac.cn)\nSubjects: Optical, Supernovae\nDescription: We obtained an optical spectrum (range 350-900 nm) of SN 2018aql, discovered by the Tsinghua-NAOC Transient Survey (TNTS), on UT Apr. 09.85 2018 with the 2.4-m telescope (+YFOSC) at LiJiang Observatory of Yunnan Observatories (YNAO). The spectrum is consistent with a type IIP supernova at a few days before the maximum light, showing a blue continuum and prominent P-Cygni features of Balmer lines. Cross-correlation with a library of supernova spectra using the \"Supernova Identification\" code (SNID; Blondin and Tonry 2007, Ap.J., 666, 1024) shows that it matches with SN 1999em at t = -4 days from the maximum light. After correcting for a redshift of 0.074 for its host galaxy (via SNID), an expansion velocity of about 12,000 km/s can be derived from the absorption minimum of Ha line. The classification spectrum is also posted on the IAU Transient Name Sever: https://wis-tns.weizmann.ac.il/object/2018aql", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Supernova", "Interstellar medium", "Black hole" ] }, "answerKey": "B" }, { "id": "atel_11625", "message": "Title: A glitch in the Crab pulsar (PSR B0531+21)\nAuthors: Benjamin Shaw (University of Manchester), Andrew Lyne (University of Manchester), Cees Bassa (ASTRON), Rene Breton (University of Manchester), Christine Jordan (University of Manchester), Michael Keith (University of Manchester), Mitchell B. Mickaliger (University of Manchester), Benjamin Stappers (University of Manchester), Patrick Weltevrede (University of Manchester)\nDate: 9 May 2018; 13:08 UT\nProvenance: Mitchell Mickaliger (mitchell.mickaliger@manchester.ac.uk)\nSubjects: Radio, Neutron Star, Pulsar\nDescription: We have detected a glitch in the Crab pulsar, B0531+21, on 2018-04-29. The Crab pulsar is regularly monitored with the 42-ft and Lovell telescopes at the Jodrell Bank Observatory as part of the pulsar timing programme. Initial analysis shows a fractional rotational spin-up of dF0/F0 = (4.08+/-0.22)E-9 and a fractional change in spin-down rate dF1/F1 = (0.46+/-0.11)E-3 (1 sigma errors). This glitch occurred 176 days after the previous glitch, which we measured to be the largest glitch ever observed in the Crab pulsar (ATEL #10939). At the time of the most recent glitch, the Crab pulsar was still in the recovery phase from the previous glitch. While the Crab pulsar is observed twice per day for a total of 11 hours, this glitch occurred between two of our observations. We currently constrain the glitch epoch to be MJD 58237.357+/-0.005. We are continuing to monitor this source, but follow-up observations are encouraged in order to help refine the glitch characteristics and also to identify any radiative effects seen at other wavelengths.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Globular cluster", "Stellar evolution", "Interstellar medium", "Neutron star" ] }, "answerKey": "D" }, { "id": "atel_11725", "message": "Title: SAO RAS Observations of current brightening of [HB89] 0716+714 blazar\nAuthors: O. I. Spiridonova, V. V. Vlasyuk, A. S. Moskvitin (SAO RAS) \nDate: 16 Jun 2018; 21:56 UT\nProvenance: Alexander Moskvitin (mosk@sao.ru)\nSubjects: Optical, Blazar\nDescription: Referred to by ATel #: 12298\nAs it was noted by some observers, the blazar [HB89] 0716+714 is undergoing new brightening phase since end of 2017 (see ATel #11107,#11339,#11676) after report of MAGIC collaboration about its strong activity in VHE (E>100 GeV) gamma rays. We performed a multicolor broad-band photometry of the selected blazars, using by the 1-meter reflector Zeiss-1000 of the Special Astrophysical Observatory of RAS (Northern Caucasus, Russia), equipped with UBVRI filters and CCD camera based on 2k x 2k EEV 42-40 chip. Our last measurements showed that blazar brightness became in some last days even higher than it was reported (ATel #11676). The results of our observations in R-band are summarized in the following table: \nCivil Date | MJD | Rmag +/- dRmag \n---|---|--- \n2018.05.15 | 58254.30 | 12.42 +/- 0.01 \n2018.06.13 | 58283.34 | 12.01 +/- 0.02 \n2018.06.14 | 58284.31 | 12.00 +/- 0.02 \n2018.06.15 | 58285.41 | 12.07 +/- 0.04 \n2018.06.16 | 58286.39 | 11.98 +/- 0.02 \nSo current brightness of the blazar [HB89] 0716+714 within last 4 days is near it's absolute maximum value in this century as it was detected by us in January of 2015 (ATel #6953). We shall continue studies the source in the following nights. Also multi-wavelength follow-up is warmly encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system", "Active galactic nucleus", "Interstellar medium", "Quasar" ] }, "answerKey": "B" }, { "id": "atel_11790", "message": "Title: UV Spectroscopy of the Superluminous Supernova SN2018bsz\nAuthors: P. Blanchard, M. Nicholl (Harvard/CfA), R. Chornock (Ohio University), E. Berger (Harvard/CfA), R. Margutti, G. Terreran, D. Coppejans, K. D. Alexander (Northwestern University), D. Milisavljevic (Purdue University)\nDate: 27 Jun 2018; 23:37 UT\nProvenance: Peter Blanchard (pblanchard@cfa.harvard.edu)\nSubjects: Ultra-Violet, Supernovae\nDescription: We obtained 3 orbits of Hubble Space Telescope observations of the Type I superluminous supernova (SLSN-I) SN2018bsz, the lowest-redshift SLSN-I at z=0.027 (ATels #11659, #11660, #11674; Hiramatsu et al. 2018), on 25 June 2018 UT. The observations consist of 2 orbits of spectroscopy with COS/FUV + G140L and 1 orbit with STIS/NUV-MAMA + G230L (PID: 15488; PI: Blanchard). The resulting UV spectrum covers a rest-frame wavelength range of ~1100 - 3100 angstroms and was obtained at a rest-frame phase of approximately 1 month after peak brightness. \nAfter correcting for Galactic extinction (E(B-V) = 0.207; Schlafly & Finkbeiner 2011) and comparing the spectrum with the near-peak UV spectra of the SLSNe-I Gaia16apd (Yan et al. 2017), SN2017egm (Yan et al. 2018), and iPTF13ajg (Vreeswijk et al. 2014), we find that SN2018bsz is overall similar in spectral shape and shows most of the same strong UV features, namely broad absorptions centered near 2650, 2200, 1750, and 1425 angstroms. However, SN2018bsz does not show obvious distinct absorption features near 2450 and 1950 angstroms (the UV2 and UV4 features in the terminology of Quimby et al. 2018). The UV2 feature has been attributed to Si III or a blend of Si III + Ti III + C II (Quimby et al. 2011; Mazzali et al. 2016) and the UV4 feature has been attributed to Fe III (Howell et al. 2013; Mazzali et al. 2016). In the spectra of Gaia16apd and other SLSNe-I, the UV2 feature appears to weaken with time (Yan et al. 2017; Quimby et al. 2018), and so its absence in SN2018bsz may be attributable to the later phase of the observations. In addition, the features that are present in SN2018bsz appear to be somewhat broader than the other SLSNe-I with UV spectra, which may be causing increased line blending. \nThe far-UV spectrum from COS shows a similar overall shape to Gaia16apd and SN2017egm, but line features appear relatively weak, which may again be due to increased line blending or the later phase of observations. \nFinally, we note that the spectral differences between SN2018bsz and the comparison objects may in part be related to having an unusual abundance pattern, as evidenced by the optical spectra (ATel #11674). \nWe thank STScI for making these observations possible.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Exoplanet", "Supernova", "Circumstellar disk", "Near-Earth object" ] }, "answerKey": "B" }, { "id": "atel_11880", "message": "Title: MASTER follow up inspection of the FRB 180714 error box.\nAuthors: P. Balanutsa, V. Lipunov, V. Kornilov, E. Gorbovskoy, N. Tiurina, O. Gress, A. Gabovich, I. Gorbunov, V. Senik, V. Vladimirov, D. Vlasenko, D. Kuvshinov (Lomonosov MSU)\nDate: 22 Jul 2018; 09:49 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Radio, Optical, Fast Radio Burst\nDescription: Referred to by ATel #: 11902\nMASTER-Kislovodsk robotic telescope (MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) was pointed to the FRB180714 (Oslowski et al., ATel #11851) 35553 sec after notice time and 6 days 31953 sec after trigger time at 2018-07-20 19:01:16 UT. On our second (180s exposure) set we not found optical transient within MASTER error-box (ra=266.55 dec=-11.7631 r=0.3) brighter then 17.0. \nThe observations made on zenit distance = 56 degrees, galaxy latitude b = 8 degree. The Moon (60 % bright part) is 21 degrees above the horizon. The distance between Moon and object is 47 The sun altitude is -19.1 degree. The object can be observed till 2018-07-21 00:17:55 \nMASTER-SAAO robotic telescope (MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) was pointed to the FRB 180714.42 39278 sec after notice time and 6 days 35678 sec after trigger time at 2018-07-20 20:03:21 UT. On our first (180s exposure) set we not found optical transient within FRB error-box (ra=266.55 dec=-11.7631 r=0.3) brighter then 19.1. \nThe observations made on zenit distance = 21 degrees, galaxy latitude b = 8 degree. The Moon (61 % bright part) is 46 degrees above the horizon. The distance between Moon and object is 47 The sun altitude is -52.8 degree. The object can be observed till 2018-07-21 03:00:43. \nMASTER-IAC robotic telescope (MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Spain (IAC Teide Observatory) was pointed to the FRB180714.42 46969 sec after notice time and 6 days 43369 sec after trigger time at 2018-07-20 22:11:32 UT. On our first (180s exposure) set we not found optical transient within Master error-box (ra=266.55 dec=-11.7631 r=0.3) brighter then 17.7. \nThe observations made on zenit distance = 42 degrees, galaxy latitude b = 8 degree. The Moon (61 % bright part) is 39 degrees above the horizon. The distance between Moon and object is 45 The sun altitude is -24.6 degree. The object can be observed till 2018-07-21 04:33:33. \nList of Optical Transients discovered by MASTER\nGlobal MASTER Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Variable star", "Neutron star, Black hole", "Near-Earth object, Black hole", "Neutron star, Nova" ] }, "answerKey": "B" }, { "id": "atel_11970", "message": "Title: Detection of the NIR counterpart of the accreting millisecond pulsar IGR J17591-2342\nAuthors: A. W. Shaw (University of Alberta), N. Degenaar (Univeristy of Amsterdam), C. O. Heinke (University of Alberta)\nDate: 19 Aug 2018; 19:14 UT\nProvenance: Aarran Shaw (aarran@ualberta.ca)\nSubjects: Infra-Red, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 12004\nWe report on near-infrared (NIR) follow-up of the new accreting millisecond X-ray pulsar IGR J17591-2342, discovered by INTEGRAL and localized by Swift and ATCA (ATel #11941, #11942, #11954). \nWe obtained imaging in the Ks and H bands, using the High Acuity Wide-field K-Band Imager (HAWK-I) mounted on UT4 of the Very Large Telescope on Cerro Paranal, Chile. Conditions were excellent, with seeing <1\". We obtained 7 exposures of 195s in Ks, with each co-added exposure consisting of 13 dithered 15s exposures. In H we obtained 7 exposures of 65s, with each co-add consisting of 13 dithered 5s exposures. Data were reduced with ESO's reflex pipeline and we extract photometry from the pipeline products.\nWe detect a source at RA (J2000) =17:59:02.87, Dec (J2000) = -23:43:08.2, with magnitudes of H=19.56 +/- 0.07 and Ks=18.37 +/- 0.07. The source position is completely consistent with the ATCA position reported by Russell et. al. (ATel #11954) and the typical astrometric uncertainty in the HAWK-I images is ~0.03\". We therefore propose that this is the NIR counterpart of the pulsar.\nThough the counterpart is faint, follow-up observations are encouraged, particularly NIR spectroscopy.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova, Pulsar", "Neutron star, Pulsar", "Repeater, Pulsar", "Neutron star, Repeater" ] }, "answerKey": "B" }, { "id": "atel_12050", "message": "Title: IGR J17591-2342 second re-brightening observed with NICER\nAuthors: P. S. Ray (U. S. Naval Research Laboratory), K. C. Gendreau, P. M. Bult, Z. Arzoumanian, T. E. Strohmayer (NASA/GSFC), G. K. Jaisawal (DTU Space, Denmark), D. Chakrabarty (MIT), D. Altamirano (University of Southampton, UK), S. Guillot (IRAP-CNRS, France), C. Ferrigno, E. Bozzo (ISDC, University of Geneva, Switzerland), A. Sanna, L. Burderi (University of Cagliari, Italy), A. Papitto (Observatory of Rome, Italy), and T. Di Salvo (University of Palermo, Italy) \nDate: 19 Sep 2018; 20:37 UT\nProvenance: Paul S. Ray (paul.ray@nrl.navy.mil)\nSubjects: X-ray, Request for Observations, Neutron Star, Transient\nDescription: Following the reports (ATel #11957, Sanna et al. 2018, arXiv:1808.10195) that IGR J17591-2342 is an accreting millisecond pulsar in outburst, NICER has continued to monitor this source. \nAfter the initial outburst, multiple instruments observed a re-brightening that began on 2018 August 18 (MJD 58348; as reported in ATel #12004). During that re-brightening, NICER observed the count rate to increase to about 3.8 mcrab (1-10 keV) around MJD 58362, then decline more quickly to about 2.3 mcrab by MJD 58367. Since then, the source has again re-brightened to its highest flux yet, climbing to 5.4 mcrab as of MJD 58376.8 (see Figure at link below for a 60-s binned light curve of the NICER data on this source). The background contribution in this energy band is about 0.5 c/s. Note that in the 1-10 keV energy band, 1 mcrab corresponds to approximately 8 c/s in NICER. \nThe pulsations remain strongly present after almost 60 days of outburst, with a fractional RMS amplitude of approximately 7% (1-10 keV), in the most recent data, so they have not disappeared as observed in some long outburst AMXP systems, such as SAX J1748.9-2021 (Altamirano et al. 2008, ApJL 674, 45) and HETE J1900.1-2455 (Galloway et al. 2007, ApJL 654, 73). The 1.2-10 keV energy spectrum can be described by an absorbed power-law model with a soft blackbody component. No evidence of a spectral state change has been seen. We found a photon index varying between 0.9-2.1, positively correlated with flux, across the NICER observations. At the same time, blackbody temperatures ranging between 0.7-1 keV are seen. The column density is 2-3E22 cm^-2, consistent with the values reported in Sanna et al. (2018, arXiv:1808.10195). \nContinued multiwavelength observations of this ongoing transient are encouraged. NICER is a 0.2-12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA.\nNICER 60-s binned light curve", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Active galactic nucleus", "Neutron star", "Accreting object" ] }, "answerKey": "C" }, { "id": "atel_12120", "message": "Title: Swift/BAT detection of a 13 crab hard X-ray flare from the FSRQ SDSS J002829.81+200026.7\nAuthors: Shangyu Sun, Dongming Mao, Jie Lin and Wenfei Yu (Shanghai Astronomical Observatory)\nDate: 17 Oct 2018; 20:33 UT\nProvenance: Wenfei Yu (wenfei@shao.ac.cn)\nSubjects: X-ray, Black Hole, Blazar, Quasar, Transient\nDescription: Referred to by ATel #: 12129\nWith the All Sky Automated Survey for SuperNovae (ASAS-SN), the flat-spectrum radio quasar (FSRQ) SDSSJ002829.81+200026.7 (z=1.552007; Alam et al. 2015) was optically detected on 2018 October 3-6 in a rapid, unprecedented factor ~100 outburst (Stanek et al. ATel #12082). Fermi-LAT reported that this source was in a gamma-ray high state during October 3-5, 2018 (Buson et al. ATel #12084), with a peak gamma-ray flux on October 4. Swift/XRT observations in October 8-9 have shown the source was under a decay in soft X-rays(Komossa et al. ATel #12094). We have investigated the observations in the same period by the Burst Alert Telescope (BAT) on board Neil Gehrels Swift observatory. We found BAT had also observed a extreme hard X-ray (15-150 keV) flare from a source coincident with the position of SDSS J002829.81+200026.7 at (R.A., Dec) = (7.124 deg, -20.007 deg)(J2000). The BAT peak flux of the flare was 13.3 +- 0.2 Crab (14.0-194.9 keV, 1 sigma error) on 2018-10-05.59265 UT. The rise of the bright hard X-ray flare was extremely rapid. The flux increased by a factor of 9.7 in about 280 seconds, and then decreased by a factor of 31 in < 4300 seconds. In the period between the BAT observation of the apparent flare peak and the following BAT survey observations, the source was outside the field of view of BAT. The entire duration of the hard X-ray flare is thus estimated shorter than about 76 minutes. Such a bright hard X-ray flare and its fast rise and rapid decay, are very rare for flares seen in quasars. The hard X-ray flare is probably associated with some violent jet activities, which deserves further multi-wavelength and multi-messenger investigations. \nWe would like to mention that the source is also known as TXS 0025+197 (Douglas et al. 1996 AJ, 111.1945D). We thank the Neil Gehrels Swift observatory for kindly providing the data to the public.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy", "Black hole", "Supernova", "Neutron star" ] }, "answerKey": "B" }, { "id": "atel_12200", "message": "Title: Recurrent Nova M31N 2008-12a: Pre-Discovery upper limit and multi-colour follow-up observations with NEXT-XMO\nAuthors: H. Tan (National Central University), X. Gao (Xinjiang Astronomical Observatory)\nDate: 10 Nov 2018; 19:23 UT\nProvenance: Martin Henze (henze@ice.cat)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 12203, 12204, 12205, 12207, 12241\nWe report the prediscovery non-detection and multi-colour follow-up of the recurrent nova M31N 2008-12a (see ATels #12177, #12179, #12181, #12182, #12189, #12190, #12195) using the 0.60-m Ningbo bureau of Education and Xinjiang observatory Telescope (NEXT) located at Xingming Observatory (IAU Code C42), Mt.Nanshan, Xinjiang, China. All photometric observations listed below were obtained in the B, V, R, I filters between 2018-11-07.5 UT and 2018-11-10.5 UT and calibrated using secondary standards in the field (cf. Darnley et al. 2016). \n \nNothing was detected at the nova position on 2018-11-06.53 UT with an upper limit of V > 21.2 mag. Together with the discovery at Liverpool Telescope on 2018-11-06.80 (ATel #12177), our non-detection constrains the outburst time with an uncertainty of only 0.27 days. \n \n \n T_mid Filter Exp(s) Photometry(mag) \n 2018-11-06.537 Clear 300*2 >21.2 \n \n 2018-11-07.580 B 300*2 18.97±0.04 \n 2018-11-07.563 V 300*2 18.87±0.04 \n 2018-11-07.554 R 300*2 18.81±0.05 \n 2018-11-07.572 I 300*2 18.78±0.11 \n \n 2018-11-09.635 B 300*2 20.49±0.26 \n 2018-11-09.643 V 300*2 20.50±0.13 \n 2018-11-09.676 R 300*2 20.29±0.18 \n 2018-11-09.665 I 300*2 >19.2 \n \n 2018-11-10.593 B 300*5 20.90±0.09 \n 2018-11-10.612 V 300*5 21.16±0.18 \n 2018-11-10.631 R 300*5 20.72±0.13 \n 2018-11-10.724 R 300*5 20.73±0.15 \n 2018-11-10.705 I 300*3 19.69±0.30", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Variable star", "Exoplanet", "Nova" ] }, "answerKey": "D" }, { "id": "atel_12270", "message": "Title: A NIR rebrightening of the Blazar NVSSJ020344+304238\nAuthors: L. Carrasco, J. Miramon, G. Escobedo, E. Recillas, A. Porras, V. Chavushyan(INAOE, Mexico)\nDate: 5 Dec 2018; 19:17 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Infra-Red, Optical, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 12806\nWe report on a NIR rebrightening of the radio source NVSSJ020344+304238, cross-identified with the high redshift quasar BZBJ0203+3042 (z=0.761) and tentatively with the Gamma-ray source 3FGLJ0203.6+3043. We have reobserved the source in the NIR, finding that on November 29th,2018 (MJD 2458451.9049) its H-band flux corresponded to H = 15.046 +/- 0.03. This flux in H is 2 times higher than the previously determined value by our team (H = 15.799 +/- 0.06 on MJD 2458146.6133). In the past, the source has presented flaring activity in the NIR (see ATEL#11215). Our observations are carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We encourage further multi wavelength coverage. Related 11215 A NIR FLARE of the Blazar NVSSJ020344+304238 10985 MASTER: blazars flares and OTs", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Circumstellar disk", "Interstellar medium", "Black hole" ] }, "answerKey": "D" }, { "id": "atel_12390", "message": "Title: First time detection of a GRB at sub-TeV energies; MAGIC detects the GRB 190114C \nAuthors: Razmik Mirzoyan on behalf of the MAGIC Collaboration\nDate: 15 Jan 2019; 01:03 UT\nProvenance: Razmik Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de)\nSubjects: Gamma Ray, >GeV, TeV, VHE, Request for Observations, Gamma-Ray Burst\nDescription: Referred to by ATel #: 12395, 12475\nThe MAGIC telescopes performed a rapid follow-up observation of GRB 190114C (Gropp et al., GCN 23688; Tyurina et al., GCN 23690, de Ugarte Postigo et al., GCN 23692, Lipunov et al. GCN 23693, Selsing et al. GCN 23695). This observation was triggered by the Swift-BAT alert; we started observing at about 50s after Swift T0: 20:57:03.19. The MAGIC real-time analysis shows a significance >20 sigma in the first 20 min of observations (starting at T0+50s) for energies >300GeV. The relatively high detection threshold is due to the large zenith angle of observations (>60 degrees) and the presence of partial Moon. Given the brightness of the event, MAGIC will continue the observation of GRB 190114C until it is observable tonight and also in the next days. We strongly encourage follow-up observations by other instruments. The MAGIC contact persons for these observations are R. Mirzoyan (Razmik.Mirzoyan@mpp.mpg.de) and K. Noda (nodak@icrr.u-tokyo.ac.jp). MAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Observatory Roque de los Muchachos on the Canary island La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Quasar", "Variable star", "Near-Earth object" ] }, "answerKey": "C" }, { "id": "atel_12475", "message": "Title: GRB 190114C: Search for ultra-high-energy neutrinos with ARIANNA\nAuthors: Christian Glaser (UC Irvine), Steven Barwick (UC Irvine), Geoffrey Gaswint (UC Irvine), Christopher Persichilli (UC Irvine)\nDate: 4 Feb 2019; 22:52 UT\nProvenance: Christian Glaser (christian.glaser@uci.edu)\nSubjects: Neutrinos, Gamma-Ray Burst\nDescription: The ARIANNA collaboration (http://arianna.ps.uci.edu/) reports: \nSwift has reported detection of the long GRB 190114C (GCN #23688). This GRB is notable for having been detected by MAGIC above 300 GeV (ATel #12390). Other observations include: ground afterglow follow-ups (GCN #23690, #23693, #23699, #23702, #23710), a spectroscopic redshift of z = 0.4245 +/- 0.0005 (GCN #23708), and Fermi LAT detection up to 23 GeV (GCN #23709). The IceCube observatory reported an upper limit on the neutrino fluence of 0.436 x GeV cm^-2 for neutrino energies between 100 TeV to 20 PeV (ATel #12395). \nThe ARIANNA high-energy neutrino detector performed a search for neutrino events within the time window 150 seconds before the Swift-BAT trigger to one hour after the trigger (2019-01-14 20:54:33 UTC to 2019-01-14 21:57:03 UTC, same time window as used by IceCube). We did not find any neutrino candidate during this time period. Assuming an E^-2 spectrum (E^2 dN/dE) spectrum we derived a 90% CL upper limit on the neutrino fluence of 5.2 GeV cm^-2 in the neutrino energy range of 1e16eV - 1e20eV with a peak sensitivity around 1e18 eV. \nARIANNA is a high-energy Askaryan neutrino detector targeting neutrino energies above 10 PeV with a peek sensitivity around 1 EeV. The ARIANNA detector is currently in its pilot phase with autonomous and independent detector stations running at Moore's Bay on the Ross ice shelf and at the South Pole. During the time of GRB 190114C, four detector stations at Moore's Bay and one detector station at the South Pole were taking data but the GRB was outside the field-of-view of the South Pole detector station.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Minor body", "Variable star", "Stellar evolution" ] }, "answerKey": "A" }, { "id": "atel_12525", "message": "Title: Discovery of an Apparent Nova in M81\nAuthors: K. Hornoch, H. Kucakova (Ondrejov), S. C. Williams (Lancaster), M. Henze (SDSU), G. Sala, J. Jose (UPC-IEEC), H. Meusinger (TLS), M. J. Darnley (LJMU), A. Kaur (PSU), D. H. Hartmann (Clemson), A. W. Shafter (SDSU)\nDate: 21 Feb 2019; 22:06 UT\nProvenance: Steven Williams (s.williams7@lancaster.ac.uk)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 12679\nThe M81 nova monitoring collaboration reports the discovery of an apparent nova in M81 on a co-added 990-s unfiltered CCD frame taken on 2019 Feb. 18.205 UT with the 0.65-m telescope at Ondrejov. \nThe object designated PNV J09552547+6903458 is located at R.A. = 9h55m25s.47, Decl. = +69o03'45\".8 (equinox 2000.0), which is 41.3\" east and 9.3\" south of the center of M81 (see link to discovery image below). \nHere we list the observing dates and corresponding photometry: \n \n \n Date [UT] | Mag | Err | Filter | Telescope \n \n 2019-02-05.083 | <20.9 | | C | OND \n 2019-02-14.987 | 20.1 | 0.4 | C | OND \n 2019-02-15.787 | 19.8 | 0.3 | C | OND \n 2019-02-17.175 | 19.4 | 0.25 | C | OND \n 2019-02-18.205 | 17.9 | 0.1 | C | OND \n \n \nThe OND 0.65-m is a reflecting telescope at the Ondrejov observatory operated jointly by the Astronomical Institute of ASCR and the Astronomical Institute of the Charles University of Prague, Czech Republic. It uses a Moravian Instruments G2-3200 CCD camera (with a Kodak KAF-3200ME sensor and standard BVRI photometric filters) mounted at the prime focus. The unfiltered OND photometry was calibrated against R-band comparison stars from Perelmuter & Racine (1995).\nDiscovery image", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Nova", "Circumstellar disk", "Binary system" ] }, "answerKey": "B" }, { "id": "atel_12600", "message": "Title: XMM-Newton, NuSTAR and Swift follow-up of the new outburst of the magnetar XTE J1810-197\nAuthors: Nanda Rea (CSIC-IEEC, Barcelona, ES), Alice Borghese (U. Amsterdam, NL), Francesco Coti Zelati (CSIC-IEEC, Barcelona, ES), on behalf of a larger collaboration\nDate: 20 Mar 2019; 10:35 UT\nProvenance: Nanda Rea (rea@ice.csic.es)\nSubjects: X-ray, Magnetar\nDescription: Referred to by ATel #: 12689\nFollowing the recent outburst of the magnetar XTE J1810-197 in radio and X-rays (ATels #12284, #12285, #12288, #12291, #12297, #12484; Gotthelf et al. 2019, arXiv:1902.08358; Dai et al. 2019, arXiv:1902.04689; Levin et al. 2019, arXiv: 1903.02660), we have activated our XMM-Newton and NuSTAR monitoring programs for magnetar outbursts, and we are observing it with Swift. \nThe source is still very bright, and it was already observed four times by NuSTAR, one by XMM-Newton and seven times by Swift. The latest XMM-Newton and NuSTAR simultaneous observations (March 3rd and 4th) found the source at a 0.3-10keV flux of 1.23(1)e-10 erg/s/cm2, with a spectrum well fitted by two absorbed blackbodies with temperatures of 0.21(3) and 0.67(1) keV . \nWe will continue monitoring the outburst decay of XTE J1810-197 with XMM-Newton, NuSTAR and Swift in the following months. Multi-band follow-up observations, especially in the low-frequency bands, and simultaneous with the X-ray observations are strongly encouraged. Please contact us if you are interested in the exact schedule of the next X-ray observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Magnetar", "Minor body", "Nova" ] }, "answerKey": "B" }, { "id": "atel_12690", "message": "Title: Recent Swift Monitoring of Black Hole Candidate GX 339-4\nAuthors: J. Chen, S. Ali, M. Balakrishnan, N. Kebede, J. M. Miller, M. T. Reynolds, B. E. Tetarenko, D. Vozza (Univ. of Michigan)\nDate: 25 Apr 2019; 14:35 UT\nProvenance: Mark Reynolds (markrey@umich.edu)\nSubjects: Radio, Infra-Red, Ultra-Violet, X-ray, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 13024, 13447\nGX 339-4 is one of the most frequently recurring black-hole low-mass X-ray binaries in our Galaxy, having undergone more than 20 outbursts since its discovery (Tetarenko+ 2016). Following on previous Atels (#12420, #12413, #12322), we have looked at the 6 most recent observations starting from the beginning of March (OBSID: 00032898195) in XRT and UVOT. \n \nGX 339-4 has been in the hard-state since mid-2015 (ATel #7962), and continual detections are made since then. Recently, on April 9th (OBSID: 00032898207), GX 339-4 was observed with XRT (1.8ks in pc mode). We have mitigated pile-up by using an annulus around the center of the source (10-60 arcseconds) for the source region. The extracted spectrum was re-binned with grppha and the spectrum had a net count rate of 0.89 counts per second. \n \nUsing an absorbed power law (tbabs*po), the 0.5-10 keV spectrum had a photon index of 1.35 +/- 0.17, which matches with previous observations made back in January 2019 (ATels #12413, #12322). This value continues to suggest that GX 339-4 is still in the \"low-hard\" state. The model returned a column density of (4.1 +/- 1.7)E21 cm^-2 and flux of (2.1 +/- 0.2)E-10 erg/cm^2/s with (chi^2/dof = 63/71). (All values are quoted with 90% confidence errors.) Comparing the flux values with recent observations made in the start (OBSID: 00032898195) and end (OBSID: 00032898205) of March, GX 339-4 shows a decline in brightness in 0.5-10 keV by a factor of ~1.5 from 5.21 to 3.46 (E-10 erg/cm^2/s). \n \nWe have also examined observations made with SWIFT/UVOT and the source has been consistently detected. An observation on March 16 (OBSID: 00032898202) with an exposure time of 820s shows a UVW2-band flux of (1.61 +/- 0.26)E-2 mJy, while a 1.3ks UVW2-band observation on March 27 (OBSID: 00032898205) reveals a flux of (1.28 +\\\\- 0.21)E-2 mJy. A recent detection on April 9 (OBSID: 00032898207) with an exposure time of 1.4ks shows a UVM2-band flux of (1.02 +/- 0.22)E-2 mJy. Both extractions have a source radius of 5\". The flux is observed to continue its decay in both the X-ray and UV bands over the past month. \n \nWe will continue our multi-wavelength monitoring of GX 339-4 with SWIFT and we thank the Neil Gehrels Swift Observatory for executing this observation. \n \nReferences: \nTetarenko et al., 2016, ApJS, 222, 15", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Accreting object", "Black hole, Stellar evolution", "Black hole, Binary system", "Black hole, Interstellar medium" ] }, "answerKey": "C" }, { "id": "atel_12775", "message": "Title: FDST spectroscopic classification of SN 2019fju\nAuthors: R. Roy (IUCAA), R. Cartier (CTIO), P. Wiseman (University of Southampton), C. Inserra (Cardiff University), C. P. Gutierrez (University of Southampton), J. Anderson (ESO), C. Angus (University of Southampton), T.-W. Chen (MPE), T. de Jaeger (UC Berkeley), C. Frohmaier (University of Portsmouth - ICG), L. Galbany (University of Pittsburg), S. Gonzalez-Gaitan (CENTRA), M. Grayling (University of Southampton), H. Kuncarayakti (University of Turku), J. Lyman (University of Warwick), T. Muller-Bravo (University of Southampton), A. Pastorello (INAF - Padova Astronomical Observatory), M. Pursiainen (University of Southampton), T. Schweyer (MPE), M. Smith (University of Southampton), M. Sullivan (University of Southampton)\nDate: 17 May 2019; 16:16 UT\nProvenance: Philip Wiseman (p.s.wiseman@soton.ac.uk)\nSubjects: Optical, Supernovae\nDescription: The Fast and Dark Side of Transients experiment (FDST; ATel #12362) reports the spectroscopic observation of SN 2019fju. The target was supplied by the Zwicky Transient Facility (https://www.ztf.caltech.edu/; Kulkarni et al. 2018, ATel 11266) and processed through the Lasair broker (Smith, Williams, et al. 2019, RNAAS, 3, 26; https://lasair.roe.ac.uk/). Classifications were done with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). \nThe observations were performed on 2019-05-16 using SPRAT (Piascik et al 2014) on the Liverpool Telescope (Steele et al. 2004). \n \n \n Survey Name | IAU Name | RA (J2000) | Dec (J2000) | Disc. Date | Source | Disc Mag | z | Type | Phase | Notes \n ZTF19aaurhox | SN2019fju | 16 32 3.98 | 42 30 42.16 | 20190513 | ZTF | 20.03 | 0.07 | Ia |pre max | (1) \n \n(1) The redshift is obtained from the SNID fit. The phase obtained from SNID is -7days.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Variable star", "Star and stellar system", "Exoplanet" ] }, "answerKey": "A" }, { "id": "atel_12840", "message": "Title: IGR J14557-5448 is likely an AGN\nAuthors: F. Ursini, L. Bassani, A. Malizia, V. Sguera (INAF-OAS Bologna), A. Bazzano, P. Ubertini, M. Fiocchi (INAF-IAPS Rome), A. J. Bird (University of Southampton)\nDate: 5 Jun 2019; 08:47 UT\nProvenance: Francesco Ursini (francesco.ursini@inaf.it)\nSubjects: X-ray, AGN\nDescription: We use a public XMM-Newton observation (Obs.ID: 0803031501, date: 2018-02-09, net exposure: 8 ks) to search for the X-ray counterpart of IGR J14557-5448, a persistent and still unidentified source seen by INTEGRAL/IBIS (Bird et al. 2016, ApJS 223,15). Within the IBIS positional uncertainty (90% confidence level), we find one hard X-ray source (>10 sigma in the 7.5–12 keV band) at coordinates: RA(J2000) = 14:55:32.400, Dec(J2000) = -54:46:29.640 (90% uncertainty around 4 arcsec). The source has a radio counterpart (MGPS J145532-544629) and an AllWISE counterpart (J145532.03-544628.7), associated to the spiral galaxy 2MASX J14553197-5446291 (also WKK98 4442, Leda 415943, PGC 415943) of still unknown redshift: the radio flux is 33.4+/-1.4 mJy at 36 cm, while the infrared colours are W1-W2=0.81 and W2-W3=3.13, typical of AGNs (Secrest et al. 2015, ApJS 221,12). \nFitting the XMM-Newton spectrum (2–10 keV) jointly with the IBIS spectrum (20–200 keV) yields a hard photon index of 1.10(+/-0.15) and a column density in excess of the Galactic value of 1.0(+/-0.3)x10^23 cm^-2, with Chi^2/dof=24/21. The observed 2–10 keV flux is 6.0(+/-0.7)x10^-13 ergs cm^-2 s^-1. These results suggest that the source could be an X-ray absorbed Seyfert 2.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Galaxy", "Globular cluster", "Stellar evolution" ] }, "answerKey": "D" }, { "id": "atel_12950", "message": "Title: OT discovery by MASTER during GW error fields inspection\nAuthors: P. Balanutsa, V. Lipunov (Lomonosov MSU), R. Rebolo, M. Serra (IAC), E. Gorbovskoy, V. Kornilov, N. Tiurina, A. Kuznetsov, O. Gress, I. Gorbunov, V. Vladimirov, D. Zimnukhov, F. Balakin, V. Senik, A. Pozdnyakov, Yu. Miloadovich (Lomonosov MSU), N. M. Budnev, O. Ershova (API ISU), A. Tlatov, D. Dormidontov (KSS of the Pulkovo Observatory), D. Buckley (SAAO), R. Podesta, C. Lopez, C. Francile, F. Podesta (OAFA, SJNU), H. Levato (ICATE, SJNU),V. Yurkov, A. Gabovich, Yu. Sergienko, (BSPU), T. Pogrosheva, V. Shumkov\nDate: 19 Jul 2019; 18:32 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Cataclysmic Variable, Gravitational Waves, Transient, Variables\nDescription: MASTER OT J203233.42+224327.0 discovery \nMASTER-IAC auto-detection system discovered OT source at (RA, Dec) = 20h 32m 33.42s +22d 43m 27.0s on 2019-07-19.01993 UT. \nThe OT unfiltered magnitude is 18.4m (limit 18.7m). There is no minor planet at this place. \nWe have reference image without OT on 2018-12-25.81367 UT with unfiltered magnitude limit 19.1m. \nThis flash is registered in the error box GW S190718y. \nSpectral observations are required. \nThe discovery and reference images are available at \nhttp://master.sai.msu.ru/static/OT/203233.42224327.0.png", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova, Nova", "Variable star, Nova", "Minor body, Nova", "Active galactic nucleus, Nova" ] }, "answerKey": "B" }, { "id": "atel_13000", "message": "Title: UV brightening of the accreting millisecond X-ray pulsar SAX J1808.4-3658\nAuthors: A. S. Parikh and R. Wijnands\nDate: 7 Aug 2019; 21:15 UT\nProvenance: Aastha Parikh (A.S.Parikh@uva.nl)\nSubjects: Ultra-Violet, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 13001, 13006, 13026, 13077\nRecently, on 30 July 2019, Russell et al., (2019) reported an optical brightening of the transiently accreting millisecond X-ray pulsar SAX J1808.4-3658 but with, at that point, no associated X-ray brightening. This optical brightening was thought to be indicative of an imminent outburst.\nSince then the source has continued to be monitored using ground-based observatories in the optical and using the Swift in the X-rays. New observations examined by Goodwin at al., (2019) show that the source has very recently further brightened in the i' band (between 4 and 6 August 2019) and in the X-rays on 6 August 2019, suggesting the onset of the anticipated new accretion outburst.\nWe have examined the recent observations of SAX J1808.4-3658 carried out by the UVOT on board Swift to determine if the source also showed a brightening in the UV emission. We used the Level 2 data products and determined the source brightness using the uvotsource tool. A circular source region, centred on the source position, having a radius 6 arcsec was used. A circular background region having a radius of 6 arcsec was placed on a source free location on the CCD. We found that the X-ray and optical brightening was accompanied by a UV brightening. This rise can be conclusively seen in the UVW2 band: 20.1 mag on 6 August (upper limit <20.9 mag on 3 August, with similar upper limits during the earlier observations) and marginally in the UVW1 band: 20.3 mag on 5 August (upper limit <20.4 mag on 1 August and during the earlier observations). This UV brightening supports the notion that the source may be exhibiting renewed outburst activity, its first since 2015.\nWe have two additional Swift UVOT observations approved (before the source is Moon constrained on 13 August) to further track the rise of the current outburst in all three UV bands per observation. We thank the Swift PI Brad Cenko and his designate B. Sbarufatti for approving these observations.\nRussell et al., (2019) ATel #12964 \nGoodwin at al., (2019) ATel #12993", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater, Pulsar", "Nova, Pulsar", "Neutron star, Pulsar", "Active galactic nucleus, Pulsar" ] }, "answerKey": "C" }, { "id": "atel_13080", "message": "Title: Reappearance of methanol maser flare in G24.33+0.14\nAuthors: P. Wolak, M. Olech, M. Szymczak, A. Bartkiewicz, M. Durjasz, (Centre for Astronomy, Faculty of Physics, Astronomy and Informatics, Nicolaus Copernicus University, Grudziadzka 5, PL-87-100 Torun, Poland)\nDate: 5 Sep 2019; 10:40 UT\nProvenance: Pawel Wolak (wolak@astro.uni.torun.pl)\nSubjects: Radio, Young Stellar Object\nDescription: A second methanol maser burst in G24.33+0.14 is being observed with the Torun 32 m radio telescope at 6.7GHz. The first flare was detected about 8 years ago (Wolak et. al. 2018, feature 1C at Fig. 1.). During the current burst the integrated flux density and flux density of feature at 115 km s-1 increased over 80 days by a factor of 2.5 and 5.5, respectively (Fig. 2.). Enhancement of intensity of methanol maser is also seen at 12.2GHz. The target is a high-mass young stellar object associated with the hydroxyl, methanol and water masers (Caswell & Green 2011). The variability characteristics suggest that the flare is due to changes in the physical conditions likely induced by an episodic accretion event. Follow-up observations are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Star and stellar system", "Globular cluster", "Stellar evolution" ] }, "answerKey": "D" }, { "id": "atel_13150", "message": "Title: Swift/XRT detects a new outburst of the Galactic Center transient AX J1745.6-2901\nAuthors: N. Degenaar (U. of Amsterdam), R. Wijnands (U. of Amsterdam), M. T. Reynolds (U. of Michigan), J. M. Miller (U. of Michigan), J. A. Kennea (PSU), on behalf of a larger collaboration\nDate: 1 Oct 2019; 07:27 UT\nProvenance: Nathalie Degenaar (degenaar@uva.nl)\nSubjects: X-ray, Neutron Star, Transient\nDescription: Referred to by ATel #: 13453, 13683, 13839, 14378, 14788, 16106\nOur daily Swift/XRT monitoring observations of the Galactic Center (Degenaar et al. 2015, JHEAp, 7, 137) show X-ray activity of a transient source located ~1.5' to the south-east of Sgr A*. This object is clearly detected in individual XRT images since September 17 (obs ID 00095329145), with a count rate of ~0.04-0.12 c/s. \nUsing the tool xrtcentroid on a combined image of the 13 observations taken between September 17 and 29 (obsID 00095329145-157), we determine that the position of the transient is RA = 17:45:36.16, DEC = -29:01:33.24 (J2000) with a 90% confidence error of 3.6\". These coordinates are consistent with the Chandra localisation (ATel #1513) of the 8.4-hr eclipsing low-mass X-ray binary and thermonuclear X-ray burster AX J1745.6-2901. We thus conclude that we have likely detected a new outburst of this transient. \nWe extracted an average spectrum from the above mentioned observations. This spectrum can be described by an absorbed power-law model with an index of 2.4 +/- 0.4 and a hydrogen column density of (2.0+/-0.3)E+23 cm-2 (1-sigma errors). The inferred 2-10 keV unabsorbed flux for this fit is (3.7+/-0.9)E-11 erg cm-2 s-1, which translates into a luminosity of ~3E35 erg/s at a distance of 8 kpc. \nAX J1745.6-2901 is very frequently active: our monitoring program previously detected outbursts from this system in 2006, 2007-2008, 2010 (e.g. Degenaar et al. 2015), 2013-2016 (e.g. ATels #5226, #9196), and two in 2017 (ATels #10323, #10900). The years-long outbursts that occurred in 2007-2008 and 2013-2016 reached a peak luminosity of several times E36 erg/s. All the other outbursts had a shorter duration (months) and a lower peak luminosity of a few times E35 erg/s. It seems that the current outburst belongs to the latter class. \nDaily Swift/XRT monitoring of the Galactic Center is ongoing and the results of new observations are automatically posted on http://www.swift-sgra.com.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Accreting object", "Binary system", "Neutron star" ] }, "answerKey": "D" }, { "id": "atel_13230", "message": "Title: Spectroscopic confirmation and photometry of the recent M31 nova AT2019sxc (= PNV J00430155+4117599)\nAuthors: S. Fabrika, O. Sholukhova, Yu. Solovyeva, D. Oparin, A. Sarkisyan, A. Vinokurov (SAO RAS), A. W. Shafter (SDSU)\nDate: 27 Oct 2019; 21:29 UT\nProvenance: Sergei Fabrika (fabrika@sao.ru)\nSubjects: Optical, Nova\nDescription: Referred to by ATel #: 13272\nWe report optical spectroscopic confirmation of the M31 nova AT2019sxc (= PNV J00430155+4117599) announced in ATel #13207. \nThe spectral data were obtained on 2019 Oct. 24.01. UT using the Russian BTA telescope equipped with the SCORPIO spectrograph. The spectrum was taken with a resolution of 5.3 Å in the 3750 - 5440 Å blue range and in the 5720 - 7400 Å red range. The widths were corrected for spectral resolution. The photometry of the nova was obtained just before the time of the BTA spectrum with the same device and gave B = 17.66 ± 0.08, V = 17.41 ± 0.09, Rc = 17.07 ± 0.05. \nThe nova shows Balmer emission lines together with many Fe II lines. In the main lines: H-alpha, H-beta, H-gamma we observed P Cyg profiles -1900 ± 100 km/s, FeII lines with P Cyg -1350 ± 70 km/s. The hydrogen lines have a width of FWHM = 1600 ± 100 km/s, while the FeII lines (4923, 5169 Å) are characterized by FWHM = 1450 ± 50 km/s. Other FeII lines are very broad and complicated. In the case of hydrogen lines, we found narrow peaks both in absorption and emission components. We have found CaII (3933, 3968 Å), NaI (5889, 5895 Å) and SiII (6347, 6371 Å) with very deep P Cyg absorption profiles -1950 ± 50 km/s along with emission components. We conclude that the M31 nova AT2019sxc belongs to the Fe II class.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova, Nova", "Binary system, Variable star", "Nova, Star and stellar system", "Nova, Variable star" ] }, "answerKey": "D" }, { "id": "atel_13290", "message": "Title: Recurrent nova M31N 2008-12a: Swift/XRT detection of the 2019 eruption\nAuthors: M. J. Darnley (LJMU), M. Henze (SDSU), I. Hachisu (Tokyo), M. Kato (Keio), J. P. Osborne (Leicester), J.-U. Ness (ESA/ESAC), A. W. Shafter (SDSU), on behalf of the 12a Collaboration\nDate: 14 Nov 2019; 11:16 UT\nProvenance: Matt Darnley (M.J.Darnley@ljmu.ac.uk)\nSubjects: X-ray, Nova\nDescription: Referred to by ATel #: 13302\nIn ATel #13269 we announced the discovery of the 2019 eruption of the recurrent nova M31N 2008-12a on 2019-11-06.71 UT (almost exactly one year since the 2018 eruption was discovered; ATel #12177). We reported the follow-up UV detection with Neil Gehrels Swift Observatory/UVOT in ATel #13274. M31N 2008-12a has now been detected in eruption 12 times in 12 consecutive years (cf. ATels #5607, #6527, #7964, #9848, #11116, #12177). Comprehensive multi-wavelength studies of previous eruptions were published by Darnley et al. (2014, 2015, 2016) and Henze et al. (2014, 2015a, 2015b, 2018), a recent review article has been published by Darnley & Henze (2019). For additional optical photometry and spectroscopy of the ongoing eruption see ATels #13273, #13274, #13279, #13281. \nHere we report the emergence of the supersoft X-ray source (SSS) phase of M31N 2008-12a. A faint X-ray counterpart was detected in a 3.6-ks Swift observation starting on 2019-11-12.33 UT (MJD 58799.33). We measured the preliminary XRT count rate to be (7.3 ± 1.6) × 10-3 ct/s. No X-ray source was detected at a significant level in the preceding 0.7-ks Swift observation on 2019-11-11.33 UT with an 3σ upper limit of 1.02 × 10-2 ct/s (nor in any of the previous daily observations since the detection of this eruption). \nIf we assume an eruption date of 2019-11-06.6 UT (MJD 58793.6), determined by fitting the Liverpool Telescope and LCO optical photometric data of the 2019 eruption to the eruption light-curve template (see Darnley et al. 2016), then the SSS counterpart appeared around day 5.7 after eruption. This preliminary estimate is consistent with the 5.9 ± 0.5 days measured in 2014 (ATel #6558, Henze et al. 2015), the 5.7 ± 0.5 days seen in 2015 (ATel #7984, Darnley et al. 2016), and the 5.8 days observed for the peculiar 2016 eruption (ATel #9872, Henze et al. 2018). The X-ray spectrum at this time is consistent with SSS emission \nWe wish to thank the Swift Team for the excellent scheduling of the observations, in particular B. Cenko, the duty scientists, and the science planners.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Globular cluster", "Quasar", "Star and stellar system" ] }, "answerKey": "A" }, { "id": "atel_13380", "message": "Title: Search for counterpart to IceCube-191231A with ANTARES\nAuthors: Alexis Coleiro (APC/Universite de Paris) and Damien Dornic (CPPM/CNRS) on behalf of the ANTARES Collaboration\nDate: 1 Jan 2020; 13:16 UT\nProvenance: Antoine Kouchner (kouchner@apc.univ-paris-diderot.fr)\nSubjects: >GeV, TeV, Neutrinos, Transient\nDescription: Using data from the ANTARES detector, we have performed a follow-up analysis of the recently reported single track-like event IceCube-191231A (GCN 26620 < https://gcn.gsfc.nasa.gov/gcn3/26620.gcn3>). The original reconstructed origin was 17 degrees below the horizon for ANTARES. \nNo up-going muon neutrino candidate events were recorded at the location of the IceCube event coordinates (accounting for the reported uncertainties) during a +/- 1h time-window centered on the IceCube event time, and over which the potential source remained visible all time. A search over an extended time window of +/- 1 day has also yielded no detection (40% visibility). \nThis leads to a preliminary 90% confidence level upper limit on the muon-neutrino fluence from a point source of 15 GeV.cm^-2 over the energy range 5.3 TeV - 5.0 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and 32 GeV.cm^-2 (960 GeV - 470 TeV) for an E^-2.5 spectrum. \nANTARES is the largest undersea neutrino detector (Mediterranean Sea) and it is primarily sensitive to astrophysical neutrinos in the TeV-PeV energy range. At 10 TeV, the median angular resolution for muon neutrinos is about 0.5 degrees. In the range 1-100 TeV ANTARES has a competitive sensitivity to this position in the sky.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy", "Neutron star", "Exoplanet", "Near-Earth object" ] }, "answerKey": "B" }, { "id": "atel_13440", "message": "Title: Independent Discovery of a Probable Nova in M81\nAuthors: K. Hornoch, H. Kucakova (Ondrejov), S. C. Williams (Turku), G. Sala, J. Jose (UPC-IEEC), B. Stecklum (TLS), M. J. Darnley (LJMU), A. Kaur (PSU), D. H. Hartmann (Clemson), A. W. Shafter (SDSU)\nDate: 2 Feb 2020; 14:26 UT\nProvenance: Steven Williams (steven.williams@utu.fi)\nSubjects: Optical, Nova, Transient\nDescription: The M81 nova monitoring collaboration reports the independent discovery of a probable nova in M81 on a co-added 3150-s unfiltered CCD frame taken on 2020 Feb. 1.016 UT with the 0.65-m telescope at Ondrejov. \nThe object was independently discovered and first announced by M. Zhang and X. Gao and designated as PNV J09554842+6907325 = AT 2020bmf. The object was designated by us as M81N 2020-02a and is located at R.A. = 9h55m48s.50, Decl. = +69o07'33\".2 (equinox 2000.0), which is 82.0\" east and 218.1\" north of the center of M81 (see link to discovery image below). \nHere we list the observing dates and corresponding photometry: \n \n \n Date [UT] | Mag | Err | Filter | Telescope \n \n 2020-01-29.055 | <21.4 | | C | OND \n 2020-02-01.016 | 20.1 | 0.15 | C | OND \n 2020-02-02.112 | 20.7 | 0.25 | C | OND \n \n \nThe OND 0.65-m is a reflecting telescope at the Ondrejov observatory operated jointly by the Astronomical Institute of ASCR and the Astronomical Institute of the Charles University of Prague, Czech Republic. It uses a Moravian Instruments G2-3200 CCD camera (with a Kodak KAF-3200ME sensor and standard BVRI photometric filters) mounted at the prime focus. The unfiltered OND photometry was calibrated against R-band comparison stars from Perelmuter & Racine (1995).\nDiscovery image", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater", "Nova", "Stellar evolution", "Star and stellar system" ] }, "answerKey": "B" }, { "id": "atel_13500", "message": "Title: Bright emission lines in the optical spectrum and the redshift of the host galaxy of TDE candidate SRGet J143359.25+400638.5\nAuthors: R. Burenin (IKI), M. Eselevich (ISZF SO RAN), I. Zaznobin (IKI), S. Sazonov (IKI), R. Sunyaev (IKI), on behalf of the Russian SRG/eROSITA Consortium\nDate: 18 Feb 2020; 18:37 UT\nProvenance: Ildar Khabibullin (khabibullin@iki.rssi.ru)\nSubjects: Optical, Transient, Tidal Disruption Event\nDescription: Referred to by ATel #: 13507, 13510\nThe host galaxy, SDSS J143359.16+400636, of the bright SRG/eROSITA X-ray TDE candidate SRGet J143359.25+400638.5 (I. Khabibullin et al., ATel #13494) was observed on Feb 18, 2020, at 4:50-6:10 UT with the Sayan observatory's AZT-33IK 1.6-m telescope using the ADAM low and medium resolution spectrograph. \nThe derived low-resolution spectrum shows a continuum with CaII, MgI and NaD absorption lines typical of an early-type galaxy, and also [OIII],4959,5007 and Halpha in emission. All the absorption and emission lines are narrow (<200 km/s) and observed at redshift z=0.0986. The equivalent widths of the [OIII],5007 and Halpha lines are 5.4 and 6.4 angstrom respectively, corresponding to a luminosity ~10^40 erg/s. \nWe also obtained direct images in g,r,i, with 15 min exposure per filter. The images show no obvious difference as compared to the SDSS ones.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system", "Exoplanet", "Pulsar", "Globular cluster" ] }, "answerKey": "B" }, { "id": "atel_13560", "message": "Title: Detection of the new magnetar Swift J1818.0-1607 in S-band using GBT\nAuthors: Yogesh Maan (API, University of Amsterdam, Amsterdam, NL) and Joeri van Leeuwen (ASTRON, Dwingeloo, NL)\nDate: 17 Mar 2020; 20:44 UT\nProvenance: Joeri van Leeuwen (leeuwen@astron.nl)\nSubjects: Radio, Neutron Star, Soft Gamma-ray Repeater, Transient, Pulsar, Magnetar\nDescription: Referred to by ATel #: 13562, 13569, 13575, 13577, 13580, 13649, 13966, 14001\nOn March 12, 2020, Swift/BAT detected a short burst from a new soft gamma-ray repeater, Swift J1818.0-1607 (GCN circular 27373). Following this burst, Enoto et al. (ATel #13551) uncovered a coherent periodicity of 1.36 s using NICER data in the 2-10 keV band. Detection of the periodicity suggested this new source to be a magnetar. Karuppusamy et al. (ATel #13553) reported discovery of radio pulsations at a dispersion measure (DM) of 706(4) cm^-3 pc, using the 100-m Effelsberg radio telescope at 1370 MHz.\nUsing the Robert C. Byrd Green Bank Telescope (GBT), we observed Swift J1818.0-1607 on March 17, 07:26 UT, with 800 MHz bandwidth around 2.0 GHz. We readily detected strong radio pulsations at a barycentric period of 1.36351 s, at a coherently dedispersed DM consistent with 706 cm^-3 pc. Assuming that the barycentric period measured by Enoto et al. was referenced to the start time of their observation on March 13, 01:38 UT, the period measured from our observations suggests a period-derivative of 9.3517(2)x10^-11. This measurement does not include the slightly larger uncertainty that is caused by the fact that the exact epoch of the X-ray periodicity measurement is not known. Using observations with Lovell and Effelsberg, Champion et al. (ATel #13559) have just reported perhaps a more precise period-derivative measurement of 8.16(2) x 10^-11. The spin-down rate is comparable to the Galactic center magnetar SGR J1745-2900 (Lynch et al. 2015), and further supports Swift J1818.0-1607 to be a magnetar. The spin-down rate measurement suggests the characteristic age of the magnetar to be less than 300 yrs, making it the youngest among the magnetars that are known to emit in radio.\nThe average profile at 2 GHz shows a faint component trailing the main peak by about 10% of the spin period, that is mostly comprised of intermittent, spiky emission. There was no hint of this component in the earlier observation reported at 1.37 GHz (ATel #13553). Data were calibrated for flux and polarisation based on standard radio sources. We find both pulse components are nearly 100% linearly polarized accompanied by a small degree of circular polarization. The mean flux density of the band-averaged profile is estimated to be about 0.05(1) mJy. Exploiting the large bandwidth, we also make a preliminary estimate of the spectral index to be -1.8(3). Extrapolating our 2 GHz flux density measurements to 1.4 GHz, and comparing with the March 14 discovery observations suggests that the magnetar's radio brightness might have decayed. However, the decrease might also be accounted for by rapid, intrinsic flux density variations which have been observed in other radio-loud magnetars.\nThe polarization profile and time-phase stack plots are available here: \nhttp://alert.eu/Swift_J1818.0-1607/\nWe thank the Green Bank Observatory and staff for the prompt allocation and scheduling of our requested director's discretionary time, and their support.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Repeater", "Neutron star, Magnetar", "Pulsar, Magnetar", "Repeater, Magnetar" ] }, "answerKey": "B" }, { "id": "atel_13620", "message": "Title: Possible Disintegration of Comet C/2019 Y4 (ATLAS)\nAuthors: Quanzhi Ye (U. Maryland), Qicheng Zhang (Caltech)\nDate: 6 Apr 2020; 17:12 UT\nProvenance: Quanzhi Ye (qye@umd.edu)\nSubjects: Optical, Comet\nDescription: Referred to by ATel #: 13622, 13634, 13651, 13813\nWe report the possible disintegration of comet C/2019 Y4 (ATLAS), revealed by the public monitoring program carried out by the 0.6-m Ningbo Education Xinjiang Telescope (NEXT). Images taken on UT 2020 April 5.6-5.9 showed an elongated pseudo-nucleus measuring about 3 arcsec in length and aligned with the axis of the tail, a morphology consistent with a sudden decline or cessation of dust production, as would be expected from a major disruption of the nucleus. The elongation is grossly consistent with the roughly +5\" in RA, -1\" in Dec astrometric residuals currently (as of MPEC 2020-G65) being reported relative to JPL orbit solution #5, implying a relative projected motion of order 5-10 m/s from the original nucleus' orbit. A disruption event could also potentially explain the large non-gravitational forces acting on the comet, as reported in CBET 4744. Composite stacks of 10 x 30-s r-filtered frames illustrating the change in morphology from April 2 to 5 can be found at https://near.earth/shared/2020/04/next_20200405.png. (The images from both days were obtained without comet-rate tracking, but the exposure was sufficiently short that the trailing of the comet due to its non-sidereal motion is only 1.3 pixel, much shorter than the elongation of the pseudo-nucleus. The direction of the trailing is also at a ~30 deg angle to the long-axis of the elongated pseudo-nucleus.)\nWe thank Man-To Hui and Xing Gao for discussion and assistance in obtaining the NEXT data.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Accreting object", "Interstellar medium", "Neutron star" ] }, "answerKey": "A" }, { "id": "atel_13680", "message": "Title: Spectroscopic classification of AT2020idu = ZTF20aavnpug = Gaia20byj as a dwarf nova\nAuthors: Keisuke Isogai (Kyoto University, Okayama Observatory), Hiroyuki Maehara (National Astronomical Observatory of Japan)\nDate: 28 Apr 2020; 19:52 UT\nProvenance: Keisuke Isogai (isogai@kusastro.kyoto-u.ac.jp)\nSubjects: Optical, Cataclysmic Variable, Transient, Variables\nDescription: I report on a spectrum of the optical transient AT2020idu = ZTF20aavnpug = Gaia20byj obtained on 2020-4-28.70 UT by using a fiber-fed integral field spectrograph (KOOLS-IFU; Matsubayashi et al. 2019) mounted on the 3.8-m telescope Seimei of Kyoto University. \n \nThis object was discovered by ZTF at r=16.95 mag on 2020-04-22.46 UT and reported to TNS as a supernova candidate. Then, Gaia reported the maximum brightness of 15.32 mag. My spectrum shows a blue continuum with an H alpha emission and no other clear features. Thus, this object can be classified as a dwarf nova. Because there is no optical counterpart in Pan-STARRS1, the outburst amplitude is larger than 6 mag. So this object will be a SU UMa or WZ Sge-type dwarf nova.\nSpectrum of AT2020idu", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy", "Variable star", "Repeater", "Near-Earth object" ] }, "answerKey": "B" }, { "id": "atel_13750", "message": "Title: MAXI/GSC observation of the onset of a giant outburst from Be/X-ray binary pulsar GRO J1008-57\nAuthors: M. Nakajima, H. Negoro (Nihon U.), T. Mihara (RIKEN), M. Aoki, K. Kobayashi, R. Takagi, K, Asakura, K, Seino, S. Mokumoto (Nihon U.), C. Guo, Y. Zhou, T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, M. Serino, S. Sugita, H. Nishida, A. Yoshida (AGU), Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.), M. Shidatsu (Ehime U.), N. Kawai, R. Adachi, M. Niwano (Tokyo Tech), S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Ishikawa, M. Tominaga, T. Nagatsuka (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, K. Kurogi, K. Miike (Miyazaki U.), T. Kawamuro (NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) \nDate: 22 May 2020; 01:41 UT\nProvenance: Motoki Nakajima (nakajima.motoki@nihon-u.ac.jp)\nSubjects: X-ray, Binary, Neutron Star, Transient, Pulsar\nDescription: A rapid brightening of the Be/X-ray binary pulsar GRO J1008-57 triggered on the MAXI/GSC nova-alert system (Negoro et al. 2016) on 2020-05-17 (MJD 58986). NICER observation about this outburst is reported in ATel #13749. After the last periastron passage on 2020 March, this source had been in the flaring state with the average flux of ∼40 mCrab for 2 months (ATel #13544). On 2020-05-06 (MJD 58975), the flux dropped once and showed an abrupt brightening after it. In the recent 10 days, the source 4-10 keV flux increased with a rate of ∼0.020 photons/cm2/sec/day. These X-ray behavior is very similar to the beginning of the 2012 giant outburst of the source (Atel#4355,#4561,#4573,#4577). See the figure for a comparison of the current and 2012 outbursts, http://maxi.riken.jp/news/en/#news-1252. Assuming that this brightening traces the 2012 giant outburst, the current outburst will reach its maximum of ∼500 mCrab at the end of May. \n \nWe encourage multi-wavelength observations to understand the physical mechanisms of the giant outburst. \n \nThe latest X-ray light-curve can be checked at the following pages; \nMAXI ( http://maxi.riken.jp/star_data/J1009-582/J1009-582.html ), \nSwift/BAT ( http://swift.gsfc.nasa.gov/results/transients/GROJ1008-57/ ), \nFermi/GBM ( https://gammaray.nsstc.nasa.gov/gbm/science/pulsars/lightcurves/groj1008.html ), and \nthe BeXRB monitor page ( http://integral.esac.esa.int/bexrbmonitor/Plots/sim_plot_GROJ1008-57.html ).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Repeater", "Circumstellar disk", "Minor body" ] }, "answerKey": "A" }, { "id": "atel_13850", "message": "Title: Trigger 980513: Swift detection of SGR Swift J1818.0-1607\nAuthors: M. G. Bernardini (INAF-OAB), P. D'Avanzo (INAF-OAB), N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC), A. Melandri (INAF-OAB), K. L. Page (U Leicester), D. M. Palmer (LANL) and T. Sbarrato (INAF-OAB)\nDate: 2 Jul 2020; 08:00 UT\nProvenance: David M. Palmer (palmer@lanl.gov)\nSubjects: X-ray, Gamma Ray, Soft Gamma-ray Repeater, Transient, Magnetar\nDescription: This is a courtesy copy of GCN #28055 (the reference for citation) for the benefit of the SGR community. \nThe authors report on behalf of the Neil Gehrels Swift Observatory Team: \nAt 07:09:38 UT on 2020-07-02, the Swift Burst Alert Telescope (BAT) triggered and located a burst from Soft Gamma Repeater SGR Swift J1818.0-1607 (trigger=980513). Swift slewed immediately to the source. The BAT on-board calculated location is RA, Dec 274.471, -16.167 which is \nRA(J2000) = 18h 17m 53s \nDec(J2000) = -16d 09' 59\" \nwith an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single-peaked structure with a duration of about 100 ms. The peak count rate was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. \nThe XRT began observing the field at 07:11:03.2 UT, 84.4 seconds after the BAT trigger. Using promptly downlinked data we find an X-ray source with an enhanced position: RA, Dec 274.5017, -16.1317 which is equivalent to: \nRA(J2000) = 18h 18m 00.40s \nDec(J2000) = -16d 07' 54.2\" \nwith an uncertainty of 3.0 arcseconds (radius, 90% containment). This location is 165 arcseconds from the BAT onboard position, within the BAT error circle, and consistent with the catalogued position of SGR Swift J1818.0-1607. This position may be improved as more data are received; the latest position is available at https://www.swift.ac.uk/sper. \nA power-law fit to a spectrum formed from promptly downlinked event data does not constrain the column density. \nUVOT took a finding chart exposure of 150 seconds with the White filter starting 87 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers none of the XRT error circle. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for the large, but uncertain, extinction expected. \nThis is the fourth time Swift has triggered on SGR Swift J1818.0-1607; with 5 additional burst detections that did not reach the level needed for a burst response ('trigger'). These detections were: \n2020-02-28T22:19:32 \n2020-03-12T21:16:47 GCN 27373 \n2020-04-13T19:34:18 \n2020-05-06T17:36:50 GCN 27696 \n2020-05-16T15:03:28 GCN 27746 \n2020-05-17T14:29:54 \n2020-05-25T20:23:45 \n2020-06-01T16:52:09", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Magnetar", "Exoplanet", "Repeater" ] }, "answerKey": "B" }, { "id": "atel_13900", "message": "Title: NuSTAR detection of Nova Reticuli 2020 = MGAB-V207\nAuthors: K. V. Sokolovsky, E. Aydi, L. Chomiuk, A. Kawash, J. Strader (MSU), K. Mukai (NASA/GSFC), K.-L. Li (NTHU), A. Babul, A. Derdzinski, B. D. Metzger, J. L. Sokoloski, E. Steinberg (Columbia), I. Vurm (Tartu), J. D. Linford, A. J. Mioduszewski (NRAO), M. P. Rupen (NRC), R. Lopes de Oliveira (U Sergipe/Obs. Nacional Brazil), K. L. Page, A. Beardmore (U Leicester), M. Orio (UoW, INAF)\nDate: 28 Jul 2020; 04:59 UT\nProvenance: Kirill Sokolovsky (kirx@scan.sai.msu.ru)\nSubjects: X-ray, Nova\nDescription: Referred to by ATel #: 14043, 14530\nThe classical nova explosion in the previously known cataclysmic variable MGAB-V207 was reported by R. H. McNaught on 2020-07-15.590 UT (CBET #4811). Pre-discovery all-sky camera images by M. A. Phillips show the nova peaking on 2020-07-11.76 at 3.7mag (CBET #4812). Considering the latest non-detection by M. A. Phillips on 2020-07-07.79 (>5.5mag), we take the pre-discovery detection by ASAS-SN (Shappee et al. 2014, ApJ, 788, 48; Kochanek et al. 2017, PASP, 129, 104502) on 2020-07-08.171 as the estimate of the eruption date. The nova was spectroscopically confirmed (ATel #13867) and classified as a He/N type (ATel #13874). GeV emission from the nova was detected by Fermi/LAT (ATel #13868). \nWe observed MGAB-V207 with NuSTAR starting on 2020-07-17.98 (ten days after eruption) for a total exposure of 67ks. The nova is detected with SNR~11 at both focal plane modules. The 3.5-78 keV count rate is gradually increasing from 0.01 to 0.02 cts/s over the duration of the NuSTAR observation. The NuSTAR spectrum can be fit by heavily absorbed optically thin thermal plasma emission (APEC) with kT = 6.5 +/-1.5 keV. The unabsorbed 3.5-78 keV flux is 1.1x10^-12 erg/cm^2/s. To obtain a good fit, we had to allow for non-solar abundances of N, O and/or Fe for both absorber and emitter. The choice of the abundances dramatically affects the absorbing column (that is normalized to Hydrogen). The same situation was described earlier for V906 Car by Sokolovsky et al. (2020, arXiv:2007.07885). \nMGAB-V207 was also observed with Swift for a total exposure of 7.9ks between 2020-07-16 (8.5 days post-eruption) and 2020-07-21. Swift/XRT operating in the windowed timing mode (to avoid optical loading) detected no X-ray source with the count rate above 0.05 cts/s (0.3-10 keV). Swift/UVOT had to be blocked due to the high optical brightness of the nova. \nThe X-ray emission observed with NuSTAR is likely produced by plasma heated by shocks deep within the expanding nova shell, which also absorbs soft X-rays. As the ejecta clears, the nova should become detectable for Swift/XRT. We encourage further multiwavelength observations of this nova. \nWe thank the teams of NuSTAR and Neil Gehrels Swift Observatory for rapid scheduling these observations. \nASAS-SN optical lightcurve of MGAB-V207", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Nova", "Galaxy", "Pulsar" ] }, "answerKey": "B" }, { "id": "atel_13980", "message": "Title: Optical outburst detected from the AM CVn binary ASASSN-14mv\nAuthors: G. Ramsay (Armagh Observatory & Planetarium), M. Green (Tel Aviv), P. Woudt (UCT), D. Steeghs (Warwick), P. Groot (Nijmegen), C. Duffy (Armagh), D. K. Galloway (Monash), V. Dhillon (Sheffield), P. O'Brien (Leicester), S. Poshyachinda (Narit), R. Kotak (Turku), L. Nuttall (Portsmouth), R. Breton (Manchester), D. Pollacco (Warwick), E. Thrane (Monash), K. Ackley (Monash), M. Dyer (Sheffield), J. Lyman (Warwick), K. Ulaczyk (Warwick), R. Fender (Oxford), E. Koerding (Nijmegen), on behalf of the GOTO and ThunderKat collaborations.\nDate: 29 Aug 2020; 17:31 UT\nProvenance: Gavin Ramsay (gavin.ramsay@armagh.ac.uk)\nSubjects: Radio, Optical, Cataclysmic Variable\nDescription: Gaia Alerts reported an outburst (Gaia20dyy, AT2020sak) from the AM CVn binary ASASSN-14mv (V490 Gem) on 2020-08-24 19:46:33 UT at G=15.6. This appears to be its first recorded outburst since the event starting 2014-12-29 which peaked at brighter than 12 mag, returning to quiescence (18 mag) approximately 3 months later. It showed a series of re-brightnening, or echo outbursts, starting around 10 days after maximum light. We carried out observations with the Gravitational-wave Optical Transient Observer (GOTO) on La Palma in response to the alert. We made a set of 7x60 s exposures using our B-band (400-510 nm); R-band (580-690 nm) and L-band (400-700 nm) filters, starting at 2020-08-29 05:45 UT. Using the output of the GOTO photometric pipeline we find ASSASN-14mv has preliminary mean magnitudes of B=15.6; R=15.1 and L=15.5 and confirm it is in outburst. We also obtained observations of ASASSN-14mv using 58 antennas of the MeerKAT radio telescope array in South Africa at a central frequency of 1.284 GHz and with a bandwidth of 856 MHz. The observations were obtained on 2020-08-28 from 06:26-08:38 UT. No radio source was detected at the position of ASASSN-14mv with a 3 sigma upper limit of 28.5 microJy. The source is currently visible at low elevation towards morning twilight and we encourage further observations to determine if the re-brightening events are also seen in this current outburst. The Gravitational-wave Optical Transient Observer (GOTO) project acknowledges the support of the Monash-Warwick Alliance; University of Warwick; Monash University; University of Sheffield; University of Leicester; Armagh Observatory & Planetarium; the National Astronomical Research Institute of Thailand (NARIT); Instituto de Astrofísica de Canarias (IAC); University of Portsmouth; University of Turku, and the UK Science and Technology Facilities Council (STFC) (https://goto-observatory.org/). ThunderKAT will run for 5 years and targets X-ray binaries, Cataclysmic Variables, Supernovae and Gamma-Ray Bursts. For further information on this programme please contact Rob Fender and/or Patrick Woudt. We thank the staff at the South African Radio Astronomy Observatory (SARAO) for their rapid scheduling of these observations. The MeerKAT telescope is operated by SARAO, which is a facility of the National Research Foundation, an agency of the Department of Science and Innovation.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Binary system", "Minor body", "Neutron star" ] }, "answerKey": "B" }, { "id": "atel_14130", "message": "Title: Recurrent Nova M31N 2008-12a: discovery of the 2020 eruption\nAuthors: )>, M. J. Darnley (LJMU), A. W. Shafter (SDSU), S. Kafka (AAVSO), S. Williams (Turku) and M. Henze (SDSU), on behalf of the 12a Collaboration\nDate: 31 Oct 2020; 07:32 UT\nProvenance: Matt Darnley (M.J.Darnley@ljmu.ac.uk)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 14131, 14138, 14140, 14141, 14142, 14152, 14158, 15034\nWe report the discovery of the predicted 2020 eruption of the remarkable recurrent M31 nova M31N 2008-12a (see ATels #5607, #6527, #7964, #9848, #11116, #12177, #13269 for earlier detections as well as Darnley et al. 2014, 2015, 2016 and Henze et al. 2014, 2015a, 2015b, 2018, for comprehensive multi-wavelength studies of previous eruptions). \n \nThe nova was clearly detected on 2020 Oct 30.893 (UT) using a single 60s Sloan-like r'-band observation obtained with the 2m fully robotic Liverpool Telescope. The discovery magnitude is 18.39 ± 0.02. We will continue to monitor the nova light curve and strongly encourage additional follow-up observations. \n \nThis is the thirteenth consecutive annual eruption of M31N 2008-12a and this marks the third eruption discovery by the Liverpool Telescope.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Pulsar", "Active galactic nucleus", "Nova", "Exoplanet" ] }, "answerKey": "C" }, { "id": "atel_14275", "message": "Title: GRB 201216C: MAGIC detection in very high energy gamma rays\nAuthors: Oscar Blanch (IFAE-BIST) on behalf of the MAGIC Collaboration\nDate: 17 Dec 2020; 17:23 UT\nProvenance: Oscar Blanch (blanch@ifae.es)\nSubjects: Gamma Ray, >GeV, TeV, VHE, Gamma-Ray Burst\nDescription: Referred to by ATel #: 14277\nOn December 16, 2020, the MAGIC telescopes observed GRB 201216C following the trigger by Swift-BAT and Fermi-GBM (Beardmore et al., GCN 29061, Fermi/GBM team GCN 29063). MAGIC started observations under good conditions about 57 seconds after the GRB onset. The preliminary off-line analyses show an excess above 5 sigma, compatible with the GRB position reported by the Swift and Fermi teams. Refined off-line analyses of the data are ongoing. \n \nWe strongly encourage follow-up observations by other instruments at all wavelengths. \n \nThe MAGIC point of contact for this burst is O. Blanch (blanch@ifae.es). Burst Advocate for this burst is F. Longo (francesco.longo@ts.infn.it). \n \nMAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Observatory Roque de los Muchachos on the Canary island La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Pulsar", "Variable star", "Globular cluster" ] }, "answerKey": "C" }, { "id": "atel_14325", "message": "Title: A very stringent upper limit to the mass-loss rate of the Type Ia SN2021J from e-MERLIN radio observations \nAuthors: M. Perez-Torres (IAA-CSIC, Granada), J. Moldon (IAA-CSIC, Granada; JBCA, Manchester), P. Lundqvist (Stockholm University), J. Bray (JBCA), D. Venkattu (Stockholm) \nDate: 18 Jan 2021; 06:38 UT\nProvenance: Miguel A. Perez-Torres (torres@iaa.es)\nSubjects: Radio, Supernovae\nDescription: Referred to by ATel #: 14595, 15077\nWe report the non-detection at radio wavelengths of the Type Ia SN 2021J discovered on 2021-01-01 11:44:04 at the position RA = 12:26:27.031 DEC = +31:13:20.59 in NGC 4414 (2021TNSTR...1...1E), at a distance of 16.6 Mpc (Kanbur et al. 2003, A&A, 411, 361), and classified as a Type Ia SN on UT 2021-01-04 (ATel #14300). \nWe observed SN 2021J on 2021-01-05 (from 22:45 UT till 07:40 on 2021-01-06) and 2021-01-08 (from 03:25 till 12:30 UT) with the electronic Multi-Element Radio Linked Interferometer Network (e-MERLIN) at a central frequency of 5.1 GHz, and with a bandwidth of 512 MHz. We found no evidence of radio emission from SN 2021J in either epoch above a 3-sigma upper limit of 45 and 60 microJy/beam, respectively, which correspond to upper limits of the monochromatic luminosity of 1.5E25 and 2.0E25 erg/s. Assuming that the first epoch happened 4.0 days after the explosion, the upper limits to the luminosity of SN 2021J correspond to 3-sigma upper limits to the mass-loss rate of the progenitor star of 7.8E-9 and 1.6E-8 solar masses per year at 4.0 days and 7.3 days after the SN explosion, for a presupernova wind of 100 km/s, using the same model as for previous Type Ia SNe (e.g., ATel #12411 for SN 2019np). The value of 7.8E-9 Msol/yr is one of the most stringent upper limits ever, only beaten by those obtained for SN 2011fe, SN 2012cg and SN 2014J, and at the same level as those for SN 2011by, SN 2011ek, SN 2012fr and SN 2012ht. \ne-MERLIN is a National Facility operated by the University of Manchester at Jodrell Bank Observatory on behalf of STFC.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Magnetar", "Quasar", "Black hole" ] }, "answerKey": "A" }, { "id": "atel_14450", "message": "Title: Fermi-LAT detection of gamma-ray flaring activity from the high-redshift FSRQ PKS B1149-084\nAuthors: R. Angioni (SSDC/INFN) on behalf of the Fermi Large Area Telescope Collaboration\nDate: 9 Mar 2021; 22:20 UT\nProvenance: Roberto Angioni (r.angioni90@gmail.com)\nSubjects: Gamma Ray, >GeV, Request for Observations, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 14453\nThe Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed enhanced gamma-ray activity from a source positionally consistent with the flat-spectrum radio quasar PKS B1149-084, also known as 4FGL J1152.3-0839 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 178.071706 deg, Decl. = -8.684254 deg (J2000; Beasley et al. 2002 ApJS, 141, 13), and redshift z=2.37 (Ellison et al. 2001 A&A, 379, 393). \nPreliminary analysis indicates that this source was in an elevated gamma-ray emission state on 8 March 2021, with a daily averaged gamma-ray flux (E>100MeV) of (6.3+/-1.6) X 10^-7 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of about 30 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL). This is the highest LAT daily flux ever observed for this source. The corresponding photon index is 2.7+/-0.3, providing a hint of spectral softening compared with the 4FGL value of 2.38+/-0.06. \nBecause Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. Target of Opportunity observations with the Neil Gehrels Swift Observatory are being proposed. We encourage further multifrequency observations of this source. For this source, the Fermi-LAT contact person is Roberto Angioni (roberto.angioni@ssdc.asi.it). \nThe Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater", "Quasar", "Magnetar", "Neutron star" ] }, "answerKey": "B" }, { "id": "atel_14520", "message": "Title: MAGIC detection of an increased activity from PG 1553+113 in very-high-energy gamma rays\nAuthors: Oscar Blanch (IFAE-BIST), on behalf of the MAGIC collaboration\nDate: 7 Apr 2021; 11:41 UT\nProvenance: Oscar Blanch (blanch@ifae.es)\nSubjects: Gamma Ray, TeV, VHE, Blazar\nDescription: Referred to by ATel #: 15915\nThe MAGIC telescopes have observed an increase in the very-high-energy (VHE; >100 GeV) gamma-ray flux from PG 1553+113 (RA=15:55:43, DEC=11:11:23, J2000.0). The preliminary analysis of the MAGIC data taken on 2021/04/06 (MJD 59310.1), during a regular monitoring of the source, indicates an integral flux of ~0.25% of the flux from the Crab nebula above 150 GeV, which is a factor of ~4 higher with respect to the low-state VHE flux from this source. \n \nPG 1553+113 is a bright VHE blazar with uncertain redshift (z>0.4; Danforth et al. 2010, ApJ 720, 976). It is one of the few blazars with a convincing quasi-periodic emission in the gamma-ray band, as observed by the Fermi-LAT satellite (Ackermann et al. 2015, ApJL 813, L41). In the next months the source is expected to approach a gamma-ray maximum according to the ~2 years periodic modulation. \n \nThe MAGIC observations were performed within the framework of a multi-year, multiwavelength campaign started in 2015. In optical, the source is currently monitored with the Telescopi Joan Oró (Montsec Observatory) as part of the Tuorla Blazar Monitoring Program (https://users.utu.fi/kani/1m/PG_1553+113.html). The long-term lightcurve shows an enhanced optical activity that started already in March, at the beginning of the 2021 monitoring campaign. \nMAGIC observations on PG 1553+113 will continue during the next months and multiwavelength observations are encouraged. The MAGIC contact persons for these observations are Oscar Blanch (blanch@ifae.es), Elisa Prandini (elisa.prandini@unipd.it), and Serena Loporchio (serena.loporchio@ba.infn.it). \n \nMAGIC is a system of two 17m-diameter Imaging Atmospheric Cherenkov Telescopes located at the Canary island of La Palma, Spain, and designed to perform gamma-ray astronomy in the energy range from 50 GeV to greater than 50 TeV.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Accreting object", "Black hole", "Supernova" ] }, "answerKey": "C" }, { "id": "atel_14600", "message": "Title: ZTF optical non-detection of Chandra Fast X-ray Transient XRT 210423\nAuthors: Igor Andreoni (Caltech), Mansi Kasliwal (Caltech), Matthew Graham (Caltech)\nDate: 5 May 2021; 04:14 UT\nProvenance: Igor Andreoni (igor.andreoni@gmail.com)\nSubjects: Optical, X-ray, Gamma-Ray Burst, Transient\nDescription: Referred to by ATel #: 14735\nThe Zwicky Transient Facility (ZTF; Bellm et al., 2019; Graham et al., 2019) observed the field where the Chandra fast transient XRT 210423 (Lin et al., ATel #14599) was found 1588 times, on 820 distinct nights, from the beginning of the survey on 2018 March 17 until 2021 May 4. \n \nWe explored ZTF data at the location of XRT 210423 using the ZTF point-spread-function (PSF) forced photometry service (Masci et al., 2018). No source was detected in individual images and no significant detection was found by binning nightly data in each g-r-i band. \n \nOn 2021 April 23, which is the date of the Chandra discovery of XRT 210423, ZTF observations of the field were not performed. A total of 43 images, taken between 2021 April 23 and 2021 May 4, were successfully processed (19 in g-band, 20 in r-band, 4 in i-band). The table below presents the closest upper limits (5 sigma) available, in each band, before and after 2021 April 23. These upper limits were computed via nightly binning of the flux measured in individual images, processed through the ZTF reduction and image subtraction pipelines at IPAC (Masci et al., 2019). \n \n\\--------------------------------- \nDate (UT) | filter | UL (mag AB) \n\\--------------------------------- \n2021-04-20 | i | >20.8 \n2021-04-21 | g | >21.5 \n2021-04-21 | r | >21.7 \n2021-04-24 | g | >20.5 \n2021-04-24 | r | >20.9 \n2021-05-01 | i | >19.6 \n\\--------------------------------- \n \nThe coordinates of XRT 210423 reported by Lin et al. (ATel #14599) are accurate within 1.0'', which is comparable with the ZTF pixel scale. Therefore it is possible that the result of the PSF forced photometry is affected by the imprecise position of the centroid. To minimize the risk of missing a possible optical source, we visually inspected the difference images acquired after April 23 2021. We did not identify any likely point source within 3'' from the nominal coordinates in individual images, images nightly stacks, and stacks of all the images available. \n \n \nBased on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-2034437 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, Deutsches Elektronen-Synchrotron and Humboldt University, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, and IN2P3, France. Operations are conducted by COO, IPAC, and UW.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object, Black hole, Star and stellar system, Nova, Supernova, Variable star", "Accreting object, Black hole, Neutron star, Nova, Supernova, Galaxy", "Accreting object, Active galactic nucleus, Neutron star, Nova, Supernova, Variable star", "Accreting object, Black hole, Neutron star, Nova, Supernova, Variable star" ] }, "answerKey": "D" }, { "id": "atel_14650", "message": "Title: A Disk Wind in the Black Hole Candidate MAXI J1803-298\nAuthors: J. M. Miller, M. T. Reynolds (Univ. of Michigan)\nDate: 21 May 2021; 14:43 UT\nProvenance: Jon Miller (jonmm@umich.edu)\nSubjects: X-ray, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 14994\nWe report on recent observations of the black hole candidate MAXI J1803-298 obtained with the Neil Gehrels Swift Observatory. The source shows strong X-ray flux dips, indicative of a viewing angle close to the plane of the accretion disk (#14609). Accretion disk winds in stellar-mass black holes are known to be equatorial (e.g. Miller et al. 2008, Ponti et al. 2012), so a disk wind is anticipated in this system as it shifts into a soft spectral state.\nSwift observations of MAXI J1803-298 obtained on 2021 May 20-21 show evidence of absorption in the Fe K band. We derived windowed timing mode XRT spectra after excluding the central 4-6 pixels in order to limit photon pile-up. The individual spectra were combined in order to improve sensitivity, and binned. The summed 6.3 ks spectrum can be fit with a combination of disk blackbody (kT = 1.1 keV) and power-law components, though the power-law is not strongly required and may partially arise owing to pile-up effects. The 0.5-10 keV absorbed flux is 1.2 E-8 erg/cm2/s (roughly 0.5 Crab).\nThe Fe K band includes a strong, broad emission line with a blue extent consistent with a high inclination, and unresolved absorption consistent with He-like Fe XXV and H-like Fe XXVI lines. At the resolution afforded by the XRT, the modest velocity shifts typical of disk winds are difficult to measure, and standard corrections for detector effects at high count rates may over-correct the energy scale. The data do not rule out static absorption but it is more likely that the absorption is tied to an outflow that can be confirmed at high resolution. Exploratory fits with photoionized absorption models suggest a column density of N_H = 2-3 E+22 cm^-2 and an ionization of log xi = 4.0-4.5. These values are more consistent with the winds found in H 1743-322, 4U 1630-472, and IGR J17091-3624 than the winds seen in GRO J1655-40, GRS 1915+105, and V404 Cyg (e.g., King et al. 2012, 2015; Miller et al. 2015; Trueba et al. 2019).\nWe thank Brad Cenko and the Swift team for granting and executing monitoring observations of MAXI J1803-298. In future work, we will examine the multi-wavelength evolution of this source.\nReferences:\nKing, A. L., et al., 2012, ApJ, 746, L20 \nKing, A. L., et al., 2015, ApJ, 813, L37 \nMiller, J. M., et al., 2008, ApJ, 680, 1359 \nMiller, J. M., et al., 2015, ApJ, 814, 87 \nPonti, G., et al., 2012, MNRAS, 422, L11 \nTrueba, N., et al., 2019, ApJ, 886, 104", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Neutron star", "Minor body, Accreting object", "Black hole, Accreting object", "Interstellar medium, Accreting object" ] }, "answerKey": "C" }, { "id": "atel_14750", "message": "Title: AT 2021rno: spectroscopic confirmation and likely third eruption of the recurrent nova M31N 1923-12c\nAuthors: M. J. Darnley (LJMU), S. C. Williams (Turku)\nDate: 4 Jul 2021; 09:35 UT\nProvenance: Matt Darnley (M.J.Darnley@ljmu.ac.uk)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 14755\nAT 2021rno reports the discovery of a transient event coincident with the position of the known M31 recurrent nova M31N 1923-12c (also M31N 2012-01b, see ATel #3914). \nA Liverpool Telescope SPRAT spectrum collected on 2021 Jul 04.16 (UT) shows strong Balmer emission lines with a FWHM of 5900 ± 300 km/s. \nThe spectrum also shows tentative evidence for He I emission lines. This would be consistent with the He/N designation of the 2012 eruption (ATel #3914). \nThe profile of the Hα and Hβ lines are highly asymmetric and may indicate that they are still optically thick. \nThis spectrum confirms that AT 2021rno is a nova eruption and the implication is that M31N 1923-12c has a recurrence period as short as 9 years. This would be more frequent than the Galactic recurrent U Sco and adds to the large population of 'rapid recurrent novae' (11 of 19 known M31 recurrent novae have recurrence periods ≤ 10 years) in M31 (Darnley & Henze, 2020)", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova, Neutron star", "Nova, Variable star", "Nova, Galaxy", "Exoplanet, Variable star" ] }, "answerKey": "B" }, { "id": "atel_14800", "message": "Title: SRGe J131014.2+444315 - a tidal disruption event at early phase\nAuthors: M. Gilfanov (IKI, MPA), S. Sazonov (IKI), P. Medvedev (IKI), G. Khorunzhev (IKI), R. Sunyaev (IKI, MPA), Y. Yao (Caltech), S. R. Kulkarni (Caltech), Y. Sharma (Caltech)\nDate: 20 Jul 2021; 08:29 UT\nProvenance: Marat Gilfanov (gilfanov@iki.rssi.ru)\nSubjects: Optical, X-ray, Tidal Disruption Event\nDescription: On June 6-7, 2021, in the course of its third all-sky survey, SRG/eROSITA discovered a new X-ray source SRGe J131014.2+444315 with a very soft spectrum with the blackbody temperature of 50+/-10 eV and the 0.3-2 keV flux of ~3.8e-13 erg/s/cm^2. The source was not detected during two previous scans of this region 6 and 12 months earlier, with an upper limit of ~1/20 of its current flux. \nOn July 6, the source was observed with Keck/LRIS, which shown narrow galaxy lines at z=0.199 on top of a blue continuum, and a broad emission complex around He II 4686A. The Keck spectrum is reminiscent of helium-rich tidal disruption events that are bright in UV/optical. ATLAS forced photometry data showed that optical brightening of the source started at some time between June 15 and June 27, roughly 1—2 weeks after the discovery of the X-rays source. \nSwift XRT observations on July 13 and 17 revealed that the source continued its rise in X-rays and reached the level of 7.2e-13 erg/s/cm2, with a consistently soft spectrum, kTbb=64+/-6 eV. UVOT observations suggest that this object is bright in the UV (absolute magnitude in UVW2=-20.4). \nRemarkably, this is the first event among optically active SRG/eROSITA TDEs, which was detected in X-rays before any optical activity was identified, suggesting that it was caught at early phase. Swift will continue monitoring of the source, follow-up visits with Keck are also planned. Further observations of the source at various wavelengths are of importance.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star, Black hole", "Quasar, Black hole", "Accreting object, Galaxy", "Accreting object, Black hole" ] }, "answerKey": "D" }, { "id": "atel_14900", "message": "Title: Near-Sun Photometric Follow-up of the Rapidly-Fading Sun-like Star ASASSN-21qj\nAuthors: D. D. Balam (DAO/National Research Council of Canada), C. E. Spratt (UVic-Ret), D. W. E. Green (CBAT) and Tyler Hrynyk (Canadian Space Agency)\nDate: 6 Sep 2021; 17:28 UT\nProvenance: David D. Balam (cosmos@uvic.ca)\nSubjects: Optical, Star, Transient, Variables\nDescription: We have taken advantage of the near-sun capabilities of the Canadian NEOSSat orbiting telescope (https://www.cadc-ccda.hia-iha.nrc-cnrc.gc.ca/en/neossat/) to perform follow-up photometry of the optical transient ASASSN-21qj (#14879), reported as under-going a rapid dimming event by the ASSASN survey, Shappee et al. 2014,(https://ui.adsabs.harvard.edu/abs/2017PASP..129j4502K/abstract) at relatively small solar elongation. The spacecraft was tasked to obtain a series of 60 second duration images over three orbits of the spacecraft that were co-added to yield image stacks of 2640, 3480 and 2460 seconds duration. We have performed differential aperture photometry using an aperture of 30 seconds of arc using the Gaia catalogue star Gaia DR2 5539975927391545344 (http://simbad.u-strasbg.fr/simbad/sim-id?Ident=%407439336&Name=TYC%207660-897-1&submit=submit) as a secondary standard in the field. The NEOSSat is an un-filtered detector, however, the sensitivity curve of the back illuminated E2V 47-20 CCD is similar to the Gaia G filter response curve. Our measurements yield the following magnitudes: UT 2021 Sept. 3.037 G_NEOSSat = 14.27(+/- 0.07), Sept. 3.169 G_NEOSSat = 14.15 (+/- 0.06) and Sept. 3.236 G_NEOSSat = 13.85 (+/- 0.07). ASASSN-21qj was 0.4 magnitudes fainter than its quiescent brightness before the field became Sun constrained on UT 2021-06-29. On UT Aug. 26 the ASSASN team reported the object as 1.5 magnitudes fainter and 24 hours later 2.2 magnitudes fainter than it quiescent brightness and dimming. Our measurements show that the star has brightened in the week since the ASASSN measurements. In addition, we have seen a brightening trend over the 7 hours of coverage of our orbiting sensor.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Exoplanet", "Active galactic nucleus", "Star and stellar system" ] }, "answerKey": "D" }, { "id": "atel_14975", "message": "Title: Spectroscopic classification of AT2021aagy/ZTF21acernhn\nAuthors: Stephanie Figuereo, Kevin McKinnon, Rafael Nunez, Puragra Guhathakurta (UCSC), Monika Soraisam (NOIRLab), Chien-Hsiu Lee (NOIRLab)\nDate: 15 Oct 2021; 21:39 UT\nProvenance: Monika Soraisam (soraisam@illinois.edu)\nSubjects: Optical, Supernovae, Transient\nDescription: We report the spectroscopic observation of the following transient from the SALVATION project (ATel #13952). It was flagged from the ZTF public alert stream by the ANTARES alert-broker. The spectrum was obtained on 2021 October 14 UT with the Kast double spectrograph on the Shane 3-m telescope at Lick Observatory. \n \n \n Name | IAU Name | RA (J2000) | Dec (J2000) | z | Type | Phase \n ZTF21acernhn | AT2021aagy | 05h23m57s | +04d22m33s | 0.065 | SN-Ia | -2 to 2 days \n Note: \n Classification for the supernova was performed with DASH (Muthukrishna et al. 2019, arXiv:1903.02557). \n Light curve can be accessed at https://antares.noirlab.edu/loci/ANT20214bajq (ZTF21acernhn).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Galaxy", "Supernova", "Black hole" ] }, "answerKey": "C" }, { "id": "atel_15100", "message": "Title: Significant optical decay and brightening in blazar PKS 0735+17 coincident with IceCube-211208A\nAuthors: K. Zhirkov, V. Lipunov, E. Gorbovskoy, P. Balanutsa, A. Kuznetsov, O. Gress, G. Antipov, D. Vlasenko, N. Tiurina, D. Zimnukhov, V. Senik, V. Topolev, A. Chasovnikov, E. Minkina, V. Grinshpun, D. Cheryasov, Ya. Kechin, Ya. Kechin, T. Pogrosheva, V. Shumkov (Lomonosov MSU), R. Rebolo, M. Serra(IAC), D. A. H. Buckley (SAAO), N. M. Budnev (ISU, API), R. Podesta, C. Lopez, F. Podesta, C. Francile (OAFA), A. Tlatov, D. Dormidontov (KSS, Pulkovo observatory), A. Gabovich (BSPU)\nDate: 10 Dec 2021; 11:15 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Neutrinos, Request for Observations, AGN, Blazar\nDescription: Referred to by ATel #: 15108, 15112, 15143, 15290\nMASTER Global Robotic Net (Lipunov et al., \"MASTER Global Robotic Net\", Advances in Astronomy, 2010, 30L) \nreports on the significant optical decay and brightening in a blazar PKS 0735+17 \nand on a significant detection of a lower limit on the degree of linear polarization. \nIn Atel #15098 we reported on the high optical state of PKS 0735+17. \nTo confirm whether or not this object might be the source of IceCube-2112108A we conducted follow-up observations at MASTER-IAC, MASTER-SAAO, MASTER-OAFA and MASTER-Kislovodsk. \nAfter analyzing our observations we discovered that PKS 0735+17 significantly decayed 4 days before the neutrino and brightened to the past level several hours after the neutrino with no significant variability afterwards. \nConsidering that TXS 0506+056, source of IceCube-170922A, showed a similar picture (Lipunov et al, ApJL, 896, L19, 2020) albeit in a shorter timescale(several hours), it is likely that PKS 0735+17 is a source of IceCube-211208A. \nPolarization observations were made by MASTER-IAC during the night of 2021-12-10. We report on a significant detection of a lower limit on the degree of linear polarization . \nJudging from these and from the detection of enhanced emission from the blazar by Fermi-LAT(Atel #15099) we conclude that the BL Lac object PKS 0735+17 is a likely source of IceCube-211208A even though it is slightly outside the 90% of the localization error-box (GCN #31191 , https://gcn.gsfc.nasa.gov/other/icecube_211208A.gcn3). \nMultiwavelength observations are highly encouraged.\nMASTER Global Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Black hole", "Active galactic nucleus, Globular cluster", "Active galactic nucleus, Interstellar medium", "Active galactic nucleus, Circumstellar disk" ] }, "answerKey": "A" }, { "id": "atel_15180", "message": "Title: MASTER OT J153539.77-461415.4 outburst detection with amplitude >5.6m in OAGH observatory\nAuthors: K. Zhirkov, V. Lipunov, V. Kornilov, A. Kuznetsov, E. Gorbovskoy, G. Antipov, D. Vlasenko (Lomonosov MSU), L. Carrasco, J. R.Valdes, V. Chavushyan, V. M.Patino Alvarez, J. Martinez, A. R.Corella, L. H.Rodriguez (INAOE, OAGH), P. Balanutsa, V. Senik, Ya. Kechin, Yu. Tselik, T. Pogrosheva, V. Shumkov, E. Minkina, A. Chasovnikov, V. Topolev, V. Grinshpun, D. Kuvshinov, D. Zimnukhov, D. Cheryasov (Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C. Lopez, F. Podesta, C. Francile (Observatorio Astronomico Felix Aguilar OAFA), R. Rebolo, M. Serra-Ricart (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), O. A. Gress, N. M. Budnev (Irkutsk State University, API), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), A. Gabovich, V. Yurkov (Blagoveschensk State Pedagogical University)\nDate: 25 Jan 2022; 16:44 UT\nProvenance: Vladimir Lipunov (lipunov2007@gmail.com)\nSubjects: Optical, Request for Observations, Cataclysmic Variable, Transient, Variables\nDescription: MASTER OT J153539.77-461415.4 discovery - dwarf nova outburst with amplitude >5.6m \nFirst optical transient, detected in MASTER-OAGH (INAOE, Mexico). \nMASTER-OAGH of Lomonosov MSU MASTER Global Robotic Net \nwas mounted in December 2021 in Mexico, Guillermo Haro Astrophysics Observatory of the National Institute of Astrophysics, Optics and Electronics. \nMASTER-OAGH consists of twin 40cm telescope, equipped with BVRI,PP filters, 4-8 square degrees field of view and has own real-time reduction and auto-detection system (Lipunov et al., MASTER Global Robotic Net, Advances in Astronomy, 2010, 30L). \nWe use the same scientific equipment at every MASTER observatory, it means the same photometry system and possibility to use own archive images since 2006y. for analysis. \nDuring Fermi trigger 664738369 (Ttrigger=2022-01-24 17:32:44.36UT, R.A.,Dec.(2000)=15h 36m 43s, -46d 38' 23\", Rstat=5.08deg.) inspection \nMASTER-OAGH auto-detection system discovered OT source at (RA, Dec) = 15h 35m 39.77s -46d 14m 15.4s at 2022-01-25.50915 UT (the second image was at 2022-01-25.54848UT with the same m_OT). \nThe OT unfiltered magnitude is 14.4m (mlim=17.6). \nTaking into account the trigger time this OT should not be connected with GRB optical counterpart. \nThe OT is seen in 3 images. There is no minor planet at this place. \nWe have reference images in MASTER archive at 2018-09-12.91464 UT with unfiltered mlim=17.8m, at 2021-02-03 23:14:29UT with unfiltered mlim=17.6, at 2016-07-09 18:19:42UT with mlim=19m . \nThere is no OT sources in Gaia,USNO inside 4\" (22m limit in history). There is VISTA source in 0.7\". \nSpectral observations are required. \nThe discovery and reference images are available at: \nhttp://master.sai.msu.ru/static/OT/MASTEROTJ153539.77-461415.4.jpg \nMASTER Global Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Star and stellar system", "Minor body", "Binary system" ] }, "answerKey": "A" }, { "id": "atel_15270", "message": "Title: SALT spectroscopic follow up of the optical transient Gaia22alz (AT2022bpq)\nAuthors: J. Brink (SAAO/UCT), E. Aydi (MSU), D. A. H. Buckley (SAAO/UCT), L. Chomiuk (MSU), A. Kawash (MSU), M. Orio (UoW/INAF), J. Mikolajewska (NCAC), K. V. Sokolovsky (MSU), J. Strader (MSU), K. Z. Stanek, C. S. Kochanek, M. R. Smith (OSU), and B. J. Shappee (Univ. of Hawaii)\nDate: 11 Mar 2022; 14:58 UT\nProvenance: Elias Aydi (aydielia@msu.edu)\nSubjects: Optical, Cataclysmic Variable, Nova, Star, Transient, Variables\nDescription: Referred to by ATel #: 15355\nWe report on follow up observations of the optical transient Gaia22alz (AT2022bpq), which was discovered by Gaia on 2022-02-04.2 UT at G = 16.87 (https://www.wis-tns.org/object/2022bpq). There is a Gaia EDR3 source matching the transient position, with an average G-magnitude of 18.3. \nPhotometry from the All Sky Automated Survey for SNe (ASAS-SN; Shappee et al. 2014, ApJ, 788, 48S and Kochanek et al. 2017PASP, 129, 4502) shows that the outburst started around 2022-01-25 and has been rising slowly in brightness since then, reaching a g-magnitude of around 15.2 on 2022-03-09 (https://asas-sn.osu.edu/sky-patrol/coordinate/3471191f-7745-41dc-8576-efc37ceefda0). \nOn 2020-03-10 we obtained a 300 s spectrum using the Robert Stobie Spectrograph (RSS; Burgh et al. 2003, SPIE, 4841, 1463), mounted on the 11m Southern African Large Telescope as part of the SALT Large Science Program on Transients. The spectrum is dominated by emission lines of Balmer, He II, He I, C IV, and the Bowen blend. The Balmer lines are characterized by a relatively narrow central emission (FWHM ~ 400-500 km/s), with a broad emission base characterized by a FWZI > 5000 km/s. The equivalent width (EW) of He II line at 4686 A is approx 1.5 times that of Hbeta. Based on the spectrophotometric observations, the transient might be an unusual disk instability (dwarf nova) outburst in a cataclysmic variable (CV) system, but further follow up are required to reach a definite classification. The slow rise of the optical light curve resembles the slowly evolving outbursts of the CV systems GK Per, V1017 Sgr, and V1047 Cen. \nFollow up observations are encouraged.\nSpectrum", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Variable star", "Near-Earth object", "Pulsar" ] }, "answerKey": "B" }, { "id": "atel_15350", "message": "Title: Changing Look NGC 3822 continues the outburst\nAuthors: V. Oknyansky (Sternberg Astronomical Institute, Moscow), N. Ikonnikova, M. Burlak, S. Tsygankov (Tuorla Observatory, Piikkio, Finland)\nDate: 27 Apr 2022; 07:17 UT\nProvenance: Victor Oknyansky (oknyan@mail.ru)\nSubjects: Optical, AGN, Black Hole, Transient\nDescription: The discovery of the outburst in the nucleus of NGC3822 and the Changing-Look AGN classification were reported in ATel #15280 (see details there). Our optical UBV photometry shows that the activity of NGC 3822 is going on and that the Changing-Look nucleus is now brightening significantly. \nWe have obtained UBV CCD photometry with the 0.6-m telescope of the SAI Caucasus Mountain Observatory for 9 dates during 21 March – 24 April 2022 . The used aperture is 10 arcsec and the U magnitudes are reduced to the U system of the UVOT Swift (using observations which were done on the same dates). From our photometry the brightness of the NGC 3822 changed from U=15.15+/-0.02 (21th March) to U=14.93 +/- 0.02 (21th April) and then moved a little bit down to U=14.97+/-0.02 (24th April). \nThis work has been supported in part by M. V. Lomonosov Moscow State University Development Program.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Galaxy", "Active galactic nucleus", "Star and stellar system" ] }, "answerKey": "C" }, { "id": "atel_15425", "message": "Title: NICER detects 528 Hz pulsations and a thermonuclear X-ray burst from MAXI J1816-195\nAuthors: P. M. Bult (NASA/GSFC), M. Ng (MIT), W. Iwakiri (Chuo U.) D. Altamirano (University of Southampton), D. Chakrabarty (MIT), K. C. Gendreau, T. E. Strohmayer, Z. Arzoumanian (NASA/GSFC), A. Sanna (University of Cagliari), S. Guillot (IRAP/CNRS), P. S. Ray (NRL), T. Mihara, T. Enoto (RIKEN), J. Homan (Eureka Scientific), E. C. Ferrara (UMCP, NASA/GSFC)\nDate: 8 Jun 2022; 23:19 UT\nProvenance: Peter Bult (p.m.bult@nasa.gov)\nSubjects: X-ray, Request for Observations, Binary, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 15426, 15427, 15431, 15437, 15445, 15458, 15470, 15471, 15484, 15769\nFollowing the MAXI/GSC detection of a new X-ray transient, MAXI J1816-195 (ATel #15418), NICER performed multiple pointings to localize the source beginning at 2022-06-07 14:32 (UTC). Starting from the nominal coordinates reported by MAXI, NICER performed a series of offset pointings with 60 s exposure for each. A preliminary source position was obtained at R.A. = 274.2205 deg, Dec = -19.627 deg (J2000), with 3 arcmin radius uncertainty set by the NICER field of view. This position is consistent with the localization of the object as determined with Swift/XRT (ATel #15421). \nAfter performing our raster scan, we obtained a 1.2 ks pointed observation on the best NICER position starting at 7:35 UTC on June 8. The average source count-rate was 470 ct/s in the 0.5-10 keV energy band. We searched this observation for the presence of coherent pulsations, finding a significant (6 sigma, single trial) signal at 528.6 Hz (using photons in the 1-10 keV range). This detection shows that MAXI J1816-195 is a neutron star and a new accreting millisecond X-ray pulsar. \nWe collected another 1.4 ks exposure starting on 18:26 UTC June 8 using the Swift/XRT coordinates. At this time the source intensity had increased to 560 ct/s, and pulsations could again be observed at >6 sigma significance. Additionally, we observed a thermonuclear X-ray burst, with a peak bolometric blackbody flux of ~4 × 10-8 erg/s/cm2. We did not observe evidence of photospheric radius expansion. Assuming the empirical Eddington luminosity of 3.8 × 1038 erg/s (Kuulkers et al. 2003, A&A 399, 663), our flux measurement places an upper limit on the source distance of 9 kpc. No burst oscillations were detected at the reported pulse frequency. \nA full pulsar timing analysis is currently underway and will be circulated as more data become available. Additional multiwavelength follow-up is strongly encouraged. \nNICER is a 0.2-12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Pulsar", "Accreting object, Pulsar", "Neutron star, Quasar", "Variable star, Pulsar" ] }, "answerKey": "A" }, { "id": "atel_15500", "message": "Title: SMC X-2 outburst reaches 1E38 erg/s\nAuthors: M. J. Coe (Soton), J. A. Kennea (PSU), P. A. Evans (Leicester), D. A.H. Buckley (SAAO), L. J. Townsend (SALT), I. Monageng (SAAO)\nDate: 5 Jul 2022; 09:00 UT\nProvenance: Malcolm Coe (mjcoe@soton.ac.uk)\nSubjects: Optical, X-ray, Binary, Neutron Star, Transient\nDescription: More than 3 weeks after its first detection by S-CUBED (ATel #15434) SMC X-2 continues to brighten in the X-rays. The most recent observations by Swift XRT on 3 July 2022 indicate it has now reached 1E38 erg/s and still getting brighter. Our previous quoted value in ATel #15434 of 3E35 erg/s was incorrect, it should have been 2E37 erg/s. Hence it is exhibiting an unusually slow brightening for what appears to be a Type II outburst (its binary period is 18.6d). Normally a Type II outburst from a Be/X-ray binary would rapidly peak in just a few days. \nAn optical red spectrum was obtained using SALT on 3 July 2022 revealed the H alpha line in emission, characteristic of these Be stars in such binary systems. The measured H alpha equivalent width was 5A, almost identical to a previous measurement taken at the SAAO 1.9m telescope in November 2013 when the source was in quiescence. This small, unchanged value indicates little or no recent growth in the circumstellar disk, yet another puzzling feature of this outburst. \nSwift XRT will continue to monitor SMC X-2 throughout this unusual extended outburst.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Circumstellar disk", "Neutron star, Active galactic nucleus", "Binary system, Binary system", "Neutron star, Binary system" ] }, "answerKey": "D" }, { "id": "atel_15575", "message": "Title: Swift Follow-up of 4U 1630-47 in Outburst\nAuthors: Jiachen Jiang (Cambridge), John Tomsick (UCB), Honghui Liu (Fudan Uni.), Andrew Fabian (Cambridge), Riley Connors (Caltech), Javier Garcia (Caltech), Jeremy Hare (Goddard)\nDate: 27 Aug 2022; 17:01 UT\nProvenance: Jiachen Jiang (jj447@cam.ac.uk)\nSubjects: X-ray, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 15924, 15988\n4U 1630-47 is a recurrent X-ray transient first discovered by Uhuru. Although some details of the binary system remain uncertain, its X-ray spectral and timing behaviours suggest a black hole candidate as the nature of the compact accretor. This object recently started a new outburst on 28 July 2022 as alerted by MAXI (ref). The MAXI monitoring program shows that the X-ray intensity (2-20 keV) reached the peak on 21 Aug 2022 at 0.8 cts/cm2/s and has been decaying since then. The daily average MAXI count rate is 0.66 cts/cm2/s on 24 Aug. The X-ray hardness defined as the MAXI count rate ratio between the 4-10 and 2-4 keV bands increased from 0.93 on 21 Aug to 1.18 on 24 Aug. We requested the first Swift observation of 4U 1630-472 during this outburst on 25 Aug. The XRT was operated in the Window Timing mode and received an average count rate of 29 cts/s. The XRT spectrum is best described by an absorbed disk blackbody model (diskbb). The line-of-sight column density is 7.72+/-0.14e22 cm-2. The inner temperature of the disk blackbody is 1.51+/-0.03 keV and the normalization parameter is 110+/-10. The 0.5-10 keV absorbed (unabsorbed) flux of this object is 4.03e-9 (1.14e-8) erg/cm2/s. We thank the Swift PI Brad Cenko for approving this ToO request. Ref: http://maxi.riken.jp/alert/novae/9788849996/9788849996.htm. \n4U 1630-47 MAXI page", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Galaxy", "Binary system", "Accreting object" ] }, "answerKey": "A" }, { "id": "atel_15700", "message": "Title: ZTF detection of the probable nova in M31 AT 2022yax\nAuthors: A. Casasbuenas Corral, G. Aznar Menargues, Y. Calatayud Borras, M. Cervera Cortes, I. Cortes-Perez, J. del Socorro Prieto, M. Delgado Mancheno, A. Ferrer I Burjachs, R. Flores le Roux, D. Galan Dieguez, S. Geraldia Gonzalez, P. Grebol Tomas, S. Navarro Umpierrez, A. Pelaez Torres, E. Reyes Rodriguez, P. Sosa Guillen, A. Vielba Trillo (ULL), E. Esparza-Borges, and I. Perez-Fournon (IAC and ULL)\nDate: 19 Oct 2022; 19:43 UT\nProvenance: Ismael Perez-Fournon (ipf@iac.es)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 15706\nWe report the ZTF detection of the probable nova in M31 AT 2022yax (ZTF22abnrgno) that was discovered by Horti-David, Sarneczky, and Vinko (Konkoly Observatory) and reported to TNS. The ZTF position from a single r-band detection on 2022-10-19 04:43:03 UT is R.A. = 00:43:45.854, Decl. = +41:15:58.61 (equinox 2000.0) and the ZTF r-band magnitude is 19.047 +/- 0.072. We encourage photometric and spectroscopic follow-up observations. Based on Zwicky Transient Facility (ZTF, Bellm et al. 2019) observations processed through the Lasair (Smith, Williams, Young et al. 2019) ALeRCE (Forster et al. 2020) and ANTARES (Matheson et al. 2021) brokers. \nZTF light curve from Lasair", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Repeater", "Nova", "Stellar evolution" ] }, "answerKey": "C" }, { "id": "atel_15810", "message": "Title: AstroSat UVIT observations of the 2022 outburst of Recurrent Nova M31N2008-12a\nAuthors: Judhajeet Basu (IIA), Sudhanshu Barway (IIA), G. C. Anupama (IIA), K. P. Singh (IISER Mohali)\nDate: 15 Dec 2022; 08:08 UT\nProvenance: Sudhanshu Barway (sudhanshu.barway@iiap.res.in)\nSubjects: Ultra-Violet, Nova\nDescription: Referred to by ATel #: 15902\nWe report the detection of the 2022 outburst of the recurrent nova M31N2008-12a (ATel #15786, #15787, #15788, #15789, #15790, #15795, #15797, #15798, #15802 ) with the 37.5 cm Ultra Violet Imaging Telescope (UVIT) on board AstroSat. The source was clearly detected at a threshold of > 5 sigma with FUV CaF2 filter centred at 148.5 nm with a width of 50 nm. \nM31N2008-12a was observed during 6 orbits of AstroSat. Orbit-wise images were stacked to obtain an image with net exposure of 7872 seconds. The recurrent nova was detected at an AB magnitude of 20.578 +/- 0.050 on 2459920.736 JD, around 4.5 days after the outburst. Detailed analysis is underway. \nUVIT L1 data was reduced using CCDLAB (Postma and Leahy, 2017) and PSF photometry was performed using standard IRAF procedures. \nWe thank the AstroSat team for their positive response to our ToO request to observe M31N2008-12a. We also thank members of ISSDC at ISRO and UVIT-POC at IIA for making the data available at the earliest.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Pulsar", "Supernova", "Nova", "Star and stellar system" ] }, "answerKey": "C" }, { "id": "atel_15870", "message": "Title: The Blazar TON 0599 is now in a particularly bright state in the optical as well\nAuthors: A. Scherbantin, K. Mannheim (all Universitaet Wuerzburg), E. Ankara, N. Bader, L. Bertsch, M. Daig, O. Domann, K. Heidemann, M. Heidemann, F. Hemrich, B. Horst, F. Kees, L. Kimmel, D. Kuberek, R. Steineke, L. Waller, D. Reinhart, N. Zottmann, M. Feige, C. Lorey (all Friedrich-Koenig-Gymnasium / Hans-Haffner-Sternwarte), D. Elsaesser (TU Dortmund)\nDate: 21 Jan 2023; 12:00 UT\nProvenance: Dominik Elsaesser (dominik.elsaesser@tu-dortmund.de)\nSubjects: Optical, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 15872, 15873, 15875, 15893\nSince mid-January, the flat-spectrum radio quasar Ton 0599 (4C 29.45, PKS 1156+295; ICRS coordinates (ep=J2000): RA 11 59 31.834 DEC +29 14 43.827, z=0.7) has been showing strong activity in both the x-ray (ATel # 15854) and gamma-ray (ATel #15853; #15859) spectral bands. \nWhile this object displayed optical brightness values in the range between 15.5 and 14.2 mag (R-band) in the last quarter of last year, we were able to measure a peak brightness of 13.373 mag in the R-band in the night from 18 January 2023 to 19 January 2023. \nSuch brightness values in the optical regime are comparable to the strong outbursts of June 2022 (R-band: 13.39 mag; ATel #15441) and January to July 2021 (R-band 14.9 to 13.5 mag; ATel #14353; #14391; #14547; #14696; #14727; #14775), and earlier flares in 2012 (ATel # 4051), 2015 (ATel # 7474), 2017 (ATel # 10948; # 10949) and 2018 (ATel # 11624). \n \n \nHere we report the following values of TON 0599 in the R-Band: \n \nJD 2459963.6294: 13.382 (0.016) \nJD 2459963.6574: 13.373 (0.004) \nJD 2459963.6713: 13.377 (0.004) \nJD 2459965.6827: 13.634 (0.075) \nJD 2459965.7213: 13.586 (0.007) \nJD 2459965.7304: 13.556 (0.008) \nJD 2459965.7556: 13.580 (0.015) \n \n \nDue to the gloomy wintry weather, we were unfortunately unable to carry out higher cadence measurements of this object, and will probably not be able to do so in the next few days either. Therefore, we strongly recommend further measurements of this object. \n \n \nThese measurements were carried out as part of the long-term AGN monitoring program of the Naturwissenschaftliches Labor fuer Schueler am Friedrich-Koenig-Gymnasium (FKG), the Universitaet Wuerzburg, and the TU Dortmund University with the 0.5m CDK astrograph at the school and university observatory Hans-Haffner-Sternwarte in D-97265 Hettstadt (Germany). \nNaturwissenschaftliches Labor fuer Schueler am Friedrich-Koenig-Gymnasium", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system, Quasar", "Active galactic nucleus, Quasar", "Active galactic nucleus, Accreting object", "Active galactic nucleus, Neutron star" ] }, "answerKey": "B" }, { "id": "atel_15930", "message": "Title: POLARIMETRIC RESULTS OF B2 1308+326\nAuthors: Jincen Jose, Suvendu Rakshit, Shivangi Pandey (ARIES), Amitesh Omar (IIT Kanpur)\nDate: 6 Mar 2023; 08:50 UT\nProvenance: Suvendu Rakshit (suvenduat@gmail.com)\nSubjects: Optical, AGN, Blazar\nDescription: Referred to by ATel #: 15931\nAuthors: Jincen Jose, Suvendu Rakshit, Shivangi Pandey (ARIES), Amitesh Omar (IIT Kanpur) The blazar B2 1308+326 (ICRS coords. (ep=J2000): RA 13 10 28.664 Dec +32 20 43.774, (z=0.996)) has been noted to undergo optical variability in recent years (reported R-mag; ATel #15441; ATel #15447; ATel #15515; ATel #15895). At MJD = 59976.0975 (2023-02-09) Atel #15895, reported that value was R=13.757 +/- 0.004. Then, on 2023-02-17, we performed an imaging-polarimetric observation of the blazar. The results are shown below. __________________________________ | MJD | r- mag | error(mag)| |---------------------------------| |59988.19476 | 14.047 | 0.017 | |59988.19895 | 13.904 | 0.017 | |_________________________________| ______________________________________________ | MJD | p (%) | PA (deg) | |----------------------------|----------------| | 59988.19 | 17.121 +- 0.002 | 54.36 +- 0.41 | |_____________________________________________| note: no correction over the degree of polarisation was done. The observation was carried out under instrument verification observations using a polarimeter setup under commissioning in the ARIES Devasthal Faint Object Spectrograph and Camera (ADFOSC; Omar et al. 2019 current science 116 1472) at 3.6-meter Devsthal Optical Telescope of ARIES, Nainital, India. Partial support of SRG-SERB, DST, New Delhi through SRG grant number SRG/2021/001334 is acknowledged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Neutron star", "Black hole", "Exoplanet" ] }, "answerKey": "C" }, { "id": "atel_15990", "message": "Title: Possible new nova or dwarf nova outburst\nAuthors: Paul Groot (Radboud University, UCT, SAAO), Paul Vreewsijk(Radboud), Kira Hanmer (UCT, SAAO, SARAO)\nDate: 15 Apr 2023; 10:59 UT\nProvenance: Paul Groot (p.groot@astro.ru.nl)\nSubjects: Optical, Binary, Cataclysmic Variable, Nova, Transient\nDescription: Paul Groot (Radboud/UCT/SAAO), Paul Vreeswijk (Radboud), Kira Hanmer (UCT/SARAO) and Cole Johnston (Radboud), on behalf of the MeerLICHT consortium, report the discovery of a new nova or dwarf nova variable, MLT J130353.92-644710.1, located at RA = 13:03:53.92, Dec = -64:47:10.1 (ICRS), with a 1-sigma location uncertainty of 0.07 arcsec in each coordinate. The source was found to be in outburst with a >4 magnitude amplitude using the 0.6m MeerLICHT wide-field imaging telescope at SAAO Sutherland on 2023-04-14 19:51:04, while twinned with the MeerKAT radio array, in a series of observations using multi-band photometry: q_AB = 15.17 +/- 0.01 at 2023-04-14 19:51:04 UT g_AB = 15.10 +/- 0.01 at 2023-04-14 19:52:23 UT i_AB = 15.24 +/- 0.01 at 2023-04-14 19:55:33 UT u_AB = 15.25 +/- 0.01 at 2023-04-14 19:58:31 UT r_AB = 15.18 +/- 0.01 at 2023-04-14 20:01:27 UT Thirty-three previous epochs with MeerLICHT since 2019-06-14 show no variable behaviour in the underlying quiescent source which was last detected at: q_AB = 19.32 +/- 0.10 at 2023-04-09 20:00:06 g_AB = 19.31 +/- 0.17 at 2023-04-09 20:02:54 i_AB = 18.71 +/- 0.16 at 2023-04-09 20:04:24 u_AB = 19.53 +/- 0.41 at 2023-04-09 20:07:22 r_AB = 19:17 +/- 0.18 at 2023-04-09 20:10:23 Gaia DR3 photometry shows a quiescent source, Gaia DR3 5862002885860903552, at G=19.25 +/- 0.02, BP = 19.28 +/- 0.10 , RP=18.67 +/- 0.10 with a parallax of 1.19 +/- 0.20 mas. Archival ATLAS photometry confirms the current outburst and shows one archival outburst, first detected on MJD = 59797 (2022-08-6) strengthening the possible compact binary nature of this source. No source is known in SIMBAD at the reported coordinates. Photometric and spectroscopic follow-up is encouraged. MeerLICHT is designed, built and run by a consortium consisting of Radboud University, University of Cape Town, the South African Astronomical Observatory, the University of Oxford, the University of Manchester and the University of Amsterdam. We acknowledge, and are grateful for, the publicly available Gaia and ATLAS archives at https://gea.esac.esa.int/archive/ and https://fallingstar-data.com/forcedphot/", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Active galactic nucleus", "Galaxy", "Minor body" ] }, "answerKey": "A" }, { "id": "atel_16050", "message": "Title: Detection of candidate progenitor of SN 2023ixf in HST archival data \nAuthors: Monika Soraisam, Tom Matheson, Jen Andrews (NOIRLab), Gautham Narayan, Patrick Aleo (UIUC), ANTARES team\nDate: 23 May 2023; 22:16 UT\nProvenance: Monika Soraisam (monika.soraisam@noirlab.edu)\nSubjects: Optical, Star, Supernovae, Transient\nDescription: Referred to by ATel #: 16060\nWe searched the HST archival data for the progenitor of SN 2023ixf. A clear source can be seen at the SN position (https://antares.noirlab.edu/loci/ANT2023l4lgj6bhp4rt) in the F814W image from the HST program 9490 (PI: Kuntz), which was observed on UT 2002-11-16. The source is, however, not visible in the bluer bands (F435W and F555W). We measure a preliminary F814W magnitude of 24.39+/-0.08 for the source. Considering it as the candidate progenitor of SN 2023ixf and using a distance modulus of 29.05 for M101 (Shappee and Stanek, 2011, ApJ, 733), we obtain an approximate absolute magnitude (no extinction correction) of -4.66, which is in line with a supergiant progenitor.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system", "Nova", "Supernova", "Circumstellar disk" ] }, "answerKey": "C" }, { "id": "atel_16110", "message": "Title: Fermi-LAT detection of renewed gamma-ray activity from the FSRQ S3 0458-02\nAuthors: Adithiya Dinesh, (Universidad Complutense de Madrid), on behalf of the Fermi Large Area Telescope Collaboration\nDate: 2 Jul 2023; 14:28 UT\nProvenance: Denis Bernard (Denis.bernard@in2p3.fr)\nSubjects: Gamma Ray, >GeV, Request for Observations, AGN, Blazar\nDescription: The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed renewed gamma-ray activity from a source positionally consistent with the flat-spectrum radio quasar S3 0458-02, also known as 4FGL J0501.2-0158 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 75.303 deg, Decl. = -1.987 deg (J2000; Johnston et al. 1995, AJ, 110, 880), and redshift z=2.286 (Strittmatter et al. 1974, ApJ, 190, 509). (Previous ATel ) \nPreliminary analysis indicates that this source was in an elevated gamma-ray emission state on June 26, 2023 , with a daily averaged gamma-ray flux (E>100MeV) of 1.7 ± 0.4 X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 7 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL). This is the highest LAT daily flux ever observed for this source. The corresponding photon index is 2.6+/-0.3, and is consistent with the 4FGL value of 2.373+/-0.014 within the uncertainties. \nBecause Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. In consideration of the ongoing activity of this source we will keep searching in the next days for any delayed gamma-ray activity. For this source, the Fermi-LAT contact person is M. Orienti (orienti@ira.inaf.it). \nThe Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Minor body", "Active galactic nucleus, Magnetar", "Active galactic nucleus, Black hole", "Minor body, Black hole" ] }, "answerKey": "C" }, { "id": "atel_16170", "message": "Title: Aql X-1: the X-rays in recent outburst keep brightening indicated by LEIA observations\nAuthors: H. N. Yang (NAOC, CAS), H. Y. Liu (NAOC, CAS), Y. Liu (NAOC, CAS), Z. X. Ling (NAOC, CAS), C. Zhang (NAOC, CAS), H. Q. Cheng (NAOC, CAS), C. Z. Cui (NAOC, CAS), D. W. Fan (NAOC, CAS), H. B. Hu (NAOC, CAS), J. W. Hu (NAOC, CAS), M. H. Huang (NAOC, CAS), C. C. Jin (NAOC, CAS), D. M. Li (BNU), D. Y. Li (NAOC, CAS), Q. X. Li (BNU), M. J. Liu (NAOC, CAS), H. Sun (NAOC, CAS), H. W. Pan (NAOC, CAS), C. Y. Wang (THU), W. X. Wang (NAOC, CAS), Y. L. Wang (NAOC, CAS), Q. Y. Wu (NAOC, CAS), X. P. Xu (NAOC, CAS), Y. F. Xu (NAOC, CAS), M. Zhang (NAOC, CAS), W. D. Zhang (NAOC, CAS), W. J. Zhang (NAOC, CAS), Y. J. Zhang (THU), D. H. Zhao (NAOC, CAS) and W. Yuan (NAOC, CAS), on behalf of the LEIA and Einstein Probe team\nDate: 3 Aug 2023; 09:37 UT\nProvenance: Yuan Liu (liuyuan@bao.ac.cn)\nSubjects: X-ray, Neutron Star, Transient\nDescription: Referred to by ATel #: 16174, 16187, 16284\nThe recurrent outburst of Aql X-1 was detected by XB-NEWS and MAXI since July 23, 2023 (ATel #16147). A follow-up observation by NICER showed that Aql X-1 was in the hard state during this outburst (ATel #16153). The increasing X-ray brightness was also reported by LEIA (Lobster Eye Imager for Astronomy; Atel #16158). Meanwhile, the observations by the 1-m and 0.5-m SAO RAS optical telescopes also shows an optical brightening in R band (Atel # 16169) , and its brightness is close to the peak in 2014 (ATel #6447). \nWe report the latest observations on Aql X-1 by LEIA, which show a significant increase in the flux of 0.5-4 keV. The spectra are fitted with an absorbed power-law with Galactic N_H=4.3e21 cm^-2. The results are listed in the table below. \n \n \n Time \tUnabsorbed Flux \tPhoton Index \tExposure \n (0.5-4keV) \t(seconds) \n (10^-9 erg/s/cm2) \n 2023-07-23T15:05:59 \t0.15 \t1.43 (fixed) \t671 \n 2023-07-26T13:46:39 \t0.58 \t1.43 (+0.42/-0.41) \t688 \n 2023-08-02T01:15:21 \t11.4 \t1.41 (+/-0.19) \t191 \n 2023-08-02T02:49:34 \t11.8 \t1.07 (+/-0.15) \t269 \n \nThe observations on 2023-08-02 show a flux comparable to the peak of the outburst in 2014 (ATel #6447). The brightening in X-ray and optical indicates this outburst is still in progress and more observations are encouraged.\nLEIA (Zhang et al, ApJL, 941, 2) is a soft X-ray Lobster-eye imager (0.5 - 4.0 keV) with a FoV of 340 square degrees aboard the SATech-01 satellite of CAS, launched on July 27, 2022.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Binary system", "Circumstellar disk", "Globular cluster" ] }, "answerKey": "A" }, { "id": "atel_16230", "message": "Title: Swift J1727.8-1613 absolute flux density and polarization measured with Submillimeter Array at 1.3mm\nAuthors: S. D. Vrtilek (CfA), M. Gurwell (CfA), M. McCollough (CfA), R. Rao (CfA)\nDate: 5 Sep 2023; 21:52 UT\nProvenance: M. L. McCollough (mmccollough@head.cfa.harvard.edu)\nSubjects: Sub-Millimeter, Black Hole, Transient, Variables\nDescription: Referred to by ATel #: 16231, 16237, 16238, 16242, 16243, 16245, 16279\nThe hard X-ray transient Swift J1727.8-1613 (originally GRB 230824A: GCN #34536, #34537) has been undergoing a bright outburst at all wavebands, from X-rays (ATel #16205, #16206, #16207, #16210, #16215, #16217), infrared (#16225), optical (ATel #16208, #16209), radio at 5.25 and 7.45 GHz (ATel #16211) and at 5 and 8 GHz (Atel #16228). Here we report detections with the SMA using 7 antennas tuned to LO 224.538 with 12 GHz bandwidth per side-band per polarization (lsb centered at 215.538; usb centered at 235.538) run in full polarization mode. On 2023 Sep 03 (03:59:52 - 07:43:43 UTC) for 148.4 min with flux density averaged over both side-bands found at 173.37 +/- 8.66 mJy with a SNR of 495. A flat spectrum (side bands differed by 2mJy) with polarization fraction 2.1 +/- 0.2% and polarization angle -3.4+/-1.5 degrees. On 2023 Sep 04 2023 Sep 04, (04:00:45 - 07:37:54 UTC) for 69.3 min with flux density averaged over both side-bands found at 150.12 +/- 10.51 mJy with a SNR of 349. A flat spectrum (side-bands differed by 2.6mJy) with polarization fraction 1.9 +/- 0.2% and polarization angle -4.1 +/-3.5 degrees. The Submillimeter Array is a joint project between the Smithsonian Astrophysical Observatory and the Academia Sinica Institute of Astronomy and Astrophysics and is funded by the Smithsonian Institution and the Academia Sinica. We recognize that Maunakea is a culturally important site for the indigenous Hawaiian people; we are privileged to study the cosmos from its summit.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Stellar evolution", "Black hole", "Exoplanet" ] }, "answerKey": "C" }, { "id": "atel_16300", "message": "Title: JHK band observations of SN2023ixf in M101 during days 12 to 112 after the explosion\nAuthors: Y. D. Mayya, L. Carrasco, G. Escobedo, A. Porras, E. Recillas, L. Felix; (INAOE, Mexico)\nDate: 19 Oct 2023; 19:49 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Infra-Red, Supernovae\nDescription: We here report the JHK band photometry of SN2023ixf covering between days 12 to 112 after the explosion. The light curve continued to rise in J-band until day 41, reaching a peak value of 11.05 mag., decreasing monotonically there afterwards. The peak H and K values reached a few days before that in the J-band, with the post-peak values at these longer wavelengths showing low-amplitude fluctuations. Observations details are same as reported in ATel #16082. Here we report the complete photometric table including those reported in ATel #16082. The Julian Day (JD) corresponding to the middle of exposures, measured magnitudes in the three bands in the Vega system, and error on each measurements for each epoch of observations are given below: JD Filter Mag error 2460094.843148 J 11.233 0.035; 2460095.762951 J 11.192 0.030; 2460096.848831 J 11.168 0.044; 2460097.811366 J 11.170 0.053; 2460121.692431 J 11.137 0.066; 2460123.720625 J 11.051 0.048; 2460125.658796 J 11.245 0.030; 2460191.633889 J 12.837 0.034; 2460192.629259 J 12.830 0.036; 2460193.630810 J 12.834 0.028; 2460194.617824 J 12.911 0.035; 2460094.835567 H 11.110 0.036; 2460095.755787 H 11.059 0.032; 2460096.847523 H 10.993 0.042; 2460097.803032 H 10.880 0.032; 2460121.688345 H 11.083 0.064; 2460123.711563 H 11.001 0.058; 2460125.653669 H 11.015 0.050; 2460191.620035 H 12.525 0.033; 2460192.619664 H 12.540 0.022; 2460193.622755 H 12.512 0.034; 2460194.615509 H 12.593 0.036; 2460094.847037 Ks 10.870 0.025; 2460095.779780 Ks 10.861 0.039; 2460096.858102 Ks 10.751 0.026; 2460097.815405 Ks 10.686 0.031; 2460121.699398 Ks 10.770 0.065; 2460123.727072 Ks 10.781 0.103; 2460125.666655 Ks 10.865 0.075; 2460191.643796 Ks 12.145 0.035; 2460192.636829 Ks 12.296 0.028; 2460193.639525 Ks 12.139 0.045; 2460194.631678 Ks 12.246 0.031. Our observations are carried out using CANICA instrument at the 2.1m telescope of the Guillermo Haro Observatory, which is operated by the National Institute for Astrophysics, Optics and Electronics (INAOE, Mexico).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater", "Supernova", "Black hole", "Binary system" ] }, "answerKey": "B" }, { "id": "atel_16380", "message": "Title: The blazar S4 0954+65: the abnormal flare in November-December\nAuthors: V. V. Vlasyuk, O. I. Spiridonova, A. S.Moskvitin, O. A.Maslennikova (Special Astrophysical Observatory of the Rus. Ac. Sci.)\nDate: 15 Dec 2023; 08:18 UT\nProvenance: Alexander Moskvitin (mosk@sao.ru)\nSubjects: Optical, Blazar\nDescription: Referred to by ATel #: 16388\nWe continued monitoring of the blazar S4 0954+65 since its last activity epoch at 2023 October, as it was presented by us in ATel #16331. The both our (1-meter and 0.5-meter) small reflectors were used within observing company. \nDue to bad weather conditions along last November we did not make it's brightness measurements after maximum R=13.22 at epoch MJD=60259. Our first observations at December 5th gave very close value R~13.40. But 3 days after brightness of S4 0954+658 increased to year's maximum at R=13.08 mag at December 8/9 (MJD=60287.05). The error of our estimate is about 0.01 mag. Our following studies showed that brightness of the blazar is still over R=13.5 mag yet. \nSo we can conclude that this object undergoing extremely high state within 40 days. This fact is very unusual for this interesting flaring blazar --- it's typical behavior consists of series of fast flares, as it was pointed out in our last paper (Vlasyuk et al, Astrophys.Bulletin,2023,v78,N4). Some signs of intraday variability in S4 0954+658 were detected and will be presented after more accurate data reduction. \nThe most of data were taken under good weather condition (seeing better 2 arcsec and normal transparency) and have typical accuracy about 0.01 mags. The worse accuracy (up to 0.02 mags) is explaining by bright Moon sky and some mediocre weather in course of some nights. \nWe strongly encourage further multi-wavelength studies.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar, Accreting object", "Black hole, Neutron star", "Black hole, Accreting object", "Black hole, Near-Earth object" ] }, "answerKey": "C" }, { "id": "atel_90", "message": "Title: The XMM-Newton/EPIC-pn Spectrum of the Millisecond X-ray Pulsar XTE J1751-305 in Outburst\nAuthors: Jon M. Miller (MIT), Eckhard Kendziorra (Tuebingen Univ.), Marcus Kirsch (SOC/ESA), Rudy Wijnands (MIT), Mariano Mendez (SRON), Michael Nowak (MIT), Bryan Gaensler (Harvard-Smithsonian CfA), Deepto Chakrabarty (MIT), and Walter H. G. Lewin (MIT)\nDate: 26 Apr 2002; 19:33 UT\nProvenance: Jon M. Miller (jmm@space.mit.edu)\nSubjects: X-ray, Binary, Neutron Star, Transient, Pulsar\nDescription: We have performed a preliminary analysis of the XMM-Newton/EPIC-pn spectrum of the accreting millisecond X-ray pulsar XTE J1751-305 (Markwardt and Swank, 2002, and in't Zand et al. 2002, IAUC 7867 ; Ehle et al. 2002, IAUC 7872 ; Markwardt and Swank, 2002, IAUC 7876 ). The observation started on 2002 April 07.54 and lasted for 34.2 ksec, and represents the first outburst spectrum from such a source at CCD resolution. \nThe 0.3-10.0 keV spectrum is well-described by black-body and power-law components, modified by photoelectric absorption in the ISM (with elemental abundances consistent with solar). We measure a 0.3-10.0 keV unabsorbed flux of 7.0 +/- 0.1 E-10 erg cm^-2 s^-1; 83% of the flux in this band is due to the hard power-law component. The equivalent neutral hydrogen column density is 0.99 +/- 0.01 E+22 atoms cm^-2. The black-body temperature is: kT = 1.06 +/- 0.01 keV, and the power-law index is: Gamma = 1.45 +/- 0.01. The normalization of the blackbody component gives an emitting radius: R = (D / 10 kpc) * 2.93 +/- 0.07 km. This radius may imply that the the emission region is a hot spot on the neutron star surface; however, the model is overly simple and we approach this interpretation with caution. (All errors are 90% confidence limits.) \nWe note broad deviations below 0.6 keV which appear as absorption. At present, it is unclear if this represents real, unresolved absorption or a defect in the instrumental response. The deviations are not removed by requiring enhanced elemental abundances in the photoelectric absorption model. Over the 0.3-10 keV band, we obtain a chi^2 fit statistic of 2771 for 1941 degrees of freedom; considering only the 0.6-10.0 keV band yields a chi^2 value of 2085 for 1883 degrees of freedom and component parameters are essentially unchanged. \nA plot from our analysis may be obtained at: http://space.mit.edu/~jmm/xtej1751-305.ps", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Neutron star", "Exoplanet", "Accreting object" ] }, "answerKey": "B" }, { "id": "atel_180", "message": "Title: INTEGRAL observes IGR J17464-3213 in the soft state\nAuthors: P. Kretschmar (ISDC, Geneva & MPE, Garching), J. Chenevez (DSRI, Copenhagen), F. Capitanio (IASF/CNR, Roma), A. Orr (ESTEC, Noordwijk), G. Palumbo (Universita degli Studi di Bologna), S. Grebenev (IKI, Moscow) \nDate: 21 Aug 2003; 18:16 UT\nProvenance: Peter Kretschmar (Peter.Kretschmar@obs.unige.ch)\nSubjects: X-ray, Gamma Ray, Black Hole, Transient\nDescription: Referred to by ATel #: 189\nThe X-ray transient and black hole candidate IGR J17464-3213 (ATEL #132) = H1743-322, XTE J1746-322 (ATEL #133, #136) has been observed again during the Galactic Center Deep Exposure of the INTEGRAL Core Program. \nCompared to previous INTEGRAL observations the source has now changed to a soft state and is visible with the JEM-X monitor. The source fluxes were ~400 mCrab and ~120 mCrab in the energy ranges 4-6 and 6-10 keV respectively. No significant flux was detected above 20 keV neither with JEM-X nor with IBIS/ISGRI. The JEM-X spectrum can be described by a blackbody model with kT~0.88+-0.07 keV using a fixed absorption value of 2.5e22 derived from earlier observations. No power law tail is required to fit the JEM-X data. \nFrom the JEM-X observations the source position is found to be R.A. = 17h46.3m, Decl. = -32o14.4' with an uncertainty of 0.5'. This is consistent with the VLA position reported in ATEL #137.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Circumstellar disk", "Black hole, Accreting object", "Binary system, Accreting object", "Black hole, Supernova" ] }, "answerKey": "B" }, { "id": "atel_270", "message": "Title: GX 339-4 going into optical/IR decline\nAuthors: Michelle Buxton, Charles Bailyn (Yale U)\nDate: 16 Apr 2004; 22:03 UT\nProvenance: Michelle Buxton (buxton@astro.yale.edu)\nSubjects: Infra-Red, Optical, Binary, Black Hole, Transient\nDescription: We have been continuously monitoring the black-hole candidate GX 339-4 with the ANDICAM instrument on the 1.3m CTIO telescope in optical and IR bands since the beginning of the latest outburst (ATEL #230, #231, #240). Recent observations indicate that the outburst is now in a declining phase. Our V- and J-band lightcurves may be viewed at http://www.astro.yale.edu/buxton/smarts/light_curves/gx339.html. \nGX 339-4 lightcurves", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Black hole", "Nova", "Magnetar" ] }, "answerKey": "B" }, { "id": "atel_330", "message": "Title: Nova in M31\nAuthors: Tzenev L. (IA, Sofia), Georgiev I.(IA, Sofia), Ovcharov E. (SU, Sofia), Stanev I. (SU, Sofia), Georgiev Ts. (IA, Sofia), Nedialkov P. (SU, Sofia)\nDate: 11 Sep 2004; 13:41 UT\nProvenance: Petko Nedialkov (japet@phys.uni-sofia.bg)\nSubjects: Optical, Nova\nDescription: NOVA IN M31\nWe report the discovery of an apparent nova located at R.A. = 0h42m42s.77, Decl. = +41o15'44\".4 (equinox 2000.0), which is 17\".4 west and 44\".0 south of the center of M31. Available B magnitude and B-V colour from CCD images taken with the 2m NAO Rozhen telescope, Bulgaria: Aug. 22.040 UT, 17.956+/-0.030; 0.122+/-0.065.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Globular cluster, Star and stellar system", "Variable star, Circumstellar disk", "Variable star, Star and stellar system", "Variable star, Accreting object" ] }, "answerKey": "C" }, { "id": "atel_400", "message": "Title: 4.85 and 10.45 GHz observations of XTE J1118+480 following the VLA measurements\nAuthors: Emmanouil Angelakis, Alexander Kraus (Max Planck Instuitute for Radio Astronomy, Bonn)\nDate: 26 Jan 2005; 22:00 UT\nProvenance: Emmanouil Angelakis (angelaki@mpifr-bonn.mpg.de)\nSubjects: Radio, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 404, 420\nObservations of the black hole candidate binary XTE J1118+480 have been carried out with the 100-m Radio Telescope at Effelsberg (Max Planck Institute for Radio Astronomy). \n\n \n\nThe observations took place during 2 time slots separated by roughly one day (between JD 2453384.47 and 2453385.41) starting approximately 1 day after the VLA observations. The first set has been carried out under unstable weather conditions whereas the second part under considerably good ones. \n \n\nThe source has been observed repeatedly at both frequencies. The weighted measured values are as follows: \n \n\n 4.85 GHz: 6.0 +/-0.2 mJy  \n10.45 GHz: 9.1 +/-1.0 mJy  \n \n\nXTE J1118+480 was also targeted with the 32 GHz receiver but unfortunately the bad weather prevented us from carrying out reliable measurements at this frequency. Nevertheless, weather permitted, future observations at these band will be attempted.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body, Binary system", "Black hole, Binary system", "Variable star, Binary system", "Neutron star, Binary system" ] }, "answerKey": "B" }, { "id": "atel_475", "message": "Title: Type confirmation of SN 2005bx\nAuthors: A. Gal-Yam, D. J. Sand, S. B. Cenko, D. C. Leonard and J. Muller (Caltech/Palomar Observatory)\nDate: 2 May 2005; 18:49 UT\nProvenance: Avishay Gal-Yam (avishay@astro.caltech.edu)\nSubjects: Optical, Supernovae\nDescription: A. Gal-Yam, D. J. Sand, S. B. Cenko, D. C. Leonard, and J. Muller report on behalf of the CCCP that a preliminarily reduced spectrum (range 4000 - 9500 A) of SN 2005bx (Rich et al., CBET # 148) obtained using the double spectrograph mounted on the Palomar Observatory 200\" Hale telescope, on Apr. 30, 2005, UT, shows this is a type IIn SN, similar to SN 1988Z (e.g., Filippenko 1997). This confirms an earlier report by the Nearby Supernova Factory (ATEL #474). Narrow Balmer emission lines with broad bases are superposed on a blue continuum. \nCCCP homepage", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Variable star", "Minor body", "Active galactic nucleus" ] }, "answerKey": "A" }, { "id": "atel_525", "message": "Title: RXTE PCA Position of HETE J1900.1-2455\nAuthors: C. B. Markwardt (U. Maryland & NASA/GSFC), P. Kaaret (U. Iowa), R. Vanderspek and E. Morgan (MIT) \nDate: 18 Jun 2005; 19:43 UT\nProvenance: Philip Kaaret (philip-kaaret@uiowa.edu)\nSubjects: X-ray, Binary, Neutron Star, Pulsar\nDescription: Referred to by ATel #: 530, 590\nRXTE PCA scans of the new millisecond pulsar HETE J1900.1-2455 (Morgan et al., ATEL #523) were performed on Jun 17 starting at 09:48 UT. The best fit position is R.A. = 19h 00m 13s, Decl. = -24d 54m 44s (J2000), with a systematic uncertainty radius of approximately 1 arcminute. This position is indeed consistent with the HETE burster (Vanderspek et al. ATEL #516), as noted by Morgan et al. (ATEL #523). The flux was approximately 23 mCrab.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body, Pulsar", "Stellar evolution, Pulsar", "Active galactic nucleus, Pulsar", "Neutron star, Pulsar" ] }, "answerKey": "D" }, { "id": "atel_600", "message": "Title: M31 optical transient\nAuthors: R. Quimby, P. Mondol, P. Hoeflich, J. C. Wheeler (University of Texas), and C. Gerardy (Imperial College)\nDate: 2 Sep 2005; 18:39 UT\nProvenance: Robert Quimby (quimby@astro.as.utexas.edu)\nSubjects: Optical, Cataclysmic Variable, Nova, Supernovae, Transient\nDescription: Referred to by ATel #: 850\nWe report the discovery of a transient near M31 using unfiltered CCD images taken on September 1.23 UT (about 18.0 mag) and September 2.23 (about 16.5 mag) using the 0.45m ROTSE-IIIb telescope at the McDonald Observatory. The object is located at RA = 00h38m49.52s DEC = +40o19'54.1\" (J2000) and was not detected in ROTSE-IIIb data from August 31.23 UT (limiting mag about 18.7). A finding chart for the transient can be found at: http://grad40.as.utexas.edu/~quimby/tss/nova5.png \nfinding chart", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Accreting object", "Galaxy", "Repeater" ] }, "answerKey": "C" }, { "id": "atel_700", "message": "Title: RXTE PCA position of XTE J1701-462\nAuthors: C. B. Markwardt (NASA/GSFC & U. Maryland), J. H. Swank (NASA/GSFC), D. Pereira (NASA/GSFC & L3)\nDate: 20 Jan 2006; 17:29 UT\nProvenance: Craig B. Markwardt (craigm@lheamail.gsfc.nasa.gov)\nSubjects: X-ray, Binary, Transient\nDescription: Referred to by ATel #: 702, 703, 704, 708, 15594\nThe RXTE PCA observed the new transient XTE J1701-462 (Remillard et al, ATEL #696) on 20 Jan 2006 at 13:31 UTC for 1500 seconds. The observation included a PCA scan over the source. The 2-10 keV flux is approximately 900 mCrab. \nThe best fit position is R.A. = 17h00m56s, Decl. = -46d10'07\" (J2000), with an estimated systematic position error of approximately 1 arcminute (the position fit is dominated by intrinsic source fluctuations and not statistics). This is 3.8 arcmin from, but consistent with, the RXTE ASM position by Remillard et al (ATEL #696).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Accreting object", "Binary system, Accreting object", "Near-Earth object, Accreting object", "Binary system, Near-Earth object" ] }, "answerKey": "B" }, { "id": "atel_775", "message": "Title: Identification of the X-ray transient Swift J061223.0+701243.9\nAuthors: D. Grupe (PSU), J. P. Osborne (U Leicester), K. L. Page (U Leicester), D. N. Burrows (PSU), J. A. Nousek (PSU), and D. P. Schneider (PSU)\nDate: 27 Mar 2006; 16:13 UT\nProvenance: Dirk Grupe (grupe@astro.psu.edu)\nSubjects: Optical, Ultra-Violet, X-ray, Binary, Cataclysmic Variable, Transient\nDescription: We report on the optical identification of the X-ray transient Swift J061223.0+701243.9 (Grupe et al., 2006, GCN #4672, GCN #4681) which is an uncatalogued object discovered serendipitously by the Swift X-ray Telescope (XRT) while observing the Swift Burst Alert Telescope (BAT) trigger 180274 (Grupe et al. 2006, GCN #4663) on 2006 February 04 starting 20:35 UT. Note that this X-ray transient was not the cause of the trigger. The X-ray position is 8 arcmin away from the BAT position, outside the BAT 3.6 arcmin error circle (Sakamoto et al. 2006, GCN #4679). \nSwift-XRT observed Swift J0612+7012 again for ~8 ks on 2006 March 06, starting at 09:21 UT over a period of about 13 hours. The spectrum during this time was well modelled by an absorbed power-law, with Gamma = 1.61 ± 0.24 and NH = (1.8 ± 0.8) x 10^{21} cm^-2 (90% containment). The mean count-rate was approximately 0.053 counts s^-1, corresponding to an observed (unabsorbed) flux of 3.20 (3.92) x 10^-12 ergs cm^-2 s^-1 in the 0.3-10 keV band. During this observation the source count rate increased from 0.05 to 0.08 counts/s over 9.6 hours, then fell over 3.2 hours to 0.03 counts/s. The results of the spectral and temporal analysis are in good agreement with those of the discovery observation of 2006 February 04. \nSwift J061223.0+701243.9 was observed on 2006 March 21 starting at 02:27 UT with the Low-Resolution Spectrograph (LRS) at the Hobby-Eberly-Telescope (HET) at McDonald Observatory for 3 times 15 minutes using grism #1 with a 2\" slit. The spectral resolution was 17A. The optical spectrum clearly shows strong hydrogen and helium emission lines, identifying this source as an X-ray binary system, either a low-mass X-ray binary or a Cataclysmic Variable. H-beta and H-alpha are clearly resolved and we found FWHM=900 km/s, while H-gamma and He II (4686) are clearly detected but the line widths are not resolved. We also found He I at 4471A and 5876A. The line widths, however, are not well-determined. Apart from the emission lines, the continuum is essentially featureless. \nThe optical position measured from the Swift UV-Optical telescope (UVOT) coadded U image is: \n \nRA-2000: 06 12 22.6 ± 0.5\" \nDec-2000: +70 12 43.4 ± 0.8\" \n \nThe UVOT determined the following observed magnitudes on 2006 March 06: \n \nV = 19.36+/-0.21 \nB = 19.69+/-0.15 \nU = 18.67+/-0.07 \nUVW1 = 19.05+/-0.08 \nUVM2 = 19.61+/-0.08", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Variable star", "Star and stellar system", "Binary system" ] }, "answerKey": "D" }, { "id": "atel_900", "message": "Title: IGR J17497-2821: Refined Swift/XRT Analysis\nAuthors: J. A. Kennea (PSU), D. N. Burrows (PSU), J. Nousek (PSU) and N. Gehrels (NASA/GSFC)\nDate: 28 Sep 2006; 16:11 UT\nProvenance: Jamie A. Kennea (kennea@astro.psu.edu)\nSubjects: X-ray, Gamma Ray, Transient\nDescription: Referred to by ATel #: 906, 907\nIGR J17497-2821 (e.g. Soldi et al., ATEL #885) has been observed by the Swift/XRT on 4 occasions from Sept 19th, 2006 to Sept 26th, 2006, since being initially detected by INTEGRAL on Sept 17th, 2006. We report on a refined analysis of these combined data. Swift/XRT positions for this source previously reported have been inconsistent (e.g. Walter et al., ATEL #889, Chaty et al., ATEL #897), this is most likely due to the point source falling on hot columns in the XRT detector, making accurate centroiding of the source difficult. By combining the four observations and correcting for the hot columns, we find a refined XRT position of: \n \nRA(J2000) = 17h 49m 38.1s, \nDec(J2000) = -28d 21m 16.9s, \n \nwith an estimated uncertainty of 5.3 arcseconds radius (90% containment). Note that this error circle is 50% larger than calculated with the standard software due to current issues with the XRT boresight (Burrows et al., GCN #5628). This position lies 4 arcseconds from the tentative IR counterpart \"candidate 3\" reported by Chaty et al. (ATEL #897), and 19 arcseconds from the originally reported Swift/XRT position (Walter et al., ATEL #889). 2MASS 17493780-2821181 lies 4.6 arcseconds from the refined position, the only cataloged source within the 90% XRT error radius. \n \nAlthough the source does show some variability over the observations in XRT, the source has not visibly faded, showing a mean XRT count rate of ~4 counts/s in Window Timing (WT) mode. The WT spectra is well fit by an absorbed power-law model, with the following parameters: \n \nN_H = (4.8 +/- 0.3) x 1022 cm-2 \nPhoton Index = 1.6 +/- 0.1 \nReduced Chi-squared = 1.2 (147 dof) \nFlux = 3.3 x 10-10 erg/s/cm2 (0.3-10.0 keV, uncorrected for absorption). \n \nAssuming a distance of 8.5 kpc for this source, and correcting for absorption, the 0.3-10.0 keV X-ray luminosity of this source is approximately 7 x 1036 erg/s. There is no evidence for any line features in the spectrum.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star, Repeater", "Variable star, Binary system", "Variable star, Black hole", "Variable star, Accreting object" ] }, "answerKey": "D" }, { "id": "atel_960", "message": "Title: A bright flaring state of SS433\nAuthors: S. Trushkin (SAO RAS), V. Goranskij (SAI Moscow U.), T. Kotani (Tokyo Tech) \nDate: 12 Dec 2006; 12:06 UT\nProvenance: Sergei Trushkin (satr@sao.ru)\nSubjects: Radio, Millimeter, Optical, X-ray, Request for Observations, Binary, Black Hole, Transient\nDescription: We report that the super-critical microquasar SS433 is the flaring state at radio waves and the optical band and would request for followup observations at all frequencies. In the monitoring program of microquasars with the RATAN-600 radio telescope (Trushkin et al., astro-ph/0611550), the flux densities at 1-22 GHz increased from a quiet optically thin synchrotron spectrum: \nS_nu[Jy] = 1.05*nu^-0.54[GHz] on 2006 Dec 6.48 (UT) to flaring one: \nS_nu[Jy] = 2.90*nu^-0.43[GHz] on 2006 Dec 8.47 (MJD54077.47) for the total range of 1-22 GHz. The CCD BVRcIj observations with the 50-cm Maksutov telescope and the 60-cm reflector of Crimean Station of SAI of Moscow U. from 2 to 10 Dec detected the associated optical flare: V=13.94 mag; Rc=12.52 mag on MJD54075.691 and B=15.61 mag; V=13.41 mag; Rc=11.99 mag on MJD54076.633. The last visual magnitude is one of the maximum values during last years. In the active state of SS433, successive flares are expected to occur with an average interval of 15.3 +- 7.3 days. This is a rare opportunity to observe transient jet eruption events from the source (Kotani et al. 2006, ApJ 637, 486). We are requesting ToO observations with RXTE during next two weeks. Light curves and daily radio spectra of SS433 could be found at: \nhttp://cats.sao.ru/~satr/XB/SS433/ss433_lc_2006dec.png \nhttp://cats.sao.ru/~satr/XB/SS433/ss433_sp_2006dec.png \nhttp://cats.sao.ru/~satr/XB/SS433/ss433_bvri_2006dec.png", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Black hole", "Stellar evolution, Black hole", "Star and stellar system, Black hole", "Binary system, Black hole" ] }, "answerKey": "D" }, { "id": "atel_1025", "message": "Title: Swift follow-up observations of the fast-transient IGR J17191-2821\nAuthors: M. Klein-Wolt (University of Amsterdam), R. Wijnands (University of Amsterdam), C. B. Markwardt (CRESST/U. Md./NASA/GSFC), J. H. Swank (NASA/GSFC)\nDate: 9 Mar 2007; 17:57 UT\nProvenance: Marc Klein-Wolt (klein@science.uva.nl)\nSubjects: X-ray, Transient\nDescription: Referred to by ATel #: 1065, 1068, 1070, 1075, 1096, 4170\nFollowing the discovery of the fast-transient IGR J17191-2821 by INTEGRAL (Turler et al. 2007, ATEL #1021) and RXTE (Swank et al. 2007, ATEL #1022), we obtained two sequences of in total 7 short Swift/XRT observations of the source on March 8. The sequences are taken in Photon Counting mode, were performed on March 8 at 02:37 and 10:44 UTC and do not show a source within the INTEGRAL error circle (2.5 arcmin, Turler et al. 2007, Atel 1021) with an upper limit of 0.0021 cnts/s. If we assume an galactic absorption of 3.4e21 cm^-2 and a photon index of 1.8 this corresponds to an 2-10 keV unabsorbed flux of 8.7*10E-14 erg/s/cm^2 or 0.004 mCrab. In the first Swift sequence we do detect a source at distance of about 3.5 arcminutes from the best (INTEGRAL) position of IGR J17191-2821 at the following position: (RA, DEC) = (259.8114, -28.3005) (J2000), with an error of 9.1 arcsec. In total we get a count rate of 0.0087 cnts/s, which corresponds to an 2-10 keV unabsorbed flux of 3.6*10E-13 erg/s/cm^2 or 0.02 mCrab (assuming the same Nh and photon index as before). In the second Swift sequence this source is not visible any more. Although the formal INTEGRAL error circle on the position of IGR J17191-2821 would suggest that the faint source we detected with Swift is unrelated to IGR J17191-2821 (its position is 1 arc-minute outside the INTEGRAL error circle for the position of IGR J17191-2821), we consider it still a small possibility that both sources are one and the same. For example, it has happened (Kuulkers et al. 2007, ATEL #1008) that the true position of transient sources can lay significantly outside the reported error circle. Irrespectively whether or not we detected the transient during our Swift observations, it is clear that over the span of 5 days (from March 3 to March 8) IGR J17191-2821 has decreased by a factor 500 or more.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Neutron star", "Black hole, Galaxy", "Black hole, Supernova", "Black hole, Near-Earth object" ] }, "answerKey": "A" }, { "id": "atel_1100", "message": "Title: GMRT Low frequency radio observation of Cyg X-3 at the time of flare\nAuthors: Sabyasachi pal and A. Pramesh Rao (NCRA-TIFR, India)\nDate: 8 Jun 2007; 14:17 UT\nProvenance: Sabyasachi Pal (spal@ncra.tifr.res.in)\nSubjects: Radio, Black Hole, Transient\nDescription: Referred to by ATel #: 14298, 14397\nTrushkin et al. (#Atel 1092) detected beginning of a new flaring activity in galactic black hole candidate Cygnus X-3. We have observed the source from UT 2.99 June to 3.08 June, 2007 in 243 and 614 MHz frequencies using Giant Meterwave Radio Telescope (GMRT). The source was variable and seemed to rise during our observation. The rising phase is also clear from swift data http://swift.gsfc.nasa.gov/docs/swift/results/transients/CygX-3/ . The average flux density during our observation in 614 MHz is 3.4+-0.2 Jy and in 243 MHz is 1.1+-0.2 Jy and the corresponding spectral index in this low frequency region is 1.1. \nFurther observations are planned.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system", "Black hole", "Interstellar medium", "Pulsar" ] }, "answerKey": "B" }, { "id": "atel_1250", "message": "Title: Revised Classification for SN 2007nm/PQT 071008:224527+103932\nAuthors: S. G. Djorgovski, A. J. Drake, A. Mahabal, C. Donalek, E. Glikman, M. J. Graham, R. Williams (Caltech); C. Baltay, D. Rabinowitz, A. Bauer, R. Scalzo, N. Ellman, J. Jerke (Yale); R. C. Thomas and P. Nugent (LBNL); J. Hennawi (UCB) and A. Myers (UIUC); A. Allan (U. Exeter), I. Steele (Liverpool JMU), and T. Brown (LCOGTN); and the PQ Survey Team\nDate: 26 Oct 2007; 21:12 UT\nProvenance: R. C. Thomas (rcthomas@lbl.gov)\nSubjects: Infra-Red, Optical, Ultra-Violet, Transient\nDescription: We report a revised classification of SN 2007nm (Palomar-QUEST transient PQT 071008:224527+103932, Drake et al. ATEL#1234) based on additional spectroscopy beyond that reported by Djorgovski et al. (ATEL#1240). Using spectra obtained by the SuperNova Integral Field Spectrograph on the 2.2-meter University of Hawaii Telescope, the Nearby Supernova Factory has observed that strong a Si II 6355 feature has not developed, and that the spectrum is more similar to that of a Type Ic supernova at an approximate redshift of z = 0.04.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova, Interstellar medium", "Supernova, Star and stellar system", "Supernova, Active galactic nucleus", "Supernova, Pulsar" ] }, "answerKey": "A" }, { "id": "atel_1325", "message": "Title: Spectroscopic confirmation of the Nova candidate ROTSE3 J004547.7+420204\nAuthors: F. Di Mille, S. Ciroi, P. Rafanelli (Università di Padova), H. Navasardyan (INAF-OAPD), F. Bufano (Univ. di Padova/INAF-OAPD)\nDate: 10 Dec 2007; 20:17 UT\nProvenance: Stefano Ciroi (stefano.ciroi@unipd.it)\nSubjects: Optical, Nova\nDescription: We report the spectroscopic confirmation of the optical nova candidate in M31 announced on ATEL #1311 also reported as M31N-2007-11e on CBAT M31 novae page. \nObservations were carried out at Asiago Observatory using the 1.82 cm telescope + AFOSC. A 3600 sec spectrum (range 360-750 nm; 2.4 nm resolution) was obtained on 2007 Nov 29.83 about 2 days after the discovery. The spectrum shows a prominent blue continuum and Balmer lines with Halpha FWHM of about 600 km/s. In addition NaI and weak FeII emission lines with a well-marked P-Cygni profile are visible. \nThe object was observed again, on Dec 05.78 about 8 days post the discovery using the same instrumentation and setup. Emission lines dominate the spectrum, showing strong Balmer lines visible up to H8. FWHM of Halpha and Hbeta increased to approximately 1400 km/s. Significantly strengthened FeII lines, FeII(42), FeII(49), FeII(74), and Ca II H+K emission are now easily detectable. The NaI D is also increased in intensity and shows the most remarkable P-Cygni profile. These features suggest that M31N-2007-11e can be ascribed to the typical FeII class of the Tololo nova classification scheme (Williams 1992,AJ,104,725)", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Nova", "Neutron star", "Stellar evolution" ] }, "answerKey": "B" }, { "id": "atel_1425", "message": "Title: RXTE PCA detects a new outburst of SAX J1750.8-2900 \nAuthors: C. B. Markwardt (CRESST/U. Md/NASA GSFC), J. H. Swank (NASA GSFC) \nDate: 15 Mar 2008; 20:32 UT\nProvenance: Craig B. Markwardt (craigm@lheamail.gsfc.nasa.gov)\nSubjects: Binary, Neutron Star, Transient\nDescription: Referred to by ATel #: 1426, 1428, 1431, 1446, 1472, 1662, 1775\nRXTE PCA monitoring scans of the galactic bulge region on 2008-03-15 at 04:23 UTC detected a brightening of the neutron star transient SAX J1750.8-2900. The last bright outburst of this source was in 2001, although it has produced low-level emission during portions the interim between then and now. The X-ray flux is approximately 230 mCrab (2-10 keV), which is similar to the peak flux during its previous bright outburst.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Minor body", "Black hole", "Galaxy" ] }, "answerKey": "A" }, { "id": "atel_1500", "message": "Title: MAGIC discovers VHE gamma ray emission from the blazar S50716+714\nAuthors: Masahiro Teshima, Spokesperson for the MAGIC collaboration\nDate: 30 Apr 2008; 15:11 UT\nProvenance: Masahiro Teshima (mteshima@mppmu.mpg.de)\nSubjects: Gamma Ray, >GeV, AGN\nDescription: Referred to by ATel #: 1502\nThe MAGIC collaboration reports the detection of the blazar S50716+714 (redshift unknown) in very high energy gamma-rays, using the 17m diameter MAGIC Cherenkov telescope on La Palma (27.8 N, 17.8 W, 2200 m asl). The observations were performed from April 22 to 24, 2008 and were triggered by the KVA Telescope due to the high optical state of the object. The source is also in a high X-ray state as reported by Swift (Giommi et al., ATel #1495). A preliminary analysis of MAGIC data (3 nights, 2.6 hours in total) revealed a signal of 6.8 sigma corresponding to a flux of F (above 400GeV) ≈ 10^(-11) ph/cm^2/s. MAGIC will continue the observation of S50716+714. Multi-frequency observations are strongly encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus", "Stellar evolution", "Pulsar", "Quasar" ] }, "answerKey": "A" }, { "id": "atel_1590", "message": "Title: Discovery of supernova candidate ROTSE3 J130014.3+275716\nAuthors: D. Chamarro, A. Uecker, F. Yuan, M. D. Sisson, C. Akerlof, T. Mckay (U. Mich.), R. Quimby (Caltech) and J. C. Wheeler (U. Texas) on behalf of the ROTSE collaboration\nDate: 25 Jun 2008; 18:10 UT\nProvenance: Fang Yuan (yuanfang@umich.edu)\nSubjects: Optical, Nova, Supernovae, Transient\nDescription: We report the discovery of a supernova candidate, located at RA: 13:00:14.31 Dec: +27:57:16.4 (J2000, uncertainty <1 \"), in unfiltered CCD images taken by the 0.45m ROTSE-IIIb telescope at McDonald Observatory, Texas. This transient was discovered at ~17.4 mag on Jun. 24.20 UT, and again imaged on Jun. 24.23 UT at a similar magnitude. It is not detected to a limiting magnitude of ~18.1 on Jun. 23.2 UT. It is about 339\" east and 94\" south from the center of Coma cluster and 44.6\" west and 2.6\" south from the center of the nearest galaxy seen in SDSS (2MASX J13001768+2757192). \nA ROTSE-III finding chart can be found at: http://www.rotse.net/rsvp/j130014.3+275716/j130014.3+275716.jpg", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Neutron star", "Near-Earth object", "Nova" ] }, "answerKey": "A" }, { "id": "atel_1725", "message": "Title: A New X-ray Outburst of the HMXB Pulsar X0535+262\nAuthors: Alan M. Levine and Ronald A. Remillard (MIT) for the RXTE team at GSFC and MIT\nDate: 19 Sep 2008; 19:14 UT\nProvenance: Alan M. Levine (aml@space.mit.edu)\nSubjects: X-ray, Request for Observations, Binary, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 2161, 14157\nThe recurrent transient accreting X-ray pulsar X0535+262 has begun its first X-ray outburst observed with RXTE since a series of three closely spaced outbursts that ended in 2005. X0535+262 was first detected by the ASM in the current outburst on MJD 54721 (2008 September 12) at an average level of 21 (5) mCrab at 2-12 keV. The source intensity has averaged 33 (5) mCrab over the 6 days beginning with MJD 54722 and appears to be roughly stationary. While these numbers suggest that the source may reach a relatively small peak intensity in this outburst, we nonetheless urge followup observations with other instruments.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater, Pulsar", "Accreting object, Pulsar", "Stellar evolution, Pulsar", "Accreting object, Magnetar" ] }, "answerKey": "B" }, { "id": "atel_1825", "message": "Title: Optical spectroscopy of transient CSS081007:030559+054715\nAuthors: O. Pejcha, J. L. Prieto & K. Denney (Ohio State University)\nDate: 31 Oct 2008; 17:11 UT\nProvenance: Jose Prieto (prieto@astronomy.ohio-state.edu)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 1835, 1847, 1873, 1910, 1938, 1940, 1942, 2331\nWe report on observations of a transient CSS081007:030559+054715 discovered by the Catalina Real-time Transient Survey (CRTS). According to CRTS photometry the object brightened by about 4 mag during the last year and is currently at about 16th magnitude. We obtained low resolution spectrum (range 4200-7500 Angstroms) on 2008 Oct 27.32 UT using Modspec instrument on 2.4m Hiltner telescope at the MDM Observatory. The spectrum shows blue continuum with very wide and prominent emission lines. The Halpha line shows three well-separated components with radial velocities of -1740, -160 and 1580 km/s. The total HWZI is 2900 km/s. Apparently similar structure is seen at the position of He II and [OIII]. Hbeta is detected but weak. There is a wide unresolved line or blend of lines at the position of Hgamma.\nThe plot of the MDM spectrum can be seen at http://www.astronomy.ohio-state.edu/~pejcha/crts_transient.\nIn addition, between 2008 Oct 27.41 and 27.48 UT we obtained 130 r band images with RETROCAM instrument also on the MDM 2.4m telescope. During that time the transient remained constant to within ~0.05 mag.\nThe transient is located at galactic coordinates of (l,b)=(172.627,-43.727), i.e. away from the Galactic center. The Schlegel et al. (1998) value of the interstellar extinction at this position is AV = 0.48 mag.\nBased on the similarity of the observed spectral features with spectra of recurrent nova CI Aql (see, e.g., Fig. 5 in Matsumoto et al. 2001, A&A, 378, 487), including large expansion velocities, we suggest that the transient CSS081007:030559+054715 represents a nova-like phenomenon, although with very unusual, gradual rise of the light curve. For any plausible distance within our Galaxy (i.e. less than 50 kpc), the absolute magnitude of CSS081007:030559+054715 is fainter than about -3 magnitudes, significantly less luminous than classical novae. However, note the large gap in the temporal coverage of the event, and the fact that it is still ongoing.\nFurther observations of this interesting transient are strongly encouraged.\nWe thank K. Z. Stanek and R. M. Wagner for useful discussions and suggestions.\nWebpage with spectra of the object.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Active galactic nucleus", "Stellar evolution", "Galaxy" ] }, "answerKey": "A" }, { "id": "atel_1900", "message": "Title: Spectroscopic Confirmation of the Recent Nova Candidate in M33, M33N 2009-01a\nAuthors: A. W. Shafter (SDSU), R. Ciardullo (PSU), M. F. Bode, M. J. Darnley (Liverpool JMU, UK), K. A. Misselt (U. Arizona)\nDate: 15 Jan 2009; 00:45 UT\nProvenance: Allen W. Shafter (aws@nova.sdsu.edu)\nSubjects: Optical, Nova, Transient\nDescription: We report spectroscopic observations of the recent M33 nova candidate, M33N 2009-01a, which was discovered on 2009 Jan. 07.54 by K. Nishiyama and F. Kabashima (CBET #1659). At our request, a spectrum (410–950 nm) of M33N 2009-01a was obtained approximately a week after discovery on 2009 Jan. 14.15 UT by J. Caldwell with the 9.2m Hobby-Eberly Telescope (+ Marcario Low-Resolution Spectrograph). The spectrum is dominated by Balmer, He II λ 4686à , and He I (λ 5015à , λ 5875à , λ 6678à , and λ 7065à ) emission features superimposed on a flat continuum. The profiles of the Hα and Hβ lines are complex, and appear to be composed of distinct broad (Hα: FWZI ~ 8500 km/s; FWHM ~ 6500 km/s) and narrow (Hα: FWHM ~ 2100 km/s) components. Given the presence of broad Balmer and Helium emission features together with the absence of significant Fe II emission, we classify this nova as a member of the He/N class defined by Williams (1992, AJ, 104, 725).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system", "Black hole", "Minor body", "Nova" ] }, "answerKey": "D" }, { "id": "atel_2000", "message": "Title: e-EVN observations of Aql X-1 in outburst\nAuthors: V. Tudose (ASTRON), Z. Paragi (JIVE), P. Soleri, D. M. Russell, D. Maitra (UvA), F. Lewis (LCOGTN/Open University), R. P. Fender (SOTON), M. A. Garrett (ASTRON), R. E. Spencer, A. Rushton (JBO)\nDate: 1 Apr 2009; 09:14 UT\nProvenance: Valeriu Tudose (vtudose@science.uva.nl)\nSubjects: Radio, Binary, Neutron Star, Transient\nDescription: Referred to by ATel #: 2317\nThe neutron star X-ray binary Aql X-1 shows quasi-periodic outbursts about once a year. These active states are relatively well covered in optical/infrared and X-ray domains. In contrast, at radio wavelengths the observations are very scarce (IAUC # 5112 ; ATEL #286; ATEL #491).\nFollowing the reports of a new outburst of the object (ATEL #1970; ATEL #1977), we observed Aql X-1 on March 25th, 2009 between 03:00-10:00 UT at 5 GHz with the European VLBI Network (EVN) using the e-VLBI technique. The radio telescopes participating in the experiment were: Effelsberg, Medicina, Onsala 25m, Torun, Westerbork, Jodrell Bank MkII and Knockin. Due to severe weather conditions or technical problems, some of the effective observing time was lost.\nWe did not detect the target. The upper limit to the flux density was 188 microJy (4 sigma).\nTogether with an unrelated project scheduled during the same observing session, these are the first experiments with full 1024 Mbps e-VLBI transfer, from 4 telescopes (Effelsberg, Onsala, Torun and Westerbork).\nQuasi-simultaneous with the radio run, we observed Aql X-1 at optical/infrared wavelengths (Faulkes, Swift) and in the X-ray band (Swift, RXTE).\ne-VLBI is a technique in which signals from widely separated radio telescopes are directly streamed to the central data processor (correlator) in real-time. The data are then immediately made available to the astronomers for further data analysis. For information about e-EVN observing opportunities, please see the EVN e-VLBI web pages. In case of further questions, please e-mail to support(at)expres-eu.org\ne-VLBI developments in Europe are supported by the EC DG-INFSO funded Communication Network Developments project 'EXPReS', Contract No. 02662. The European VLBI Network is a joint facility of European, Chinese, South African and other radio astronomy institutes funded by their national research councils.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Quasar", "Stellar evolution", "Neutron star" ] }, "answerKey": "D" }, { "id": "atel_2050", "message": "Title: Swift/XRT monitoring of XMMU J174716.1-281048: still active!\nAuthors: Melania Del Santo (INAF/IASF-Roma), Patrizia Romano (INAF/IASF-Palermo), Lara Sidoli (INAF/IASF-Milano) and Angela Bazzano (INAF/IASF-Roma)\nDate: 18 May 2009; 13:52 UT\nProvenance: Melania Del Santo (melania.delsanto@iasf-roma.inaf.it)\nSubjects: X-ray, Binary, Neutron Star, Transient\nDescription: Referred to by ATel #: 2624, 3471, 7293\nThe Very Faint X-ray Transient (VFXT) XMMU J174716.1-281048 (ATel #147 and Sidoli et al., 2006, A&A 456, 287) is being observed with Swift/XRT since May 2007 (ATel #1078), in order to monitor the level of activity during the latest outburst, which started in 2003 (Del Santo et al., 2007, A&A 468, L17; ATels #1078, #1136, #1174, #1496). XMMU J174716.1-281048 is indeed the first source classified as \"quasi persistent\" VFXT. Previous Swift/XRT observation in April 2008 (ATel #1496) detected the source at a rate of (2.89+/-0.48)E-02 counts/s (0.2-10 keV). \nSwift/XRT observed the field of XMMU J174716.1-281048 on 2009 March 5, and, as a pointed target of opportunity observation, on 2009 May 15. The source is still active, with a 0.2-10 keV count rate of (2.51+/-0.66)E-02 and (2.40+/-0.58)E-02 count/s, respectively. The estimated 2-10 keV unabsorbed flux is 2.7E-12 erg/cm2/s (assuming a power law model with a photon index of 2.25, absorbed by a column density of 9E22 cm-2, ATel #1078), which translates in luminosity of 2E34 erg/s (d=8 kpc, as from ATel #1207). \nThe source luminosity has been constant in this last year, while it has decreased by more than a factor of two with respect to the 2007 Swift (ATel #1078). The duration of the outburst is probably more than six years, confirming the recurrence time estimated by Del Santo et al. (2007, A&A 468, L17). \nWe will continue the monitoring of the source flux in the next months with Swift/XRT. \nWe would like to thank the Swift Team for making these observations possible, in particular N. Gehrels, the duty scientists as well as the science planners.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Binary system", "Neutron star, Interstellar medium", "Neutron star, Accreting object", "Neutron star, Globular cluster" ] }, "answerKey": "A" }, { "id": "atel_2130", "message": "Title: RXTE PCA and Swift BAT detects the Millisecond Pulsar Swift J1756.9-2508 in Outburst\nAuthors: A. Patruno (U. Amsterdam),C. B. Markwardt (U. Maryland and NASA/GSFC), , T. E. Strohmayer (NASA/GSFC), J. H. Swank (NASA/GSFC), S. E. Smith (WIS/NASA/GSFC),D. Pereira (Wyle IS and NASA/GSFC)\nDate: 14 Jul 2009; 20:16 UT\nProvenance: Alessandro Patruno (a.patruno@uva.nl)\nSubjects: X-ray, Request for Observations, Binary, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 2138, 11505\nWe report a detection of increased activity of the accreting millisecond X-ray pulsar Swift J1756.9-2508 observed with the RXTE-PCA monitoring on July 8, 9hr UTC. Increased flux is detected simultaneously on the Swift-BAT camera. RXTE-PCA follow up observations starting on July 13, 23hr UTC, detected the source in the 2-16 keV band at a flux level of approximately 19 mCrab, rising to 22 mCrab on July 14, 2hr UTC. Swift J1756.9-2508 was previously observed in outburst in June 2007 (Atel #1107), suggesting a recurrence time of approximately 2 years. Barycentered data at the Swift-XRT position (Krimm et al. 2007) show a peak in the power density spectrum which is entirely consistent with the 182.0658 Hz reported by Krimm et al. (2007). More PCA observations are planned. Follow-up observations at other wavelengths are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium, Neutron star", "Accreting object, Neutron star", "Accreting object, Black hole", "Accreting object, Exoplanet" ] }, "answerKey": "B" }, { "id": "atel_2190", "message": "Title: On the NIR counterpart candidate to XTE J1652-453\nAuthors: M. A.P. Torres (CfA), D. Steeghs (Warick/CfA), P. G. Jonker (SRON/CfA), J. E. McClintock (CfA), N. Morrell, M. Roth (LCO)\nDate: 4 Sep 2009; 21:29 UT\nProvenance: Manuel Torres (mtorres@cfa.harvard.edu)\nSubjects: Infra-Red, Black Hole, Neutron Star, Transient\nDescription: We report on near-infrared follow-up observations of the field containing the currently active X-ray transient XTE J1652-453 (Markwardt et al. ATel #2107, #2120). A Ks= 16.9 +/- 0.3 mag NIR counterpart candidate has been suggested on the basis of its coincidence with the radio localization for the X-ray source (Calvelo et al. ATel #2135, Reynolds et al. ATel #2125). \nWe have acquired a series of 15s Ks-band images on 2009 Jul 15 23:02 - 23:14 UT and again on 2009 Aug 28 23:33-23:46 using the PANIC camera attached to the 6.5m Magellan Baade telescope at Las Campanas observatory. The frames (totaling 450s on source for both nights) were acquired under good sky conditions with seeing of 0.8'' and 0.4'', respectively. Additional 3s exposures of the field were obtained during the first night for an absolute flux calibration of the data. The astrometric and photometric scale were defined using 2MASS sources in the field of view achieving a positional RMS of 0.1 arcsec and a zero-point error < 0.1 mag.\nOur relative (PSF-fitting) photometry on the two data sets shows no significant variability for the suggested NIR counterpart (labeled as star B in Reynolds et al. ATel #2125). We determine a mean magnitude of Ks = 16.9 +/- 0.1. Note here that the Aug 28 (MJD 55071.98) data set was acquired when the X-ray flux had declined by a factor of ~4 compared to the X-ray flux measured on Jul 15 (MJD 55027.96; see RXTE PCA light curve).\nThe non-variable nature of star B suggests that it could be an unrelated interloper star and that the NIR counterpart was fainter than Ks=19 (Jul) and Ks > 20 (Aug) as estimated from the 3-sigma upper limit magnitudes of our images. For completeness sake, we also determine Ks-band magnitudes of 16.508 +/- 0.05, 14.421 +/- 0.005, 15.219 +/- 0.011 and 15.808 +/- 0.016 for stars A, 1,2 and 3 as labeled in Reynolds et al.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova, Black hole", "Active galactic nucleus, Variable star", "Magnetar, Black hole", "Active galactic nucleus, Black hole" ] }, "answerKey": "D" }, { "id": "atel_2275", "message": "Title: 2S 1417-624 in Outburst\nAuthors: Elif Beklen (METU) and Mark H. Finger (USRA) for the GBM Pulsar Project Team\nDate: 30 Oct 2009; 18:48 UT\nProvenance: Dr. Mark H. Finger (Mark.Finger@msfc.nasa.gov)\nSubjects: X-ray, Gamma Ray, Binary, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 2276, 5782, 11479, 14349\nObservations with the GBM on Fermi show that the transient Be/X-ray binary pulsar 2S 1417-624 is currently in outburst. Coherent pulsations from the source at a 17.5 s period have been detected in the GBM data since October 18. The rms pulsed flux has been increasing, reaching 12 mCrab (12-52 keV) during October 28-29. From October 24.0 to 30.0 the spin frequency (corrected using the binary orbital elements of Inam et al. 2004) increased at a rate of (8.5 +/- 1.0) x 10E-12 Hz/s, reaching 57.09623(14) mHz on October 29.0 (MJD 55133.0). \nThe Swift/BAT monitoring shows a flux of 40 mCrab on October 29 and 90 mCrab on October 30. The last reported detection of this source was made with INTEGRAL in 2008 July (ATel# 1613). \nGBM Pulsar Project", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Neutron star", "Variable star", "Stellar evolution" ] }, "answerKey": "B" }, { "id": "atel_2325", "message": "Title: GASP detection of a fast optical brightening of the blazar 3C 454.3\nAuthors: M. Villata and C. M. Raiteri (INAF, Osservatorio Astronomico di Torino, Italy), V. M. Larionov and T. S. Konstantinova (Astronomical Institute, St.-Petersburg State University, Russia), K. Nilsson and M. Pasanen (Tuorla Observatory, University of Turku, Finland), D. Carosati (EPT Observatories, Tijarafe, La Palma, Spain), for the GASP Collaboration\nDate: 3 Dec 2009; 12:18 UT\nProvenance: Claudia M. Raiteri (raiteri@oato.inaf.it)\nSubjects: Optical, AGN\nDescription: Referred to by ATel #: 2326, 2328, 2329, 2332, 2333, 2345, 2352, 3003, 3047\nWith reference to the recent very strong gamma-ray activity of the blazar 3C 454.3 detected by Fermi-GST and AGILE (ATel #2322), the GLAST-AGILE Support Program (GASP) of the Whole Earth Blazar Telescope (WEBT) reports on a simultaneous fast optical brightening of the source. After the mild activity registered in August-October 2009 (R ~ 14.5-15), the optical brightness decreased to R ~ 15-15.2 in November. Starting from this level, a very fast flux increase has led to a brightening of more than 1 mag between November 21 and December 1-2, when reaching R ~ 14.1.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus", "Globular cluster", "Nova", "Supernova" ] }, "answerKey": "A" }, { "id": "atel_2400", "message": "Title: ATCA detection of increased radio emission from XTE J1752-223\nAuthors: Catherine Brocksopp (MSSL), Stephane Corbel (CEA Saclay & Universite Paris Diderot), Tasso Tzioumis (ATNF), Rob Fender (University of Southampton), Mickael Coriat (CEA Saclay & Universite Paris Diderot)\nDate: 23 Jan 2010; 23:25 UT\nProvenance: Catherine Brocksopp (cb4@mssl.ucl.ac.uk)\nSubjects: Radio, Request for Observations, Binary, Black Hole, Transient\nDescription: Following the announcement that the new X-ray transient source, XTE J1752-223 (ATel. 2258), is making a transition from the hard to the intermediate state (ATel. 2387, 2391, 2396), we have observed the radio counterpart with the Australia Telescope Compact Array and the new CABB back-end. The radio source has risen from the previous ~2 mJy plateau to 20 mJy at 1.2, 2.5, 5.5, 9, 17, 19 GHz on January 21. The increased flux density, flat spectrum and compact nature of the radio source suggest that a major ejection event is imminent and we encourage continued observations at all frequencies. VLBI observations of the jet ejecta would be particularly valuable.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Circumstellar disk", "Neutron star", "Black hole" ] }, "answerKey": "D" }, { "id": "atel_2520", "message": "Title: A new outburst of the SFXT IGR J08408-4503 observed by Swift \nAuthors: P. Romano (INAF-IASF Palermo), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), C. B. Markwardt (GSFC/UMD), D. N. Burrows (PSU), M. M. Chester (PSU), G. Cusumano (INAF-IASF Palermo), P. Esposito (INAF-IASF Milano), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), V. La Parola (INAF-IASF Palermo), S. Vercellone (INAF-IASF Palermo), N. Gehrels (GSFC) \nDate: 29 Mar 2010; 11:23 UT\nProvenance: Pat Romano (romano@ifc.inaf.it)\nSubjects: X-ray, Gamma Ray, Request for Observations, Binary, Transient\nDescription: Referred to by ATel #: 3586, 5190\nThe Swift Burst Alert Telescope (BAT) triggered on a new outburst from the Supergiant Fast X-ray Transient (SFXT) IGR J08408-4503 on 2010 March 28 at 15:53:38 UT (image trigger=417420). Swift did not execute an immediate slew, because of an Earth-limb constraint. \nUsing the BAT data from T-220 to T+280 s, the emission starts at ~T-120 and ends at ~T+120 s. The peak emission occurs at ~T+10 s at about 0.09 counts/cm2/s. The partial coding was 92%. The time-averaged spectrum from T-96.8 to T+118.6 s is best fit by a power law with an exponential cutoff. This fit gives a photon index of 0.27 +/- 1.78, and Epeak of 28.4 +/- 11.6 keV (chi squared 69.7 for 56 d.o.f.). The 1-s peak flux measured from T+13.04 s in the 15-150 keV band is 0.4 +/- 0.1 ph/cm2/s. A fit to a simple power law gives a photon index of 2.40 +/- 0.29 (chi squared 76.1 for 57 d.o.f.). All the quoted errors are at the 90% confidence level. \nThe XRT began observing the field at 16:48:29.2 UT, 3290.9 seconds after the BAT trigger, for two orbits. At that time, the source count rate was ~ 0.1 counts/s. The spectrum (PC mode data, T+3298 to 10460 s) can be fitted with an absorbed power-law with a photon index of 1.2+/-0.4 and an absorbing column density of NH=[9 (+6,-4)]E21 cm-2. The average 2-10 keV unabsorbed flux is ~9E-12 erg/cm2/s. \nPreviously, Swift observed flares from this source on 2006 October 4 (Gotz et al. 2007,ApJ,655,L101; Romano et al. 2009,MNRAS,392,45), 2008 July 05 (Romano et al. 2009,MNRAS,392,45), 2008 September 21 (Sidoli et al. 2009,MNRAS,397,1528), and 2009 August 28 (ATel #2178). The historical light curve from the BAT hard X-ray transient monitor (Krimm et al, 2006, ATel #904; 15-50 keV) can be found at http://swift.gsfc.nasa.gov/docs/swift/results/transients/weak/IGRJ08408-4503 . \nWe would like to thank the Swift Team for making these observations possible, in particular the duty scientists as well as the science planners.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus", "Star and stellar system", "Supernova", "Galaxy" ] }, "answerKey": "C" }, { "id": "atel_2580", "message": "Title: A New Supernova Discovery/Classification\nAuthors: Peter Nugent (Lawrence Berkeley National Laboratory), Mark Sullivan (University of Oxford) & D. Andrew Howell (LCOGT/UCSB)\nDate: 22 Apr 2010; 22:50 UT\nProvenance: Peter Nugent (penugent@lbl.gov)\nSubjects: Optical, Request for Observations, Supernovae\nDescription: The Type Ia supernova science working group of the Palomar Transient Factory (ATEL#1964) reports the discovery of a nearby supernova, PTF10fps. The supernova is at RA = 13:29:25.11 Dec = +11:47:46.4 (J2000), on the outskirts of NGC 5177 at a redshift of 0.0216. The supernova was discovered on Apr. 16.2 UT when it was at magnitude 18.0 in R-band (calibrated wrt the USNO catalog). There was nothing at this location on Apr 11.2 UT to a limiting magnitude of 20.9. A confirmation spectrum was taken on the Double Beam Spectrograph on the Palomar Hale telescope on Apr. 17 UT by R. Ellis and J. Cooke. Classification of the spectrum was carried out using Superfit (Howell et al. 2005) and in comparison to SNF20080514-002 (ATEL#1532) which showed it to be approximately 13 days before peak brightness. STIS/UV spectroscopic observations on the Hubble Space Telescope were triggered by the ToO program \"Verifying the Utility of Type Ia Supernovae as Cosmological Probes: Evolution and Dispersion in the Ultraviolet Spectra \" (PI: R. Ellis) and by Swift with the ToO program \"Unveiling New Classes of Transients with Palomar Transient Factory\" (PI: S. Kulkarni). We strongly encourage additional follow-up of this source at all wavelengths.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Galaxy", "Globular cluster", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_2640", "message": "Title: Optical Photometry of the New Optical Transient SN 2010da in NGC 300\nAuthors: Howard E. Bond (STScI)\nDate: 26 May 2010; 01:25 UT\nProvenance: Howard E. Bond (bond@stsci.edu)\nSubjects: Optical, Supernovae, Transient, Variables\nDescription: Referred to by ATel #: 2660, 3726\nMulticolor images of the new optical transient in NGC 300, discovered by B. Monard (CBET #2289 and private communication), were obtained on 2010 May 25.37 by J. Espinoza with the SMARTS 1.3m telescope at Cerro Tololo and the ANDICAM camera. The transient has received the designation SN 2010da, although spectroscopic observations and the low luminosity suggest that it is most probably an LBV-like outburst on a dust-enshrouded massive star and not a true supernova (e.g., ATEL #2632, #2633, #2636, #2637, #2638). \nThe 1.3m measurements were calibrated approximately through observations of a Landolt standard field, but the uncertainties are larger than normal, perhaps of order +/-0.1 mag, due to the large difference in airmass between the frames. The results are V = 16.28, B-V = 0.33, V-R = 0.36, and V-I = 0.62. The relatively blue color confirms that the transient does not currently suffer a large amount of extinction (cf. ATEL #2633). \nI plan to continue to monitor the light curve of this outburst, for comparison with the optical transient of 2008 in the same galaxy (Bond et al., 2009, ApJ, 695, L154), also discovered by Monard.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova, Star and stellar system, Variable star", "Supernova, Star and stellar system, Near-Earth object", "Supernova, Star and stellar system, Circumstellar disk", "Galaxy, Star and stellar system, Variable star" ] }, "answerKey": "A" }, { "id": "atel_2760", "message": "Title: Pre-discovery detection of the nova candidate M33N 2010-07a in XMM-Newton OM observations\nAuthors: W. Pietsch, F. Haberl (Max-Planck-Institut fuer extraterrestrische Physik, MPE), B. F. Williams (University of Washington), W. P. Blair (John Hopkins University), T. J. Gaetz (Harvard-Smithonian Center for Astrophysics, CFA), K. S. Long (Space Telescope Science Institute), T. G. Pannuti (Morehead State University), P. P. Plucinsky (CFA), P. F. Winkler (Middlebury College) as part of the XMM-Newton M33 Large Program collaboration\nDate: 27 Jul 2010; 13:09 UT\nProvenance: Wolfgang Pietsch (wnp@mpe.mpg.de)\nSubjects: Optical, X-ray, Nova\nDescription: Nishiyama and Kabashima discovered the nova candidate M33N 2010-07a on unfiltered images taken around 2010-07-17.798 UT (see CBET #2375). No source was present in their images taken on 2010-03-18.44 UT, in their earlier images and other deep optical images. \n \nThe \"Deep XMM-Newton Legacy survey of M 33\" (PI Williams) will cover the entire D25 isophote of the galaxy with a total of seven contiguous 100 ks exposures. The first two observations (ObsID 0650510101 and 0650510201) started on 2010-07-09.30 UT and 2010-07-11.29 UT, respectively. \n \nM33N 2010-07a was in the field of view of the XMM-Newton Optical Monitor OM during ObsID 0650510101. We detect a source at RA = 01h33m36.84s, Dec = +30d46'22.6\" (J2000, accuracy of 0.3\", comparing to USNO B1 catalogue, Monet et al. 2003, AJ 125, 984) consistent with the position of the nova candidate. We determined the source brightness in the U, B, UVW1 and UVM2 filters as mag 19.7(1), 19.1(1), 20.4(1), and >21.0, respectively. The magnitudes are given in the AB system (see Oke 1974, ApJS 27, 21). The detection of a new source in the OM coincident with the nova candidate indicates that the outburst must have occurred already more than 8 days before the original nova discovery. \n \nIn X-rays, no source was detected within 56.4\" and 19.9\" in the XMM-Newton observatory survey (observations from 2000-2003, 0.2-4.5 keV, limiting luminosity 1x1035 erg s-1; Pietsch et al. 2004, A&A 426, 11) and in the Chandra observatory ChASeM33 survey (2000-2006, 0.35-8.0 keV, 2.1x1034 erg s-1, Tuellmann et al. 2010, in preparation), respectively. M33N 2010-07a was in the field of view of the EPIC pn instrument during both XMM-Newton large project observations. We do not detect X-ray emission from the nova candidate (3 sigma upper limits of 0.42x10-3 ct s-1 and 3.0x10-3 ct s-1 in the 0.2-1 keV band). Assuming an energy conversion factor of 1.04x10-11 erg cm-2 ct-1 for the EPIC pn thin filter observations (black body spectrum and Galactic foreground absorption of 6.66x1020 cm-2, see Pietsch et al. 2005, A&A 442, 925) leads to unabsorbed fluxes and luminosities in M 33 (assumed distance 817 kpc) of 4.4x10-15, 3.1x10-14 erg cm-2 s-1 and 3.5x1035, 2.5x1036 erg s-1, respectively. These upper limits are well below the luminosities reported for the supersoft source phase of novae, which however mostly is detected weeks to months after the optical outburst.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater", "Binary system", "Nova", "Active galactic nucleus" ] }, "answerKey": "C" }, { "id": "atel_2850", "message": "Title: Outburst of Aql X-1 as observed by RXTE and Swift\nAuthors: Sabyasachi Pal (ICRAR-UWA)\nDate: 20 Sep 2010; 16:45 UT\nProvenance: Sabyasachi Pal (spal@cyllene.uwa.edu.au)\nSubjects: X-ray, Request for Observations, Binary, Neutron Star, Star, Transient\nDescription: Referred to by ATel #: 2871, 2891, 2902, 2911, 3686\nAll Sky Monitor (ASM) on-board Rossi X-ray Timing Explorer and Burst Alert Telescope (BAT) on-board Swift detected an outburst of low-mass X-ray binary Aql X-1. The source re-brightened after an outburst in July 2010 (ATEL #2742, #2744, #2748). \nThe outburst started near MJD 55440 (1st Sept 2010) and right now, in 2-10 keV, the source is near its peak with ASM count rate 27.75 counts/s (~370 mCrab) recorded on MJD 55455.16 (UT 16.16 Sept 2010). BAT recorded peak in 15-50 keV on MJD 55450 (UT 11 Sept 2010) with 0.027+-0.007 counts/sec rate and on the next day the source count rate rapidly fall near its quiescent value indicating transition to softer state. \nFurther multi wavelength follow-up of the event is encouraged. \nSwift/BAT transient monitor data is provided by the Swift/BAT team and ASM data is provided by ASM/RXTE team.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Pulsar", "Supernova", "Galaxy" ] }, "answerKey": "A" }, { "id": "atel_2925", "message": "Title: Increased optical activity of Be/X binary system SAX 2103.5+4545 suggests a new outburst in X-rays\nAuthors: U., Kiziloglu, N., Kiziloglu, A. Baykal (METU); S. C. Inam (Baskent)\nDate: 12 Oct 2010; 11:26 UT\nProvenance: Umit Kiziloglu (umk@astroa.physics.metu.edu.tr)\nSubjects: Optical, Binary, Transient, Pulsar\nDescription: Referred to by ATel #: 2928, 4068\nWe report on the recent optical activity of the high-mass X-ray binary system SAX 2103.5+4545. The source was monitored by ROTSEIIId telescope (Akerlof et al., 2003, PASP, 115, 132) on Bakirlitepe, TUBITAK National Observatory, Turkey. After about 3 years of its optical quiescence, the system shows an increase in the optical brightness starting from August 2010, from its quiescence value of R ~13.2 in ROTSE R-band. The previous 2007 X-ray outburst reported in ATEL #1063 and ATEL #1064 of the source was occurred at optical brightness of R ~12.8 (Kiziloglu et al. 2009, A&A, 508, 895). The object is at R 12.72+/-0.02 on October 11, 2010. We have observed the optical counterpart of the X-ray binary SAX2103.5+4545 with the RTT150 telescope and TFOSC. The spectra obtained on September 17, 2010 showed a weak H alpha line emission feature with a double-peak profile of equivalent width 0.42+-0.02 angstrom. The brightening of the system and H alpha line emission shows a new disc formation around the Be star. All the optical activity observed are signatures of a new X-ray activity of the source.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Binary system", "Accreting object", "Stellar evolution" ] }, "answerKey": "B" }, { "id": "atel_3030", "message": "Title: NIR flaring of the FRQS B3 1708+433\nAuthors: L. Carrasco, A. Carramiñana, J. R. Valdes, E. Recillas, G. Escobedo, A. Porras, Y. D. Mayya (INAOE, Mexico)\nDate: 13 Nov 2010; 18:31 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Infra-Red, Optical, Gamma Ray, >GeV, Request for Observations, AGN, Blazar, Quasar\nDescription: We report the ongoing NIR flare of the flat spectrum radio source B31708+433, a z=1.027 Flat Radio QSO also known as CGRaBS J1709+4318, identified with a flaring FERMI/LAT source reported by Allafort et.al in (ATel #3026). The source was not detected by the 2mass NIR survey (estimated H magnitude limit for this field ~16.4). Yet, on November 13th,2010 (JD 2455513.551228), we detected a strong NIR source coincident with the radio position. We determined the flux from this object to correspond to H = 13.055 +/- 0.05, J = 13.848 +/- 0.05 and Ks = 12.040 +/- 0.06. That is at least 3.2 mag brighter than the limiting flux of the 2mass in the H band. Henceforth, this QSO has had a recent increase in flux of 20 approximately. This NIR flux enhancement is consistent with the FERMI/LAT detection of the source. Observations were carried out with the 2.1m telescope of the Guillermo Haro Observatory of the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. Our observation provides further support for the identification of the Gamma Ray source with the radio one. We encourage further multi wavelength coverage for this variable source.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar, Interstellar medium", "Neutron star, Active galactic nucleus", "Quasar, Black hole", "Quasar, Active galactic nucleus" ] }, "answerKey": "D" }, { "id": "atel_3090", "message": "Title: EVLA and Swift Follow Up of PTF10abpr\nAuthors: Mansi Kasliwal (Caltech), Dale Frail (NRAO), Robert Quimby, Eran Ofek, Shri Kulkarni, Assaf Horesh (Caltech), Avishay Gal-Yam, Iair Arcavi (Weizmann Institute), Fang Yuan, Carl Akerlof (U. Michigan), and Tim McKay (Minnesota) report on behalf of the Palomar Transient Factory collaboration\nDate: 25 Dec 2010; 02:39 UT\nProvenance: Mansi Manoj Kasliwal (mansi@astro.caltech.edu)\nSubjects: Radio, Optical, Ultra-Violet, X-ray, Supernovae, Transient\nDescription: We triggered our NRAO Target Of Opportunity program \"Exploring Transients in the Local Universe\" and used the Expanded Very Large Array (EVLA) to observe PTF10abpr (ATEL#3089), a Type II supernova at a distance of 20 Mpc. The EVLA observations were made on 2010 December 11.22 UT. We detect no radio emission at a center frequency of 8.46 GHz down to a 3-sigma limit of 81 uJy. \nUnder our ongoing PTF/Swift program, we began observations of PTF10abpr on December 10.01 UT. We measure the following preliminary UVOT (Vega) magnitudes for the transient: U=17.8, UVW1=18.9, UVM2=19.8, UVW2=19.9. Note that these values may include some contamination from the host galaxy. This source was not detected by the XRT. \nWe thank the EVLA team and the Swift team for promptly undertaking these target of opportunity observations. \nFurther monitoring is ongoing.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Supernova", "Exoplanet", "Galaxy" ] }, "answerKey": "B" }, { "id": "atel_3210", "message": "Title: First hard X-ray detection of the neutron star X-ray transient SAX J1806.5-2215 with INTEGRAL\nAuthors: M. Del Santo (INAF/IASF-Roma, Italy), P. Romano (INAF/IASF-Palermo, Italy), L. Sidoli, S. Mereghetti (INAF/IASF-Milano, Italy), C. Ferrigno (ISDC, Switzerland), N. Degenaar, R. Wijnands (University of Amsterdam, The Netherlands), E. Kuulkers (ESA/ESAC, Spain), A. Nucita (University of Salento, Italy), V. Savchenko (ISDC, Switzerland)\nDate: 7 Mar 2011; 21:13 UT\nProvenance: Melania Del Santo (melania.delsanto@iasf-roma.inaf.it)\nSubjects: X-ray, Binary, Neutron Star, Transient\nDescription: Referred to by ATel #: 3218, 3381, 3926, 4017\nIn the framework of the INTEGRAL observations of the Galactic Inner Disc, we obtained the first hard X-ray detection above 20 keV of the source SAX J1806.5-2215 (in't Zand et al. 1998, NuPhS, 69, 228). The currently on-going outburst (ATels #3202, #3193) of this so-called \"burst-only\" source (Cornelisse et al. 2004, NuPhS, 132, 518) has been detected by INTEGRAL on 2011 March 06 from 10:01 to 23:21. The IBIS/ISGRI (25.5 ks exposure time) significance levels are 15 sigma and 8 sigma in the 20-40 keV and 40-80 keV energy bands, respectively. The corresponding fluxes are 21.2+/-1.4 mCrab and 23.6+/-3.0 mCrab, respectively. \nThe source is also detected by JEM-X. The joint JEM-X1, JEM-X2 and IBIS/ISGRI spectrum can be well fitted (red. chi^2=0.9 (13 d.o.f.)) by a simple power-law with photon index 2.0 +/-0.3, consistent with the findings of Degenaar et al. (ATel #3202). The estimated fluxes are 3.8E-10 erg/cm^2/s in 2-10 keV and 3.2E-10 erg/cm^2/s in 20-80 keV. For a distance of 8 kpc (the upper limit reported in Cornelisse et al. 2002, A&A 392, 931), this translates into a 2-10 keV luminosity of ~3E36 erg s-1 which is roughly a factor of 1.5 higher than the last Swift/XRT pointing (ATel #3202). We found no type-I X-ray bursts either in the IBIS/ISGRI, or in the JEM-X light curves. \nFurther INTEGRAL and Swift observations are planned. \nWe encourage further monitoring at all wavelengths of this source.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Binary system", "Stellar evolution", "Neutron star" ] }, "answerKey": "D" }, { "id": "atel_3330", "message": "Title: MAXI/GSC detection of a new X-ray transient MAXI J1543-564\nAuthors: H. Negoro (Nihon U.), S. Nakahira (RIKEN), Y. Ueda (Kyoto U.), T. Mihara, M. Sugizaki, M. Serino, T. Yamamoto, T. Sootome, M. Matsuoka (RIKEN), S. Ueno, H. Tomida, M. Kohama, M. Ishikawa (JAXA), N. Kawai, M. Morii, K. Sugimori, R. Usui, T. Toizumi (Tokyo Tech), A. Yoshida, K. Yamaoka (AGU), H. Tsunemi, M. Kimura, H. Kitayama (Osaka U.), M. Nakajima, F. Suwa, M. Asada, H. Sakakibara (Nihon U.), K. Hiroi, M. Shidatsu (Kyoto U.), Y. Tsuboi, T. Matsumura, K. Yamazaki (Chuo U.) report on behalf of the MAXI team\nDate: 8 May 2011; 16:55 UT\nProvenance: Hitoshi Negoro (negoro@phys.cst.nihon-u.ac.jp)\nSubjects: X-ray, Black Hole, Neutron Star, Star, Transient, Pulsar\nDescription: Referred to by ATel #: 3331, 3334, 3336, 3341, 3355, 3359, 3364, 3365, 3372, 3407, 3662, 8582\nAt 2011-05-08 04:21 UT (MJD=55689.18125), the MAXI/GSC alert system triggered a new X-ray transient at the position: \n(R.A., Dec) = (+235.788 deg, -56.421 deg) = (15 43 09.1, -56 25 16) (J2000) \nwith a systematic uncertainty of 0.2 deg. \nThe 2-20 keV X-ray flux from the source has increased since 2011-05-07, reaching 21+-5 mCrab on average at scan transits from 2011-05-07 13:07 to 2011-05-08 04:21. The source is too faint for the MAXI/GSC to detect any significant variability. Its energy spectrum, however, tends to become softer after the detection. \n \nThere is no known X-ray source within the error circle, and no bright sources are found on archival ROSAT all-sky survey images. We tentatively refer this transient as MAXI J1543-564. Follow-up observations are strongly encouraged. \nMAXI Home Page", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Accreting object, Pulsar", "Stellar evolution, Neutron star, Pulsar", "Black hole, Neutron star, Pulsar", "Black hole, Star and stellar system, Pulsar" ] }, "answerKey": "C" }, { "id": "atel_3400", "message": "Title: Swift/XRT detection of PSN J13303600+4706330 (PTF11eon)\nAuthors: Raffaella Margutti, Alicia Soderberg (Harvard University)\nDate: 3 Jun 2011; 18:54 UT\nProvenance: Alicia M. Soderberg (asoderberg@cfa.harvard.edu)\nSubjects: X-ray, Supernovae\nDescription: Referred to by ATel #: 3402, 3413, 3414, 3432, 3456, 3641\nSwift observed the new Type IIP PSN J13303600+4706330 (PTF11eon; ATEL #3398) on 2011 Jun 3rd at 12:06:18 UT for 2.4 ksec. An X-ray source is clearly detected at coordinates: \nRA(hh mm ss.s) = 13h30m05.22s \nDec(dd mm ss.s) = +47:10:12.41 \n(J2000) with an error radius of 4.80 (arc sec, 90% c.l.). This position is consistent with the optical position (ATEL #3398). \nThe estimated count rate is ~0.013 c/s. Adopting a power-law spectral model with photon index of Gamma=2 the observed count rate translates into a 0.3-10 keV flux of ~5e-13 erg/sec/cm2 after correcting for the Galactic column density in the direction of the event which is N_H=1.81 10^20 cm-2 (Karberla 2005). \nWe thank the Swift team for approving this ToO request.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater", "Galaxy", "Supernova", "Pulsar" ] }, "answerKey": "C" }, { "id": "atel_3475", "message": "Title: New deep minimum of the cataclysmic variable V794 Aquilae\nAuthors: S. Boeva, G. Latev, K. Stoyanov, R. Zamanov (Institute of Astronomy and National Astronomical Observatory, Bulgaria)\nDate: 6 Jul 2011; 14:17 UT\nProvenance: R. K. Zamanov (rkz@astro.bas.bg)\nSubjects: Optical, Cataclysmic Variable\nDescription: We report a deep low state of the cataclysmic variable star V794 Aql. On the night of 2011 July 4, we observed V794 Aql with the 50/70cm Schmidt and 60cm telescopes of the National Astronomical Observatory Rozhen, Bulgaria, equipped with FLI PL 16803 and FLI PL 9000 CCD cameras, respectively. The obtained average magnitudes are as follows: \nJD=2455747.52, B = 18.49 ± 0.12 – 3x300 sec exp-time; \nJD=2455747.50, V = 18.40 ± 0.11 – 5x300 sec; \nJD=2455747.50, R = 17.77 ± 0.05 – 4x300 sec; \nJD=2455747.49, I = 17.31 ± 0.09 – 3x300 sec. \nThe low photometric states of members of the nova-like VY Sculptoris class are rare phenomena, caused by the cessation of mass transfer. After the first possible low state of V794 Aql in 1932, there are two known deep minima of brightness - in 1985 (Honeycutt & Schlegel, 1985, PASP, 97, 1189) and in 1995 (Honeycutt & Robertson, 1998, AJ, 116, 1961), when the star has faded to V=17-18 mag. Our observations indicate that V794 Aql is in a deep minimum (fainter than V=18 mag) now. \nFollow-up observations are essential for further study of this low state.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Neutron star", "Accreting object", "Variable star" ] }, "answerKey": "D" }, { "id": "atel_3540", "message": "Title: Spectroscopic Confirmation of N Lup 2011\nAuthors: Frederick M. Walter (Stony Brook University)\nDate: 9 Aug 2011; 20:55 UT\nProvenance: Fred Walter (fwalter@mail.astro.sunysb.edu)\nSubjects: Optical, Nova\nDescription: I confirm that the eruptive variable in Lupus, reported as a possible nova (AAVSO Special Notice #247; vsnet-alerts 13560 and 13569) is an Fe II nova near maximum. A low dispersion blue spectrum (4.1A resolution; 3700-5400A) obtained with the SMARTS 1.5m RC spectrograph at Cerro Tololo, Chile, on 2011 August 9.013 UT shows emission lines of the Hydrogen Balmer series Hβ through H-10, and of Fe II multiplet 42 atop a flat continuum. Hβ has an equivalent width of -130A. The strong emission lines have P Cygni profiles, with absorption components blueshifted by about 1000 km/s", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Globular cluster", "Supernova", "Nova" ] }, "answerKey": "D" }, { "id": "atel_3625", "message": "Title: MAXI and RXTE-ASM detect superburst candidate for 4U 1820-30\nAuthors: Jean in 't Zand (SRON), Motoko Serino (RIKEN), Nobuyuki Kawai (Tokyo Tech), Craig Heinke (U. Alberta)\nDate: 2 Sep 2011; 13:03 UT\nProvenance: Jean in' t Zand (jeanz@sron.nl)\nSubjects: X-ray, Binary, Neutron Star\nDescription: Referred to by ATel #: 4622, 14871\nOn March 17, 2010, MAXI/GSC and RXTE/ASM data detected a flare from the prototypical ultracompact X-ray binary 4U 1820-30 that has a duration of at least 57 min and a peak 4-10 keV flux of 1.9 Crab units. Given the duration and the fact that 4U 1820-30 for decades only exhibited fluxes below 0.5 Crab (e.g., Priedhorsky & Terrell, ApJ, 284, L17, 1984; Zdziarski et al., MNRAS 377, 1006, 2007) except during thermonuclear (type-I) X-ray bursts (e.g., Galloway et al., ApJS 179, 360, 2008), we tentatively identify this as a superburst. This would be the second superburst from 4U 1820-30, 10.5 yr after the first one (Strohmayer & Brown, ApJ, 566, 1045, 2002). \nThe MAXI/GSC flare data consist of a single 50-s long scan over the source centered on 17:22:03 UT (MJD 55272.72365) during which the triangular scan response is accurately followed so that the source must be constant during this time within statistical margins. Ordinary X-ray bursts from 4U 1820-30 are always shorter with e-folding decay times that are less than 8 s (e.g., Cornelisse et al., A&A, 405, 1033, 2003; Galloway et al. 2008). The fitted 4-10 keV flux is 1.9+/-0.1 Crab units. This is, within 10%, consistent with the peak flux of ordinary X-ray bursts from 4U 1820-30 (e.g., Galloway et al. 2008). The last MAXI scan over 4U 1820-30 prior to the high point is 1.5 hr before. It shows a flux of 0.30+/-0.05 Crab units. In the 24 hrs prior to the high point the average flux is 0.33 +/- 0.02 Crab units. The first data point after the high point is 1.5 hr later, at 0.50+/-0.06 Crab. The next one is 12 hr later at 0.43+/-0.06 Crab. \nThe ASM data nearest to the MAXI high point are 2 consecutive dwells 57 min afterward with an average flux of 0.50+/-0.03 Crab. The next ASM dwell is 9.0 hrs afterward with a flux of 0.30+/-0.03 Crab. The last ASM data prior to the high MAXI point is 15.9 hr before, at a flux of 0.33+/-0.02 Crab. \nThe flux histories from MAXI and ASM are roughly equivalent with an e-folding decay time of 0.5+/-0.1 hr. This is 2 times smaller than the first superburst, but the sampling is very sparse. In fact, the flux profile is consistent with the profile of the first superburst if it would have started roughly 0.5 hr before the high MAXI point. \nThe (10-20 keV)/(4-10 keV) flux hardness ratio of the high MAXI data point is 0.65+/-0.06 (after subtraction of pre-flare fluxes). The ratio is 0.25+/-0.04 for the 24-hr pre-flare data. This rough doubling of the hardness ratio is as expected between the persistent and thermonuclear emission. \nThe first SWIFT-BAT data point after the MAXI high point is 1.2 hr afterward. The 15-50 keV is 1.6+/-0.4 times higher than the daily average. \nThe 10.5 yr superburst recurrence time would be consistent with the ~13 yr prediction by Strohmayer & Brown (2002) for 4U 1820-30. Note that this applies to a hydrogen-deficient system which is different than for all other known superbursters except possibly 4U 0614+09 (Keek & in 't Zand, Proc. 7th INTEGRAL Workshop, 2008). However, the duty cycles of RXTE-ASM and MAXI for superbursts are not a perfect 100% but perhaps around 50% and, so, there is a non-negligible chance that a superburst was missed.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Neutron star", "Star and stellar system", "Globular cluster" ] }, "answerKey": "B" }, { "id": "atel_3690", "message": "Title: UV Brightening of PSN J10081059+5150570\nAuthors: P. Roming (SwRI), T. Pritchard (PSU), P. Brown (UU)\nDate: 18 Oct 2011; 19:12 UT\nProvenance: Pete Roming (proming@swri.edu)\nSubjects: Optical, Ultra-Violet, Supernovae, Variables\nDescription: Referred to by ATel #: 3749, 3895, 4062\nPSN J10081059+5150570 is a supernova impostor in the galaxy UGC 5460 (CBAT 2851). Swift began monitoring the object on JD-2455838 and is continuing the monitoring campaign. Compared to the first epoch of Swift-UVOT observations, we report the object has brightened by ~4 mag in the uvw2 and uvm2 filters, ~3 mag in the uvw1 and u filters, ~1.5 mag in the b filter, and ~1 mag in the v. The current (~JD-2455852.5) magnitude of PSN J10081059+5150570 is 15.67+/-0.12, 15.49+/-0.08, 15.38+/-0.09, 14.83+/-0.09, 15.48+/-0.08, and 15.35+/-0.07 for the uvw2, uvm2, uvw1, u, b, and v filters, respectively. No correction for the Galactic extinction in the direction of the object (E(B-V)=0.010 mag) has been performed. The contribution of the host galaxy has also not been subtracted. We are grateful to the Swift team for making these observations possible. Further observations are ongoing.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova, Variable star", "Supernova, Galaxy", "Supernova, Stellar evolution", "Supernova, Black hole" ] }, "answerKey": "A" }, { "id": "atel_3800", "message": "Title: A new nova candidate in M31\nAuthors: Y. Cao (Caltech) and M. M. Kasliwal (Carnegie Institution for Science & Princeton University) on behalf of the Palomar Transient Factory collaboration\nDate: 9 Dec 2011; 05:31 UT\nProvenance: Yi Cao (smartcaoyi@gmail.com)\nSubjects: Optical, Nova\nDescription: Referred to by ATel #: 3825\nWe report discovery of a new nova candidate in M31 at RA(J2000)=00:42:06, DEC(J2000)=+41:01:29 on Dec 7.08 with a magnitude of R=18.6. Nothing was there on the image taken on Dec 6.33 with a limiting magnitude of R=19.5. All images are taken in daily monitoring of M31 in PTF (Rau et al. 2009; Law et al. 2009). Photometry is calibrated with the USNO-B1.0 catalog. This object is internally designated as PTF11rdv.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Magnetar", "Binary system", "Galaxy" ] }, "answerKey": "A" }, { "id": "atel_3950", "message": "Title: Swift/XRT follow-up observation of IGR J18179-1621\nAuthors: J. Li, S. Zhang, Y. P. Chen (IHEP, China), M. Tuerler (ISDC, Univ. of Geneva, Switzerland), J. Chenevez (DTU Space, Denmark); E. Bozzo, C. Ferrigno, A. Tramacere (ISDC, U. of Geneva, Switzerland); I. Caballero, J. Rodriguez (CEA Saclay, France); M. Cadolle-Bel, C. Sanchez-Fernandez (ESA/ESAC, Spain); M. del Santo, A. Tarana, M. Fiocchi(INAF/IASF-Roma, Italy), P. R. den Hartog (Stanford, USA), I. Kreykenbohm, M. Kuehnel (Dr. Karl Remeis Obs. and ECAP, Germany), A. Paizis (INAF/IASF-Milano, Italy), G. Puehlhofer (IAA-Tuebingen, Germany), K. Watanabe (FGCU, USA), G. Weidenspointner (MPE and MPI HLL, Germany)\nDate: 2 Mar 2012; 13:29 UT\nProvenance: Jian Li (jianli@ihep.ac.cn)\nSubjects: X-ray, Gamma Ray, Binary, Black Hole, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 3988, 13737\nFollowing the discovery of IGR J18179-1621 (Tuerler et al. ATel #3947) on 2012-02-29, we requested two Swift ToO, which were executed on 2012-02-29 from 20:10:02 to 22:00:01 UT and on 2012-03-01 15:25:55 from to 2012-03-01 15:59:48 UT for a total exposure of ~3.9 ks. These two observations were carried out in Photon Counting mode and the sky image is piled up. We have corrected the pile up effect in our analysis. Using the online Swift tool we find an enhanced position of \n \nRA = 274.4675 (18h 17m 52.20s), \nDec = -16.3589 (-16d 21' 31.9'') (J2000), \n \nwith a 90% confidence level error of 2.2 arcsec, consistent with the position measured by INTEGRAL/JEM-X (ATel #3947)(We have used the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue, see http://www.swift.ac.uk/user_objects and Evans et al. 2009, MNRAS, 397, 1177). \n \n \nThe two XRT spectra can be well fitted (reduced chi^2=0.72 for 47 dof and reduced chi^2=0.98 for 49 dof ) with an absorbed power-law model. The spectral parameters we derived in the 1-10 keV energy band are (model and flux uncertainties are 90% c. l.): In 2012-02-29, N_H = 11.0+/-2.7 e22 atoms/cm2 and photon index = 0.4+/-0.4. The 1-10 keV unabsorbed flux is 4.5+/-0.5 e-10 erg/cm2/s. In 2012-03-01, N_H = 15.1+/-3.6 e22 atoms/cm2 and photon index = 0.7+/-0.4. The 1-10 keV unabsorbed flux is 4.2+/-0.8 e-10 erg/cm2/s. \n \n \nWe derive from Swift/XRT a flux, between 3-10 keV, of 21.5+/-1.8 mCrab on 2012-02-29 and 22.0+/-2.2 mCrab on 2012-03-01, consistent with what was derived from JEM-X observation (ATel #3947).This may mean that IGR J18179-1621 now is still in a relatively bright phase. \n \n \nNo significant variation of the source spectral parameters are revealed in the XRT data. \n \n \nWe notice that the absorption is much larger than the Galactic column density (1.2e22 atoms/cm2 as estimated at the source position by using the tool available at the HEASARC website, Kalberla et al. 2005), and hence indicates an additional absorption intrinsic to the source. \n \n \nIn ATel #3947 absorption line was claimed in joint ISGRI/JEMX energy spectrum, suggestive of having a high mass X-ray binary pulsar. We confirm the detection of a possible period at ~11.8 seconds by using a Lomb-Scargle method on all available Swift/XRT data corrected for pile-up. This is consistent with the period reported by J. P. Halpern (ATEL #3949). The estimated pulsed fraction is ~22%. \n \n \nAn infrared counterpart is found within the XRT error box (at 0.33\"): 2MASS J18175218-1621316 with coordinates RA =274.467438 dec=-16.358791 and an uncertainty of about 0.1\". This source has a well measured magnitude only in the Ks band: Ks=11.14.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system, Near-Earth object", "Binary system, Pulsar", "Circumstellar disk, Pulsar", "Stellar evolution, Pulsar" ] }, "answerKey": "B" }, { "id": "atel_4050", "message": "Title: INTEGRAL catches a type-I X-ray burst from the unclassified X-ray source 1RXS J180408.9-342058\nAuthors: J. Chenevez (DTU Space, Denmark), E. Kuulkers (ESA/ESAC, Spain), S. Brandt (DTU Space, Denmark), R. Wijnands (UvA, The Netherlands), J. Alfonso-Garzón (CAB/INTA-CSIC, Spain), V. Beckmann (APC, France), T. Bird (Southampton, UK), M. Del Santo (INAF/IASF-Roma, Italy), A. Domingo (CAB/INTA-CSIC, Spain), K. Ebisawa (ISAS, Japan), P. Jonker (SRON, The Netherlands), P. Kretschmar (ESA/ESAC, Spain), C. Markwardt (GSFC, USA), T. Oosterbroek (ESA/ESTEC, The Netherlands), A. Paizis (INAF-IASF, Italy), K. Pottschmidt (UMBC/NASA GSFC, USA), C. Sánchez-Fernández (ESA/ESAC, Spain)\nDate: 18 Apr 2012; 12:02 UT\nProvenance: Jerome CHENEVEZ (jerome@space.dtu.dk)\nSubjects: X-ray, Neutron Star, Transient\nDescription: Referred to by ATel #: 4085, 6997, 7008, 7039, 7255, 7352\nDuring INTEGRAL Galactic Bulge monitoring (ATel #438; Kuulkers et al. 2007, A&A, 466, 595) observations performed on April 16, 2012, between 5:12 and 8:53 (UTC), the twin X-ray monitor JEM-X detected an X-ray burst starting at UTC 8:37:09 from the position: \nRA= 271.020° \nDEC=-34.344° \nwith an error radius of 1.2' (at 95% confidence level). \nThis position lies only 57'' from the unclassified X-ray source 1RXS J180408.9-342058, and we tentatively associate the origin of the burst with this source. \n \nThe burst peak flux reaches 3.2 Crab (9.3 ×10-8 erg/cm2/s) in the 3-25 keV band. The burst duration, rise time, and exponential decay measured in the same energy band are about 45 s, 8 s and 35 s, respectively (see Galloway et al., ApJS 179, 360, 2008, for definitions). \nThe hardness evolution shows evidence for hardening during the rising phase and cooling during the decay of the burst. \n \nThe source is not detected in the mosaic images of the whole observation excluding the burst time interval (for a remaining combined effective exposure of 1.5 ks), leading to persistent flux upper limits at 3 σ of 6 mCrab (10-10 erg/cm2/s) and 3 mCrab (3 × 10-11 erg/cm2/s) between 3-10 keV and 10-25 keV, respectively. \n \nWe have performed a follow-up observation with Swift on April 17, between 18:44 and 20:16 UTC for a total exposure time of 1 ks. \nA single object is detected in the JEM-X error circle at: \nRA= 271.0335° \nDec= -34.3471° \nwith an error radius of 3.8'' (90% confidence). \nThis position lies 15.6'' from the position of 1RXS J180408.9-342058 with an error of 16'' in the ROSAT source catalog (Voges et al., A&A 349, 389, 1999). \n \nThe Swift/XRT spectrum fitted by an absorbed power-law model (nH= 4.6-2.8+4.1 ×1021 cm-2 and photon index = 3.6-1.2+1.8) leads to a 0.3-10 keV flux of 1.11-0.33+0.50 × 10-12 erg/cm2/s. The 0.3-10 keV unabsorbed flux is 9.1-6.6+75.8 ×10-12 erg/cm2/s. \n \nWe conclude that the observed event is consistent with a type I (thermonuclear) X-ray burst, and 1RXS J180408.9-342058 is thus harboring a neutron star as primary. Assuming the burst reaches the Eddington luminosity limit for helium-rich material of LEdd=3.8 ×1038 erg/s (Kuulkers et al., A&A 399, 663, 2003), this places the source at an upper limit distance of 5.8 kpc. Hence, the derived unabsorbed flux translates to a persistent 0.3-10 keV upper limit luminosity of only 3.7-2.6+31.3 ×1034 erg/s.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Neutron star", "Stellar evolution", "Globular cluster" ] }, "answerKey": "B" }, { "id": "atel_4110", "message": "Title: Detection of hard X-ray emission from Nova Sgr 2012 with Swift\nAuthors: Thomas Nelson (Minnesota), Koji Mukai (UMBC and NASA/GSFC), Jennifer Sokoloski (Columbia), Laura Chomiuk (NRAO and CfA), Michael Rupen (NRAO) and Amy Mioduszewski (NRAO)\nDate: 11 May 2012; 19:14 UT\nProvenance: Thomas Nelson (tnelson@physics.umn.edu)\nSubjects: Ultra-Violet, X-ray, Nova\nDescription: We observed Nova Sgr 2012 (PNV J17452791-2305213) with the Swift satellite on 2012 May 10, 40 days after the discovery of this nova. The total exposure time with the XRT instrument was 6280 s. In contrast to the non-detections reported in ATels #4061 and #4088, Swift/XRT clearly detected X-ray emission from the nova on 2012 May 10.\nA total of 249 source counts were detected within a circular region with a radius of 20 pixels centered on the position of the nova, resulting in a 0.3-10 keV count rate of 0.039 c/s. The source spectrum was quite hard, with emission detected at energies up to 10 keV. Modeling the spectrum as an absorbed thermal plasma with the APEC model in XSpec, we find a best fit N(H) of (3 +/- 1) x 10^21 cm^-2, and a lower limit to the plasma temperature of 2.7 x 10^8 K (kT > 23 keV). The 0.3-10 keV flux is 2.7e-12 erg/s/cm^2.\nThe UVOT instrument obtained images in the UVM2 band, with a total exposure time of 6213 s. Nova Sgr 2012 was detected with an average UVM2 magnitude of 16.0 +/- 0.2.\nThese observations were obtained as part of the E-Nova project (formerly the EVLA Nova Project, see link below), an effort to obtain high quality radio light curves and complimentary multiwavelength observations of novae visible to the Jansky Very Large Array.\nE-Nova Project", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova, Circumstellar disk", "Quasar, Variable star", "Nova, Variable star", "Nova, Pulsar" ] }, "answerKey": "C" }, { "id": "atel_4225", "message": "Title: Fermi LAT detection of renewed gamma-ray activity from the FSRQ PKS 2326-502\nAuthors: F. D'Ammando (Dip. Fisica, Univ. Perugia) and E. Torresi (INAF-IASF Bologna) on behalf of the Fermi Large Area Telescope Collaboration\nDate: 29 Jun 2012; 06:03 UT\nProvenance: Filippo D'Ammando (filippo.dammando@iasf-roma.inaf.it)\nSubjects: Gamma Ray, >GeV, Request for Observations, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 4232\nThe Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope has observed an increasing gamma-ray flux from a source positionally consistent with the Flat Spectrum Radio Quasar PKS 2326-502 (also known as 2FGL J2329.2-4956, Nolan et al. 2012, ApJS, 199, 31; R.A.=23:29:20.880 Dec.=-49:55:40.68, J2000.0, Costa and Loyola 1996, A&AS, 115, 75) at redshift z=0.518 (Jauncey et al. 1984, ApJ, 286, 498). \nPreliminary analysis indicates that the source on June 27, 2012 showed a gamma-ray daily flux (E>100 MeV) of (1.4+/-0.3) x10^-6 ph cm^-2 s^-1 (errors are statistical only), a factor of 11 greater than the average flux reported in the second Fermi LAT catalog (2FGL, Nolan et al. 2012, ApJS, 199, 31). High level gamma-ray activity from this source was detected in August 2010 by Fermi-LAT (ATel #2783) and November 2010 by AGILE (ATel #3008). \nThis source is one of the \"LAT Monitored Sources\" and consequently a preliminary estimation of the daily gamma-ray flux observed by Fermi LAT is publicly available (link: http://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/ ). \nBecause Fermi operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. In consideration of the ongoing activity of this source we encourage multiwavelength observations. For PKS 2326-502 the Fermi LAT contact person is Filippo D'Ammando (filippo.dammando@fisica.unipg.it). \nThe Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Minor body", "Quasar", "Pulsar" ] }, "answerKey": "C" }, { "id": "atel_4380", "message": "Title: Swift J174510.8-262411: GROND discovery of a candidate near-IR counterpart\nAuthors: Arne Rau, Fabian Knust, D. Alexander Kann, Jochen Greiner (all MPE Garching) \nDate: 17 Sep 2012; 15:21 UT\nProvenance: Arne Rau (arau@mpe.mpg.de)\nSubjects: Optical, Transient, Variables\nDescription: Referred to by ATel #: 4381, 4388, 4394, 4410, 4417, 4456, 4760\nWe observed the new transient Swift J174510.8-262411 / Swift trigger #533836 (Cummings et al. 2012, GCN 13744; Cummings et al. 2012, GCN #13745) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) at the 2.2m MPG/ESO telescope at La Silla Observatory (Chile). Observations were obtained on September 17th 01:40 UT and 03:49 UT for ~20min each and were compared to publicly available deep near-IR images obtained on June 24th 2011 as part of the VISTA Variables in the Via Lactea Survey (Minniti et al. 2010, New Astronomy, 15, 433; Saito et al. 2010, The Messenger, 141, 24). \n \nWithin the 5.8\" Swift/XRT error circle (Cummings et al. 2012, GCN 13744) we identify a variable source in the GROND images that has brightened by approx. 3 magnitudes with respect to the deeper VISTA J-band image. We suggest this object to be the near-IR counterpart of Swift J174510.8-262411. Its position is \n \nRA(J2000) = 17:45:10.82 \nDec(J2000) = -26:24:12.7 \n \nwith an uncertainty of 0\"4 in both coordinates and it has an observed AB magnitude of \n \nJ~16.5 +/- 0.5 \n \ncalibrated against 2MASS field stars. The high stellar density and moderate seeing (~1\"9) lead to a rather large uncertainty in the photometry and an further analysis (e.g., multi-band magnitudes and spectral energy distribution) requires future observations under more favorable conditions. \n \nAn image of the field can be found here: \n \nhttp://www.mpe.mpg.de/~arau/transients/swiftJ1745-2624.html", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Active galactic nucleus", "Binary system", "Black hole" ] }, "answerKey": "A" }, { "id": "atel_4440", "message": "Title: Swift follow-up of the flaring blazar OJ 248\nAuthors: F. D'Ammando (Univ. Perugia, INFN), and M. Orienti (Univ. Bologna, INAF-IRA Bologna) on behalf of the Fermi Large Area Telescope Collaboration\nDate: 1 Oct 2012; 09:15 UT\nProvenance: Filippo D'Ammando (filippo.dammando@fisica.unipg.it)\nSubjects: Optical, Ultra-Violet, X-ray, Gamma Ray, AGN, Black Hole, Blazar, Quasar\nDescription: Following the gamma-ray flaring activity of the flat spectrum radio quasar OJ 248 (also known as 2FGL J0830.5+2407, Nolan et al. 2012, ApJS, 199, 31) detected by Fermi LAT starting from 2012 September 23 (ATel #4421) a Swift target of opportunity observation was performed on September 28. \nSwift/XRT data were taken in Photon Counting mode for a total exposure of about 4.0 ksec. The X-ray spectrum (0.3-10 keV) can be fit by an absorbed power law model with a HI column density consistent with the Galactic value in the direction of the source (n_H = 2.9 x 10^20 cm^-2, Kalberla et al. 2005, A&A, 440, 775) and a photon index of 1.5+/-0.1. The corresponding observed 0.3-10 keV flux is (10.1+/-0.8) x10^-12 erg cm^-2 s^-1. This flux is about a factor of 5 higher than that observed by Swift/XRT on 2012 March 30, (1.8+/-0.7) x10^-12 erg cm^-2 s^-1, with a photon index of 1.8+/-0.4. Taking into consideration the Swift/XRT observations performed during 2008-2012, OJ 248 on 2012 September 28 reached the highest count rate in the 0.3-10 keV energy range (see http://www.swift.psu.edu/monitoring/source.php?source=QSOB0827+243 ) . \nSimultaneous Swift/UVOT observations on 2012 September 28 found OJ 248 about 0.7 mag brighter in U-band (U = 15.93+/-0.06), 0.4 mag brighter in W1-band (W1 = 15.96+/-0.07), and 0.3 mag brighter in W2-band (W2 = 16.20+/-0.06) compared to the UVOT observations performed on 2012 March 30. \nSwift observations confirmed the ongoing high activity of OJ 248. Further multiwavelength observations are encouraged. For this source the Fermi LAT contact person is M. Orienti (orienti@ira.inaf.it). \nWe would like to thank the Swift Team for making these observations possible.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Black hole, Quasar", "Active galactic nucleus, Supernova, Quasar", "Active galactic nucleus, Black hole, Stellar evolution", "Active galactic nucleus, Black hole, Repeater" ] }, "answerKey": "A" }, { "id": "atel_4575", "message": "Title: PESSTO spectroscopic observation of LSQ12fuc\nAuthors: M. Turatto (INAF - Padova Astronomical Observatory), S. Marchi (U. de Chile), S. Gonzalez-Gaitan (U. de Chile), \t\tF. Bufano (UNAB), F. Forster (U. de Chile), J. Anderson (U. de Chile), \t\tS. Taubenberger (MPA Garching), S. Valenti (UCSB/LCOGT), A. Pastorello, \t\tS. Benetti (INAF - Padova Astronomical Observatory), S. J. Smartt, \t\tK. Smith, D. Young (Queens University Belfast), M. Sullivan (University \t\tof Southampton), A. Gal-Yam, O. Yaron (Weizmann Institute for Science), \t\tC. Baltay, N. Ellman, E. Hadjiyska, R. McKinnon, D. Rabinowitz, E. \t\tS. Walker (Yale University), U. Feindt, M. Kowalski (Universitat Bonn), P. Nugent (LBL Berkeley)\nDate: 15 Nov 2012; 16:55 UT\nProvenance: Stefano Benetti (stefano.benetti@oapd.inaf.it)\nSubjects: Optical, Supernovae, Transient\nDescription: PESSTO, the Public ESO Spectroscopic Survey for Transient Objects (see Valenti et al., ATel #4037; http://www.pessto.org ), reports the spectroscopic observation of SN LSQ12fuc (ATel 4537) with the ESO New Technology Telescope at La Silla on 2012 November 05.24 UT using EFOSC2 and Grism 13 (3700-9300A, 18A resolution). The object shows lines of HI, NaI, CaII, FeII with P-Cyg profiles typical of SNII. The expansion velocity of the photosphere is significantly slow (v(Halpha)= 3850 km s-1) compared to normal SNII. The best match provided by GELATO (Harutyunyan et al. 2008, A.Ap. 488, 383) is with the low-luminosity SNe 1994N and 1999br one month after maximum (Pastorello et al. 2003, MNRAS 347, 74). Despite such spectral similarity, LSQ12fuc is about 2 mag brighter, with an absolute magnitude -16.5 derived from LSQ photometry. Superposed to the SN spectrum are visible narrow components of H(aplha), H(beta) and weak [SII] 6717-6731 at a redshift compatible to that of the host galaxy (z=0.0430) thus probably associated to an underlying HII region.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Globular cluster", "Star and stellar system", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_4625", "message": "Title: Broadband Photometry of 214869 (2007 PA8): A Slowly Rotating Potentially Hazardous Asteroid.\nAuthors: M. Hicks (JPL/Caltech), M. Brewer (VCC), J. Somers (Moorpark College)\nDate: 7 Dec 2012; 00:37 UT\nProvenance: Michael D. Hicks (Michael.Hicks@jpl.nasa.gov)\nSubjects: Optical, Asteroid, Planet (minor), Near-Earth Object, Potentially Hazardous Asteroid\nDescription: The near-Earth asteroid 214869 (2007 PA8) was discovered on 2007 August 09 by the LINEAR NEO survey (MPEC 2007-P35). With a Minimum Orbit Intersection Distance MOID=0.0214 AU and expected diameter D~2km, this object has been designated as a Potentially Hazardous Asteroid (PHA) by the IAU Minor Planet Center. Also, with a Tisserand Invarient T_J=2.95, 2007 PA8's orbit is consistent with the Jupiter-family periodic comets. The asteroid was the subject of extensive radar observation with the Goldstone 70-m system during the 2012 apparition (http://www.jpl.nasa.gov/news/news.php?release=2012-350), constraining the object's size, shape, and rotational state. We obtained two nights of Bessel BVRI and three nights of Bessel R observations of the object at the JPL Table Mountain Observatory (TMO) 0.6-m telescope. Our observational circumstances are summarized in Table 1. \n \nThe object's rotationally averaged colors (B-R=1.180+/-0.019 mag; V-R=0.415+/ 0.011 mag; R-I=0.326+/-0.010 mag) were found most compatible with an Xc-type spectral classification (Bus Taxonomy)/C-type (Tholen Taxonomy). This association was obtained through a comparison of our colors with the 1341 asteroid spectra in the SMASS II database (Bus & Binzel 2002) [Figure 1 and Table 2]. A solar phase curve generated from our data [Figure 2] yielded an absolute magnitude H_R=16.07 mag and phase parameter g=0.08. Both the object's colors and solar phase behavior are consistent with a relatively dark and primitive surface composition. \n \nAlthough our photometry was sparse, Fourier analysis allowed us to estimate a best-fit rotational period P_rot=95.1+/-3.4 hr [Figure 3], within the 3-4 day period range reported from the radar observations. Our colors and phase curve allowed us to determine an absolute magnitude H_V = 16.47 mag. For small solar system bodies in this size range (16< H_V <17), 2007 PA8 is rotating quite slowly [98% percentile; Figure 4]. Assuming a geometric albedo rho=0.05, typical for C-type asteroids, we compute an effective diameter D~3km, much larger than the D~1.6km reported by the JPL radar team. 2007 PA8 would require an anomalously high albedo rho=0.18 to to match the radar-derived effective diameter. \n \nCopyright 2012. All rights reserved. The research described in this telegram was carried out at the Jet Propulsion Laboratory, under a contract with the National Aeronautics and Space Administration. The student participation was supported by the National Science Foundation under REU grant AST-1156756 to Los Angeles City College.. \n \n\n \n \n Table 1: Observational Circumstances. \n \n UT Time r delta phase V Filters Observers \n [AU] [AU] [deg] [mag] \n 2012 10 02.26 1.240 0.241 6.4 14.1 R Hicks \n 2012 10 17.34 1.124 0.132 14.9 13.0 BVRI Brewer, Hicks \n 2012 10 28.36 1.052 0.068 29.1 11.8 BVRI Somers, Hicks \n 2012 10 30.35 1.041 0.059 34.3 11.6 R Hicks \n 2012 10 31.35 1.035 0.055 37.6 11.6 R Hicks \n \n \n Table 2: Best-fit SMASS II spectral analogs. \n \n Taxonomic Class \n Misfit Object Name (Tholen) (Bus) \n 1.067 1015 Christa C Xc \n 1.191 4256 Kagamigawa Xc \n 1.419 209 Dido C Xc \n 1.741 52 Europa CF C \n 1.879 2560 Siegma Xc", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution, Near-Earth object", "Minor body, Near-Earth object", "Minor body, Binary system", "Minor body, Magnetar" ] }, "answerKey": "B" }, { "id": "atel_4710", "message": "Title: Bright PSN in PGC082417\nAuthors: S. Shurpakov, P. Balanutsa, V. Lipunov, D. Denisenko, E. Gorbovskoy, V. Yecheistov, N. Tiurina, V. Kornilov, A. Belinski, N. Shatskiy, V. Chazov, A. Kuznetsov, D. Zimnukhov (Moscow State University, SAI), V. Krushinsky, I. Zalozhnih, A. Popov, A. Bourdanov, A. Punanova (Ural Federal University), K. Ivanov, S. Yazev, N. Budnev, E. Konstantinov, O. Chuvalaev, V. Poleshchuk, O. Gress (Irkutsk State University), A. Parkhomenko, A. Tlatov, D. Dormidontov, V. Senik (Kislovodsk solar station of the Pulkovo observatory RAS), V. Yurkov, Y. Sergienko, D. Varda, E. Sinyakov (Blagoveshchensk Educational University), V. Shumkov, P. Podvorotny (MASTER team members), H. Levato, C. Saffe (ICATE), C. Mallamaci, C. Lopez and F. Podest (Observatorio Astronomico Felix Aguilar; OAFA)\nDate: 7 Jan 2013; 11:24 UT\nProvenance: Vladimir Lipunov (lipunov2007@gmail.com)\nSubjects: Optical, Supernovae\nDescription: Referred to by ATel #: 4711\nMASTER OT J093135.12+352342.4 - PSN\nMASTER-Amur auto-detection system discovered OT source at (RA, Dec) = 09h 31m 35.12s +35d 23m 42.4s on 2013-01-06.78565 UT. The OT unfiltered magnitude is 16.7m (limit 18.9m). The OT is seen in 2 images. There is no minor planet at this place. We have reference image without OT on 2012-12-21.73097 UT with unfiltered magnitude limit 19.0m. \nThis is PSN in PGC082417 galaxy with offset 2.2E and 11.6N arcsec. \nSpectral observations are required. \nThe discovery and reference images are available at: http://observ.pereplet.ru/images/034115.13152303.9.png \nList of optical transients discovered by MASTER\nGlobal MASTER Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Quasar", "Accreting object", "Interstellar medium" ] }, "answerKey": "A" }, { "id": "atel_4775", "message": "Title: Latest OIR Mags of PKS 1424-41\nAuthors: Imran Hasan, Emily MacPherson, Michelle Buxton, Charles Bailyn, Meg Urry, Jedidah Isler (Yale University)\nDate: 31 Jan 2013; 21:42 UT\nProvenance: Michelle Buxton (buxton@astro.yale.edu)\nSubjects: Infra-Red, Optical, Blazar\nDescription: Referred to by ATel #: 4819\nWe report optical and near-infrared magnitudes for the Blazar PKS 1424-41. This object was detected on January 8th by the LAT Fermi Gamma-ray Telescope which reported an increasing gamma-ray flux (see ATel #4714). Fermi also provided an R magnitude measurement of 14.74 (+/-0.04) performed by ATOM. Swift/XRT has supplied a follow-up observation in the X-Rays, and reported an X-Ray flux increase on January 9th compared to previous observations in May of 2011 (see ATel #4717). Additional SWIFT observations were performed January 24th and 27th, finding the X-ray flux to still be increasing (see ATel #4770). As part of our blazar monitoring program, we observe blazars reported to be in a high flux state by Fermi-LAT in optical and near-infrared bands. We are currently observing PKS 1424-41 on a daily cadence. PKS 1424-41 was observed on January 28th and 29th, 2013 under photometric conditions using the SMARTS 1.3 meter telescope with the ANDICAM instrument, located at CTIO. For January 28th we find the following magnitudes: B=15.43, V=14.85, R=14.29, J=12.48, K=10.63; For January 29th we find the following magnitudes: B=15.33, V=14.75, R=14.24, J=12.25, K=10.56. We estimate our errors to be +/- 0.03 mag in the optical and +/- 0.05 mag in the near-infrared. Further multiwavelength observations are encouraged. We will continue to monitor this source on a nightly cadence using the SMARTS 1.3m telescope and ANDICAM instrument.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Black hole", "Minor body", "Galaxy" ] }, "answerKey": "B" }, { "id": "atel_4890", "message": "Title: Classification of PSN J14244257-0312309 as an Old Type II Supernova\nAuthors: M. Childress, R. Scalzo, F. Yuan, B. Tucker, B. Schmidt (Australian National University)\nDate: 15 Mar 2013; 03:54 UT\nProvenance: Michael Childress (mjc@mso.anu.edu.au)\nSubjects: Optical, Supernovae\nDescription: We report spectroscopic classification of the supernova candidate PSN J14244257-0312309 as an old Type II SN. We obtained a 20-minute spectrum of PSN J14244257-0312309 on 2013 March 14.72 with the Wide Field Spectrograph (WiFeS - Dopita et al., 2007, ApSS, 310, 255) on the ANU 2.3m telescope at Siding Spring Observatory, NSW Australia, using the B3000/R3000 gratings (3500-9800 A, 1 A resolution). The object spectrum was compared to supernova spectral templates using SNID (Blondin & Tonry, 2007, ApJ, 666, 1024), and the top matches were consistently Type IIP SNe at ages of 2-3 months with mean redshift of z=0.008+-0.003, consistent with the redshift of the apparent host galaxy NGC 5604 of 0.009166 (Theureau et al., 1998, A&AS, 130, 333 -- via NED). The SN has a cool spectrum characterized by broad P-cygni Halpha emission with an absorption mininum at 7700 km/s, and photospheric velocity of 3500 km/s as measured from Fe II 5018. The spectrum is consistent with a typical type IIP SN at the end of the plateau phase.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system", "Neutron star", "Supernova", "Variable star" ] }, "answerKey": "C" }, { "id": "atel_4950", "message": "Title: Radio Detection and X-ray Limits for Nova Cep 2013\nAuthors: L. Chomiuk (MSU/NRAO), T. Nelson (Minnesota), M. Rupen (NRAO), K. Mukai (UMBC/GSFC), J. Sokoloski, J. Weston, Y. Zheng (Columbia), A. Mioduszewski (NRAO), U. Munari (INAF Asiago\nDate: 4 Apr 2013; 17:36 UT\nProvenance: Laura Chomiuk (chomiuk@pa.msu.edu)\nSubjects: Radio, Ultra-Violet, X-ray, Nova\nDescription: Referred to by ATel #: 5269, 5375, 5389\nWe report radio continuum observations from the Karl G. Jansky Very Large Array (VLA) and X-ray observations from Swift for Nova Cep 2013 (discovered on 2013 Feb 2.4; CBET #3397). Nova Cep 2013 had an expansion velocity of 1,200 km/s and optical decline time of t_2 = 12 days (CBET #3397; ATel #4893); its optical light curve faded dramatically on March 13, perhaps signifying dust formation (ATel #4893). We have acquired two epochs of VLA observations to date. The first, on 2013 Feb 14.0 UT, yielded non-detections: 8 +/- 10 microJy at 7.4 GHz and -51 +/- 39 microJy at 36.5 GHz. The nova was detected in our second epoch, on 2013 Mar 22.5, with flux densities: 189 +/- 20 microJy at 7.4 GHz and 718 +/- 51 microJy at 36.5 GHz. We also obtained two observations of Nova Cep 2013 with the XRT and UVOT instruments onboard the Swift satellite. The first Swift observation was carried out on 2013 Feb 8.3 (5.9 days after discovery.) The total XRT exposure time was 3688 s. The source was not formally detected, although 2 photons were present within a 10 pixel radius circle centered on the source position. The resulting 99% confidence level upper-limit on the 0.3-10.0 keV count rate, determined using the Bayesian method of Kraft, Burrows and Nousek (1991) is 3.2 e-3 cts/s. A faint UV source is detected at the position of the nova in the 2629 s UVOT exposure, with a magnitude in the UVM2 filter (central wavelength = 2246 Angstroms) of 19.96 +/- 0.14 (stat) +/- 0.03 (sys). The second Swift observation was obtained on 2013 Feb 22.1 (19.7 days after discovery.) Nova Cep was not detected in the 5809 s XRT exposure, with a 99% confidence level upper limit on the 0.3-10 keV count rate of 8.0e-4 cts/s. The UVM2 magnitude measured during the 5727 s UVOT exposure was 19.54 +/- 0.08 (stat) +/- 0.03 (sys), about 0.4 mags brighter than in the first observation. Radio observations are ongoing, and we encourage observations at other wavelengths. Kraft, R. P., Burrows, D. N. & Nousek, J. A., 1991, ApJ 374, 334\nE-Nova Project", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus", "Nova", "Near-Earth object", "Galaxy" ] }, "answerKey": "B" }, { "id": "atel_5100", "message": "Title: Spectroscopic Classification of LSQ13apt (=PSN J22103421-2239480) with WiFeS\nAuthors: M. Childress, R. Scalzo, B. Tucker, F. Yuan, B. Schmidt (Australian National University), E. Hadjiyska, E. S. Walker, D. Rabinowitz, C. Baltay, N. Ellman, R. McKinnon, (Yale University), P. Nugent (LBL), U. Feindt, M. Kowalski (U. Bonn)\nDate: 4 Jun 2013; 07:07 UT\nProvenance: Michael Childress (mjc@mso.anu.edu.au)\nSubjects: Optical, Supernovae\nDescription: We report the spectroscopic classification of LSQ13apt (=PSN J22103421-2239480) with the Wide Field Spectrograph (WiFeS - Dopita et al., 2007, ApSS, 310, 255) on the ANU 2.3m telescope at Siding Spring Observatory, NSW Australia, using the B3000/R3000 gratings (3500-9800 A, 1 A resolution). LSQ13apt was discovered on 2013 May 29 by the La Silla Quest Survey (see Hadjiyska et al., ATel #3812) and on 2013 May 31 by Berto Monard. A 40 minute spectrum of the SN shows cler signatures of the Type Ia supernova, with Si II 6355, Ca II H&K and the IR triplet, and Fe II lines near 5000 A. Classification with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024) shows good matches to normal SNe Ia at maximum light at a mean redshift of 0.034 +- 0.006, consistent with the redshift of the putative host galaxy ESO 532-25 (z=0.031465 - Da Costa et al., 1991, ApJS, 75, 935). Given this host redshift, we calculate the velocity of the absorption minimum of the Si II 6355 line to be at 10,300 km/s. \n \n \n Name | RA (J2000) | Dec (J2000) | Disc. Date | Disc. Source | Disc Mag | z | Type | Phase | Notes \n \n LSQ13apt | 22 10 34.21 | -22 39 48.0 | 20130529 | LSQ, Monard | 17.4 | 0.034 | Ia | +0 | (1) \n \nDiscovered as PSN J22103421-2239480 by Monard on 2013 May 31", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Globular cluster", "Near-Earth object", "Supernova", "Neutron star" ] }, "answerKey": "C" }, { "id": "atel_5160", "message": "Title: VLA observations of iPTF13bvn (Erratum)\nAuthors: Atish Kamble (Harvard), Alicia Soderberg (Harvard), on behalf of a larger collaboration\nDate: 24 Jun 2013; 19:08 UT\nProvenance: Alicia M. Soderberg (asoderberg@cfa.harvard.edu)\nSubjects: Radio, Supernovae\nDescription: This is a correction to ATEL #5154. The date of VLA observations was incorrectly reported as 2013 April 27.0 UT. The correct date is 2013 June 19.1 UT. We apologize for any inconvenience.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Globular cluster", "Active galactic nucleus", "Near-Earth object" ] }, "answerKey": "A" }, { "id": "atel_5280", "message": "Title: ASAS-SN confirmation of PNV J00444739+4122136 in M31\nAuthors: J. L. Prieto (Princeton), B. Shappee, C. S. Kochanek, K. Z. Stanek (OSU), and the ASAS-SN team\nDate: 14 Aug 2013; 23:20 UT\nProvenance: Jose L. Prieto (jose@obs.carnegiescience.edu)\nSubjects: Optical, Nova, Transient\nDescription: We report the ASAS-SN detection of PNV J00444739+4122136, the M31 nova candidate discovered by K. Nishiyama & F. Kabashima on UT Aug. 14.683. The transient was detected, and flagged as a transient candidate, in images obtained on UT Aug. 14.415 at V=16.8 mag. No source is detected on UT Aug 12.58 or in earlier images (V > 17 mag).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Nova", "Variable star", "Galaxy" ] }, "answerKey": "B" }, { "id": "atel_5340", "message": "Title: Near Infrared Photometry of Nova Del 2013\nAuthors: Cass, A. C., Carlon, R. L., Corgan, D. T., Dykhoff, D. A., Gehrz, R. D. , and Shenoy, D. P. (Minnesota Institute for Astrophysics, Minneapolis, MN, USA)\nDate: 29 Aug 2013; 19:19 UT\nProvenance: Robert Gehrz (gehrz@astro.umn.edu)\nSubjects: Infra-Red, Nova\nDescription: Referred to by ATel #: 5404\nSubjects: Infra-Red, Nova We report RIJHKLM photometry of Nova Del 2013 taken on August 28.13 UT using an As:Si bolometer mounted on the 0.76-m infrared telescope of the University of Minnesota's O'Brien Observatory (Marine on St. Croix, Minnesota, USA). Vega (alpha Lyrae) was used as the standard star. On this date we find: R = 5.6 +/- 0.1, I = 5.2 +/- 0.1, J = 4.5 +/- 0.1, H = 4.7 +/- 0.1, K = 4.7 +/- 0.1, L = 3.3 +/- 0.2, M = +1.8 +/- 0.3. The deviations from an optically thin free-free slope are consistent with reports that strong near-IR hydrogen emission lines are present in the spectrum ( see ATELs 5336 and 5337). Our observations were made possible by a generous gift from Edward Glickman and technical support by A. Knutson and J. Marchetti.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Pulsar", "Quasar", "Repeater" ] }, "answerKey": "A" }, { "id": "atel_5425", "message": "Title: KAIT discovery of an uncataloged quasar at z = 1.08 : KAIT J20233743-19163425\nAuthors: W. Zheng, University of California, Berkeley, S. B. Cenko, NASA / Goddard Space Flight Center, P. L. Kelly, K. I. Clubb, M. L. Graham, J. Mauerhan, A. V. Filippenko, University of California, Berkeley\nDate: 26 Sep 2013; 22:22 UT\nProvenance: Weikang Zheng (zwk@umich.edu)\nSubjects: Optical, Quasar\nDescription: The object KAIT J20233743-19163425, which has a corresponding USNO B1.0 counterpart (0707-0791917) at the same location with B2 = 20.57 mag in USNO B1.0 catalog, was found to be brightened by more than 0.5 mag in the KAIT clear-band image on June 17 UT during our normal supernova searching campaign. A CCD spectrum (range 450-960 nm) was obtained with the 10-m Keck II telescope (+ DEIMOS spectrograph) at Keck Observatory on Sep. 10.36 UT. The spectrum shows a blue continuum with a strong, broad emission line around 5800A having FWHM ~ 20 nm. The spectrum shape matches the composite SDSS quasar spectrum, assuming the broad emission feature is produced by Mg II 280nm, placing the object at redshift of z = 1.08. An finding chart was posted at the following website: http://astro.berkeley.edu/~zwk/findingchart/KAIT_J20233743-19163425.jpg", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Exoplanet", "Pulsar", "Quasar", "Circumstellar disk" ] }, "answerKey": "C" }, { "id": "atel_5500", "message": "Title: Observations of Nova Mon 2012 after it emerged from the conjunction with the Sun\nAuthors: U. Munari (INAF Padova), A. Siviero (Univ. Padova), M. Zerjal (Univ. Ljubljana), S. Dallaporta (ANS Collaboration)\nDate: 22 Oct 2013; 17:30 UT\nProvenance: U. Munari (ulisse.munari@oapd.inaf.it)\nSubjects: Optical, Nova\nDescription: We resumed the photometric and spectroscopic monitoring of Nova Mon 2012 (V959 Mon) as soon as it emerged from the conjunction with the Sun in early September, using the same instrumentation adopted by Munari et al. (2013, MNRAS, 435, 771) to investigate the earlier evolution.\nThe photometric decline is monitored with ANS Collaboration telescope 030 and it is proceeding very smoothly. The nova is still considerably bright. Our observations for Sept 03.113, 13.126, 24.116 and Oct 18.086 UT give for B band 14.557, 14.668, 14.767, 14.919, for V 13.803, 13.814, 13.884, 14.067, for Rc 14.049, 14.111, 14.164, 14.322, and for Ic 14.032, 14.080, 14.110 and 14.259 mag, respectively.\nThe nova was already well into its nebular stage before entering the conjunction with the Sun, but a number of changes occurred during the period of invisibility. We have obtained with the Asiago 1.22m telescope + B&C spectrograph a low resolution spectrum (3320-7920 Ang range, 2.3 Ang/pix dispersion) on Oct 17.008 UT, and with the Asiago 1.82m + Echelle spectrograph a high resolution spectrum (resolving power 20,000) on Oct 19.197 UT, close in time with the lower resolution observation for Oct 21.451 UT recently reported by Woodward et al. (ATel #5499).\nComparing the Asiago 1.22m spectrum for Oct 17.008 with an identical one we obtained on 2013 March 21.833 we find that the ratio [OIII] 4959+5007 / [NeV] 3345+3436 has increased from 1.4 to 8.7, [OIII] 4959+5007 / Hbeta from 18 to 29, and [NeIII] 3869+3968 / [NeV] 3345+3426 from 0.60 to 1.22, while [NeV] 3345+3426 / Hbeta declined from 15.7 from 3.3, HeI 5876 / HeII 5412 from 6.3 to 3.4, and [FeVII] 6087 / Hbeta from 0.29 to 0.13. The ratio between HeI lines and Hbeta, and [OI] 6300+6364 and Hbeta remained constant. The 6300/6364 ratio for [OI] has increased from 1.1 to 1.4, still very far from the 3.1 value of optically thin conditions.\nSignificant changes affected the emission line profiles too, which have been 3D modelled by Ribeiro et al. (2013, ApJ 768, 49) for the early nova evolution. Comparing the Echelle spectrum for Oct 19.197 UT with an identical one for 2013 April 25.838 UT, the [OIII] double peaked profile of April (characterized by a width at half maximum of 2220 km/s, and a velocity separation of 1200 km/s for the two peaks) has now turned into a trapezoidal profile with a much flatter top and a width at half maximum of 2080 km/s, while the blend with the strong [NII] 6548, 6584 doublet now complicates a lot the profile of Halpha that shows a width at half maximum of 2710 km/s.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Variable star", "Supernova", "Neutron star" ] }, "answerKey": "A" }, { "id": "atel_5610", "message": "Title: Bright Highly Variable Slowly Moving Object Detected by MASTER\nAuthors: D. Denisenko, E. Gorbovskoy, V. Lipunov, P. Balanutsa, N. Tiurina, V. Kornilov, A. Belinski, N. Shatskiy, V. Chazov, A. Kuznetsov, A. Rufanov, V. Vladimirov, V. Yecheistov (Moscow State University, SAI), A. Parkhomenko, A. Tlatov, D. Dormidontov, V. Senik (Kislovodsk Solar Station of Pulkovo Observatory), V. Yurkov, Y. Sergienko, D. Varda, E. Sinyakov, A. Gabovich (Blagoveshchensk Educational University), K. Ivanov, S. Yazev, N. Budnev, E. Konstantinov, O. Chuvalaev, V. Poleshchuk, O. Gress (Irkutsk State University), V. Krushinsky, I. Zalozhnih, A. Popov, A. Bourdanov (Ural Federal University), P. Podvorotny, V. Shumkov, S. Shurpakov, (MASTER team members), H. Levato, C. Saffe (ICATE), C. Mallamaci, C. Lopez, F. Podest (OAFA)\nDate: 29 Nov 2013; 09:13 UT\nProvenance: Vladimir Lipunov (lipunov2007@gmail.com)\nSubjects: Optical, A Comment, Asteroid, Comet\nDescription: Referred to by ATel #: 5616\nMASTER Moving Object - MASDB2\nMASTER-Amur (D54) auto-detection system discovered OT source at (RA, Dec) = 07h 49m 13.45s -07d 03m 50.7s on 2013-11-28.74126 UT. The OT unfiltered magnitude is 15.7m (limit 17.8m). Object is visible on 6 images with 60-sec exposures starting from 17:45:37 to 17:54:28 UT. \n50 minutes later the object was detected again 12\" away, having moved by 9\"N, 8\"E. MASTER-Amur auto-detection system discovered OT source at (RA, Dec) = 07h 49m 12.83s -07d 03m 42.7s on 2013-11-28.77992 UT. The OT unfiltered magnitude is 15.8m (limit 17.8m). Object is visible on 6 images with 60-sec exposures starting from 18:36:04 to 18:46:34 UT. \nThe object was checked using Minor Planet Checker and NEO Checker. The only known object within 15' radius was 18.8m asteroid (74067) 1998 MH3 more than 7' away, yet moving to the south at 36\" per hour. \nThe following astrometry was obtained using 7 images of 12: \n \n \n MASDB2 * C2013 11 28.74037 07 49 13.45 -07 03 51.2 16.2 R D54 \n MASDB2 C2013 11 28.74288 07 49 13.41 -07 03 50.7 16.3 R D54 \n MASDB2 C2013 11 28.74530 07 49 13.37 -07 03 49.9 15.8 R D54 \n MASDB2 C2013 11 28.77625 07 49 12.91 -07 03 45.4 15.7 R D54 \n MASDB2 C2013 11 28.77749 07 49 12.89 -07 03 44.4 16.4 R D54 \n MASDB2 C2013 11 28.78028 07 49 12.83 -07 03 43.3 15.8 R D54 \n MASDB2 C2013 11 28.78269 07 49 12.73 -07 03 42.8 16.3 R D54 \n \n \nThe object was reported to the Minor Planet Center as MASDB2 and was posted at the NEO Confirmation Page with the NEO rating of 86. Using the MPC ephemeris, we have attempted a follow up with MASTER-Kislovodsk telescope. Two triplets of 60-sec unfiltered exposures were obtained: one on 21:50:42-21:53:43 UT and the other on 22:20:44-22:23:47 UT. The limiting magnitudes were 18.5-18.7m. Object was not detected neither near the ephemeris position, nor in the whole 2x2 deg FOV. \nWe note that the object is showing fast variability with a period of about 5 minutes (or 10 minutes, supposing double-peaked light curve). The amplitude of variations is about 0.8m, from 15.7 to 16.5 unfiltered magnitude, and did not change in 50 minutes between two MASTER-Amur observations. This leads us to the conclusion that the object could be a tumbling near-Earth asteroid or a man-made object. We have checked the list of recent spacecraft launches but found no matches. \nThere are 13 images of the object with next photometry: \n \n \n Date time Exp.time\tLimit Filt.\tTube.\traw_id Mag \n \n 2013-11-28 17:45:37\t60\t17.3\tW\tWEST \t557232 16.2 \n 2013-11-28 17:47:25\t60\t17.3\tW\tWEST \t557235 15.9 \n 2013-11-28 17:49:15\t60\t17.3\tW\tWEST \t557236 16.4 \n 2013-11-28 17:50:56\t60\t17.2\tW\tWEST \t557239 16.3 \n 2013-11-28 17:52:44\t60\t17.3\tW\tWEST \t557241 15.9 \n 2013-11-28 17:54:28\t60\t17.3\tW\tWEST \t557242 16.4 \n 2013-11-28 18:36:04\t60\t17.3\tW\tWEST \t557288 16.0 \n 2013-11-28 18:37:48\t60\t17.3\tW\tWEST \t557291 15.9 \n 2013-11-28 18:39:35\t60\t17.3\tW\tWEST \t557293 16.3 \n 2013-11-28 18:41:24\t60\t17.3\tW\tWEST \t557295 16.7 \n 2013-11-28 18:43:05\t60\t17.3\tW\tWEST \t557296 15.9 \n 2013-11-28 18:44:52\t60\t17.5\tW\tWEST \t557299 16.4 \n 2013-11-28 18:46:34\t60\t17.5\tW\tWEST \t557300 16.3 \n \n \n \n \n \n The accuracy is about 0.1. \n \n \n \n \n The video (13 images) is available at http://master.sai.msu.ru/static/asterod_lc.gif \n \n \n \n We encourage the follow-up observations with the large field \n instruments. We also request the possible identification with the \n man-made objects. \n \n \n The video (13 images) is available at http://master.sai.msu.ru/static/asterod_flash.gif \n \n \n List of Optical Transients discovered by MASTER\n \n \n \n \n \n \n \n Global MASTER Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Minor body", "Near-Earth object", "Exoplanet" ] }, "answerKey": "B" }, { "id": "atel_5675", "message": "Title: Swift/BAT detects hard X-ray emission from RX J0520.5-6932 \nAuthors: H. A. Krimm (CRESST/GSFC/USRA), S. D. Barthelmy (GSFC), W. Baumgartner (CRESST/GSFC/UMBC), J. Cummings (CRESST/GSFC/UMBC), N. Gehrels (GSFC), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D. Palmer (LANL), T. Sakamoto (Aoyama Gakuin Univ.), M. Stamatikos (OSU/GSFC), T. Ukwatta (MSU) \nDate: 19 Dec 2013; 21:28 UT\nProvenance: Hans A. Krimm (Hans.Krimm@nasa.gov)\nSubjects: X-ray, Binary, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 5719, 5856\nThe Be/X-ray binary RX J0520.5-6932 has been detected in the 15-50 keV band in the Swift/BAT hard X-ray transient monitor. The source was detected in the BAT monitor starting on 2013 December 18 (MJD 56644) with a count rate of 0.003 +/- 0.0005 ct/s/cm^2 (~14 mCrab). Archival data was searched back to the beginning of 2013 and no other time intervals (on the time scale of one day) were found with a significant rate increase above background. There have been four sub-threshold detections onboard Swift/BAT in 2009, 2011, 2013 and most recently on 2013 December 18 at 07:31:16.592 UT. \nThe source was confirmed as a Be/X-ray binary by Vasilopoulos et al. (ATel #4748) and more recently was seen to be in outburst in Swift/XRT (Vasilopoulos et al., ATel #5673) starting on 2013 December 18. The source was detected by BATSE during an April 1995 outburst using the earth-occultation technique (Edge et al. 2004, MNRAS 349, 1361). The peak BATSE flux at that time was ~20 mCrab. \nSwift/BAT transient monitor light curve for RX J0520.5-6932", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Neutron star", "Magnetar", "Interstellar medium" ] }, "answerKey": "B" }, { "id": "atel_5775", "message": "Title: ASAS-SN Discovery of a Large Amplitude (Delta V ~ 7 mag) CV Candidate\nAuthors: B. J. Shappee, K. Z. Stanek, C. S. Kochanek, T. W.-S. Holoien, J. Jencson, U. Basu J. F. Beacom (Ohio State), J. L. Prieto (Princeton), D. Szczygiel, G. Pojmanski (Warsaw University Observatory), J. Brimacombe (Coral Towers Observatory), D. Bersier (LJMU)\nDate: 18 Jan 2014; 22:50 UT\nProvenance: Benjamin Shappee (shappee@astronomy.ohio-state.edu)\nSubjects: Optical, Cataclysmic Variable\nDescription: During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or \"Assassin\"), using data from the recently expanded quadruple 14-cm \"Brutus\" telescope in Haleakala, Hawaii, we discovered a new bright transient source:\n \n \n Object RA (J2000) DEC (J2000) Disc. UT Date Disc. V mag \n ASASSN-14ac 7:52:54.9 +53:05:31.2 2014 Jan. 18.31 14.54 \n \nASASSN-14ac was discovered in images obtained 2014 UT Jan. 18.31 at V~14.5 and was detected in images obtained 2014 UT Jan. 17.46, but was undetected (V > 17) in images obtained on 2014 UT Jan. 11.29. The discovery image can be found here. Vizier reveals a 0.1\" SDSS match to a blue g=21.6 star. ASASSN-14ac is most likely a CV with a very strong, nearly 7 mag outburst. Given the large amplitude of its outburst, ASASSN-14ac may be a WZ Sge-type dwarf nova. \nWe thank LCOGT and its staff for their continued support of ASAS-SN.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Pulsar", "Binary system", "Repeater" ] }, "answerKey": "A" }, { "id": "atel_5900", "message": "Title: 500th Optical Transient discovered by MASTER\nAuthors: D. Denisenko, V. Lipunov, E. Gorbovskoy, P. Balanutsa, N. Tiurina, V. Kornilov, N. Shatskiy, V. Chazov, A. Kuznetsov, A. Rufanov, V. Vladimirov, V. Yecheistov (Moscow State University, SAI), V. Yurkov, Y. Sergienko, D. Varda, E. Sinyakov, A. Gabovich (Blagoveshchensk Educational University), K. Ivanov, S. Yazev, N. Budnev, E. Konstantinov, O. Chuvalaev, V. Poleshchuk, O. Gress (Irkutsk State University), A. Parkhomenko, A. Tlatov, D. Dormidontov, V. Senik (Kislovodsk Solar Station of Pulkovo Observatory), V. Krushinsky, I. Zalozhnih, A. Popov, A. Bourdanov (Ural Federal University), P. Podvorotny, V. Shumkov, S. Shurpakov (MASTER team members), H. Levato, C. Saffe (ICATE), C. Mallamaci, C. Lopez, F. Podest (OAFA)\nDate: 18 Feb 2014; 15:09 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Cataclysmic Variable, Transient\nDescription: MASTER OT J065921.17+102943.0 - possible Cataclysmic Variable\nMASTER-Amur auto-detection system discovered OT source at (RA, Dec) = 06h 59m 21.17s +10d 29m 43.0s on 2014-02-18.50572 UT. The OT unfiltered magnitude is 15.6m (limit 17.5m). The OT is seen in 2 images. There is no minor planet at this place. We have reference image without OT on 2012-09-24.83476 UT with unfiltered magnitude limit 18.3m. \nThe OT at quiescence is identical to the blue star USNO-B1.0 1004-0122737 (06 59 21.152 +10 29 43.43 pmRA=8 pmDE=-8 B1=19.35 R1=N/A B2=19.40 R2=17.19 I=18.75). Color-combined (BRIR) finder chart is uploaded to http://master.sai.msu.ru/static/OT/J065921+102943-BRIR5x5.jpg (2x zoom). The object is showing the large variability between 1st and 2nd epoch Palomar plates. Comparison of POSS-I and POSS-II red plates is posted at http://master.sai.msu.ru/static/OT/J065921+102943-POSS-Red.jpg \nThere is nothing at this position in 1RXS, 2MASS, GCVS and AAVSO VSX. This area of sky in Monoceros is not covered by GALEX, SDSS and CRTS. \nBased on the proper motion and amplitude of variability, MASTER OT J065921.17+102943.0 is most likely a cataclysmic variable. Follow up observations are required. The discovery and reference images are available at: http://master.sai.msu.ru/static/OT/065921.17102943.0.png \nList of 500 Optical Transients discovered by MASTER\nGlobal MASTER Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Variable star", "Pulsar", "Repeater" ] }, "answerKey": "B" }, { "id": "atel_6025", "message": "Title: TCP J17154683-3128303 = Nova Scorpius 2014\nAuthors: M. Jelinek, R. Cunniffe, A. J. Castro-Tirado (IAA-CSIC Granada), O. Rabaza (Univ. de Granada) and R. Hudec (AUS-CAS, Ondrejov)\nDate: 30 Mar 2014; 11:30 UT\nProvenance: Alberto J. Castro-Tirado (ajct@iaa.es)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 6032, 6034\nFollowing the discovery on Mar 26 of a 10th mag new source in Scorpius dubbed TCP J17154683-3128303 by Nishiyama & Kabashima (CBAT Transient Object Follow-up Reports), also detected by Swift on Mar 27 (ATEL#6015), we report an optical spectrum obtained with the COLORES spectrograph at the TELMA 0.6m robotic telescope (equipped by COLORES) at the BOOTES-2 astronomical station in EELM-CSIC (Malaga, Spain). The spectrum, covering the range 380-920 nm has been taken on Mar 30, 04:37 UT and shows broad emission lines of Balmer series, He I 501.6, 587.8, 706.5, and probably of O I 844.6, suggesting a nova in early phase (Nova Scorpius 2014) thus confirming the earlier suggestion by Ayani and Maeno (CBAT Transient Object Follow-up Reports). The BOOTES-2/TELMA COLORES optical spectrum of Nova Scorpius 2014 is posted at bootes.iaa.es .", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Interstellar medium", "Variable star", "Pulsar" ] }, "answerKey": "A" }, { "id": "atel_6120", "message": "Title: MAXI/GSC detection of a bright X-ray flare from FK Aqr\nAuthors: S. Nakahira (JAXA), A. Kawagoe, Y. Tsuboi (Chuo U.), H. Negoro ,M. Nakajima, K. Fukushima, T. Onodera, K. Suzuki, M. Fujita, T. Namba, F. Honda (Nihon U.), T. Mihara, M. Sugizaki, M. Morii, M. Serino, J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN), S. Ueno, H. Tomida, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA), N. Kawai, T. Yoshii, Y. Tachibana (Tokyo Tech), A. Yoshida, T. Sakamoto, Y. Kawakubo, H. Ohtsuki (AGU), H. Tsunemi, D. Uchida (Osaka U.), Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.), M. Yamauchi, Y. Morooka (Miyazaki U.), K. Yamaoka (Nagoya U.) report on behalf of the MAXI team\nDate: 5 May 2014; 17:56 UT\nProvenance: Satoshi NAKAHIRA (nakahira@crab.riken.jp)\nSubjects: X-ray, Star\nDescription: On 2014-05-05 11:35:08 (UT) UT (=MJD 56782.48273), the MAXI/GSC transient alert system triggered ( trigger ID= 6782395557) on enhanced X-ray emission at (R.A., Dec) = (339.761 deg, -20.383 deg). \nWe obtained a refined position of the source at, \n(R.A., Dec) = (339.714 deg, -20.523 deg) = (22 38 51, -20 31 22) (J2000) \nwith a statistical error of 0.18 degree radius with an additional systematic uncertainty of 0.1 degree (90% containment radius). \nThis position is consistent with a dMe star, FK Aqr. \n \nThe 2-20 keV flux averaged over the triangular transit was about 175±25 mCrab, corresponding to a luminosity of 3 ×1031 ergs s-1 for an assumed distance of 8.6 pc. The flux decayed to an upper limit of ~20 mCrab at the next scan performed 92 minutes later. This flare from FK Aqr is the 2nd detection with MAXI/GSC, and is the largest among the two flares.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system", "Star and stellar system", "Neutron star", "Interstellar medium" ] }, "answerKey": "B" }, { "id": "atel_6200", "message": "Title: SXP1062 in outburst\nAuthors: R. Sturm (MPE, Garching), L. M. Oskinova (Institute for Physics and Astronomy, University Potsdam), F. Haberl (MPE), Y.-H. Chu (Department of Astronomy, University of Illinois), V. Henault-Brunet (University of Surrey), J. Gallagher (Department of Astronomy, University of Wisconsin-Madison), M. A. Guerrero (Instituto de Astrofisica de Andalucia, IAA-CSIC), S. Popov (Sternberg Astronomical Institute, Moscow State University), M. Schurch (University of Cape Town)\nDate: 4 Jun 2014; 08:15 UT\nProvenance: Richard Sturm (rsturm@mpe.mpg.de)\nSubjects: X-ray, Binary, Neutron Star, Transient, Pulsar\nDescription: We report a new X-ray outburst of SXP1062, a Be/X-ray binary associated with a supernova remnant and located in the Wing of the Small Magellanic Cloud. \n \nIn a 2195 s Swift/XRT observation (ObsID 00091814001) starting on 2014-06-01 09:44 (UT), the source was detected with 608±25 raw background-subtracted counts. \nThe Swift/XRT spectra can be described well by an absorbed power law with a photon index of Γ=0.70±0.13. For the SMC column density, we obtain an upper limit of NH< 1.6 × 1021 cm-2. The SMC absorption was modelled with SMC abundance set to 0.2 Zsolar for elements heavier than helium. An additional Galactic foreground absorption was set to 6 × 1020 cm-2. We derive an observed flux of 24.5±2.5 × 10-12 erg cm-2 s-1 in the 0.2-10.0 keV band corresponding to an unabsorbed luminosity of 1.09 × 1037 erg s-1 (assuming a distance of 60 kpc). This is the highest X-ray luminosity observed from SXP1062 so far. The spectral shape is consistent with that seen during the previous outburst in Oct. 2012 (Sturm et al. 2013, A&A 556, A139) \nThe preceding Swift observation (ObsID 00032580059) was obtained on 2014-05-18 02:00 with the XRT exposure time of 1561 s. The count rate was below 0.0056 cts s-1, i.e. a factor of 50 fainter than in the most recent observation we report here. \n \nThe elapsed time between this outburst and two previous outbursts seen in the optical I band is consistent, strongly supporting the orbital period interpretation by Schmidtke et al. (ATel #4596). Therefore, the currently ongoing outburst is likely of type-I and we expect an optical/NIR outburst as well. \n \nWe will follow this outburst with a sequence of Chandra and SALT observations. \n \nAll uncertainties are given for 90% confidence. \nWe acknowledge the use of public data from the Swift data archive and thank the Swift team for accepting and scheduling the target of opportunity observation.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star, Binary system", "Neutron star, Supernova", "Pulsar, Binary system", "Repeater, Binary system" ] }, "answerKey": "A" }, { "id": "atel_6325", "message": "Title: New Cataclysmic Variable in Kepler field discovered by MASTER\nAuthors: D. Denisenko, V. Lipunov, E. Gorbovskoy, N. Tiurina, P. Balanutsa, V. Kornilov, N. Shatskiy, V. Chazov, A. Kuznetsov, V. Vladimirov, V. Yecheistov (Moscow State University, SAI), V. Yurkov, Y. Sergienko, D. Varda, E. Sinyakov, A. Gabovich (Blagoveshchensk Educational University), K. Ivanov, S. Yazev, N. Budnev, E. Konstantinov, O. Chuvalaev, V. Poleshchuk, O. Gress (Irkutsk State University), A. Parkhomenko, A. Tlatov, D. Dormidontov, V. Senik (Kislovodsk Solar Station of Pulkovo Observatory), V. Krushinsky, I. Zalozhnih, A. Popov, A. Bourdanov (Ural Federal University), P. Podvorotny, V. Shumkov, S. Shurpakov (MASTER team members), H. Levato, C. Saffe (ICATE), C. Mallamaci, C. Lopez, F. Podest (OAFA)\nDate: 18 Jul 2014; 21:15 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Cataclysmic Variable, Transient\nDescription: Referred to by ATel #: 6584\nMASTER OT J194955.17+455349.6 - new CV in Kepler field\nMASTER-Amur auto-detection system discovered OT source at (RA, Dec) = 19h 49m 55.17s +45d 53m 49.6s on 2014-07-18.55647 UT. The OT unfiltered magnitude is 16.4m (limit 17.6m). The OT is seen in 3 images. There is no minor planet at this place. We have reference image without OT on 2011-08-26.58258 UT with magnitude limit in R filter 18.6m. \nThe OT at quiescence is identical to the blue star USNO-B1.0 1358-0337295 (19 49 55.184 +45 53 51.21 pmRA=0 pmDE=0 B1=19.58 R1=18.93 B2=17.84 R2=19.08 I=17.31). The star is showing significant variability between Palomar plates. Vmag in GSC 2.3.2 is 17.55. Color-combined (BRIR) finder chart is uploaded to http://master.sai.msu.ru/static/OT/J194955+455349-BRIR5x5.jpg (2x zoom). There is a faint X-ray source 1RXS J194954.8+455347 with 12\" error circle, flux 0.0284+/-0.0072 cnt/s and hardness ratios HR1=1.00+/-0.18, HR2=0.50+/-0.22 formally 5\" away. There is nothing at this position in 2MASS, GCVS and AAVSO VSX. This area of sky in Cygnus is not covered by SDSS, GALEX, NEAT and CRTS. \nThe object is included into Kepler Input Catalog as KIC 9358280. The Kepler-INT survey (Greiss et al., 2012) gives the following magnitudes (rounded to 0.01): U=18.15 g=19.35 r=18.85 i=18.28 Ha=17.81 for KIS J194955.17+455350.9 and U=18.71 g=19.70 r=19.13 i=18.57 Ha=17.92 for KIS J194955.19+455350.9 (the same object observed at different epochs). Based on the H-alpha emission, MASTER OT J194955.17+455349.6 is a new cataclysmic variable, likely a dwarf nova in outburst. Follow up observations are required. The discovery and reference images are available at: http://master.sai.msu.ru/static/OT/194955.17455349.6.jpg \nWe note that MASTER OT J193347.47+442455.5 (ATel #6317), MASTER OT J185510.67+434138.0 = KIC 7873220 (ATel #6228) and MASTER OT J185624.15+400311.8 (ATel #6187) are also located in Kepler field. \nList of Optical Transients discovered by MASTER\nGlobal MASTER Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Variable star", "Stellar evolution", "Nova" ] }, "answerKey": "B" }, { "id": "atel_6375", "message": "Title: Detection of a Blue Point Source at the Location of Supernova 2011dh\nAuthors: Gaston Folatelli (Kavli IPMU), Schuyler D. Van Dyk (IPAC/Caltech), Omar G. Benvenuto (IALP/UNLP), Melina C. Bersten (Kavli IPMU), Hanindyo Kuncarayakti (MAS/University of Chile), Keiichi Maeda (Kyoto University), Ken'ichi Nomoto (Kavli IPMU), Robert M. Quimby (SDSU)\nDate: 7 Aug 2014; 19:28 UT\nProvenance: Gaston Folatelli (gaston.folatelli@ipmu.jp)\nSubjects: Optical, Ultra-Violet, Binary, Supernovae\nDescription: We report Hubble Space Telescope (HST) observations of the field of the Type IIb Supernova 2011dh in M51 performed with the Wide Field Camera 3 (WFC3), UVIS channel and filters F225W and F336W on 2014 August 7.2 UT as part of our Cycle 21 program GO-13426 (PI: G. Folatelli; joined with GO-13433, PI: J. Maund). The near-UV images show the presence of a blue point source at the location of the SN. We are confident that the new object is coincident with the fading SN that Van Dyk et al. (2013, ApJ, 772, L32) identified in WFC3 images from 2013 to 0.07 UVIS pixel, or 2.8 milliarcsec (i.e., 0.1 pc at the assumed distance of 8.4 Mpc for M51). Preliminary photometry done with the Dolphot v2.0 (Dolphin 2000, PASP, 112, 1383) package yielded flight-system magnitudes of F225W = 24.6 +/- 0.1 mag, and F336W = 24.9 +/- 0.1 mag. The source's UV brightness and color is compatible with it being the companion star of the disappeared yellow supergiant progenitor (Van Dyk et al. 2013, ApJL, 772, L32; Ergon et al. 2014, A&A, 562, 17). We estimate the flux from the SN ejecta to be negligible in this wavelength range. If the contribution from an unresolved light echo can be discarded, this detection provides further confirmation for the interacting binary progenitor proposed by Bersten et al. 2012, ApJ, 757, 31, and Benvenuto, Bersten, & Nomoto 2013, ApJ, 762, 74. More detailed analysis is ongoing.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Supernova", "Black hole", "Interstellar medium" ] }, "answerKey": "B" }, { "id": "atel_6550", "message": "Title: MAXI/GSC detection of a new X-ray outburst from the LMXB 4U 1608-52\nAuthors: H. Negoro (Nihon U.), M. Serino (RIKEN), S. Ueno, H. Tomida, S. Nakahira, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA), T. Mihara, M. Sugizaki, M. Morii, J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN), N. Kawai, T. Yoshii, Y. Tachibana (Tokyo Tech), A. Yoshida, T. Sakamoto, Y. Kawakubo, H. Ohtsuki (AGU), H. Tsunemi, D. Uchida (Osaka U.), M. Nakajima, K. Fukushima, T. Onodera, K. Suzuki, T. Namba, M. Fujita, F. Honda (Nihon U.), Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.), Y. Tsuboi, A. Kawagoe (Chuo U.), M. Yamauchi, Y. Morooka, D. Itoh (Miyazaki U.), K. Yamaoka (Nagoya U.)\nDate: 7 Oct 2014; 16:33 UT\nProvenance: Hitoshi Negoro (negoro@phys.cst.nihon-u.ac.jp)\nSubjects: X-ray, Neutron Star, Transient\nDescription: Referred to by ATel #: 9330\nThe MAXI/GSC nova alert system detected renewed X-ray activity from the low mass X-ray binary 4U 1608-52 (X 1608-522) at UT 13:00 on 2014 October 5 (MJD 56935). The 4-10 keV X-ray fluxes obtained with MAXI/GSC were 34 +- 18 mCrab averaged over 2 scan transits from 16:53 to 18:26 on Oct. 4, 107 +- 16 mCrab over 4 scans from 13:00 to 17:38 on Oct. 5, and 298 +- 29 mCrab over 3 scans from 12:12 to 15:17 on Oct. 6. \nSince the 15-50 keV X-ray flux obtained with Swift/BAT on Oct. 6 was still below the detection (http://http://swift.gsfc.nasa.gov/results/transients/H1608-522/), the source was in a soft state. \n \nThis is the 6th outburst from the source since the long outburst in 2007-2009 (Linares et al. ATel #2264). The previous outbursts were starting on 2010 March 2 (ATel #2462), 2011 March 24 (ATel #3237), 2012 October 10 (ATel #4478), 2013 May 27 (ATel #5094) and 2014 January 16 (ATel #5990). \n\nMAXI 4U 1608-52", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Repeater", "Neutron star", "Star and stellar system" ] }, "answerKey": "C" }, { "id": "atel_6625", "message": "Title: A New Highly Variable X-ray Source at z ~ 1.5 in the Chandra Deep Field-South Survey\nAuthors: Bin Luo (Penn State), W. N. Brandt (Penn State), Franz Bauer (Pontificia Universidad Catolica de Chile)\nDate: 26 Oct 2014; 21:54 UT\nProvenance: Bin Luo (bul119@psu.edu)\nSubjects: X-ray, AGN, Variables\nDescription: We discovered a new highly variable Chandra source in the ongoing Chandra Deep Field-South (CDF-S) survey. The J2000 source position is RA=53.094681 and DEC=-27.694768, with a positional uncertainty ~0.6\". It was not detected in the previous 4 Ms of Chandra exposure (1999-2010), yet it was detected in the newly obtained 1.06 Ms of Chandra exposure (17 observations between 2014-06-09 and 2014-10-17) with ~85 counts in the 0.5-2 keV band. Compared to the upper limit from the previous 4 Ms exposure, the 0.5-2 keV count rate has increased by a factor of >13.9. The source is ~6.4' away from the average Chandra aim point. It was not present in the 3 Ms XMM-Newton CDF-S catalog either (Ranalli et al. 2013).\nThe X-ray source is very soft, with no detection in the 2-8 keV band. The effective power-law photon index is thus constrained to be Gamma>2.1. We cannot constrain any count rate variability between the individual 2014 observations, largely due to the limited number of counts. Breaking these 2014 observations into two segments (before and after 2014-09-26) suggests a ~15% decrease in count rate, although this value is still within the uncertainty of the count rate measurements. At a redshift of 1.51 (see below), the 0.5-2 keV luminosity is ~1.3E43 erg/s. The X-ray source has an optical counterpart ~0.4\" away (RA_op=53.0946848, DEC_op=-27.6946506), with AB magnitudes R~24.0, z~23.3, and Ks~21.7 (Hsu et al. 2014). This counterpart has a relatively reliable photometric redshift of 1.51 (Hsu et al. 2014). We caution that there is a brighter optical source nearby (1.9\" away, RA_op2=53.094074, Dec_op2=-27.694773, R~21.5) that might contaminate low-resolution follow-up observations. A comparison of the counterpart in the MUSYC R-band image (Cardamone et al. 2010) and a VIMOS 550s R-band pre-image (PI Pentericci, program ID 194.A-2003A), obtained at 2014 Oct 01 08:20:09.6 UT with 0.66\" seeing and at 1.03 airmass, shows no obvious change in magnitude. Given that the latter image is concurrent with the X-ray outburst, there appears to be no change in R-band which could be associated with this soft X-ray rise. The nature of this X-ray source remains unclear. However, given its non-detection in the previous 4 Ms of Chandra exposure over the last ~14 years, the factor of >13.9 increase in flux, and the lack of significant flux variability over the last ~4 months (observed frame), it could be associated with a stellar tidal disruption event or an AGN that varies strongly on long timescales. The chance of finding one tidal disruption event in the currently 5 Ms CDF-S survey is broadly consistent with theoretical expectations (e.g., Wang & Merritt 2004) or the upper limit constrained from the 1 Ms CDF-S and 2 Ms Chandra Deep Field-North (CDF-N) data (Luo et al. 2008). The new CDF-S survey will continue monitoring this source with Chandra till the end of 2014. Observations in the optical/UV would be helpful to constrain its nature.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Stellar evolution", "Active galactic nucleus, Stellar evolution", "Active galactic nucleus, Pulsar", "Active galactic nucleus, Binary system" ] }, "answerKey": "B" }, { "id": "atel_6775", "message": "Title: NIR photometry the AGN candidate MASTER OTJ010728.48+033348.4\nAuthors: L. Carrasco, E. Recillas, A. Porras, D. Y. Mayya, J. Leon-Tavares, V. Chavushyan, A. Carraminana, (INAOE, Mexico)\nDate: 1 Dec 2014; 21:36 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Infra-Red, Optical, X-ray, Gamma Ray, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 6779\nFollowing the report on flaring activity of MASTER OTJ010728.48+033348.4 by Shumkov et al.,2014 (Atel #6762). We carried out NIR photometry recently, On November 30th,2014 (JD2456991.8114), we found this object with a flux corresponding to H = 15.754 +/- 0,05, J = 15.754. +/- 0.,05 and Ks = 14.436 +/- 0.06. The object is coincident with the radio source PMNJ0107+0333 and the Rosat source 1RXJ010729.5+033341. The NIR colors are consistent with those of AGN's. These flux values are more than 2 magnitudes brighter than the upper limits in the 2MASS Survey, confirming the variable nature of this object at NIR wavelengths. We plan to follow its behavior in the NIR in order to correlate those data with other time variable data. Our observations were carried out with the 2.1m telescope of the Guillermo Haro Observatory of the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We encourage further multi wavelength coverage of this object.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Active galactic nucleus", "Exoplanet", "Black hole" ] }, "answerKey": "B" }, { "id": "atel_6840", "message": "Title: Asiago spectroscopic classification of MASTER OT J062509.46+283255.1\nAuthors: L. Tartaglia (INAF Osservatorio Astronomico di Padova), \t\tF. Huang (Beijing Normal University), A. Pastorello, S. Benetti, \t\tE. Cappellaro, N. Elias-Rosa, P. Ochner, G. Terreran, L. Tomasella, M. Turatto \t\t(INAF Osservatorio Astronomico di Padova)\nDate: 20 Dec 2014; 10:05 UT\nProvenance: Enrico Cappellaro (enrico.cappellaro@oapd.inaf.it)\nSubjects: Optical, Supernovae\nDescription: The Asiago Transient Classification Program (Tomasella et al. 2014, AN, 335, 841) reports the spectroscopic classification of MASTER OT J062509.46+283255.1 (ATel #6833). \nThe observations were performed with the Asiago 1.82 m Copernico Telescope (+AFOSC; range 340-820 nm; resolution 1.2 nm), equipped with a new CCD (Andor IKON L936) with higher response both in the UV and in the NIR. \n \n \n Name | Date (UT) | z | Type | Phase \n MASTER OT J062509.46+283255.1 | 20141219.92 | 0.029 | Ia | 2 weeks after maximum \n \nClassification was done with GELATO (Harutyunyan et al. 2008, A&A, 488, 383) and SNID (Blondin and Tonry 2007, ApJ, 666, 1024). The Asiago classification spectra are posted at the website http://sngroup.oapd.inaf.it.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Supernova", "Binary system", "Neutron star" ] }, "answerKey": "B" }, { "id": "atel_6960", "message": "Title: Possible ongoing hard-to-soft transition of GX 339-4\nAuthors: Authors: S. E. Motta (ESA/ESAC), T. M. Belloni (INAF-OAB)\nDate: 20 Jan 2015; 10:13 UT\nProvenance: Tomaso Belloni (belloni@merate.mi.astro.it)\nSubjects: X-ray, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 7009, 7201, 7434, 7649, 10797\nThe latest MAXI observation of the black-hole candidate GX 339-4 (19 January 2015) shows that the source might be leaving the low-hard state. The BAT count rate (15-50 keV) has been dropping for the last 5 days (from ~360 mCrab to ~180mCrab), suggesting that a transition to the soft state might be ongoing. Since GX 339-4 is currently not observable by Swift/XRT nor by any other X-ray satellite because of sun constraints, we cannot exclude that the observed drop in the hard count rate is due to a transition back to the hard-state. We note, however, that even though transitions back to the hard state have been observed in the past (2004, 2009 and 2012, Motta et al. 2011, MNRAS, 418, 2292 and ATel #4247) have never been so fast. If what we are observing is a hard-to-soft transition, based on previous outbursts considerable further softening is expected in the next few days. In particular, the radio emission is expected to evolve and lead to a major ejection. Multi-wavelength observations are encouraged.\nCurrent X-ray evolution of GX 339-4", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system", "Accreting object", "Pulsar", "Black hole" ] }, "answerKey": "D" }, { "id": "atel_7050", "message": "Title: MASTER: possible SN during Fermi Lat GRB150210A inspection\nAuthors: O. Gress(ISU), V. Lipunov, E. Gorbovskoy(Lomonosov MSU, SAI), K. Ivanov, N. Budnev, S. Yazev, E. Konstantinov, O. Chuvalaev, V. Poleshchuk (Irkutsk State University), P. Balanutsa , V. Kornilov, A. Kuznetsov, , N. Tiurina , D. Denisenko (Lomonosov Moscow State University, SAI), A. Tlatov, D. Dormidontov, V. Senik, A. Parkhomenko, (Kislovodsk solar station of the Pulkovo observatory RAS), D. Buckley, S. Potter, A. Kniazev, M. Kotze (South African Observatory), V. Krushinsky, I. Zalozhnih, A. Popov, A. Bourdanov (Ural Federal University), V. Yurkov, Y. Sergienko, A. Gabovich (Blagoveshchensk Educational University), V. Shumkov, S. Shurpakov (MASTER team members)\nDate: 11 Feb 2015; 21:09 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Cataclysmic Variable, Star, Supernovae, Transient\nDescription: Referred to by ATel #: 7052\nMASTER OT J072940.10+141425.5- possible SuperNova during Fermi alert GRB150210.94 \nMASTER-Tunka auto-detection system ( Lipunov et al., 2010 ) discovered OT source at at (RA, Dec) = 07h 29m 40.10s +14d 14m 25.5s on 2015-02-11.64502 UT during Fermi alert GRB150210.94 , see Gorbovskoy et al. GCN 17446 . \nThe OT unfiltered magnitude is 17.4m (the limit is 20.0m). This possible SuperNova is located in 0.2”W 2.8”N from the center on unknown galaxy (Sloan’s spiral galaxy). \nThere are 31 images with OT on this night in MASTER-Tunka database. \nWe have reference image without OT on 2012-02-18.58510 UT with unfiltered magnitude limit 19.8m. \nThe discovery and reference images are available at: http://master.sai.msu.ru/static/OT/MASTERJ072940.10+141425.5.jpg\nSpectral observations are required. \nList of Optical Transients discovered by MASTER\nGlobal MASTER Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Exoplanet", "Supernova", "Black hole" ] }, "answerKey": "C" }, { "id": "atel_7125", "message": "Title: KAIT Discovery and Follow-up Observations of a Possible Young Supernova Candidate in UGC 3777: PSN J07164258+2951227\nAuthors: W. Zheng, P. Kelly, A. V. Filippenko (UC Berkeley)\nDate: 23 Feb 2015; 10:15 UT\nProvenance: Weikang Zheng (zwk@umich.edu)\nSubjects: Optical, Supernovae\nDescription: We report the discovery, with the 0.76-m Katzman Automatic Imaging Telescope (KAIT) at Lick Observatory, of a possible new supernova in the nearby galaxy UGC 3777 (z = 0.010717). The object, dubbed (by the IAU) PSN J07164258+2951227, is located at (J2000.0) coordinates RA = 07:16:42.58, Dec = +29:51:22.7. Following discovery in an unfiltered image obtained at 05:11 UT on 2015 Feb. 23, we manually started a sequence of follow-up observations in the B, V, R, I, and clear (roughly R) filters beginning about 1.3 hours later. Using stars from the USNO-B1 catalog for reference, we measure R = 17.2 mag at this time. The object was not detected in a previous KAIT image taken four days earlier, on Feb. 19, with a limit of R ~ 18.5 mag, indicating that the object might be young if it is a SN. Spectroscopic observations are encouraged. A finding chart is available at the following website: http://astro.berkeley.edu/~zwk/findingchart/PSN_J07164258+29512272.jpg", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Supernova", "Minor body", "Neutron star" ] }, "answerKey": "B" }, { "id": "atel_7200", "message": "Title: MAXI/GSC detection of a new X-ray transient MAXI J0511-522\nAuthors: M. Serino (RIKEN), H. Negoro (Nihon U.), T. Yoshii (Tokyo Tech), S. Ueno, H. Tomida, S. Nakahira, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA), T. Mihara, M. Sugizaki, M. Morii, J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN), N. Kawai, Y. Tachibana (Tokyo Tech), A. Yoshida, T. Sakamoto, Y. Kawakubo, H. Ohtsuki (AGU), H. Tsunemi, D. Uchida (Osaka U.), M. Nakajima, K. Fukushima, T. Onodera, K. Suzuki, T. Namba, M. Fujita, F. Honda (Nihon U.), Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.), Y. Tsuboi, A. Kawagoe (Chuo U.), M. Yamauchi, Y. Morooka, D. Itoh (Miyazaki U.), K. Yamaoka (Nagoya U.)\nDate: 11 Mar 2015; 05:49 UT\nProvenance: Motoko Suzuki (motoko@crab.riken.jp)\nSubjects: X-ray, Binary, Black Hole, Neutron Star, Transient\nDescription: Referred to by ATel #: 7210\nThe MAXI/GSC nova alert system triggered a faint X-ray transient at 03:06:21 on March 11, 2015. We obtained the source position at \n(R.A., Dec) = (77.752 deg, -52.204 deg) = (05 11 00, -52 12 14) (J2000) \nwith long and short radii of 0.57 deg and 0.47 deg, respectively. The roll angle of long axis from the north direction is 81.0 deg counterclockwise. There is an additional systematic uncertainty of 0.1 deg (90% containment radius). \nThe 4-10 keV flux has increased since March 10.3. The average 4-10 keV flux from March 10.3 to 11.2 is 0.018 +/- 0.005 photons/cm2/s (corresponding to 14+/-4 mCrab). We tentatively name the source MAXI J0511-522. There is a cataloged X-ray source near the position, 1H 0513-518, apart from the best position by 38', but the nature of this source is not known. The follow-up observations are strongly encouraged to reveal the nature of the source. \nThe latest light curves and images of MAXI J0511-522 by MAXI/GSC is placed at the following URL: \nhttp://maxi.riken.jp/top/index.php?cid=1&jname=J0511-522", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Minor body", "Black hole", "Variable star" ] }, "answerKey": "C" }, { "id": "atel_7320", "message": "Title: ASAS-SN Discovery of A Probable Supernova in NGC 5227\nAuthors: J. Brimacombe (Coral Towers Observatory), T. W.-S. Holoien, K. Z. Stanek, C. S. Kochanek, A. B. Danilet, G. Simonian, U. Basu, N. Goss, J. F. Beacom, T. A. Thompson (Ohio State), B. J. Shappee (Hubble Fellow, Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), D. Bersier (LJMU), Subo Dong (KIAA-PKU), P. R. Wozniak (LANL), E. Falco (CfA), D. Szczygiel, G. Pojmanski (Warsaw University Observatory), S. Kiyota (Variable Star Observers League in Japan), R. A. Koff (Antelope Hills Observatory), G. Krannich (Roof Observatory Kaufering), B. Nicholls (Mt. Vernon Obs., New Zealand)\nDate: 30 Mar 2015; 21:23 UT\nProvenance: Thomas Holoien (tholoien@astronomy.ohio-state.edu)\nSubjects: Optical, Supernovae, Transient\nDescription: Referred to by ATel #: 7323\nDuring the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or \"Assassin\"), using data from the quadruple 14-cm \"Brutus\" telescope in Haleakala, Hawaii, we discovered a new transient source, most likely a supernova, in the galaxy NGC 5227: \n \n \n Object RA (J2000) DEC (J2000) Disc. UT Date Disc. V mag \n ASASSN-15fz 13:35:25.14 +01:24:33.0 2015-03-30.57 16.9 \n \nASASSN-15fz was discovered in images obtained on UT 2015-03-30.57 at V~16.9 mag. We do not detect (V>17.8) the object in images taken on UT 2015-03-29.34 and before. An image obtained by J. Brimacombe on UT 2015-03-30.75 with the CDK 43-cm telescope at Savannah Skies Observatory confirms the discovery of the transient. This figure shows the archival DSS image of the host (left) and the J. Brimacombe confirmation image (right). The red circle has a radius of 5\" and is centered on the position of the transient in the J. Brimacombe image. \nThe position of ASASSN-15fz is approximately 8.0\" South and 9.3\" East from the center of the galaxy NGC 5227 (z=0.017479, d=77 Mpc, via NED), giving an absolute V-band magnitude of approximately -18.2 (m-M=34.43, A_V=0.68). Follow-up observations are encouraged. \nWe thank LCOGT and its staff for their continued support of ASAS-SN. ASAS-SN is supported in part by Mt. Cuba Astronomical Foundation. For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Minor body", "Pulsar", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_7425", "message": "Title: INTEGRAL measures the hard X-ray spectrum of the Be/X-ray binary XTE J1859+083\nAuthors: D. Malyshev, C. Ferrigno (ISDC/University of Geneva, Switzerland) D. Gotz (CEA/Saclay, France)\nDate: 21 Apr 2015; 12:22 UT\nProvenance: Carlo Ferrigno (Carlo.Ferrigno@unige.ch)\nSubjects: X-ray, Neutron Star, Transient, Pulsar\nDescription: During the INTEGRAL observations performed from 2015 April 17, 19:47 to April 19, 20:01 UTC, the IBIS/ISGRI instrument detected a highly significant signal from a transient source, positionally coincident with the Be/X-ray pulsar XTE J1859+083 (ra, dec) = (284.78 ; 8.25) , which is reported to be in outburst since 2015-02-08 (ATeL #7034). \nThe source is detected in the IBIS/ISGRI mosaic images with fluxes 62 ± 2 mCrab in the 20-40 keV energy band and 40 ± 2 mCrab in 40-80 keV band (effective exposure of 39 ks). During these observations, XTE J1859+083 was outside of the lower energy range JEM-X instrument field of view. \nTo obtain a broad-band estimate of the source spectrum, we have extracted the average Swift/XRT spectrum from the public archive using the Leicester online tool (http://www.swift.ac.uk/user_objects/). In the archive, there are 6.2 ks of data available in window-timing mode, which is not affected by pile-up at the source flux level. The observations are taken in several snapshots between 2015-03-12 and 2015-04-08 and the spectrum is grouped to have at least 30 counts per bin. \nWe fitted the averaged Swift/XRT and IBIS/ISGRI spectra using an absorbed cut-of power law and inter-calibration constant to account for the source variability. The fit (χ2red. = 0.9 for 636 d.o.f.) yields NH=2.19±0.07 × 1022 cm-2, Γ=1.25±0.05, and Ecut=26±4 keV. The 1-10 and 20-100 keV absorbed fluxes are 6.0×10-10 and 8.5 ×10-10 erg/cm2/s, respectively. We caveat that XTE J1859+083 is variable and these spectral properties should be considered as a a rough estimate of the average source properties, which are consistent with its proposed high mass X-ray binary nature.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Neutron star", "Exoplanet", "Minor body" ] }, "answerKey": "B" }, { "id": "atel_7550", "message": "Title: Spectroscopic Classification of ASASSN-15jm\nAuthors: A. S. Piascik, I. A. Steele (Liverpool JMU)\nDate: 22 May 2015; 10:29 UT\nProvenance: Iain Steele (iainsteele@mac.com)\nSubjects: Optical, Supernovae, Transient\nDescription: We conducted two spectroscopic observations of transient ASASSN-15jm at 2015-05-21T:00:45:16 and 2015-05-22T00:33:10 UT. \nThis transient was identified by the All Sky Automated Survey for SuperNovae (ASAS-SN) in ATel #7536 in host galaxy 2MASX J17210913+2534558. \nTwo spectra were obtained in the visible, 400-800nm, with resolution R~350, using the SPRAT spectrograph on the Liverpool Telescope located at Roque de los Muchachos. \nClassification using SNID (SNID; Blondin and Tonry 2007, Ap.J. 666, 1024) indicates it is a type Ia supernova with closest matching spectrum SN2003hu and estimated z=0.05. \nLiverpool Telescope", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova, Pulsar", "Near-Earth object, Interstellar medium", "Supernova, Stellar evolution", "Supernova, Interstellar medium" ] }, "answerKey": "D" }, { "id": "atel_7625", "message": "Title: ASAS-SN Discovery of A Probable Bright Supernova in IC 4303\nAuthors: S. Kiyota (Variable Star Observers League in Japan), J. Brimacombe (Coral Towers Observatory), T. W.-S. Holoien, K. Z. Stanek, C. S. Kochanek, J. S. Brown, A. B. Danilet, G. Simonian, U. Basu, J. F. Beacom, T. A. Thompson (Ohio State), B. J. Shappee (Hubble Fellow, Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), D. Bersier (LJMU), Subo Dong (KIAA-PKU), E. Falco (CfA), P. R. Wozniak (LANL), D. Szczygiel, G. Pojmanski (Warsaw University Observatory), E. Conseil (Association Francaise des Observateurs d'Etoiles Variables), G. Masi (Virtual Telescope Project, Ceccano, Italy), B. Nicholls (Mt. Vernon Obs., New Zealand), J. Nicolas (Groupe SNAUDE, France), D. E. Polsgrove, D. J. Della-Rose, S. J. Novotny (Falcon Telescope Network, US Air Force Academy)\nDate: 12 Jun 2015; 16:40 UT\nProvenance: Thomas Holoien (tholoien@astronomy.ohio-state.edu)\nSubjects: Optical, Supernovae, Transient\nDescription: During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or \"Assassin\"), using data from the double 14-cm \"Cassius\" telescope in Cerro Tololo, Chile, we discovered a new bright transient source, most likely a supernova, in the galaxy IC 4303. \nASASSN-15kz was discovered in images obtained on UT 2015-06-12.07 at V~15.9 mag. We do not detect (V>17.0) the object in images taken on UT 2015-06-08.11 and before. Images obtained by S. Kiyota on UT 2015-06-12.43 using a 0.5m CDK + FLI PL-9000 at the ITelescope.NET site at Siding Springs Observatory and by J. Brimacombe on UT 2015-06-12.64 with the CDK 43-cm telescope at Savannah Skies Observatory confirm the discovery of the transient. This figure shows the archival DSS image of the host (left) and the S. Kiyota confirmation image (right). The red circle has a radius of 4\" and is centered on the position of the transient in the S. Kiyota image. \nThe position of ASASSN-15kz is approximately 5.2\" North and 6.0\" East from the center of the galaxy IC 4303 (z=0.008022, d=37.1 Mpc, via NED), giving an absolute V-band magnitude of approximately -17.1 (m-M=32.86, A_V=0.165). Properties of the new source and photometry are summarized in the tables below: \n \n \n Object RA (J2000) DEC (J2000) Disc. UT Date Disc. V mag Approx. Abs. Mag Offset from Host (\") \n ASASSN-15kz 13:37:18.67 -28:39:23.55 2015-06-12.07 15.9 -17.1 7.94 \n \n \n \n Obs. UT Date V mag \n 2015-06-08.11 >17.0 \n 2015-06-12.07 15.9 \n \nFollow-up observations are encouraged. \nWe thank LCOGT and its staff for their continued support of ASAS-SN. ASAS-SN is supported in part by Mt. Cuba Astronomical Foundation. For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Pulsar", "Interstellar medium", "Galaxy", "Accreting object" ] }, "answerKey": "C" }, { "id": "atel_7710", "message": "Title: Further Rapid Optical Photometry of V404 Cyg\nAuthors: R. I. Hynes (Louisiana State University), E. L. Robinson (University of Texas at Austin), J. Morales (University of Texas at El Paso)\nDate: 25 Jun 2015; 02:59 UT\nProvenance: Robert Hynes (rih@phys.lsu.edu)\nSubjects: Optical, Black Hole, Transient\nDescription: Referred to by ATel #: 7714, 7718, 7721, 7722, 7725, 7734, 7740, 7959\nWe obtained a second time-resolved observation of the outbursting black hole X-ray transient V404 Cyg (ATEL #7677 and references therein) for about two hours on 2015 June 19.35-19.44 UT using the Argos photometer on the 2.1m Otto Struve Telescope at McDonald Observatory. Our observation was performed as described in ATEL #7677 except that we used 1 second exposures. \nThe optical counterpart continued to be extremely variable, but consistent with the rising trend reported by ATEL #7696 and ATEL #7708 was brighter, ranging from r magnitude 11.0 to 13.0 during our observation. A plot of our lightcurve is available here. \nExamining our lightcurves from the two nights we highlight three remarkable behaviors. \ni) Rapid variability, on timescales faster than 20 seconds and with large amplitudes, can quite abruptly appear and disappear. On June 18 we observed this variability present most of the time, but then during the largest flare it disappeared. On June 19 we saw a mostly very smooth lightcurve (as also seen by ATEL #7686), but with a short period (about 1000 secs) when intense rapid variability was present. During this episode we observed up to 0.3-0.4 mag flares within single 1 second exposures, and so these are unresolved by our 1 second cadence. These variations occur on timescales more than an order of magnitude shorter than the light travel time across the accretion disk, and so are unlikely to be caused by the disk reprocessing X-ray emission. They may instead be associated with optical jet emission as suggested in other black hole binaries showing very rapid variability (see discussion and references in ATEL #7686) \nii) Twice on June 19, at the two brightest points in the lightcurve around r = 11.4, there were very short episodes of flaring lasting for less than a minute, which again had peak amplitudes around 0.3 mag. We have examined these images carefully and know of no artifacts that could explain them, so believe they are intrinsic to the source. It is unclear if these represent the same behavior as described in i) or a distinct very transient phenomenon associated with reaching a certain luminosity threshold. \niii) On two occasions (June 18, JD 2,457,191.87, June 19, JD 2,457,192.87), we see extended, smooth decays. A third event may happen at the end of the June 18 lightcurve, but interrupted by flares. The cleanest example on June 19 can be fitted well by an exponentially decaying component with an e-folding time of about 70 seconds.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova, Variable star", "Minor body, Variable star", "Black hole, Pulsar", "Black hole, Variable star" ] }, "answerKey": "D" }, { "id": "atel_7770", "message": "Title: NIR Photometry of the Quasar BZQJ1432-1801\nAuthors: L. Carrasco, E. Recillas, A. Porras, J. Leon-Tavares, V. Chavushyan, A. Carraminana (INAOE, Mexico)\nDate: 7 Jul 2015; 17:13 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Infra-Red, Optical, Gamma Ray, AGN, Blazar, Quasar\nDescription: We report on NIR photometry of the high redshift quasar (z=2.331) BZQJ1432-1801, associated with the radio source PKS1430-178 and probably associated with the Gamma-ray source Fermi J1433-1806 (ATel # 6310). On June 11th, 2015 (MJD 2457184.7007), we found the source with a NIR flux corresponding to H = 17.394 +/- 0.05. At this time the object is significantly brighter than it was at the time of the 2mass survey. Our observations are carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We strongly encourage further multiwavelength coverage.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater", "Supernova", "Active galactic nucleus", "Quasar" ] }, "answerKey": "D" }, { "id": "atel_7900", "message": "Title: MASTER: Bright Dwarf Nova outburst (with superhumps) and its Binary Period Discovery\nAuthors: O. Gress, V. Kornilov, V. Lipunov (Lomonosov MSU), D. Buckley (SAAO), E. Gorbovskoy (SAI MSU), N. Samus (INASAN, MSU), P. Balanutsa, N. Tiurina, A. Kuznetsov, V. Chazov, D. Vlasenko, I. Gorbunov (Lomonosov Moscow State University, Sternberg Astronomical Institute), S. Potter, M. Kotze (South African Astronomical Observatory), R. Rebolo, M. Serra-Ricart , N. Lodieu, G. Israelian (The Instituto de Astrofisica de Canarias), N. Budnev, K. Ivanov (Applied Physics Institute, Irkutsk State University), A. Tlatov, D. Dormidontov, V. Senik (Kislovodsk Solar Station of the Pulkovo Observatory), V. Krushinski, I. Zalozhnykh (Ural Federal University), Yu. Sergienko, A. Gabovich, V. Yurkov (Blagoveschensk Educational State University)\nDate: 10 Aug 2015; 19:22 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Request for Observations, Cataclysmic Variable, Transient, Variables\nDescription: MASTER OT J144927.01-324406.8 - New Dwarf Nova with binary period determination\nMASTER-SAAO auto-detection system ( Lipunov et al., Advances in Astronomy, MASTER Global Robotic Net, 2010 ) discovered OT source at (RA, Dec) = 14h 49m 27.01s -32d 44m 06.8s on 2015-08-09.71103 UT. \nThe OT unfiltered magnitude is 14.5m (the limit is 18.7m). The OT is seen in 192 images. There is no minor planet at this place. \nThe binary period P ~ 0.075d = 108 min. The light curve is available at http://master.sai.msu.ru/static/OT/MASTER_OT_J144927.01_324406.8.jpg \nThere is GALEX source at this place. \nSpectral observations are required. \nThe discovery and reference images are available at: http://master.sai.msu.ru/static/OT/144927.01-324406.8.png \nList of Optical Transients discovered by MASTER\nMASTER Global Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Variable star", "Pulsar", "Supernova" ] }, "answerKey": "B" }, { "id": "atel_7980", "message": "Title: Recurrent Nova M31N 2008-12a: on-going Liverpool Telescope photometry of the 2015 eruption\nAuthors: M. J. Darnley (LJMU), M. Henze (IEEC/CSIC), A. W. Shafter (SDSU), M. Kato (Keio University), for a larger collaboration\nDate: 2 Sep 2015; 12:49 UT\nProvenance: Matt Darnley (M.J.Darnley@ljmu.ac.uk)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 7984, 8029, 8033, 8062\nIn ATel #7964 we reported the discovery of the 2015 eruption of the recurrent nova M31N 2008-12a (Darnley et al. 2014, 2015, Henze et al. 2014, 2015a). Also see ATel #7965, #7967, #7968, #7969, #7974, #7976, #7979. \nThis recurrent nova has a remarkably short duty cycle of either 6 months or 1 year, and this is the eighth eruption detected in as many years (dating back to 2008; Henze et al. 2015b). \nHere we present additional late-time photometry obtained by the Liverpool Telescope (all times UT). All data reported here are from single exposures and make up a small subset of our entire dataset. \n` 2015 Sep 02.204 u' = 19.1 ± 0.2 \n2015 Sep 02.227 B = 20.88 ± 0.07 \n2015 Sep 02.234 V = 21.07 ± 0.08 \n2015 Sep 02.241 r' = 20.90 ± 0.07 \n2015 Sep 02.248 i' = 21.0 ± 0.1 `\nThe surface brightness of M31 at the position of the nova is approximately u'=22.0, B=22.3, V=22.0, r'=22.2, and i'=22.0, so at ~5 days since detection the 2015 eruption will soon be rendered unobservable from most ground-based (seeing limited) facilities.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Galaxy", "Active galactic nucleus", "Supernova" ] }, "answerKey": "A" }, { "id": "atel_8075", "message": "Title: MASTER: PSN in PGC2695052 during Inspect of Fermi trigger 464366002\nAuthors: O. Gress, V. Lipunov, E. Gorbovskoy, V. Kornilov, P. Balanutsa, N. Tiurina, A. Kuznetsov, I. Gorbunov, D. Vlasenko, V. Vladimirov (M. V.Lomonosov Moscow State University, SAI), N. Budnev, K. Ivanov (Irkutsk State University, Applied Physics Institute), A. Tlatov, V. Senik D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), Yu. Sergienko, A. Gabovich, V. Yurkov (Blagoveschensk Educational State University), V. Krushinskiy (Ural Federal University), D. Buckley, S. Potter, M. Kotze (South African Astronomical Observatory), R. Rebolo, M. Serra-Ricart, N. Lodieu, G. Israelian (The Instituto de Astrofisica de Canarias)\nDate: 20 Sep 2015; 20:44 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Request for Observations, Supernovae, Transient, Variables\nDescription: MASTER OT J040140.85+670613.9 discovery - PSN in 13\"W,19.7\"N of PGC2695052, - during Fermi trigger 464366002 MASTER's Inspect\nDuring MASTER's inspect of Fermi GRB150919.61 error-box MASTER-Tunka auto-detection system ( Lipunov et al., Advances in Astronomy, MASTER Global Robotic Net, 2010 ) discovered OT source at (RA, Dec) = 04h 01m 40.85s +67d 06m 13.9s on 2015-09-19.84794 UT. \nThe OT unfiltered magnitude is 17.7m (the limit is 19.4m). \nThe OT is seen in 3 images. There is no minor planet at this place. We have reference image without OT on 2010-10-14.87517 UT with 19.0 infiltered magnitude limit. \nSpectral observations are required. \nThe discovery and reference images are available at http://observ.pereplet.ru/images/MASTEROTJ040140.85670613.9.png \nThis PSN is in 13\"W,19.7\"N of elliptical PGC2695052 galaxy. \nList of Optical Transients discovered by MASTER\nMASTER Global Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Neutron star", "Galaxy", "Repeater" ] }, "answerKey": "C" }, { "id": "atel_8175", "message": "Title: MAXI/GSC detection of the X-ray outburst from Be/X-ray binary pulsar GS 0834-430\nAuthors: M. Nakajima (Nihon U.), T. Mihara, M. Sugizaki (RIKEN), S. Ueno, H. Tomida, S. Nakahira, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA), M. Serino, M. Shidatsu, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN), N. Kawai, M. Arimoto, T. Yoshii, Y. Tachibana, Y. Ono, T. Fujiwara (Tokyo Tech), A. Yoshida, T. Sakamoto, Y. Kawakubo, H. Ohtsuki (AGU), H. Tsunemi, R. Imatani (Osaka U.), H. Negoro, K. Tanaka, T. Masumitsu (Nihon U.), Y. Ueda, T. Kawamuro, T. Hori (Kyoto U.), Y. Tsuboi, S. Kanetou (Chuo U.), M. Yamauchi, D. Itoh (Miyazaki U.), K. Yamaoka (Nagoya U.), M. Morii (ISM)\nDate: 16 Oct 2015; 04:46 UT\nProvenance: Motoki Nakajima (nakajima.motoki@nihon-u.ac.jp)\nSubjects: X-ray, Binary, Neutron Star, Transient, Pulsar\nDescription: The MAXI/GSC detected an X-ray outburst from Be/X-ray binary pulsar GS 0834-430. The MAXI/GSC data shows that the current brightening started from October 5 (MJD 57300), corresponding to the ~0.12 orbital phase (Porb=105.8 d, T0=56124.5(MJD); Wilson et al. 1997). The day-averaged flux in the 4-10 keV energy band reached 0.033 +- 0.007 photons/s/cm2 (27 +- 6 mCrab) on October 12 (MJD 57307). The flux increase rate between October 7 (MJD 57302) and October 12 (MJD 57307) is 4.71e-3 phtons/s/cm2/day. Compared with the flux increase rate (25.0e-3 phtoons/s/cm2/day) of the 2012 outburst (Atel #4218,#4235), the current increase rate is only 0.19 of it. The Swift/BAT monitor also detected the current outburst, and exhibited similar results to the MAXI/GSC. \n \nThe latest light curve can be checked at the following page; \nhttp://maxi.riken.jp/top/index.php?cid=1&jname=J0835-431", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system, Neutron star", "Exoplanet, Neutron star", "Binary system, Circumstellar disk", "Binary system, Quasar" ] }, "answerKey": "A" }, { "id": "atel_8225", "message": "Title: FLOYDS Classification of ASASSN-15rv as a Post-Peak Type Ia Supernova\nAuthors: G. Hosseinzadeh, D. A. Howell, I. Arcavi, C. McCully (LCOGT/UCSB), S. Valenti (UC Davis)\nDate: 29 Oct 2015; 23:47 UT\nProvenance: Iair Arcavi (iarcavi@lcogt.net)\nSubjects: Optical, Supernovae\nDescription: We obtained a spectrum of ASASSN-15rv (ATel #8211) on 2015 October 29.6 UT with the robotic FLOYDS instrument mounted on the Faulkes Telescope South. Using Superfit (Howell et al. 2005, ApJ, 634, 119) and SNID (Blondin & Tonry 2007, ApJ, 666, 1024), we find good fits both to Type Ia supernovae 1-2 weeks after maximum light and Type Ic supernovae near maximum light at redshifts around z=0.04. At this redshift, the most recent photometry point (October 24.2) in ATel #8211 corresponds to an absolute magnitude of -19.5, favoring the Type Ia classification.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Star and stellar system", "Supernova", "Globular cluster" ] }, "answerKey": "C" }, { "id": "atel_8340", "message": "Title: Swift Follow-up of Recent Gamma-ray Flaring Activity from the FSRQ B2 1846+32B\nAuthors: Roopesh Ojha (NASA/GSFC/UMBC) and Bryce Carpenter (CUA/NASA/GSFC) on behalf of the Fermi Large Area Telescope Collaboration\nDate: 26 Nov 2015; 16:33 UT\nProvenance: Roopesh Ojha (Roopesh.Ojha@gmail.com)\nSubjects: Ultra-Violet, X-ray, Gamma Ray, >GeV, AGN, Blazar, Quasar\nDescription: Following the gamma-ray detection of flaring activity from the flat spectrum radio quasar (FSRQ) B2 1846+32B by Fermi-LAT (>100 MeV) on 19 November 2015 (ATel #8315), a Swift target of opportunity observation was performed on 21 November 2015. \nSwift/XRT data were taken in Photon Counting mode for a total exposure of about 5 ksec. The X-ray spectrum (0.5-10 keV) can be fit by an absorbed power-law model with an HI column density set to the Galactic value of 8.35x10^20 cm^-2 (Kalberla et al. 2005, A&A, 440, 775) using the abundances of Wilms et al. (2000, ApJ, 542, 914) and the cross sections of Verner et al. (1996, ApJ, 465, 487). The observed flux is (4.4^{+0.8}_{-0.7})x10^-12 erg cm^-2 s^-1 with a photon index of 1.3 +/- 0.2. This is approximately 4.4 times the flux observed on 16 January 2013 when the object was not in an elevated gamma-ray state. \nA simultaneous Swift/UVOT observation was made with the UVM2 filter yielding a magnitude of 16.64+/-0.07. We do not find any past observations to compare this to. \nFurther multiwavelength observations are encouraged. For this source the Fermi-LAT contact person is Roopesh Ojha (Roopesh.Ojha@gmail.com). \nWe would like to thank the Swift Team for making these observations possible, in particular K. L. Page as the Swift Observatory Duty Scientist.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Interstellar medium", "Quasar", "Pulsar" ] }, "answerKey": "C" }, { "id": "atel_8425", "message": "Title: INTEGRAL/JEM-X reports enhanced activity from the HMXB 4U 1036-56\nAuthors: J. Chenevez (DTU Space, Denmark), M. Fiocchi, A. Bazzano, L. Natalucci, P. Ubertini (INAF-IAPS Roma, Italy), V. Sguera (INAF-IASF Bologna, Italy), E. Kuulkers (ESA/ESAC, Spain), on behalf of a larger collaboration\nDate: 17 Dec 2015; 11:42 UT\nProvenance: Jerome CHENEVEZ (jerome@dsri.dk)\nSubjects: X-ray, Binary, Neutron Star, Transient, Pulsar\nDescription: Referred to by ATel #: 8435, 10486\nDuring the Galactic Plane Scanning performed by INTEGRAL on December 11th, 2015, the X-ray monitor JEM-X has detected enhanced activity from the high mass X-ray binary (HMXB) 4U 1036-56, aka RX J1037.5-5647. The position of the source was covered by the JEM-X field of view two times between UTC 6:55 and 12:38. The source was only detected at 4σ between 3-10 keV for a total effective exposure of 2.7 ks in the combined JEMX-1+2 mosaic. \nThe averaged 3-10 keV flux was 5.2 +/- 1.5 mCrab, which, at the 5 kpc source distance (Motch et al. 1997, A&A 323, 853), leads to a luminosity of about 2.7×1035 erg/s. We derive a 5σ upper limit of 2 mCrab between 10-25 keV. The source was not detected by IBIS/ISGRI with an exposure of 4 ks leading to a 3σ upper limit of 6 mCrab in the band 22-60 keV. \nThe source was not detected at all the last time its position was observed by INTEGRAL on November 23rd, 2015. \n\n4U 1036-56 is a Be X-ray pulsar (e.g. Torres et al. 2012, ApJ 761, 49), whose last outburst was reported by Swift in February 2012 (Krimm et al. ATel #3936).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater, Pulsar", "Neutron star, Quasar", "Neutron star, Star and stellar system", "Neutron star, Pulsar" ] }, "answerKey": "D" }, { "id": "atel_8500", "message": "Title: INTEGRAL observes a bright flare and spectral changes in V404 Cyg: possible hard to soft transition ahead?\nAuthors: S. E. Motta (Uni. Oxford), C. Sanchez-Fernandez, E. Kuulkers, J. Kajava (ESA/ESAC), E. Bozzo (Uni. Geneva) \nDate: 3 Jan 2016; 11:39 UT\nProvenance: Sara Elisa Motta (sara.motta@physics.ox.ac.uk)\nSubjects: X-ray, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 8501, 8507, 8510, 8512, 8516, 8520\nWe report the results of ongoing INTEGRAL TOO observations of V404 Cyg in spacecraft revolutions 1627 (from 2015-12-29 01:43 to 2015-12-31 03:04), and 1628 (from 2015-12-31 15:43 to 2016-01-02 19:41). The total observation time per revolution is ~170 ks. \nDuring revolution 1627, V404 Cyg was observed by ISGRI and JEM-X instruments with following fluxes and significances: \nIBIS/ISGRI 20-40 keV 2.67 +/- 0.09 cts/s ( 16.4 +/- 0.5 mCrab ) signif. = 31 \nIBIS/ISGRI 40-80 keV 1.83 +/- 0.06 cts/s ( 23.8 +/- 0.8 mCrab ) signif. = 31 \nJEM-X 1 3-10 keV 0.77 +/- 0.04 cts/s ( 3.3 +/- 0.2 mCrab ) signif. = 22 \nJEM-X 1 10-20 keV 0.33 +/- 0.03 cts/s ( 5.3 +/- 0.5 mCrab ) signif. = 11 \nJEM-X 2 3-10 keV 0.72 +/- 0.03 cts/s ( 3.1 +/- 0.2 mCrab ) signif. = 23 \nJEM-X 2 10-20 keV 0.32 +/- 0.03 cts/s ( 5.2 +/- 0.4 mCrab ) signif. = 13 \nIn Rev. 1627 the source has globally brightened by a factor of about 3 compared to revolution 1626 (from 2015-12-26 07:59 to 2015-12-28 12:00, ATel #8475). The JEM-X + ISGRI spectrum can be fitted with a simple power law model (photon index 1.71 +/- 0.03). \nDuring revolution 1628 the flux of V404 Cyg has increased further. The JEM-X and ISGRI light curves show significant flaring activity. Three main flaring periods are visible in different energy bands both in IBIS/ISGRI and JEM-X, with peaks at the times indicated below: \nJMX1: 3-10 keV: \nTime (UTC) Peak Flux (Crab) \n2015-12-31 17:19:32.422 1.383 +/- 0.09 \n2015-12-31 18:38:22.351 2.95 +/- 0.13 \n2016-01-01 00:18:01.448 3.66 +/- 0.14 \nJMX1: 10-20 keV: \nTime (UTC) Peak Flux (Crab) \n2015-12-31 17:19:12.422 2.68 +/- 0.23 \n2015-12-31 18:38:05.951 6.12 +/- 0.35 \n2016-01-01 00:18:01.448 6.99 +/- 0.36 \nISGRI, 20-40 keV \nTime (UTC) Peak Flux (Crab) \n2015-12-31 17:19:31.529 2.83 +/- 0.13 \n2015-12-31 18:38:06.427 7.9 +/- 0.3 \n2016-01-01 00:18:00.186 9.28 +/- 0.24 \nISGRI, 40-80 keV \nTime (UTC) Peak Flux (Crab) \n2015-12-31 17:19:11.530 5.4 +/- 0.2 \n2015-12-31 18:38:06.427 15.27 +/- 0.46 \n2016-01-01 00:17:39.688 15.28 +/- 0.38 \nThe first flaring period probably corresponds to the flare detected by Swift/BAT (Trigger 668949, CGN circular 18785) in the 15-150 keV energy band. The second flaring period most likely corresponds to the flares detected by MAXI on MJD 57387 at 18:38:04UT reported in ATel #8494. The last and strongest flaring period has been partially observed by Swift/XRT. In Obs. 00031403134 (started on 2016-01-01T17:30:58) a flare is visible in the Swift/XRT light curve (0.6-10keV energy band). \nThe JEM-X + ISGRI spectrum taken in rev. 1628 cannot be fitted with a simple power law and looks complex as in many spectra taken in June-July 2015. The hard tail now show a clear cutoff at ~150 keV, with a power law photon index of 1.3. Based on previous experience, this photon index probably indicates the presence of a fairly strong reflection component (Motta et al. in prep.) rather than an hardening of the source. The appearance of an high-energy cutoff and of a reflection component, might indicate that V404 Cyg is going through or will soon go through a canonical hard to soft transition. \nThe JEM-X and ISGRI light curves can be found here: ftp://ftp.sciops.esa.int/pub/ekuulker/JEMX_ISGRI_1628_lcr.pdf \nMulti-Wavelength observations, especially in radio, are strongly encouraged in order to confirm a possible state transition.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Pulsar", "Black hole", "Stellar evolution", "Exoplanet" ] }, "answerKey": "B" }, { "id": "atel_8575", "message": "Title: A new NIR Flare of the QSO PKS0336-019\nAuthors: L. Carrasco, J. Miramon, E. Recillas, A. Porras, V. Chavushyan, A. Carraminana (INAOE, Mexico)\nDate: 22 Jan 2016; 08:04 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Infra-Red, Optical, Gamma Ray, AGN, Blazar, Quasar\nDescription: Referred to by ATel #: 8598, 10185\nWe report on a NIR flare of the high redshift QSO PKS0336-019 (z=0.852), also known as CTA026 associated with the gamma-ray source 2FGL0309.1+1027. Our most recent NIR photometry for this source shows that on January 12th,2016 (JD2457399.7414), the object brightness corresponded to H = 13.558 +/- 0.06. In a previous observation in this band (MJD2457375.78) this object had H = 14.563 +/- 0.03. Hence, the object has increased its luminosity by a factor of 2.5 in this short lapse. Our observations are carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We strongly encourage further multiwavelength coverage.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Quasar", "Stellar evolution", "Magnetar" ] }, "answerKey": "B" }, { "id": "atel_8670", "message": "Title: Spectroscopic Classification of PSN J15502534+1856075 as a Type II Supernova\nAuthors: G. Halevi, H. Yuk, I. Shivvers, A. V. Filippenko (UC Berkeley)\nDate: 10 Feb 2016; 22:24 UT\nProvenance: Isaac Shivvers (ishivvers@berkeley.edu)\nSubjects: Optical, Supernovae\nDescription: We report that a CCD spectrum (range 350-1050 nm) of PSN J15502534+1856075 was obtained on Feb. 07.6 UT with the Kast spectrograph on the 3-m Shane telescope at Lick Observatory. The spectrum shows that the object, located in NGC 6004, is a Type II supernova about one to two months after explosion; strong hydrogen Balmer lines and other normal Type-II features with well-developed P-Cygni profiles are visible on a continuum. The object was classified through cross-correlation with a collection of supernova spectra using the \"SuperNova Identification code\" (SNID; Blondin & Tonry 2007, Ap.J., 666, 1024), which indicates good matches with several Type IIP supernovae from a few weeks to a few months past explosion.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Magnetar", "Near-Earth object", "Minor body" ] }, "answerKey": "A" }, { "id": "atel_8750", "message": "Title: Spectroscopic Classification of AT 2016aqp as a Type II-P Supernova\nAuthors: Chuan-Jun Wang and Ju-Jia Zhang (Yunnan observatories)\nDate: 28 Feb 2016; 02:04 UT\nProvenance: Ju-Jia Zhang (jujia@ynao.ac.cn)\nSubjects: Optical, Supernovae\nDescription: We obtained an optical spectrum (range 350-900 nm) of AT 2016aqp on UT 2016 Feb. 27.5 with the Li-Jiang 2.4 m telescope (LJT + YFOSC) at Li-Jiang observatory of Yunnan Observatories. The pectrum is similar to that of a Type-IIP supernova at a few days after explosion. Cross-correlation with a library of supernova spectra using the \"Supernova Identification\" code (SNID; Blondin and onry 2007, Ap.J. 666, 1024) shows that it matches with SN 2005cs at t = +4 days. Given a recession velocity of 4720 km/s for the host galaxy PGC 16065, an expansion velocity of about 8700 km/s can be deduced from the H-alpha absorption minimum.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Interstellar medium", "Nova", "Star and stellar system" ] }, "answerKey": "A" }, { "id": "atel_8850", "message": "Title: NIR Flare of the Blazar FBQS J102311.5+394815\nAuthors: L. Carrasco, A. Porras, E. Recillas, V. Chavushyan, J. Leon-Tavares (INAOE, Mexico)\nDate: 21 Mar 2016; 20:02 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Infra-Red, Optical, Gamma Ray, AGN, Blazar, Quasar\nDescription: We report a NIR flare of the high redshift (z=1.254) FBQSJ102311.5+394815, cross correlated with the gamma-ray source 1FGLJ1023.6+3937 and the radio source 4C+40.25. On March 18th,2016 (MJD 2457465.82) We found this source with a flux corresponding to H = 14.900 +/- 0.03, while on MJD 2457375.01 had H = 15.792 +/- 0.05. Hence it has had an increment of 0.9mag in this lapse. Apparently, the source has been monotonically increasing since MJD 2455603, when it was H = 16.922 +/- 0.08. Our observations are carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We strongly encourage further multiwavelength coverage.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Quasar", "Minor body, Quasar", "Binary system, Quasar", "Black hole, Quasar" ] }, "answerKey": "D" }, { "id": "atel_8950", "message": "Title: Possible Nova in M31 detected by MASTER\nAuthors: E. Popova, V. Lipunov(Lomonosov MSU), A. Tlatov (KSS), R. Rebolo (IAC), E. Gorbovskoy, N. Tiurina, P. Balanutsa, A. Kuznetsov, V. Kornilov, V. Vladimirov, I. Gorbunov (Lomonosov Moscow State University, SAI), M. Serra Ricart, G. Israelian (IAC), V. Senik, D. Dormidontov A. Parkhomenko (Kislovodsk Solar Station, Pulkovo observatory)\nDate: 15 Apr 2016; 08:57 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Request for Observations, Nova, Transient, Variables\nDescription: Referred to by ATel #: 9116, 9390, 9394, 14703\nMASTER OT J004528.12+414117.6 discovery - possible Nova in M31\nMASTER-Kislovodsk auto-detection system ( Lipunov et al., \"MASTER Global Robotic Net\", Advances in Astronomy, 2010, 349171 ) discovered OT source at (RA, Dec) = 00h 45m 28.12s +41d 41m 17.6s on 2016-04-10.03461 UT. \nThe OT unfiltered magnitude is 19.0m (the limit is 19.5m). \nThe OT is seen in 3 image. There is no minor planet at this place. We have reference image without OT on 2016-02-08.68476 UT with unfiltered magnitude limit 21.1m. \nWe reobserved it with unfiltered m_OT=18.6 on 2016-04-13 05:11:28.249UT in MASTER-IAC \n\nSpectral observations are required. The discovery and reference images are available at: http://master.sai.msu.ru/static/OT/004528.12414117.6.png \nMASTER Global Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Accreting object", "Nova", "Galaxy" ] }, "answerKey": "D" }, { "id": "atel_9030", "message": "Title: Changing-type Seyfert NGC 2617 brightens again\nAuthors: V. L. Oknyansky (Sternberg Astronomical Institute, Moscow), N. A. Huseynov (Shamakhy Astrophysical Observatory, Azerbaijan), V. M. Lipunov, E. S. Gorbovskoy, A. S. Kuznetsov, P. V. Balanutza, V. I. Metlov (Sternberg Astronomical Institute, Moscow), C. M. Gaskell (UCSC)\nDate: 7 May 2016; 10:44 UT\nProvenance: Victor Oknyansky (oknyan@mail.ru)\nSubjects: Optical, AGN\nDescription: Referred to by ATel #: 11703, 16324\nWe report another brightening of NGC 2617, an AGN which underwent a dramatic change from a largely obscured Seyfert 1.8 to an unobscured Seyfert 1 between 2003 to 2013 (Shappee et al. 2013, ATel #5010; Shappee et al. 2014, ApJ, 788, 48). Spectroscopy and BVRIJHK photometry from January 2016 revealed that NGC 2617 was continuing to be in a high state (Oknyansky et al. 2016, ATel#9015). We report here a new brightening. CCD photometry with the 50-cm Maksutov AZT-5 telescope of SAI MSU Crimean Station on Apr.28 showed that NGC 2617 had a B magnitude of 14.84 in a 10-arcsecond aperture. This was 0.15 mag. brighter than on April 22. Unfiltered CCD photometry with a 15-arcsecond (8-pixel) aperture by the MASTER Global Robotic Network during May 1-5 confirms that NGC 2617 continues to be in a bright state and continues to vary. It is brighter than on Apr. 22 by about 0.1 mag. Light curves with new points can be seen here. (B is shown at the top and the unfiltered MASTER relative magnitudes at bottom – see ATel #9015 for details.)", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Active galactic nucleus", "Stellar evolution", "Globular cluster" ] }, "answerKey": "B" }, { "id": "atel_9100", "message": "Title: Gaia16alq type Ia SN observed during its maximum\nAuthors: Carrasco, J. M. (Institut de Ciencies del Cosmos-University of Barcelona); Burgaz, U. (Ege University); Kolaczkovski, Z., Mikolajczyk, P. (Instytut Astronomiczny Uniwersytetu Wroclawskiego); Wiersema, K. (University of Leicester); Jordi, C. (Institut de Ciencies del Cosmos-University of Barcelona); Vilardell, F. (Institut d'Estudis Espacials de Catalunya)\nDate: 30 May 2016; 14:37 UT\nProvenance: Josep Manel Carrasco Martínez (carrasco@am.ub.es)\nSubjects: Optical, Supernovae, Transient\nDescription: We provide fitting of the lightcurve observed for Gaia16alq type Ia SN (see ATEL#8991) including observations obtained during its peak in four passbands (BVRI).\nOur observations were obtained from three different observatories: Joan Oró Telescope at Observatori del Montsec (Sant Esteve de la Sarga, Spain), Bialkow Observatory (Wroclaw Astronomical Institute,Polland) and Leicester Telescope.\n * Obtained parameters from SNooPy code using max_model with dm15 option (EBV and EBV2 models were also tested but best results were obtained with max_model). SnooPy code accounts for the Milky Way E(B-V) colour excess based on the coordinates of the source. \n * Lightcurve fitting can be seen in this webpage\n * Obtained parameters from SNooPy \nDM = 34.689 +/- 0.036 \nEBVhost = 0.241 +/- 0.016 \ndm15 = 0.915 +/- 0.008 \nTmax = 57508.950 +/- 0.067 \nRmax = 16.111 +/- 0.003 \nImax = 16.522 +/- 0.007 \nVmax = 15.818 +/- 0.005 \nBmax = 16.109 +/- 0.004 \n\n * Absolute Magnitudes calculated from m - M = DM \n\nBmax = -18.58 +/- (0.004+/-0.036) \nVmax = -18.871 +/- (0.005+/-0.036) \nImax = -18.167 +/- (0.007+/-0.036) \nRmax = -18.578 +/- (0.003+/-0.036) \n\nerrors come from both DM and individual m errors found by SNooPy \n\n\nThese days Gaia16alq is having the 2nd peak on the I-band and all other bands such as the small drop and increase on R are following the template smoothly. Future fittings adding more observations could enhance the derivation of these preliminary analysis.\nObservatori Astronomic del Montsec", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Supernova", "Exoplanet", "Active galactic nucleus" ] }, "answerKey": "B" }, { "id": "atel_9200", "message": "Title: MASTER-Tunka: bright SN in edge-on UGC05919\nAuthors: O. Gress (ISU), V. Lipunov (Lomonosov MSU), N. Budnev, K. Ivanov (Irkutsk State University, Applied Physics Institute), N. Tiurina, E. Gorbovskoy, P. Balanutsa, A. Kuznetsov, D. Vlasenko, V. Kornilov, D. Kuvshinov (Lomonosov Moscow State University, SAI), V. Shumkov, N. Kochutina, S. Shurpakov (MASTER-team)\nDate: 29 Jun 2016; 19:42 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Supernovae, Transient, Variables\nDescription: MASTER OT J104916.33+582039.9 discovery - PSN in 16.5W,2.5S of UGC05919\nMASTER-Tunka auto-detection system ( Lipunov et al., \"MASTER Global Robotic Net\", Advances in Astronomy, 2010, 349171 ) discovered OT source at (RA, Dec) = 10h 49m 16.33s +58d 20m 39.9s on 2016-06-29.68150 UT. \nThe PSN unfiltered magnitude is 15.9m (limit 18.7m). \nThe OT is seen in 3 images. There is no minor planet at this place. \nWe have reference image without OT on 2016-03-14.71617 UT with 19.5m unfiltered magnitude limit in MASTER-Tunka. The nearest image without PSN was made at MASTER-IAC on 2016-05-28 22:30:58UT with unfiltered m_lim=19.8 \nSpectral observations are required. \nThe discovery and reference images are available at http://observ.pereplet.ru/images/MASTEROTJ104916.33+582039.9.jpg \nList of Optical Transients discovered by MASTER\nMASTER Global Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Magnetar", "Interstellar medium", "Supernova" ] }, "answerKey": "A" }, { "id": "atel_9250", "message": "Title: Liverpool Telescope Spectrum of OGLE-2016-NOVA-02\nAuthors: S. C. Williams (Lancaster), M. J. Darnley (LJMU)\nDate: 16 Jul 2016; 10:47 UT\nProvenance: Steven Williams (scw@astro.ljmu.ac.uk)\nSubjects: Optical, Nova, Transient\nDescription: We obtained a spectrum of OGLE-2016-NOVA-02 (ATel #9246) with the FRODOSpec spectrograph (Barnsley et al. 2012) on the 2.0m Liverpool Telescope (Steele et al. 2004) on 2016 July 15.97 UT. The spectrum was taken using the higher resolution mode, which gives a wavelength coverage of 5900 to 8000Å and resolution of R = 5300 in the red arm (no significant features were detected in the blue arm, which covers 3900 to 5100Å). \nThe strongest feature in the spectrum is an O I emission line at 7774Å, which has a FWHM of 1800±100 km/s. The only other line significantly detected is Hα, for which we measure a FWHM of 2100±200 km/s. This spectrum is consistent with OGLE-2016-NOVA-02 being a highly reddened classical nova eruption.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Globular cluster", "Accreting object", "Nova" ] }, "answerKey": "D" }, { "id": "atel_9375", "message": "Title: Liverpool Telescope Spectrum of Classical Nova ASASSN-16ig\nAuthors: S. C. Williams (Lancaster), M. J. Darnley (LJMU)\nDate: 15 Aug 2016; 11:46 UT\nProvenance: Steven Williams (scw@astro.ljmu.ac.uk)\nSubjects: Optical, Nova\nDescription: Referred to by ATel #: 9377, 9379, 9613\nWe obtained an optical spectrum of classical nova ASASSN-16ig in Sagittarius (see ATels #9343, #9352, #9359, CBET 4295, 4299) with the FRODOSpec spectrograph (Barnsley et al. 2012) on the 2.0m Liverpool Telescope (Steele et al. 2004) on 2016 August 11.88 UT. The spectrum was taken using the higher resolution mode, which gives a wavelength coverage of 3900 to 5100Å and 5900 to 8000Å, with a resolution of R ~ 5400. \nThe spectrum shows Balmer emission (Hα, Hβ, Hγ and Hδ) with strong P-Cygni absorption components. Hα and Hβ clearly display a `double' absorption structure with one minimum at approximately -800 km/s and one at around -1500 km/s. Measuring the absorption component of Hα indicates a maximum velocity of 2300 km/s. This two-component absorption profile is also seen on the O I 7774 Å emission line. We detect the Fe II (42) and (74) multiplets, again with strong absorption components and minima at -800 km/s. Some of the Fe II lines also show evidence of the higher velocity absorption component seen in Hα, Hβ and O I. The spectrum shows absorption from the N I (3) triplet with the minima blueshifted by approximately 700 km/s. We also detect absorption from the Si II (2) doublet (minima at around -800 km/s). Our results are in good agreement with CBET 4299.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Minor body", "Binary system", "Nova" ] }, "answerKey": "D" }, { "id": "atel_9450", "message": "Title: Renewed Gamma-Ray Emission from the blazar PKS 1510-089 Detected by AGILE\nAuthors: P. Munar-Adrover (INAF/IAPS), C. Pittori (ASDC and INAF/OAR), A. Bulgarelli (INAF/IASF-Bo), F. Lucarelli, F. Verrecchia (ASDC and INAF/OAR), G. Piano (INAF/IAPS), V. Fioretti, A. Zoli (INAF/IASF-Bo), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), S. Vercellone (INAF/IASF-Pa), G. Minervini (CIFS and INAF/IAPS), E. Striani (CIFS and INAF/IAPS), M. Cardillo (INAF/OA-Arcetri and INAF/IAPS), F. Gianotti, M. Trifoglio (INAF/IASF-Bo), A. Giuliani, S. Mereghetti, P. Caraveo, F. Perotti (INAF/IASF-Mi), A. Chen (Wits University), A. Argan, E. Costa, E. Del Monte, I. Donnarumma, Y. Evangelista, M. Feroci, F. Lazzarotto, I. Lapshov, L. Pacciani, P. Soffitta, S. Sabatini, V. Vittorini (INAF/IAPS), G. Pucella, M. Rapisarda (ENEA-Frascati), G. Di Cocco, F. Fuschino, M. Galli, C. Labanti, M. Marisaldi (INAF/IASF-Bo), A. Pellizzoni, M. Pilia, A. Trois (INAF/OA-Cagliari), G. Barbiellini, E. Vallazza (INFN Trieste), F. Longo (Univ. Trieste and INFN Trieste), A. Morselli, P. Picozza (INFN and Univ. Roma Tor Vergata), M. Prest (Univ. dell'Insubria), P. Lipari, D. Zanello (INFN and Univ. Roma Sapienza), P. W. Cattaneo, A. Rappoldi (INFN Pavia), S. Colafrancesco (INAF/OAR and Wits University), N. Parmiggiani (University of Modena and Reggio Emilia), A. Ferrari (Univ. Torino and CIFS), A. Antonelli (ASDC and INAF/OAR), P. Giommi (ASDC), L. Salotti, G. Valentini, and F. D'Amico (ASI)\nDate: 4 Sep 2016; 14:05 UT\nProvenance: Pere Munar-Adrover (pere.munar@iaps.inaf.it)\nSubjects: Gamma Ray, AGN, Black Hole, Blazar, Transient\nDescription: Referred to by ATel #: 9455, 9520\nAGILE is currently detecting enhanced gamma-ray emission above 100 MeV from a source which position is consistent with the blazar PKS 1510-089. (the last activity of this source was reported in ATel #9350). \nIntegrating from 2016-09-02 01:00 UT to 2016-09-04 01:00 UT, a preliminary maximum likelihood analysis yields a detection above 100 MeV positioned at Galactic coordinates (l,b) = (350.48, 40.76) +/- 0.7 (stat.) +/- 0.1 (syst.). The gamma-ray flux is F =(3.2 +/- 1.0) x 10E-6 ph/cm2/sec with a significance level above 5 sigma. \nThis measurement was obtained with AGILE observing a large portion of the sky in spinning mode. Multifrequency observations of the source are strongly encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Black hole", "Globular cluster", "Near-Earth object" ] }, "answerKey": "B" }, { "id": "atel_9510", "message": "Title: Amplitude correction to ATEL #9509\nAuthors: T. Pogrosheva, O. Gress, V. Lipunov (Lomonosov MSU), Podesta R. (OAFA), Levato H.(ICATE), Gorbovskoy E., Tyurina N.,Balanutsa P., Kuznetsov A., Kornilov V., Kuvshinov D., Vladimirov V., Ivanov K.(Lomonosov MSU), Saffe C.(ICATE), Lopez C., Podesta, F.(OAFA)\nDate: 20 Sep 2016; 00:43 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, A Comment\nDescription: There is a star in VIZIER at the position of MASTER OT J220559.40-341434.9 (ATEL #9509) with known B2=18.24,R2=18.4(USNO-B1) and UV (GALEX, it means the possible accretion to white dwarf). MASTER unfiltered W is calibrated by USNO-B1 as w=0.2B+0.8R, so current outburst's Amplitude is more then 3.9m (not 7.5). There is reference image with unfiltered m_OT=18.4 on 2016-08-02.21091 UT(m_lim=20.3m). \nMASTER Global Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system", "Circumstellar disk", "Globular cluster", "Neutron star" ] }, "answerKey": "A" }, { "id": "atel_9650", "message": "Title: Violent optical activity of the blazar OJ 287\nAuthors: V. Larionov, A. A. Mokrushina and T. S. Grishina (St. Petersburg University, Russia)\nDate: 19 Oct 2016; 12:19 UT\nProvenance: V. Larionov (vlar@astro.spbu.ru)\nSubjects: Optical, AGN, Black Hole, Blazar, Quasar\nDescription: Referred to by ATel #: 9675, 9709, 12086\nWe perform optical photometric and polarimetric monitoring of a sample of gamma-bright blazars using 0.7-m AZT-8 telescope (Crimean Astrophysical Observatory) and 0.4-m LX-200 telescope (St.Petersburg), as a part of WEBT/GASP project. Confirming X-ray and UV Swift data reported in ATel#9629, we report that OJ 287 reached R=12.96 in the night of 2016 October 18, TJD 57680.64. This is the highest value that we observed during our monitoring of this blazar since 2002. R band light curve for OJ 287 can be seen on our web-page.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Black hole", "Black hole, Variable star", "Black hole, Circumstellar disk", "Black hole, Active galactic nucleus" ] }, "answerKey": "A" }, { "id": "atel_9750", "message": "Title: Discovery of a Possible Nova in M31\nAuthors: Hiroyuki Maehara (Okayama Astrophysical Observatory, NAOJ, NINS)\nDate: 12 Nov 2016; 10:48 UT\nProvenance: Hiroyuki Maehara (h.maehara@oao.nao.ac.jp)\nSubjects: Optical, Nova, Transient, Variables\nDescription: Referred to by ATel #: 9751\nWe report the discovery of a possible nova in M31 on V-band CCD images taken on 2016-11-12.372 UT with the 1.05-m Schmidt telescope and KWFC (Sako et al. 2012, SPIE, 8446, 84466L) at Kiso Observatory, the University of Tokyo. The object is located at R.A. = 00:45:15.63, Decl. = +41:39:06.5 (equinox 2000.0; position uncertainty 0.14\"). The following V-band magnitude and upper limit were obtained using the 1.05-m telescope at Kiso: \n \n \n Date(UT) Magnitude Filter Remarks \n 2016-11-11.372 <19.2 V # upper limit \n 2016-11-12.372 18.18+/-0.08 V", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Nova", "Active galactic nucleus", "Galaxy" ] }, "answerKey": "B" }, { "id": "atel_9825", "message": "Title: ASASSN-16oj: Discovery of A Probable Supernova in SDSS J053208.29-020407.9\nAuthors: T. W.-S. Holoien, K. Z. Stanek, C. S. Kochanek, J. S. Brown, J. Shields (Ohio State), B. J. Shappee (Hubble Fellow, Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), D. Bersier (LJMU), Subo Dong, S. Bose, Ping Chen (KIAA-PKU), J. Brimacombe (Coral Towers Observatory)\nDate: 5 Dec 2016; 16:55 UT\nProvenance: Thomas Holoien (tholoien@astronomy.ohio-state.edu)\nSubjects: Optical, Supernovae, Transient\nDescription: Referred to by ATel #: 9829\nDuring the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN or \"Assassin\"), using data from the quadruple 14-cm \"Cassius\" telescope in Cerro Tololo, Chile, we discovered a new transient source, most likely a supernova, in the galaxy SDSS J053208.29-020407.9. \nASASSN-16oj (AT 2016ips) was discovered in images obtained on UT 2016-12-05.15 at V~17.0 mag. We also detect the object in images obtained on UT 2016-12-02.17 (V~17.1), UT 2016-11-28.45 (V~17.0), UT 2016-11-24.21 (V~17.4), and UT 2016-11-21.23 (V~17.2). We do not detect (V>17.2) the object in images taken on UT 2016-11-20.23 and before. This figure shows the archival DSS image of the host (left), the ASAS-SN V-band reference image of the host (center), and the ASAS-SN V-band discovery image (right). The red circle has a radius of 5\" and is centered on the position of the transient in the discovery image. \nThe position of ASASSN-16oj is approximately 15.9\" South and 16.3\" East from the center of the galaxy SDSS J053208.29-020407.9, which has no redshift available in NED. We note that the V-band extinction at the location of the transient is A_V=1.5, meaning the transient may be quite luminous. Properties of the new source and photometry are summarized in the tables below: \n \n \n Object RA (J2000) DEC (J2000) Disc. UT Date Disc. V mag Approx. Abs. Mag Offset from Host (\") \n ASASSN-16oj 05:32:09.380 -02:04:23.88 2016-12-05.15 17.0 N/A 22.77 \n \n \n \n Obs. UT Date V mag \n 2016-11-20.23 >17.2 \n 2016-11-21.23 17.2 \n 2016-11-24.21 17.4 \n 2016-11-28.45 17.0 \n 2016-12-02.17 17.1 \n 2016-12-05.15 17.0 \n \nFollow-up observations are encouraged. \nWhile we are participating in the TNS system to minimize potential confusion, ASAS-SN will continue using ASASSN-16xx transient names as our primary nomenclature (including supernovae, but also other classes of transients), and we encourage others to do the same. We prefer merging the names as ASASSN-16xx (AT2016xyz) to preserve, rather than anonymize, the origin of the transient. \nWe thank LCOGT and its staff for their continued support of ASAS-SN. ASAS-SN is supported by NSF grant AST-1515927, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, the Chinese Academy of Sciences South America Center for Astronomy (CASSACA), and the Mt. Cuba Astronomical Foundation. For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy", "Active galactic nucleus", "Circumstellar disk", "Pulsar" ] }, "answerKey": "A" }, { "id": "atel_9900", "message": "Title: Spectroscopic classification of ASASSN-16pa as a normal Type Ia supernova\nAuthors: N. Morrell, M. Phillips (Las Campanas Observatory), Benjamin J. Shappee (Hubble Fellow, Carnegie Observatories), Subo Dong (KIAA-PKU)\nDate: 25 Dec 2016; 23:11 UT\nProvenance: Benjamin Shappee (bshappee@obs.carnegiescience.edu)\nSubjects: Optical, Supernovae\nDescription: We report on an optical spectroscopic observation of supernova candidate ASASSN-16pa (ATel #9893, AT 2016izf) using the du Pont 2.5-m telescope (+ WFCCD) at Las Campanas Observatory on UT 2016-12-25.04. The target was discovered by the All-Sky Automated Survey for Supernovae (ASAS-SN; Shappee et al. 2014, ApJ, 788, 48). We used SNID (Blondin & Tonry, 2007, ApJ, 666, 1024) to identify the type and phase of the SN spectra.\nThe spectrum matches with SNe Ia-norm, few days before maximum (-1.3 +/- 4.7). SNID estimates z=0.034 (0.005).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Supernova", "Active galactic nucleus", "Black hole" ] }, "answerKey": "B" }, { "id": "atel_10075", "message": "Title: Optical brightening of Swift J1753.5-0127 observed with the Faulkes Telescope North\nAuthors: Ahlam Al Qasim, Aisha AlMannaei, David M. Russell (NYU Abu Dhabi), Fraser Lewis (Faulkes Telescope Project & Astrophysics Research Institute, LJMU), Guobao Zhang, Joseph D. Gelfand (NYU Abu Dhabi)\nDate: 14 Feb 2017; 14:39 UT\nProvenance: David M. Russell (dave.russell5@gmail.com)\nSubjects: Optical, X-ray, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 10081, 10097, 10110, 10114, 10118, 10288, 10325, 10562, 10664, 16262\nWe have continued monitoring Swift J1753.5-0127, the black hole candidate X-ray binary, with the 2-m Faulkes Telescope North after it became once again visible from the ground. Last year, we reported an optical fading of the source towards quiescence (ATel #9708, #9739). Follow-up radio (ATel #9765), X-ray (ATel #9735) and optical (ATel #9741, #9758) observations confirmed the source was very faint compared to the last 11 years. \n \nWe report our new magnitudes of the object in the i'-band and the V-band as follows. V = 18.37 +- 0.06; i' = 17.92 +- 0.05 on 30 January 2017 (MJD 57783.7) and V = 17.27 +- 0.05; i' = 16.95 +- 0.02 on 13 February (MJD 57797.6). The latest magnitudes are similar to that before the fading in August 2016; we observe that it is now as bright as it was during July 2016. During the recent brightening, the V-i' color of the source seems to have shifted back to what it originally was before fading away, getting bluer as it has brightened, probably due to an increase in temperature of the accretion disc. The source is 4.0 magnitudes brighter in V-band since it was detected at V = 21.25 +- 0.03 on 8 November 2016 with the Nordic Optical Telescope (ATel #9741). \n \nThe re-brightening exhibits surprising behavior since it was expected to fade into quiescence after its dramatic fading, and perhaps become undetectable. Re-flares are not uncommon in X-ray binary outburst decays, but returning to the previous bright flux level is highly unusual (another case was the neutron star system IGR J00291+5934; Lewis et al. 2010). It is unclear whether the source will continue to brighten, remain steady like it was before the fade, or exhibit flares before fading once more into quiescence. Multi-wavelength observations are encouraged during this time. We are requesting Swift observations spanning the next two weeks. The Faulkes Telescope observations are part of an on-going monitoring campaign of ~ 40 low-mass X-ray binaries (Lewis et al. 2008). This work makes use of observations from the Las Cumbres Observatory (LCO).\nSwift J1753.5-0127 Faulkes Telescope light curve", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Binary system", "Near-Earth object, Binary system", "Quasar, Binary system", "Pulsar, Binary system" ] }, "answerKey": "A" }, { "id": "atel_10150", "message": "Title: CNEOST OT PTSS-17dmk, discovery - new OT, no VIZIER data\nAuthors: Bin Li, Haibin Zhao(PMO), Xiaofeng Wang, Wenxiong Li (Tsinghua University), Zhijian Xu , Hanjie Tan (CCU), Lifan Wang (PMO), Jujia Zhang (YNAO)\nDate: 8 Mar 2017; 03:05 UT\nProvenance: Bin Li (libin0129@yahoo.com)\nSubjects: Optical, Nova, Transient\nDescription: Referred to by ATel #: 10151\nPTSS (Purple Mountain Observtory(PMO) & Tsinghua Supernova Survey ) discovered OT source PTSS-17jdx at (RA, Dec) = 13h20m53.59s -04d14m04.70s on 2017-02-07.727524 UT with the 1.04/1.8 Schmidt Telescope( named Chinese Near Earth Object Survey Telescope , CNEOST ) at Xuyi station of PMO. \nThe OT PTSS-17jdx SDSS-r magnitude is 17.5m. There is no any source in VIZIER. More details are shown follows. \n \n \n Filter| UT| Mag| Errer-mag | Limite Mag( 3 sigma) \n SDSS-r | 2017-03-07.764455| 17.593| 0.071| 19.919 \n SDSS-r | 2017-03-07.745990| 17.551| 0.058| 20.185 \n SDSS-r | 2017-03-07.727524| 17.620| 0.065| 20.120 \n SDSS-r | 2017-02-24.824783| 18.661| 0.195| 18.978 \n SDSS-r | 2017-02-24.807106| 18.233| 0.075| 20.414 \n SDSS-r | 2017-02-24.789429| 18.243| 0.090| 20.177 \n \nCNEOST", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar, Supernova", "Nova, Supernova", "Circumstellar disk, Supernova", "Nova, Near-Earth object" ] }, "answerKey": "B" }, { "id": "atel_10250", "message": "Title: S-CUBED detection of an outburst of SXP 59.0 in the SMC\nAuthors: J. A. Kennea (PSU), P. A. Evans (Leicester) and M. J. Coe (Southampton)\nDate: 8 Apr 2017; 03:37 UT\nProvenance: Jamie A. Kennea (kennea@astro.psu.edu)\nSubjects: X-ray, Neutron Star, Transient, Pulsar\nDescription: The Swift SMC Survey (S-CUBED) is a weekly shallow (60s exposure) survey consisting of 142 tiles aimed at covering the SMC to monitor SMC X-ray sources and search for transient outbursts. In S-CUBED observations taken on March 30th, 2017 at 13:00UT, in a single 60s exposure tile, a bright X-ray source was detected at the following location: RA/Dec(J2000) = 13.7355, -72.4487, which is equivalent to: \n \nRA(J2000) = 00h 54m 56.53s, \nDec(J2000) = -72d 26’ 55.4s, \n \nwith an estimated uncertainty of 4.1 arc-seconds radius (90% confidence). This position lies close to (7.6 arc-seconds) the SMC HMXB SXP 59.0. The measured count rate in the 60s Photon Counting mode exposure is 0.9 +/- 0.2 c/s. A previous observation of this field taken on March 22nd, 2017 showed a marginal detection in 60s exposure, with a count rate of 0.2 +/- 0.1 c/s, previous observations resulted in upper limits on the source brightness of typically < 0.2 c/s per observation. Therefore this is the first detected outburst of this source, detected by S-CUBED, since observations of this region began on Jun 8th, 2016. \nA 3ks Target of Opportunity observation of this source was taken by Swift starting at 14:41UT on April 7th, 2017 (there was a delay in follow-up due to observing constraints). XRT data were taken in Windowed Timing (WT) mode to improve timing accuracy and avoid pile-up. In these data we detect a bright point source, consistent with the PC mode localization. This source has brightened since the March 30th, 2017 observation, to an XRT count rate of 2.1 +/- 0.1 c/s. \nAn analysis of the timing mode data reveals the presence of pulsations at a period of 59.045s, unambiguously confirming that this source is SXP 59.0, which is entering a new bright outburst phase. \nThe spectrum can be well fit by an absorbed power-law model, with a photon index of 0.96 +/- 0.10. The fitted flux value is 8 x 10-11 erg/s/cm2 (0.5 - 10 keV), assuming an SMC distance of 61 kpc, this equates to a luminosity of 4 x 1037 erg/s (0.5 - 10 keV). \nObservations of SXP 59.0 by Swift and S-CUBED will continue.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Exoplanet", "Circumstellar disk", "Nova" ] }, "answerKey": "A" }, { "id": "atel_10320", "message": "Title: ASASSN-17fk: Discovery of A Probable Supernova in NGC 2076\nAuthors: Subo Dong (KIAA-PKU), K. Z. Stanek, C. S. Kochanek, J. S. Brown, T. W.-S. Holoien, J. Shields, T. A. Thompson (Ohio State), B. J. Shappee (Hubble Fellow, Carnegie Observatories), J. L. Prieto (Diego Portales; MAS), D. Bersier (LJMU), S. Bose, Ping Chen (KIAA-PKU), J. Brimacombe (Coral Towers Observatory)\nDate: 25 Apr 2017; 01:10 UT\nProvenance: Subo Dong (dongsubo@pku.edu.cn)\nSubjects: Optical, Supernovae\nDescription: During the ongoing All Sky Automated Survey for SuperNovae (ASAS-SN, Shappee et al. 2014), using data from the quadruple 14-cm \"Brutus\" telescope in Haleakala, Hawaii and the 14-cm \"Cassius\" telescope in Cerro Tololo, Chile, we discovered a new transient sources, most likely supernovae, in the galaxy NGC 2076. \nASASSN-17fk (AT 2017dhr) was discovered in images obtained on UT 2017-04-20.98 at V~16.4 mag. We also detected the object in images taken on 2017-04-14.99 at V~17.0 mag, and we do not detect (V>17.0) the object in images taken on UT 2017-04-12.01 and before. An image obtained on 2017-04-24.73 by Las Cumbres Observatory (LCO) 1m telescope at SAAO confirms the discovery of the transient. This figure shows the archival Pan-STARRS (Chambers et al. 2016, arXiv:1612.05560) r-band image of the host (left) and the LCO confirmation image (right). The red circle has a radius of 3\" and is centered on the position of the transient in the LCO image. \nThe position of ASASSN-17fk is close to the center (within ~10\") of the galaxy NGC 2076 (z=0.007145, d=30Mpc, via NED), giving an absolute V-band magnitude of approximately -16.2 (m-M=32.4, A_V=0.23) without taking host extinction into account, while host extinction might be important since its apparent position is near a dust lane. \n \n \n Object RA (J2000) DEC (J2000) Disc. UT Date Disc. V mag Approx. Abs. Mag Offset from Host (\") \n ASASSN-17fk 05:46:47.27 -16:47:00.30 2017-04-20.98 16.4 -16.2 10 \n \nASASSN-17fk photometry: \n \n \n Obs. UT Date V mag \n 2017-04-12.01 >17.0 \n 2017-04-14.99 17.0 \n 2017-04-20.98 16.4 \n \nFollow-up observations are encouraged. \nWhile we are participating in the TNS system to minimize potential confusion, ASAS-SN will continue using ASASSN-17xx transient names as our primary nomenclature (including supernovae, but also other classes of transients), and we encourage others to do the same. We prefer merging the names as ASASSN-17xx (AT 2017xyz) to preserve, rather than anonymize, the origin of the transient. \nWe thank Las Cumbres Observatory and its staff for their continued support of ASAS-SN. ASAS-SN is funded in part by the Gordon and Betty Moore Foundation through grant GBMF5490 to the Ohio State University, NSF grant AST-1515927, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, the Chinese Academy of Sciences South America Center for Astronomy (CASSACA), and the Mt. Cuba Astronomical Foundation. For more information about the ASAS-SN project, see the ASAS-SN Homepage and the list of all ASAS-SN transients.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Supernova", "Magnetar", "Globular cluster" ] }, "answerKey": "B" }, { "id": "atel_10380", "message": "Title: X-ray emission of SN 2017eaw and its progenitor\nAuthors: A. K. H. Kong (NTHU & Oxford), K. L. Li (Michigan State)\nDate: 15 May 2017; 20:32 UT\nProvenance: Albert Kong (akong@phys.nthu.edu.tw)\nSubjects: X-ray, Supernovae, Transient\nDescription: Referred to by ATel #: 10381, 10427\nFollowing the discovery of the Type II supernova 2017eaw in the nearby galaxy NGC 6946 (ATel #10372,#10374,#10376,#10377), we have searched for X-ray emission of the supernova and its progenitor with archival data from the Swift X-ray Telescope and the Chandra X-ray Observatory. Swift TOO observations were triggered shortly after the discovery. The first Swift observation was performed on 2017 May 14, 14:09 UT for 1.95 ks. SN 2017eaw is marginally seen in the 0.3-10 keV image. There are 7 counts in a circular region of 25 arcsec in radius centered at the SN, corresponding to 0.02 counts per pixel. With 10 counts in a source-free region covering 2025 pixels, the background is about 0.005 counts per pixel. Using a binomial distribution, the chance probability that all 7 counts or more are background is 0.2%. With 5.6+/-2.5 background subtracted counts and assuming an absorbed power-law of photon index of 2 and a Galactic N_H of 2e21 cm^-2, the 0.3-10 keV unabsorbed flux is 1.69e-13 erg/s/cm^2 corresponding to 6.1e38 erg/s (d=5.5 Mpc). \n \nThe second Swift observation was taken on 2017 May 14, 22:00 UT for 980 s. In a 25 arcsec circular region, we obtained 8.8+/-3.0 background subtracted counts. Using the above spectral model, the 0.3-10 keV luminosity is 1.9e39 erg/s. This indicates that the X-ray brightness of the SN is increasing. \n \nWe also examined archival Chandra images taken before the onset of the SN to look for X-ray emission from the progenitor (ATel #10373,#10378). Six observations were taken between 2001 and 2012 and we combined all the observations together. At the position of the SN, the effective exposure time is about 162 ks. No source is visible at the SN position. Assuming the same spectral model, we set a 3-sigma 0.3-10 keV luminosity limit of 5.4e36 erg/s.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova, Star and stellar system", "Supernova, Circumstellar disk", "Supernova, Neutron star", "Exoplanet, Star and stellar system" ] }, "answerKey": "A" }, { "id": "atel_10450", "message": "Title: Outburst behavior in Aql X-1\nAuthors: Tolga Dincer, Charles D. Bailyn, Bryndis Cruz (Yale)\nDate: 31 May 2017; 20:48 UT\nProvenance: Tolga Dincer (tolga.dincer@yale.edu)\nSubjects: Infra-Red, Optical, Neutron Star, Transient\nDescription: Referred to by ATel #: 10452, 10541\nATEL#10441 has reported on the possible start of a new outburst in Aql X-1. As part of our X-ray binary monitoring program, we perform optical and near-infrared photometric observations of Aql X-1 with the SMARTS 1.3m telescope, located at CTIO. From our last four observations the optical magnitudes are: \n \n \n MJD (UTC)\t V-mag R-mag I-mag \n \n 57888.3 (May 15)\t 19.46 18.54 17.83 \n \n 57893.3 (May 20)\t 19.26 18.48 17.64 \n \n 57901.3 (May 28)\t 18.58 17.86 16.95 \n \n 57904.2 (May 31)\t 18.15 17.49 - \n \n \nThe combined errors due to photometry and calibration are typically ~0.05 mag. The flux from the first two observation sets is dominated by the unresolved nearby star (Dipankar & Bailyn 2008, ApJ, 688, 549), but the last two observations clearly show a significant brightening in all bands. Furthermore, the Swift BAT light curve (https://swift.gsfc.nasa.gov/results/transients/AqlX-1/) of the source within the last several days (MJD 57899-57904) show hard X-ray activity significantly above the detection limit. Both results confirm the start of a new outburst in Aql X-1. Our regular monitoring observations of Aql X-1 will continue. We encourage further multiwavelength observations of Aql X-1.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Minor body", "Neutron star", "Quasar" ] }, "answerKey": "C" }, { "id": "atel_10575", "message": "Title: Correction to ATEL #10559\nAuthors: C. Rojas-Bravo, E. Xhakaj, Y.-C. Pan, C. D. Kilpatrick, R. J. Foley (UCSC)\nDate: 15 Jul 2017; 03:45 UT\nProvenance: Yen-Chen Pan (ypan6@ucsc.edu)\nSubjects: Optical, Supernovae\nDescription: In ATEL #10559 we report a wrong target name and coordinates in the table. The AT2017fbv (=Gaia17bqy), which was classified as a IIn/Ibn, should read AT2017fav (=ATLAS17hrf). We thank Andrea Pastorello for pointing this out, and we apologize for any inconvenience caused by this error.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Repeater", "Magnetar", "Interstellar medium" ] }, "answerKey": "A" }, { "id": "atel_10710", "message": "Title: ASAS-SN Discovery of a Bright Be Star Undergoing a Possible Outburst\nAuthors: T. Jayasinghe, K. Z. Stanek, C. S. Kochanek (OSU), J. Thorstensen (Dartmouth), J. Rupert (MDM Observatory), J. L. Prieto (Diego Portales; MAS), J. V. Shields, T. A. Thompson (OSU), T. W.-S. Holoien, B. J. Shappee (Carnegie Observatories), Subo Dong (KIAA-PKU)\nDate: 5 Sep 2017; 17:31 UT\nProvenance: Krzysztof Stanek (stanek.32@osu.edu)\nSubjects: Optical, Variables\nDescription: Referred to by ATel #: 10713, 10740\nAs part of an ongoing effort by ASAS-SN project (Shappee et al. 2014; Kochanek et al. 2017) to characterize and catalog all bright variable stars (e.g., Jayasinghe et al. 2017, ATel #10634, #10677), we report the discovery of a bright Be star undergoing a possible outburst.\nThe source ASASSN-V J010932.93+614659.0 (position from Gaia, g~12.1, parallax=0.60 +/- 0.33 mas) is a Tycho2 source that was previously classified as a K02 subgiant using a best-fit synthetic spectrum (Pickles & Depagne 2010). The ASAS-SN light curve shows a current brightening event (~0.3 mag) over a period of >320 days. A low resolution spectrum of ASASSN-V J010932.93+614659.0 was obtained with the MDM 2.4m telescope + OSMOS spectrometer(range 3960-6850 Angstroms; FWHM res. 4 Angstroms) on the 30th of August 2017. The spectrum shows Balmer and He I lines in absorption and strong narrow H-alpha in emission, characteristic of a Be-type star.\nWe thank Las Cumbres Observatory and its staff for their continued support of ASAS-SN. ASAS-SN is funded in part by the Gordon and Betty Moore Foundation through grant GBMF5490 to the Ohio State University, NSF grant AST-1515927, the Mt. Cuba Astronomical Foundation, the Center for Cosmology and AstroParticle Physics (CCAPP) at OSU, and the Chinese Academy of Sciences South America Center for Astronomy (CASSACA).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Pulsar", "Globular cluster", "Variable star", "Magnetar" ] }, "answerKey": "C" }, { "id": "atel_10825", "message": "Title: NuSTAR Observation of GX 339-4 in the early stages of its 2017 outburst\nAuthors: J. A. Garcia (Caltech), F. Harrison (Caltech), J. Tomsick (Berkeley), K. Foster (Caltech), F. Fuerst (ESAC), D. Walton (Cambridge), Y. Xu (Caltech), J. Steiner (MIT), J. McClintock (SAO), J. Wilms (Remeis), T. Dauser (Remeis), T. Maccarone (TTU), T. Dincer (Yale), C. Bailyn (Yale), N. Sridhar (IISER-B), J. Wang (Fudan)\nDate: 5 Oct 2017; 22:06 UT\nProvenance: Javier Garcia (javier@caltech.edu)\nSubjects: X-ray, Binary, Black Hole\nDescription: Referred to by ATel #: 11208, 12322, 15615\nGX 339-4 is a transient binary black hole system with recurrent outbursts every 2-3 years, with the last full outburst observed during 2014-2016. A new outburst has been reported after a brightening observed in the optical on September 2017 (ATel #10797), as well as detections in X-rays with Swift (ATel #10798), and in radio with ATCA (ATel # 10808). We have triggered the first of a series of ToO observations from our GO program with the Nuclear Spectroscopic Telescope Array (NuSTAR; Harrison et al. 2013, ApJ, 770, 103). \nNuSTAR observed GX 339-4 on 2017 October 2 03:40:06 UT with an exposure time of ~23.2 ks. Both Focal Point Modules A and B (FPMA/FPMB) detected the source at approximately 2 counts per second, and a flux of ~2.6 mCrab (~8.e-11 ergs/cm^2/s; 2-10 keV). The source counts consistently dominate the background counts over the entire band (3-79 keV). This is the lowest flux observed by NuSTAR for this source, including the latest observations during the decay of the 2015 outburst. \nThe spectra were fitted with a Comptonization model (nthComp) including Galactic absorption (TBabs) with a column density fixed at N_H=5.e21 cm^-2. A hard power-law continuum is detected with Gamma=1.62+/-0.01. No cutoff at high energies can be detected. The residuals show weak emission feature near 6.4 keV, consistent with Fe K reflection from the accretion disk. However, no Fe K-edge or Compton hump signatures can be detected. We fitted the emission with a Gaussian profile finding the centroid at E=6.43(+0.08,-0.06) keV, with a poorly constrained width of sigma=0.13+/-0.13 keV. We measured the equivalent width of the Fe K line to be EW=91(+2,-1) eV, which is remarkably consistent with a previous Suzaku measurement at a similar flux level (Tomsick et al. 2009, ApJL, 707, 87). \nAdditional NuSTAR observations will be triggered later in the outburst in order to track the evolution of the Fe K emission and other disk reflection features during the rise of the system in its hard state. We thank the NuSTAR team for the prompt scheduling of this observation.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system, Black hole", "Binary system, Near-Earth object", "Binary system, Star and stellar system", "Binary system, Supernova" ] }, "answerKey": "A" }, { "id": "atel_10890", "message": "Title: Subaru/FOCAS Optical Spectroscopy for a possible IceCube-170922A counterpart TXS 0506+056\nAuthors: Tomoki Morokuma (The University of Tokyo), Yasuyuki T. Tanaka (Hiroshima University), Kouji Ohta (Kyoto University), Yoshiki Matsuoka, Takuji Yamashita, Nanako Kato (Ehime University)\nDate: 25 Oct 2017; 04:36 UT\nProvenance: Tomoki Morokuma (tmorokuma@ioa.s.u-tokyo.ac.jp)\nSubjects: Optical, Neutrinos, Blazar\nDescription: We performed optical spectroscopic observations on September 30 and October 1, 2017 (UT) with the 8.2-m Subaru telescope and Faint Object Camera and Spectrograph (FOCAS) for TXS 0506+056 which is a possible counterpart to the IceCube-170922A high-energy neutrino event (Tanaka et al. 2017, ATel #10791). The wavelength ranges covered are 4700-8200A (1.34 angstroms per pixel) and 7500-10500A (0.74 angstroms per pixel), and the obtained spectral resolutions are R~400 and 1200, respectively. The signal-to-noise ratios are roughly 100 per pixel. As reported by Steele (2017, ATel #10799), van Soelen et al. (2017, ATel #10830), Coleiro & Chaty (2017, ATel #10840), we do not find any other significant absorption or emission lines than the atmospheric and Galactic lines.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object, Active galactic nucleus", "Repeater, Active galactic nucleus", "Accreting object, Repeater", "Accreting object, Pulsar" ] }, "answerKey": "A" }, { "id": "atel_11000", "message": "Title: NIR brightening of the high redshift the blazar BZQJ0348-2749\nAuthors: L. Carrasco, G. Escobedo, E. Recillas, A. Porras, V. Chavushyan, D. Y. Mayya (INAOE, Mexico)\nDate: 23 Nov 2017; 20:03 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Infra-Red, Optical, Gamma Ray, AGN, Blazar, Quasar, Transient\nDescription: We report on the NIR brightening of the high redshift QSO BZQJ0348-2749 (z=0.991). On November 14th, 2017 MJD(24578071.8911), we found the source with NIR fluxes J =14.650 +/- 0.03, H = 13.940 +/- 0.02 and Ks = 12.843 +/- 0.08 While, on MJD 2456650.75 the flux in the H band corresponded to H = 15.530 +/- 0.05. Hence, the source has increased its flux by a factor of 4.3 in this lapse. The source is brightest since the time we started monitoring it (MJD 2455459.97), when the flux in the H band was H = 15.393 +/- 0.15 Our observations are carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We encourage further multi wavelength coverage.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system", "Black hole", "Near-Earth object", "Variable star" ] }, "answerKey": "B" }, { "id": "atel_11050", "message": "Title: DAO Spectroscopic classification of SN 2017iuu = ATLAS17nnf \nAuthors: D. D. Balam, Dominion Astrophysical Observatory, National Research Council of Canada, K. Thanjavur (University of Victoria), E. Hsiao ( Florida State University) and M. L. Graham (University of Washington)\nDate: 11 Dec 2017; 21:20 UT\nProvenance: David D. Balam (cosmos@uvic.ca)\nSubjects: Supernovae\nDescription: D. D. Balam, Dominion Astrophysical Observatory, National Research Council of Canada, K. Thanjavur (University of Victoria), E. Hsiao, Florida State University and M. L. Graham (University of Washington) report that a spectrogram (range 390-710 nm, resolution 0.3 nm) of 2017iuu = ATLAS17nnf (J. Tonry, B. Stalder, L. Denneau, A. Heinze, H. Weiland (IfA, University of Hawaii), A. Rest (STScI), K.W. Smith, S. J. Smartt, M. Fulton, O. McBrien (Queen's University Belfast), obtained on Dec. 11.33 UT with the 1.82-m Plaskett Telescope of the National Research Council of Canada, shows it to be a normal type Ia supernova near maximum light. Cross-correlation with a library of supernova spectra using the \"Supernova Identification\" code (Blondin and Tonry 2007, Ap.J. 666,1024) suggests that 2017iuu is most similar to the normal type-Ia supernova 1994ae at 3 days past maximum light. There are several possible host galaxies with no published redshifts. Our solution yields a redshift of 0.043 for this object.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Circumstellar disk", "Variable star", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_11130", "message": "Title: Recurrent nova M31N 2008-12a: Swift/XRT detection of the 2017 eruption\nAuthors: M. Henze (SDSU), M. J. Darnley (LJMU), A. W. Shafter (SDSU), S. Kafka (AAVSO), M. Kato (Keio University), S. C. Williams (Lancaster), for a larger collaboration\nDate: 5 Jan 2018; 19:18 UT\nProvenance: Martin Henze (henze@ice.cat)\nSubjects: Ultra-Violet, X-ray, Nova, Transient\nDescription: Referred to by ATel #: 11133, 11149, 11214, 12207\nIn ATel #11116 we announced the discovery of the predicted 2017 eruption of the recurrent nova M31N 2008-12a on 2017-12-31.77 UT. We reported the follow-up UV detection with Swift/UVOT in ATel #11121. This is the 10th observed eruption in 10 consecutive years of this unique nova system (cf. ATels #5607, #6527, #7964, #9848). Comprehensive multi-wavelength studies of previous eruptions were published by Darnley et al. (2014, 2015, 2016) and Henze et al. (2014, 2015a, 2015b, 2018 subm.). For additional optical photometry and spectroscopy of the ongoing eruption see ATels #11116, #11117, #11118, #11124, #11125, #11126. \nHere we report the start of the supersoft X-ray source (SSS) phase of M31N 2008-12a. A faint X-ray counterpart was detected in a 5.2-ks Swift observation starting on 2018-01-05.48 UT. We measured the preliminary XRT count rate to be (3.1±1.0) × 10-3 ct/s (corrected for vignetting, dead time and PSF). No X-ray source was detected in the preceding 1.2-ks Swift observation on 2018-01-04.48 UT with an 3σ upper limit of 6.0 × 10-3 ct/s. \nIf we assume an eruption date of 2017-12-31.77 UT (MJD 58118.77), identical to the discovery date (ATel #11116), then the SSS counterpart appeared around day 4.7 after eruption. This preliminary estimate is somewhat earlier than the 5.9±0.5 days measured in 2014 (ATel #6558, Henze et al. 2015), the 5.7±0.5 days seen in 2015 (ATel #7984, Darnley & Henze et al. 2016), and the 5.8 days observed for the peculiar 2016 eruption (ATel #9872). This might suggest an earlier eruption date, which we are currently working on constraining more accurately. \nIn addition, the nova is still detected as an UV source but its magnitude has declined significantly to uvw2 = 19.3±0.1 mag (cf. ATel #11121). Our preliminary magnitudes use the UVOT photometric system (Poole et al. 2008, Breeveld et al. 2011) and have not been corrected for extinction. \nWe wish to thank the Swift Team for the rapid scheduling of the observations, in particular B. Cenko, the duty scientists, and the science planners.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Near-Earth object", "Quasar", "Repeater" ] }, "answerKey": "A" }, { "id": "atel_11220", "message": "Title: X-ray and UV observations of Nova Mus 2018 with Swift\nAuthors: Thomas Nelson (U. Pittsburgh), Koji Mukai (NASA/GSFC & UMBC), Laura Chomiuk, Kwan-Kok Li, Adam Kawash (MSU), J. L. Sokoloski (Columbia), Michael Rupen (Herzberg Astrophysics), Justin Linford (GWU), Amy Mioduszewski (NRAO)\nDate: 24 Jan 2018; 15:43 UT\nProvenance: Thomas Nelson (tjnelson@pitt.edu)\nSubjects: Ultra-Violet, X-ray, Nova\nDescription: Referred to by ATel #: 11298, 11377\nWe observed Nova Mus 2018 (PNV J11261220-6531086) with the Neil Gehrels Swift Observatory on 2018 January 21, 18 days after the initial rapid rise to V=8.8 on 2018 January 3.24 (see link below for more details). Due to the optical brightness of the nova, the XRT instrument was operated in Windowed Timing mode. The net exposure time was 1465s, during which the nova was not detected. The 3-sigma upper limit on the 0.3-10 keV count rate is 0.025 cts/s. \n \nA UV image of the nova was also obtained with the UVOT instrument in the UVM2 filter (central wavelength 224.6nm). Nova Mus 2018 is saturated in the 659s exposure, indicating m_uvm2 < 10.42 mags. \n \nAdditional Swift monitoring of this nova will take place with weekly cadence over the next two months.\nCBAT page for Nova Mus 2018", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Supernova", "Nova", "Variable star" ] }, "answerKey": "C" }, { "id": "atel_11310", "message": "Title: Swift J1658.2-4242: Swift BAT and XRT refined analysis\nAuthors: A. Y. Lien (GSFC/UMBC), J. A. Kennea (PSU), S. D. Barthelmy (GSFC), A. P. Beardmore (U. Leicester), P. A. Evans (U Leicester), H. A. Krimm (NSF/USRA), D. Malesani (DARK/NBI), C. B. Markwardt (GSFC), D. M. Palmer (LANL), K. L. Page (U Leicester), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL)\nDate: 16 Feb 2018; 19:10 UT\nProvenance: Amy Lien (amy.y.lien@nasa.gov)\nSubjects: X-ray, Gamma Ray, Transient\nDescription: Referred to by ATel #: 11311, 11318, 11321, 11322, 11334, 11336, 11358, 11375\nUsing the data set from the recent telemetry downlink, we report further analysis of the new Galactic transient, Swift J1658.2-4242 (trigger #810300) (Barthelmy et al., GCN Circ. 22416). \n \nUsing the BAT data from T+210 to T+963 sec, the BAT ground-calculated position is RA, Dec = 254.537, -42.712 deg which is \nRA(J2000) = 16h 58m 08.8s \nDec(J2000) = -42d 42' 42.1\" \nwith an uncertainty of 3.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 78%. \n \nThe BAT mask-weighted light curve shows a continuous weak emission that starts before and ends after the event data range from T+210 s to T+963 s. Data from the BAT transient monitor (Krimm et al. 2013) show the source starts flaring around Feb. 14, 2018, and has reached a brightness of ~ 70 mCrab (15-50 keV). This is generally consistent with the detections reported by INTEGRAL (Grebenev et al., ATEL 11306). \n \nThe BAT time-averaged spectrum from T+210.00 to T+963.02 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.98 +- 0.28. The fluence in the 15-150 keV band is 2.2 +- 0.4 x 10-6 erg/cm2. All the quoted errors are at the 90% confidence level. \n \nSwift/XRT began observation of the transient at 06:54 UT and observed the target in a mixture of Windowed Timing and Photon Counting mode for a total of 3.1 ks. In XRT data we localize the transient, utilizing UVOT to reduce the systematics on astrometry, to the following coordinates: RA/Dec(J2000) = 254.55266, -42.69845, which is equivalent to: \n \nRA(J2000) = 16h 58m 12.64s, \nDec(J2000) = -42d 41m 54.4s, \n \nwith an estimated uncertainty of 1.6 arc-seconds radius (90% confidence). We note that this position lies 0.4 arc-seconds from the IR source VVV J165812.62-424154.78, from the VISTA Variables DR2 catalog (Minniti et al., 2017), which has magnitudes H=16.2 and K=15.252. In addition G343.2514+00.0537, a source in the GLIMPSE catalog, is also consistent with the XRT localization. \n \nSpectral fits to the PC and WT data are consistent, although as WT data are unaffected by pile-up we report that fit here. The spectrum is well fit by a highly absorbed power-law model, with NH = 1.9 +/- 0.5 1023 cm-2, and photon index = 1.7 +/- 0.5. The average flux, corrected for absorption, is ~1.6 x 10-9 erg/s/cm2 (0.3 - 10 keV). The light-curve shows some evidence of fading during the observed period, although planned later observations of the new transient will be required to determine any fading. \n \nWe find no evidence of pulsations or QPOs in the XRT data, although as the data are mainly taken in PC mode and suffer from pile-up, this does not place strong constraints on the presence of any periodicities in the data. \n \nThe results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/810300/BA/ \n \nThe results of the BAT transient monitor are available at https://swift.gsfc.nasa.gov/results/transients/weak/SwiftJ1658.2-4242/", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Pulsar", "Exoplanet", "Accreting object", "Quasar" ] }, "answerKey": "C" }, { "id": "atel_11375", "message": "Title: Swift J1658.2-4242 as observed by AstroSat LAXPC\nAuthors: Aru Beri (U. Southampton), Tomaso Belloni (INAF-OAB), Federico Vincentelli (INAF-OAB and U. Insubria), Poshak Gandhi, Diego Altamirano (U. Southampton)\nDate: 1 Mar 2018; 21:43 UT\nProvenance: Poshak Gandhi (p.gandhi@soton.ac.uk)\nSubjects: X-ray, Black Hole, Neutron Star, Transient\nDescription: Referred to by ATel #: 12072\nWe report on preliminary analysis of an AstroSat observation of the newly discovered X-ray transient, Swift J1658.2-4242 [J1658] (GCN #22416, #22417, #22419; ATel #11306, #11307, #11310, #11311, #11318, #11321, #11336). The observation of J1658 was performed between 2018-02-20 18:21:45 UT and 2018-02-21 04:25:38 UT, covering 7 satellite orbits, for a total of 20 ks exposure. We analyzed the data from the LAXPC instrument, covering the energy range 3-80 keV (Antia et al. 2017 ApJS 231 10). \n \nPower density spectra show the presence of band-limited noise plus a strong (rms of ~16%) and sharp Quasi-Periodic Oscillation (QPO), whose centroid frequency increased with time from ~1.6 to 2 Hz. The total 0.1-20 Hz fractional rms is ~34% over 3-80 keV. The presence of such a QPO indicates that the source was in the hard intermediate state during these observations. The power density spectrum combined from all three LAXPC cameras is shown at the link below. \n \nSpectral fitting was performed over the energy range of 4-60 keV for the cameras LAXPC10 and 20, with LAXPC30 excluded due to a suspected gas leak leading to loss of efficiency. The continuum spectra can be approximately described by an absorbed disk blackbody and cutoff power law. A systematic error of 4% was included while performing spectral fitting. We obtained an N(H) = 1.6(+/-0.2)x10^{23} cm^{-2} (consistent with a NuSTAR observation carried out ~4 days prior to ours; ATel #11321), an inner disk temperature of 1.4+/-0.1 keV, a power law photon index of 1.76+/-0.06 and a high-energy cutoff of 46+/-3 keV. We obtained a reduced Chi^2 = 0.82 for 292 degrees of freedom. All uncertainties are stated at a 1-sigma confidence level. The 3-80 keV unabsorbed flux was 3.6x10^{-9} ergs cm^{-2} s^{-1}, corresponding to a luminosity of 3x10^{37} ergs s^{-1} at 8 kpc. The power law to disk flux ratio is ~8 over 3-80 keV. Analysis of the other AstroSat instruments is underway. \n \nAcknowledgment: The authors would like to thank all the AstroSat operations team members for scheduling the ToO observation, and for prompt provision of the data. \nClick here for AstroSat/LAXPC Power Spectrum", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Neutron star", "Black hole, Supernova", "Black hole, Variable star", "Black hole, Interstellar medium" ] }, "answerKey": "A" }, { "id": "atel_11475", "message": "Title: Spectroscopic Confirmation of TCP J07134590-2112330 as a Galactic Classical Nova in Canis Major \nAuthors: Jay Strader, Laura Chomiuk, Arash Bahramian, Sam Swihart (Michigan State)\nDate: 25 Mar 2018; 04:21 UT\nProvenance: Laura Chomiuk (chomiuk@pa.msu.edu)\nSubjects: Optical, Nova, Transient\nDescription: TCP J07134590-2112330 was discovered by Yuji Nakamura on 2018 March 24.5 UT as a 12 mag optical transient. We obtained spectroscopic observations of TCP J07134590-2112330 with the Goodman spectrograph on the 4-m SOAR telescope on 2018 Mar 25.1 UT, with a low-resolution spectrum (R~1200) covering 3850--7850 A. The spectrum indicates that TCP J07134590-2112330 is a young classical nova, with strong hydrogen Balmer emission lines and additional strong lines of [O I] and Fe II. The Balmer lines show P Cygni profiles; the FWHM of the H alpha emission component is 1250 km/s, and the absorption trough extends to -2000 km/s. Astrometry of the acquisition image implies that this transient is identical to a source in the Pan-STARRS1 catalog with g=21.5 and r=21.2. The Pan-STARRS1 J2000 position of TCP J07134590-2112330 is RA = 07h13m45.843s , Dec = -21d12'31.28\", with a catalog uncertainty of about 25 mas per coordinate.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Galaxy, Star and stellar system", "Nova, Star and stellar system", "Nova, Variable star", "Stellar evolution, Star and stellar system" ] }, "answerKey": "B" }, { "id": "atel_11580", "message": "Title: Swift detections of the flaring blazar GAIA 18ayp (PKS 2333-415) in X-rays and the UV\nAuthors: Dirk Grupe (Morehead State University), S. Komossa (MPIfR), R. Angioni (MPIfR, Univ. Wuerzburg), N. Schartel (ESA - ESAC)\nDate: 26 Apr 2018; 22:14 UT\nProvenance: Dirk Grupe (dgrupe007@gmail.com)\nSubjects: Ultra-Violet, X-ray, Gamma Ray, AGN, Blazar\nDescription: We report Swift observations of the z=1.41 QSO GAIA 18ayp (PKS 2333-415) which was detected by GAIA in an optically flaring state on 2018-April-14. Swift observed GAIA 18ayp on 2018 April 23 for a total of 1.4 ks. The QSO is clearly detected in X-rays and the UV. The X-ray position found using the enhanced XRT position (Goad et al. 2007, Evans et al. 2009) is RA-2000 = 23 36 34.1, Dec-2000 = -41 15 21.4 with an uncertainty of 3.0\". This position coincides with the z=1.41 blazar PKS 2333-415. The X-ray spectrum in the observed 0.3-10 keV band can be fitted with an absorbed power law model with the absorption column density fixed to the Galactic value (1.71e20 cm^-2). The X-ray photon index is Gamma = 1.65+/-0.43. The flux in the observed 0.3-10 keV band is (1.2+/-0.2)e-15 W m^-2. In the UVOT, the QSO was observed in the W1 and M2 filters with 17.65+/-0.10 and 18.27+/-0.07 mag in the Vega system, respectively (not corrected for Galactic extinction). In the 0.1-300 GeV gamma-ray band, the blazar is associated to the Fermi-LAT catalog source 3FGL J2336.5-4116 (Acero et al. 2015, ApJS, 218, 23). No significant gamma-ray emission positionally consistent with this source was detected by the LAT on the time scales corresponding to the optical and X-ray observations reported above, showing that there is no gamma-ray flaring activity corresponding to the multi-wavelength variability. We derive an upper limit on the gamma-ray flux (E>100 MeV) in the time period 14-23 April 2018 of 8.0 x 10^-8 photons cm^-2 s^-1.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Variable star", "Active galactic nucleus, Binary system", "Accreting object, Variable star", "Quasar, Variable star" ] }, "answerKey": "A" }, { "id": "atel_11650", "message": "Title: MASTER-Tavrida: FSRQ optical flare\nAuthors: T. Pogrosheva, V. Lipunov, V. Kornilov, E. Gorbovskoy (Lomonosov MSU, Physics Department, SAI)\nDate: 17 May 2018; 16:13 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Request for Observations, AGN, Blazar, Quasar, Transient\nDescription: MASTER OT J113627.31+340738.9 detection - flat-spectrum radio quasar optical flare, ampl>1.5m \n \nMASTER-Tavrida auto-detection system ( Lipunov et al., \"MASTER Global Robotic Net\", Advances in Astronomy, 2010, 30L ) \ndiscovered OT source at (RA, Dec) = 11h 36m 27.31s +34d 07m 38.9s on 2018-05-16.87374 UT. \nThe OT unfiltered magnitude is 18.5m (limit 19.7m). \nThe OT is seen in 4 images. There is no minor planet at this place. \nWe have reference image without OT on 2017-04-16.94588 UT with unfiltered magnitude limit 20.0m, on 2018-04-12 19:04:50UT with mlim=19.8m. \nSpectral observations are required. \nThe discovery and reference images are available at: \nhttp://master.sai.msu.ru/static/OT/MASTEROTJ113627.31+340738.9.png \nList of Optical Transients discovered by MASTER\nMASTER Global Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Stellar evolution", "Repeater", "Circumstellar disk" ] }, "answerKey": "A" }, { "id": "atel_11750", "message": "Title: Optical follow-up observation of AT2018cow/ATLAS18qqn\nAuthors: Myungshin Im (SNU), Gu Lim (SNU), Jinguk Seo (SNU), Gregory S. Paek (SNU), Hwara Kim (SNU), Joonho Kim (SNU), Changsu Choi (SNU), Hyun-Il Sung (KASI), on behalf of a larger collaboration\nDate: 21 Jun 2018; 13:11 UT\nProvenance: Myungshin Im (myungshin.im@gmail.com)\nSubjects: Optical, Cataclysmic Variable, Gamma-Ray Burst, Supernovae, Transient\nDescription: Referred to by ATel #: 11753, 11757, 11758, 11772\nAt 2018-06-20 UT, we observed the transient, AT2018cow/ATLAS18qqn (Smartt et al. ATel #11727) using various telescopes including the SNU Astronomical Observatory (SAO) 1m telescope, the LOAO 1m telescope, the McDonald 0.8 m telescope, and the Lee Sang Gak Telescope (LSGT) at SSO. A series of BVRI and griz data were obtained. From the SAO 1m telescope image taken at 2018-06-20 12:34:26 UT, we find the following magnitudes (host light is not subtracted) for the object. The magnitudes are in Vega system, and calibrated against APASS stars in the vicinity. V = 14.21 +- 0.02, R = 14.29 +- 0.03. The observation of this object is continuing. We thank the operators of the LOAO 1m telescope, Jae-Hyuk Yoon and In-Kyung Baek for their assistance with the observation.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova, Exoplanet", "Nova, Black hole", "Nova, Supernova", "Minor body, Supernova" ] }, "answerKey": "C" }, { "id": "atel_11800", "message": "Title: A flare of the H2O maser IRAS 16293-2422\nAuthors: Nuriya Ashimbaeva, Evgeny Lekht, Mikhail Pashchenko, Georgij Rudnitskij (Moscow State University, Sternberg Astronomical Institute), Alexandr Tolmachev (Pushchino Radio Astronomy Observatory)\nDate: 30 Jun 2018; 17:35 UT\nProvenance: Georgij Rudnitskij (gmr@sai.msu.ru)\nSubjects: Radio, Request for Observations, Young Stellar Object\nDescription: We report a new flare of the source of maser radio emission in the H2O line at 22.235 GHz IRAS 16293-2422. The source is associated with a young stellar system at a distance of about 140 pc (S.A. Dzib et al. 2018, A&A 614, A20). Observations were carried out at the 22-meter radio telescope in Pushchino, Russia. The spectrum contains a strong single peak at VLSR=1.6-1.7 km/s. During June 2018 its flux density doubled. The history of its flux density variations in 2018 is: Feb 27 - 230 Jy; Mar 13 - 271 Jy; Apr 24 - 2405 Jy; May 31 - 4723 Jy; Jun 25 - 9043 Jy; Jun 27 - 8878 Jy. The PDF graphs of the line profile can be downloaded from the indicated link. The source strongly flared several times since 1999, when we began to monitor it. Previous results (together with its OH observations) were reported by P. Colom et al. 2016, Astron. Reports 60, 730.\nPDF graphs of the H2O line profile", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Supernova", "Variable star", "Star and stellar system" ] }, "answerKey": "D" }, { "id": "atel_11900", "message": "Title: VLBI Detection and Astrometry for AT2018cow\nAuthors: M. Bietenholz (York U., Canada, & HartRAO/SARAO, South Africa), R. Margutti (NWU, USA), K. Alexander (CfA, USA), M. Argo (U. Central Lancashire, UK), N. Bartel (York U., Canada), D. Coppejans (NWU, USA), M. Drout (Carnegie, USA), T. Eftekhari (CfA, USA), C. Guidorzi (U. Ferrara, Italy), D. Milisavljevic (Purdue U., USA), G. Terreran, (NWU, USA)\nDate: 31 Jul 2018; 14:58 UT\nProvenance: Michael Bietenholz (mbieten@yorku.ca)\nSubjects: Radio, Supernovae, Transient\nDescription: Referred to by ATel #: 12067\nWe obtained 22-GHz VLBI observations of AT2018cow with the NRAO VLBA and Effelsberg telescopes. The midpoint of the observations was 2018 July 8.1 UT. We detect the source with a total flux density of ~5 mJy. We obtain a preliminary position of RA = 16h 16m 00.2242s, dec = 22d 16' 04.890\" with an estimated uncertainty of 60 micro-arcsec. Our position is more accurate than the previously reported one from e-MERLIN (Atel #11819) but only 3.2 milliarcsecond different, and therefore consistent within the estimated uncertainties. The position is based that of the phase-reference source, JVAS J1619+2247.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Accreting object", "Binary system", "Exoplanet" ] }, "answerKey": "A" }, { "id": "atel_11975", "message": "Title: Swift follow-up of a bright optical outburst from SS 433 \nAuthors: I. Khabibullin (MPA, IKI RAS), A. Semena, P. Medvedev, I. Mereminskiy (IKI RAS)\nDate: 21 Aug 2018; 16:00 UT\nProvenance: Ilya Mereminskiy (i.a.mereminskiy@gmail.com)\nSubjects: X-ray\nDescription: Referred to by ATel #: 11989\nWe present results of the Swift observation of SS 433 performed in follow-up of a bright optical outburst reported in ATel#11870. \nThe observation started at 2018-07-25 07:19:01T (MJD=58324.30567, ObsID 00035190036), i.e. 7.534d after the outburst. The observation consisted of two segments separated by 0.397d (34.3ks). Total exposure time with the Swift/XRT for two segments equals 1030.5s collected in Photon Counting mode, 353.5s for the first segment and 677s for the second one. The UVOT accumulated image in U-filter during the single exposure with 350s duration started 87s after the beginning of the first XRT segment. \nThe light curve and spectra were extracted from the 50'' circular aperture, the background was extracted from the annulus surrounding the source with 96'' inner radius and 480'' outer radius. Data reduction and processing have been performed using the standard Swift routines (XRTDAS) and XSELECT tool of the heasoft package (v6.24) and most recent calibration data. \nThe source has been detected in 0.3-10 keV band by XRT and in U band by UVOT with the mean background-corrected count rates 0.48±0.02 cts/s and 3.01±0.16 cts/s, respectively. The latter corresponds to the flux density Fλ=4.8±0.24 erg/s/cm2 /Å=180±1 µJy (17.51 Vega magnitude) in the U band, consistent with previous Swift observations of Dolan et al. 2007 and ATel#6364. \nThe 0.5-10 keV light curve shows significant variation between the two segments, with the first one being on average a factor of 1.5 brighter then the second one. There is no significant variation in relative contributions of narrower bands, which indicates absence of strong variation in the absorbing column density or relative contribution of the jets and the hard (cold reflection) component (see Khabibullin et al. 2016). The only exception might be a significant increase in [6-10] keV count rate during the second segment of the observation. This conclusion is confirmed by analysis of the spectra extracted from the full observation and individual segments. \nWe fit the spectra with with a model consisting of bremsstrahlung continuum and line emission from the pair of baryonic relativistic jets (as described in Medvedev et al. 2018). The spectral shape of all three datasets appeared to be consistent with the latest XMM-Newton observation, but with the overall normalization 0.23±0.03, NH=1.25±0.15×1022 cm-2, and redshift of the blue jet zb=-0.034±0.026 (redshift of the other jet is not constrained). This is consistent with the expectation for the SS 433's precession phase at the moment of the observation (0.22). \nImportantly, fitting of the spectrum with simpler models (e.g. absorbed powerlaw or bremsstrahlung) results in significantly lower values of NH because of the dominant contribution of jets spectral line emission below 2 keV. The bremsstrahlung continuum has temperature 30 keV and unabsorbed 0.5-10 keV flux 4.0×10-11 erg/s/cm-2. The jets line emission gives unabsorbed 0.5-10 keV flux at level 2.6×10-11 erg/s/cm-2 (1.8×10-11 erg/s/cm-2 below 2 keV). \nThe detected X-ray emission corresponds to the class of SS 433's low X-ray states, which are 3-5 times dimmer then the more common normal out-of-eclipse states (Marshall et al. 2013). This is illustrated by comparison of the current observation with Chandra/HETGS data of another low-state spectrum (ObsID 1020). The latter indeed has similar overall intensity, however, with a slight excess at low energies. \nNoteworthy, according to the RATAN-600 radio light curve, SS 433 experienced another bright radio outburst at the moment of the X-ray observation reported here. \nWe are grateful for Swift team for rapid scheduling of our observations. \nData products and supplementary materials", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system", "Repeater", "Near-Earth object", "Star and stellar system" ] }, "answerKey": "A" }, { "id": "atel_12060", "message": "Title: Discovery of FRB 180923 at the Parkes Radio Telescope\nAuthors: S. Bhandari (CSIRO/ATNF), M. Caleb (University of Manchester, UoM), E. F. Keane (Square Kilometre Array), A. Jameson (Swinburne University of Technology, SUT), B. W. Stappers (UoM), W. Farah (SUT), M. Bailes (SUT), E. D. Barr (Max Planck Institut fuer Radioastronomie, MPIfR), N. D. R. Bhat (Curtin University), M. Burgay (INAF), R. P. Eatough (MPIfR), C. Flynn (SUT), J. Green (CSIRO), F. Jankowski (UoM), S. Johnston (CSIRO), M. Kramer (MPIfR), L. Levin (UoM), V. Morello (UoM), C. Ng (University of British Columbia), E. Petroff (ASTRON), A. Possenti (INAF), N. Primak (Auckland University of Technology, AUT), W. van Straten (AUT), C. Tiburzi (Universitaet Bielefeld), V. Venkatraman Krishnan (MPIfR)\nDate: 25 Sep 2018; 10:18 UT\nProvenance: Evan Keane (ekean@jb.man.ac.uk)\nSubjects: Radio, Neutron Star, Fast Radio Burst\nDescription: The SUPERB project (Keane et al. 2018, MNRAS, 473, 116) detected a fast radio burst (FRB) on UTC 2018-09-23-04:03:38.06 with the Parkes radio telescope at 1.4 GHz. The FRB was detected in beam 01 of the 21-cm multi-beam receiver (Staveley-Smith et al. 1996, PASA, 13, 243) centred at RA: 15:10:55.4 and DEC: -14:06:10.2 with a positional uncertainty of approximately 14 arcminutes (FWHM of the Parkes beam). It is not detected in any other beam. The burst had a signal-to-noise ratio (S/N) = 13 and a dispersion measure (DM) of 548(3) pc/cc which is a factor ~12 larger than the maximum dispersion measure of the Milky Way along this line of sight, 46.6 pc/cc according to the NE2001 electron density model (Cordes and Lazio 2002, astro-ph/0207156), 39.0 pc/cc according to the YMW16 electron density model (Yao et al 2017 ApJ, 835, 29). This translates to a maximum inferred redshift of z ~ 0.5 if the FRB lies along an average line of sight through the Universe (Ioka 2003 ApJ, 598, 79; Inoue 2004, MNRAS, 348, 999). \nFRB180923 is 20(1) ms wide and had a measured fluence and energy of 2.9(3) Jy ms and ~4.5E32 J respectively. The pulse shows a frequency-dependent scattering tail with a scattering time of 16(2) ms at 1.4 GHz. There are no pulsars reported in the ATNF pulsar catalog within 7 degrees of the burst position. \nThe event occurred at a time of heightened radio frequency interference (RFI) and, as such, we had to perform a longer than usual verification analysis, in turn delaying the release of this alert with respect to our usual targets. In this case the detection S/N was in fact 14, higher than the optimised S/N once RFI had been excised. Immediately following the detection we performed a calibration observation and continued to monitor the field to search for any possible repetition. No repetition has been observed. The linear polarization did not exceed the S/N threshold of 3 and no rotation measure could be recovered. We encourage follow-up with other available facilities at different wavelengths and observing windows.\nTwo plots of the burst can be found at the link below. \nPlots of FRB 180923", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Circumstellar disk", "Repeater", "Binary system", "Neutron star" ] }, "answerKey": "D" }, { "id": "atel_12125", "message": "Title: Erratum of ATEL #12123\nAuthors: M. Cardillo (INAF/IAPS)\nDate: 18 Oct 2018; 10:00 UT\nProvenance: MARTINA CARDILLO (martina.cardillo@iaps.inaf.it)\nSubjects: Gamma Ray, Pulsar\nDescription: Referred to by ATel #: 12753\nThere was a misprint in ATEL #12123: we executed a one day integration, from 2018-10-16 22:49 UT to 2018-10-17 22:49 UT and NOT from 2018-10-16 22:49 UT to 2018-08-17 22:49 UT. \nBelow you find the correct information. \nAGILE is detecting an intense gamma-ray flare above 100 MeV from the direction of the Crab Nebula. \nIntegrating on one day, from 2018-10-16 22:49 UT to 2018-10-17 22:49 UT, a maximum likelihood analysis yields a detection at a significance level of about 5.5 sigma, and a flux F = (1.1 ± 0.4) x 10^-5 ph/cm^2/s (E > 100 MeV). This is a factor 5 higher than the average flux (2.2 ± 0.1) x 10^-6 ph/cm^2/s (E > 100 MeV) reported in the First AGILE catalog. \nThe AGILE-GRID detection was obtained while AGILE is observing in spinning mode, surveying a large fraction of the sky each day. The source can be monitored with the public mobile application \"AGILEScience\" developed by the AGILE Team, available for both Android and iOS devices.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Near-Earth object", "Pulsar", "Circumstellar disk", "Binary system" ] }, "answerKey": "B" }, { "id": "atel_12225", "message": "Title: Detection of a new X-ray outburst of Aquila X-1 by Neil Gehrels Swift Observatory\nAuthors: Jie Lin, Shangyu Sun, and Wenfei Yu (Shanghai Astronomical Observatory)\nDate: 18 Nov 2018; 07:56 UT\nProvenance: Wenfei Yu (wenfei@shao.ac.cn)\nSubjects: X-ray, Request for Observations, Binary, Neutron Star, Transient\nDescription: Aquila X-1 is one of the neutron star LMXB transients with frequent outbursts in the past few decades. It has been inactive in the X-ray band for about 250 days since its latest outburst reported in 2018 Feb (e.g. Atel#11382). \nThe hard X-ray monitoring observations performed with Swift/BAT indicated that the X-ray intensity of Aquila X-1 in the 15-50 keV band has increased from 13+/-11 mCrab to 38+/-9 mCrab in the last 10 days, which suggests that Aquila X-1 may be in a new X-ray outburst again. However, the sun angle of Aquila X-1 is lower than 60 degrees. Therefore it was uncertain whether the enhance X-ray flux came from the source or not. Therefore, we proposed a Swift ToO pointed observation towards Aquila X-1 to confirm if it is indeed in a new X-ray outburst. \nThe Swift/XRT observation was performed with the WT mode for about 500 seconds, starting at 17:19:04 of 2018-11-17 (UTC). We did a quick analysis of the XRT data only. The net XRT X-ray count rate was 30.4+/-0.3 cps, corresponding to about 50 mCrab in the XRT band. We fitted the XRT energy spectrum in the 0.6-10 keV band with an absorbed power-law model, which gave a hydrogen column density of 3.0+/-0.2 x10^21 cm^-2 and a power-law index of 1.81+/-0.04. The X-ray flux in the 0.6-10 keV energy band is estimated as 1.65+/-0.03 x10^-9 ergs/s/cm^2, corresponding to an X-ray luminosity of 3.0x10^36 ergs/s at a source distance of 3.9 kpc. Therefore, we conclude that Aquila X-1 is in a new X-ray outburst. \nWe would like to thank the PI of the Neil Gehrels Swift Observatory for approving our request and scheduling the ToO observation, and the Guest Observer Facility for providing BAT monitoring data to the public.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Binary system", "Neutron star", "Nova" ] }, "answerKey": "C" }, { "id": "atel_12325", "message": "Title: \"Resurrection\" of the 1991T-like SN Ia ASASSN-18ro\nAuthors: Subo Dong, Subhash Bose (KIAA-PKU), M. Stritzinger (Aarhus), K. Z. Stanek, C. S. Kochanek, T. A. Thompson (OSU), J. Prieto (UDP), B. Shappee (Hawaii), T. Holoien (Carnegie)\nDate: 24 Dec 2018; 05:13 UT\nProvenance: Subo Dong (dongsubo@pku.edu.cn)\nSubjects: Optical, Supernovae\nDescription: Referred to by ATel #: 12355\nASASSN-18ro (a.k.a., SN 2018evt, RA: 13:46:39.21 Dec: -09:38:35.75 ) was discovered by All-Sky Automated Survey for Supernovae (ASAS-SN; Shappee et al. 2014; Atel #11963) on UT 2018-08-11.00 at V ~ 16.5 mag (absolute magnitude M_V ~ -18.8 mag) in the host galaxy MCG -01-35-011 (z = 0.024971; A_V = 0.15 mag for Galactic extinction via NED). It was classified by ePESSTO as a SN Ia (best match SN Ia 1991T-like; Atel #11947).\nRecent ASAS-SN observations of ASASSN-18ro show that it is at g ~ 16.4 mag on UT 2018-12-16.36 and g ~ 16.6 mag on 2018-12-22.09. Therefore, after 4 months of its discovery, the luminosity of ASASSN-18ro is still at about -19 mag, and such a high late-time luminosity is not compatible with the light curve of a typical (1991T-like) SN Ia. We note that ZTF and Gaia also recently detect ASASSN-18ro at a similar brightness, i.e. r = 16.24 +/- 0.02 mag on UT 2018-12-16.54 from ZTF (available via Lasair: https://lasair.roe.ac.uk/object/ZTF18actuhrs/) and G = 16.32 mag on UT 2018-12-17.18 from Gaia Transient Alerts (http://gsaweb.ast.cam.ac.uk/alerts/alert/Gaia18dwd/).\nRe-inspection of the ePESSTO spectrum (taken with the ESO-NTT / EFOSC2-NTT at UT 2018-08-12.9995; available via TNS: https://wis-tns.weizmann.ac.il/object/2018evt) shows a prominent H-alpha emission line with FWHM ~ 1000 km/s (EW ~ 22 Angstrom). The archival 6dF spectrum (available via NED) at the nucleus of the host galaxy does not show any H-alpha emission. The H-alpha emission line likely origins from CSM interactions, which may also explain the high late-time luminosity of ASASSN-18ro. We note that some 1991T-like SNe Ia have been shown to have evidence of CSM interactions (e.g., Harris et al., 2018, ApJ, 868, 21; Graham et al., 2018, arXiv:1812.02757 and references therein).\nFurther follow-up observations are strongly encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova", "Minor body", "Pulsar", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_12400", "message": "Title: ePESSTO spectroscopic classification of optical transients\nAuthors: F. Ragosta (U. Federico II/OACN), F. Olivares (MAS/U. de Chile), O. Rodriguez (UNAB/MAS), G. Pignata (UNAB/MAS), Cristina Barbarino (Stockholm), Stefan Taubenberger (MPA-Garching), C. Inserra (Cardiff), E. Kankare (Turku), K. Maguire (QUB), S. J. Smartt (QUB), O. Yaron (Weizmann), D. R. Young (QUB) I. Manulis (Weizmann)\nDate: 16 Jan 2019; 16:56 UT\nProvenance: Giuliano Pignata (pignago@gmail.com)\nSubjects: Optical, Supernovae\nDescription: ePESSTO, the extended Public ESO Spectroscopic Survey for Transient Objects (see Smartt et al. 2015, A&A, 579, 40 http://www.pessto.org ), reports the following supernova classifications. Targets were supplied by the Zwicky Transient Facility (https://www.ztf.caltech.edu/; Kulkarni et al. 2018, ATel 11266) data stream processed through the Lasair broker (http://lasair.roe.ac.uk/). All observations were performed on the ESO New Technology Telescope at La Silla on 2019 January 15, using EFOSC2 and Grism 13 (3985-9315A, 18A resolution). Classifications were done with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024) and GELATO (Harutyunyan et al., 2008, A&A, 488, 383). Classification spectra and additional details can be obtained from http://www.pessto.org (via WISeREP) and the IAU Transient Name Server. \n \n \n Survey Name | IAU Name | RA (J2000) | Dec (J2000) | Disc. Date | Source | Disc Mag | z | Type | Phase | Notes \n ZTF19aabimbg | AT2019th | 05:10:39.26 | +17:36:45.1 | 20190107 | ZTF | 15.0 | 0.0 | CV | - | (1) \n \n(1) Previously classified and reported to the TNS by the Global SN Project", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Minor body", "Exoplanet", "Neutron star" ] }, "answerKey": "A" }, { "id": "atel_12480", "message": "Title: MAXI J1348-630: SALT optical spectroscopy during outburst\nAuthors: P. A.Charles (Southampton), D. A.H. Buckley, E. Kotze, S. B.Potter, J. K.Thomas (SAAO/SALT), P. Gandhi, J. A.Paice (Southampton)\nDate: 7 Feb 2019; 20:35 UT\nProvenance: Phil Charles (pac2soton@gmail.com)\nSubjects: Optical, X-ray, Black Hole, Neutron Star, Transient, Variables\nDescription: Referred to by ATel #: 12520, 13459, 13539\nFollowing the discovery (ATEL #12425) and subsequent optical identification (ATEL #12430) of MAXI J1348-630, we have undertaken intermediate dispersion spectroscopy of the optical counterpart with the Robert Stobie Spectrograph on SALT, in Sutherland, South Africa, as part of the SALT Transients programme. We obtained 3 spectra (exposure times 1200s, 2x1600s) on 2019 Jan 29 and 30 (UT 00-01h) using the G0900 grating, covering the spectral range 4200-7300Å at a resolving power of ~1000 (spectral resolution ~6.5Å) and under good observing conditions. \nAll spectra are largely featureless, apart from relatively weak H, HeII emission lines and interstellar absorption features. We find broad (~700 km/s), single-peaked emission at Hα (EW~3Å), plus broad HeII emission (EW~2Å) and the Bowen blend. The continuum appears reddened, as intimated in ATEL #12439 and #12456, and we find diffuse interstellar absorption at 4430Å (EW=2.25Å), 6283Å and the NaD lines (EW=2.0Å). Assuming standard interstellar absorption parameters for the 4430Å DIB (Herbig 1975 ApJ 196, 129) and NaD lines (Barbon et al 1990 A&A 237, 79), this implies an Av of ~2-3 mags, consistent with the X-ray absorbing column of ~7x1021 cm-2 inferred from Swift observations quoted in ATEL #12439. Our spectra are similar to other LMXB X-ray transients in outburst, and if it is a BH system (ATEL #12447) then it is likely at a distance >3kpc (ATEL #12439), again consistent with the reddening given its galactic latitude (-1.4 degs). Further spectroscopic study is encouraged as the outburst progresses, and especially into quiescence.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Accreting object", "Black hole, Variable star", "Star and stellar system, Variable star", "Black hole, Star and stellar system" ] }, "answerKey": "B" }, { "id": "atel_12550", "message": "Title: Asiago spectroscopic classification of ASASSN-19ec\nAuthors: Fiore (INAF OAPd), S. Schuldt, C. Vogl, S. Taubenberger (MPA, Garching), S. Benetti, E. Cappellaro, L. Tomasella, M. Turatto (INAF OAPd)\nDate: 5 Mar 2019; 08:50 UT\nProvenance: Lina Tomasella (lina.tomasella@oapd.inaf.it)\nSubjects: Supernovae\nDescription: The Asiago Transient Classification Program (Tomasella et al. 2014, AN, 335, 841) reports the spectroscopic observation ASASSN-19ec (Atel #12547; aka AT2019bkh), discovered by ZTF, ATLAS and ASAS-SN surveys. \nThe observation was performed with the Asiago 1.82m Copernico Telescope (+AFOSC; range 340-820 nm; resolution 1.4 nm). \n \n \n \n Survey name | IAU name | Host galaxy | Disc. Date (UT) | Obs. Date (UT) | redshift | type | phase | notes \n ASASSN-19ec | SN2019bkh | MCG+05-31-141 | 2019-03-03 09:07:12 | 2019-03-05 03:39:22 | 0.019512 | Ia | -10d | (1) \n \n(1) Also reported as ZTF19aakzwao with discovery date 2019-02-26 07:19:12, and as ATLAS19dqw with discovery date 2019-03-03 12:17:16. Spectrum similar to those of several type Ia SNe (in agreement with the classification reported in TNS by Fremling, et al.), with a best match about ten days before maximum light. The velocity of the ejecta, as measured from SiII 635.5 nm, is around 13100 km/s, using the redshift of the host galaxy as reported by Haynes et al. 1997, AJ 113, 1197 (via NED). \nThe classification was performed using the GELATO (Harutyunyan et al. 2008, A&A, 488, 383) \nand SNID (Blondin and Tonry 2007, ApJ, 666, 1024) tools. \nPadova-Asiago SN Group", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Repeater", "Globular cluster", "Supernova" ] }, "answerKey": "D" }, { "id": "atel_12625", "message": "Title: MASTER: new OT, 6.5mag amplitude outburst\nAuthors: D. Savinov, V. Shumkov, V. Lipunov (Lomonosov MSU), D. Buckley (SAAO), V. Vladimirov, E. Gorbovskoy, V. Kornilov, N. Tiurina, P. Balanutsa, A. Kuznetsov, D. Zimnukhov, D. Kuvshinov (Lomonosov Moscow State University, SAI), R. Podesta, C. Lopez, C. Francile, F. Podesta (OAFA, SJNU), H. Levato (ICATE, SJNU), R. Rebolo, M. Serra (IAC), O. Gress, N. M. Budnev (API ISU), V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (BSPU), A. Tlatov, V. Senik, D. Dormidontov (KSS of Pulkovo observatory), T. Pogrosheva\nDate: 3 Apr 2019; 14:27 UT\nProvenance: Nataly Tyurina (tiurina@sai.msu.ru)\nSubjects: Optical, Cataclysmic Variable, Transient, Variables\nDescription: MASTER OT J141757.08-451601.3 discovery - 6.5mag amplitude outburst\nMASTER-SAAO auto-detection system ( Lipunov et al., \"MASTER Global Robotic Net\", Advances in Astronomy, 2010, 30L ) \ndiscovered OT source at (RA, Dec) = 14h 17m 57.08s -45d 16m 01.3s on 2019-04-03.02571 UT. \nThe OT magnitude in 'R' filter is 15.5m (mlim=18.3). The OT is seen in 2 images (opened survey mode of MASTER observations). There is no minor planet at this place. \nWe have reference image on 2019-03-02.05494 UT with 'R' filter 18.6m, the nearest in time image is on 2019-03-18 00:14:35 with mlim_R=18.0, on 2016-03-12 00:45:36UT with unfiltered mlim=20.6 (MASTER_W=0.2B+0.8R calibrated by thousands USNO-B1 field stars). \nThere is no any sources in VIZIER database, it means 22m POSS limits in history and more then 6.5magnitude of current outburst amplitude. \nSpectral observations are required. \nThe discovery and reference images are available at: \nhttp://master.sai.msu.ru/static/OT/141757.08-451601.3.png \nMASTER Global Robotic Net", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Variable star", "Magnetar", "Repeater" ] }, "answerKey": "B" }, { "id": "atel_12700", "message": "Title: Nasu telescope array observations of the recent Cyg X-3 flare at 1.4GHz\nAuthors: K. Tsubono, K. Asuma, H. Nakajima, T. Daishido (Waseda Univ.), K. Niinuma, T. Aoki (Yamaguchi Univ.), and K. Takefuji (NICT)\nDate: 28 Apr 2019; 03:51 UT\nProvenance: Kimio Tsubono (tsubono.kimio@aoni.waseda.jp)\nSubjects: Radio, Binary, Black Hole, Transient\nDescription: Referred to by ATel #: 12741, 12764, 12880, 13866\nOn April 18, a major radio flare from Cyg X-3 was detected with Metsahovi Radio Observatory at 37 GHz (ATel #12668). Following that, recent enhanced gamma-ray emissions originating from Cyg X-3 were reported by the AGILE team (ATel #12677, #12678).\nWith the Nasu telescope array, we have been monitoring Cyg X-3 daily from April 14 (drift-scan mode). On April 18, we could observe the appearance of a new activity of Cyg X-3 with the flux level of 1.14 +/- 0.02 Jy (UT 21:45) at 1.4 GHz. During next five days the observed flux was increasing up to 5.9 +/- 0.4 Jy on April 24 21:21 UT. Thirteen days light curve including preceding four days data with five-sigma noise level can be shown in the figure below. \nWe will continue our radio monitoring for a while.\nThe Nasu telescope array is a spatial FFT interferometer consisting of linearly aligned eight antennas with 20-m spherical dishes. This type of interferometer was developed to survey transient radio sources with a high angular resolution that of 160-m dish and at the same time with a wide field-of-view that of 20-m dish.\n13 days light curve of Cyg X-3 at 1.4GHz", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Binary system, Repeater", "Binary system, Black hole", "Supernova, Black hole", "Neutron star, Black hole" ] }, "answerKey": "B" }, { "id": "atel_12780", "message": "Title: X-ray non-detection of black hole transient MAXI J1535-571\nAuthors: A. S. Parikh, R. Wijnands, T. D. Russell (UvA)\nDate: 20 May 2019; 08:41 UT\nProvenance: Aastha Parikh (A.S.Parikh@uva.nl)\nSubjects: X-ray, Black Hole, Transient\nDescription: MAXI J1535-571 is a candidate black hole low-mass X-ray binary that was discovered in outburst in September 2017 (Barthelmy et al. 2017, Negoro et al. 2017). We have monitored the source using the Neil Gehrels Swift Observatory/X-ray Telescope (Swift/XRT) since its discovery. Its main outburst ended in 2018 May, after which it was followed by several re-brightenings (e.g., Parikh et al. 2018). MAXI J1535-571 exhibited at least 5 such re-brightenings. However, these re-brightenings ceased at the end of January 2019 and the source entered a quasi-steady state during which its intensity was found to only vary by a factor of 3, hovering around an average XRT count rate of ~0.2 c/s (0.5-10 keV). This quasi-steady state lasted ~3.5-4.5 months. We fit the spectrum extracted from the combined quasi-steady state XRT data with an absorbed power-law model find a photon index of Gamma ~ 1.7 (and the equivalent hydrogen column density was found to be Nh ~ 2.6E22 cm^-2). MAXI J1535-571 exhibited an average luminosity of ~3.7E34 erg/s (0.5-10 keV; assuming d = 4 kpc) during this quasi-steady state.\nA short XRT observation (~500 s) of MAXI J1535-571 carried out on 11 May 2019 showed that the source was no longer detected, with an upper limit corresponding to 5.2E-3 c/s (using the 90% prescription by Gehrels, 1986). The source was detected at a count rate of 0.2 c/s (0.5-10 keV) ~27 days prior to this observation. We requested an additional XRT observation having a longer exposure time in order to further constrain the source activity level after the non-detection. We obtained an XRT observation on 17 May 2019 (having an exposure of ~2.3 ks) during which the source was again not detected. We combined the data from these two observations in which the source was not detected (observation ID: 00010264119 and 00010264120) to obtain an upper limit of 8.6E-4 c/s. We calculated the luminosity corresponding to this upper limit using XSpec, assuming the same spectral parameters as those observed during the quasi-steady state. We find that the upper limit corresponds to a luminosity of <8E32 erg/s (0.5-10 keV; d = 4 kpc). Our approved XRT monitoring of MAXI J1535-571 continues for 1 more month, observing the source once every two weeks, allowing us to track if the source becomes active again.\nWe thank the Swift team for approving and scheduling scheduling our requested observations.\nBarthelmy et al. 2017, GCN #21792 \nGehrels, 1986, ApJ, 303, 336 \nNegoro et al. 2017, ATel #10699 \nParikh et al. 2018, ATel #11652", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Minor body", "Variable star", "Pulsar" ] }, "answerKey": "A" }, { "id": "atel_12875", "message": "Title: HET Spectroscopic Observation of AT 2019fdr\nAuthors: B. Thomas (ICG Portsmouth, UT Austin), J. Vinko (Konkoly Obs, U Szeged, UT Austin), J. C. Wheeler (UT Austin)\nDate: 18 Jun 2019; 09:33 UT\nProvenance: Jozsef Vinko (vinko@astro.as.utexas.edu)\nSubjects: Optical, AGN, Transient\nDescription: An optical spectrum (range 460-1000 nm, resolution 1900) of AT 2019fdr was obtained with the \"Low Resolution Spectrograph-2\" (LRS2) on the 10m Hobby-Eberly Telescope at McDonald Observatory by M. Shetrone on 2019-06-16.16 UT. \nThe spectrum shows obvious Balmer features at z = 0.2667, but no broad lines expected of a supernova. Cross-correlation with a library of SN spectra using the \"Supernova Identification\" code (SNID; Blondin and Tonry 2007, Ap.J., 666, 1024) shows that our spectrum matches with several AGN templates, although the light curve behaviour is peculiar for an AGN. Further follow up is encouraged. \nOur spectrum is posted on the IAU Transient Name Server: http://wis-tns.weizmann.ac.il/object/2019fdr/", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Pulsar", "Supernova, Accreting object", "Active galactic nucleus, Minor body", "Active galactic nucleus, Accreting object" ] }, "answerKey": "D" }, { "id": "atel_12960", "message": "Title: Unambiguous radio detection of the tidal disruption event AT2019dsg with e-MERLIN\nAuthors: M. Perez-Torres (IAA-CSIC, Spain), J. Moldon (JBCA, Manchester), S. Mattila (Univ. of Turku, Finland), A. Alberdi (IAA-CSIC, Spain), R. Beswick (JBCA, Manchester), S. Ryder (Macquarie Univ., Australia), E. Varenius (JBCA, Manchester), M. Fraser (Univ. College, Dublin), P. Jonker (SRON, Netherlands), E. Kankare (Univ. of Turku, Finland), E. Kool (Stockholm Univ., Sweden). \nDate: 26 Jul 2019; 07:45 UT\nProvenance: Miguel A. Perez-Torres (torres@iaa.es)\nSubjects: Radio, Transient, Tidal Disruption Event\nDescription: Referred to by ATel #: 13105\nWe report the first detection at radio wavelengths of the nuclear transient AT2019dsg, which was discovered by the Zwicky Transient Facility on UT 2019 Apr 9 (TNS Report No. 33340) in the center of the galaxy 2MASX J20570298+1412165 (z=0.0512). AT2019dsg has been classified as a tidal disruption event (TDE), based on the spatial coincidence with the nucleus of its host galaxy and its optical properties (ATel #12751). AT2019dsg is an X-ray bright TDE (ATel #12777, ATel #12825), and 15 GHz observations on 2019 May 16.24 reported a possible radio counterpart of AT2019dsg (ATel #12798), although the quoted radio position was more than 6\" off the optical one. \nHere we report electronic Multi-Element Remotely Linked Interferometer Network (e-MERLIN) observations of AT2019dsg at a frequency of 5.07 GHz on 2019 June 3 and 2019 June 20, which show the unambiguous detection of AT2019dsg at with e-MERLIN on 2019 June 20. The array included five antennas (Mk2, Pi, Da, De, and Cm), but not the Lovell telescope, resulting in synthesized Gaussian beams of approximately 77x32 (83x35) milliarcseconds at position angle of about 25 (28) deg on the 3rd and 20th of June, respectively. We centered our 5 GHz observations at the RA(J2000.0)= 20:57:02.97 and DEC(J2000.0)=+14:12:15.86, and imaged a 4x4 sq. arcsecond region around that position. While AT2019dsg is not detected on 2019 June 3 down to a 3-sigma level of 100 microJy, it is clearly detected on 2019 June 20 with a peak flux density of 354 +/- 23 microJy/b at the following position: RA(J2000.0)=20:57:02.96502; DEC(J2000.0)=+14:12:16.2898. The positional uncertainty is about 12 and 4 mas in RA and DEC, respectively. \nThe radio emission detected on 2019 June 20 corresponds to a monochromatic 5.07 GHz luminosity of (2.01 +/- 0.13)*1e28 erg/s/Hz at an age of 72 days, for an assumed luminosity distance of 228 Mpc. This value is typical of other nearby, radio loud TDEs, e.g., Arp299B-AT1 (Mattila et al. 2018, Science, 6401, 482), ASASSN-14li (Alexander et al. 2016, ApJ, 819, L25), AT2019azh (ATel #12870) at similar ages, albeit much fainter than the TDE Sw J1644+57 at z=0.35. \nFurther approved e-MERLIN observations are underway to trace the radio evolution of the TDE AT2019dsg. We thank the e-MERLIN staff for supporting our observing program.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Neutron star", "Variable star", "Interstellar medium" ] }, "answerKey": "C" }, { "id": "atel_13020", "message": "Title: Aql X-1: a new outburst is in progress\nAuthors: O. I. Spiridonova, V. V. Vlasyuk, A. S.Moskvitin, O. A.Maslennikova, R. I.Uklein (Special Astrophysical Observatory of the Rus. Ac. Sci.)\nDate: 13 Aug 2019; 11:00 UT\nProvenance: Alexander Moskvitin (mosk@sao.ru)\nSubjects: Optical, Transient\nDescription: Referred to by ATel #: 13953\nWithin a course of optical monitoring campaign of Soft X-ray Transient (SXT) Aql X-1 performed with the 1-m SAO RAS optical telescope in June-August we have detected indications on start a new outburst. According to our preliminary results in R-band, it's brightness increased between first decades of July and August. Our estimates of brightness of Aql X-1 optical counterpart in R-band in May-June were between 18.1 and 18.5 mag. Meanwhile, R-magnitude for epochs after July 4th demonstrated some trend for increasing, as seen in Table. \nDate | JD | R_mag \n---|---|--- \n20190704 | 2458669.4 | 18.05 \n20190806 | 2458702.4 | 17.00 \n20190807 | 2458703.2 | 16.90 \n20190811 | 2458707.4 | 16.70 \nTypical errors of brightness estimates are about 0.05 mag and should be decreased after more accurate data reduction. Measurements at August, 11 were obtained with midband filter and had some worse accuracy due to bright sky background (about 0.1 mag). Further observations of Aql X-1 in X-ray, UV, Optical, IR and Radio ranges are highly encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Interstellar medium", "Minor body", "Active galactic nucleus" ] }, "answerKey": "A" }, { "id": "atel_13100", "message": "Title: Interstellar Comet gb00234\nAuthors: Piotr Guzik (Jagiellonian Univ.), Michal Drahus (Jagiellonian Univ.), Krzysztof Rusek (AGH UST), Waclaw Waniak (Jagiellonian Univ.), Giacomo Cannizzaro (SRON), Ines Pastor Marazuela (Univ. of Amsterdam, ASTRON)\nDate: 11 Sep 2019; 21:16 UT\nProvenance: Michal Drahus (drahus@oa.uj.edu.pl)\nSubjects: Optical, Comet\nDescription: We report the identification of an interstellar minor body in the stream of astrometric positions that are being submitted to the Minor Planet Center. The body labelled gb00234 was initially identified on 8 September 2019 at 04:15 UT by our software \"Interstellar Crusher\" (custom Python code that operates on Bill Gray's Find Orb), which monitors the Possible Comet Confirmation Page performing a real-time search for hyperbolic orbits among newly discovered minor bodies. Visual inspection of the input data and orbital fits confirmed the identification. The object was discovered by Gennady Borisov (station L51) on 30 August 2019 at 01:03 UT. At the time of writing, 129 astrometric positions obtained over a 12.42-day interval yield the following hyperbolic solution (epoch 2019 Sep. 11.0 TT): \n \nT = 2019 Dec. 9.745968 +/- 0.94 TT \ne = 3.1551235 +/- 0.13 \nq = 1.95954186 +/- 0.035 au \nPeri. = 210.22059 +/- 0.90 deg (2000.0) \nNode = 307.71365 +/- 0.33 deg (2000.0) \nIncl. = 44.49503 +/- 0.34 deg (2000.0) \n(mean residual: 0.49 arcsec) \n \nThe orbital elements imply a hyperbolic excess speed of 30 km/s, comparable to `Oumuamua, the excess speed of which was 26 km/s. \n \nFollowing the identification, we obtained short series of g' and r'-band images on 10 September 2019 at 05:38 UT and 14:57 UT, using the William Herschel Telescope on La Palma and the Gemini North telescope on Mauna Kea, respectively. The images show an extended coma and a broad, short tail (roughly antisolar direction), making it clear that this second-known interstellar interloper is a comet. \n \ngb00234 is currently at a low solar elongation of ~43 deg, making more detailed observations difficult. Observing conditions will be improving, though, as the elongation increases and the body is on its way in (perihelion at 1.96 au and perigee at 1.89 au, both in December 2019). \n \nBased in part on observations obtained at the Gemini Observatory, which is operated by the Association of Universities for Research in Astronomy, Inc., under a cooperative agreement with the NSF on behalf of the Gemini partnership: the National Science Foundation (United States), the National Research Council (Canada), CONICYT (Chile), Ministerio de Ciencia, Tecnologia e Innovacion Productiva (Argentina), and Ministerio da Ciencia, Tecnologia e Inovacao (Brazil). The William Herschel Telescope is operated on the island of La Palma by the Isaac Newton Group of Telescopes in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. We thank the staff of both observatories for assistance and are indebted to the Director of Gemini Observatory for allocating Gemini North time for this program. M.D. and P.G. are grateful for support from the National Science Centre of Poland through SONATA BIS grant 2016/22/E/ST9/00109 and Polish Ministry of Science and Higher Education grant DIR/WK/2018/12. G.C. acknowledges support from European Research Council Consolidator Grant 647208. I.P.M. acknowledges funding from the Netherlands Research School for Astronomy (NOVA5-NW3-10.3.5.14).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium, Minor body", "Interstellar medium, Exoplanet", "Interstellar medium, Interstellar medium", "Interstellar medium, Quasar" ] }, "answerKey": "A" }, { "id": "atel_13175", "message": "Title: Outburst of comet P/2008 Y1 (Boattini)\nAuthors: Outburst of comet P/2008 Y1 (Boattini)\nDate: 8 Oct 2019; 20:13 UT\nProvenance: Michael Kelley (msk@astro.umd.edu)\nSubjects: Optical, Comet\nDescription: Referred to by ATel #: 13181\nWe report the discovery of an apparent outburst of comet P/2008 Y1 (Boattini), recently recovered by G. Borisov on 2019 Sep 2 UTC with the temporary designation P/2019 R1 (CBET #4663). We searched the Zwicky Transient Facility (Bellm et al. 2019, PASP, 131, a8002) survey archive for images of the comet based on the revised orbit. It was observed and detected on 14 nights between 2019 Jul 15 to 2019 Oct 05 UTC. Photometry up to 2019 Sep 22 measured with a 5\" radius aperture is tabulated below, calibrated to the PS1 catalog (Tonry et al. 2012, ApJ, 750, 99). We estimate a coma color of g-r=0.60±0.02 mag. The photometry approximately follows the trend: r=16.06 + 5 log10(Delta) + 15 log10(rh) + Phi(phase) (RMS 0.09 mag), where Delta is the observer-comet distance, rh is the heliocentric distance, and Phi(phase) is the Halley-Marcus phase function (Schleicher & Bair 2011, AJ 141, 177) at the given phase angle, expressed in magnitudes. Between 2019 Aug 21.51 and 24.50 UTC, 9 to 12 days before recovery, the comet brightened from g=18.03±0.07 to 17.39±0.05 mag, then slowly returned to its nominal brightness by 2019 Sep 10.49 UTC. The event appears to be a cometary outburst, with a strength of at least -0.62±0.05 mag.\n \n \n Date rh Delta Phase Filter m unc r Trend Residuals \n (UTC) (au) (au) (deg) (mag) (mag) (mag) (mag) (mag) \n ------------- ------ ----- ----- ------ ----- ----- ----- ----- --------- \n 2019-07-15.49 -1.439 1.704 36.5 r 18.49 0.09 18.49 18.53 -0.04 \n 2019-07-30.47 -1.359 1.595 39.2 g 18.48 0.06 17.88 17.98 -0.10 \n 2019-07-30.49 -1.359 1.595 39.2 r 17.93 0.05 17.93 17.98 -0.05 \n 2019-08-21.51 -1.284 1.497 41.8 g 18.03 0.07 17.43 17.45 -0.02 \n 2019-08-24.50 -1.279 1.489 42.0 g 17.39 0.05 16.79 17.41 -0.62 \n 2019-08-28.49 -1.273 1.480 42.2 g 17.41 0.03 16.81 17.36 -0.55 \n 2019-08-28.51 -1.273 1.480 42.2 r 16.81 0.02 16.81 17.36 -0.55 \n 2019-08-31.48 -1.270 1.474 42.4 g 17.69 0.03 17.09 17.34 -0.25 \n 2019-08-31.51 -1.270 1.474 42.4 r 17.10 0.02 17.10 17.34 -0.24 \n 2019-09-07.49 1.268 1.465 42.5 g 17.85 0.04 17.25 17.31 -0.06 \n 2019-09-07.52 1.268 1.465 42.5 r 17.21 0.03 17.21 17.31 -0.10 \n 2019-09-10.49 1.269 1.462 42.6 g 17.91 0.04 17.31 17.31 -0.00 \n 2019-09-10.51 1.269 1.462 42.6 r 17.30 0.03 17.30 17.31 -0.01 \n 2019-09-13.47 1.271 1.460 42.5 r 17.30 0.05 17.30 17.32 -0.02 \n 2019-09-14.52 1.273 1.459 42.5 r 17.38 0.05 17.38 17.33 0.05 \n 2019-09-22.49 1.286 1.457 42.4 r 17.42 0.06 17.42 17.39 0.03 \n 2019-09-22.52 1.286 1.457 42.4 g 18.17 0.07 17.57 17.39 0.18 \n \nColumns - rh, heliocentric distance (negative for pre-perihelion); Delta, observer-comet distance; Phase, Sun-comet-observer angle; Filter, ZTF bandpass name; m, apparent magnitude through filter in 5\" radius aperture; unc, uncertainty on m; r, effective r-band lightcurve after transforming g- into r-band photometry; Trend, the best-fit trend; and Residuals, the residuals from the fit.\nThis work makes use of observations obtained with the Samuel Oschin Telescope 48-inch at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-1440341 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, the University of Washington, Deutsches Elektronen-Synchrotron and Humboldt University, Los Alamos National Laboratories, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, and Lawrence Berkeley National Laboratories. Operations are conducted by COO, IPAC, and UW.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Pulsar", "Minor body", "Globular cluster" ] }, "answerKey": "C" }, { "id": "atel_13250", "message": "Title: MeerKAT upper limit on Swift J1713.4-4219 2019 outburst\nAuthors: Julien N. Girard (CEA-Saclay), Evangelia Tremou (CEA-Saclay), Stephane Corbel (CEA-Saclay), Rob Fender (Oxford & UCT), Patrick Woudt (UCT), James Miller-Jones (Curtin) on behalf of the ThunderKAT collaboration\nDate: 31 Oct 2019; 17:39 UT\nProvenance: Evangelia Tremou (evangelia.tremou@cea.fr)\nSubjects: Radio, Binary, Black Hole, Neutron Star, Transient\nDescription: As part of the ThunderKAT Large Survey Programme (Fender et al.2017, arXiv:1711.04132), we observed the transient reported in ATEL #13169, #13226 and #13247 of the candidate black hole transient Swift J1713.4-4219 (ATEL #2300). Radio measurements with MeerKAT (60 antennas) were performed on on MJD 58782.57 (2019-10-26 13:52 UTC) 3.53 days after detection and localization by Swift XRT (ATel #13226).\nWe observed the phase calibrator J1744-5144 for 2 minutes before and after a 15-minute scan on the J1713.4-4219. J1939-6342 was used as the primary flux and bandpass calibrator. Data were taken at a central frequency of 1.28 GHz with a bandwidth of 856 MHz over 4096 channels. Calibration and imaging were performed using standard techniques and Direction-Dependent calibration and imaging (Tasse et al. 2018, A&A 611, A87) to account for the effect of strong sources in the field.\nWe report a 3-sigma upper limit of 115µJy at the position of Swift J1713.4-4219. Distance to the object is unknown to deduce the associated radio luminosity.\nThunderKAT will run for 5 years and targets X-ray binaries, Cataclysmic Variables, Supernovae and Gamma-Ray Bursts. As part of this programme we perform weekly monitoring observation of all bright, active, southern hemisphere X-ray binaries in the radio band. For further information on this programme please contact Rob Fender and/or Patrick Woudt. We thank the staff at the South African Radio Astronomy Observatory (SARAO) for scheduling and carrying out these observations. The MeerKAT telescope is operated by SARAO, which is a facility of the National Research Foundation, and agency of the Department of Science and Technology. We acknowledge the use of the Inter-University Institute for Data Intensive Astronomy (IDIA) data intensive research cloud for data processing. IDIA is a South African university partnership involving the University of Cape Town, the University of Pretoria and the University of the Western Cape. We acknowledge the use of the Nançay Data Center computing facility (CDN - Centre de Données de Nançay). The NDC is hosted by the Station de Radioastronomie de Nançay in partnership with Observatoire de Paris, Université d'Orléans, OSUC and the CNRS. The CDN is supported by the Region Centre Val de Loire, département du Cher.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Neutron star", "Circumstellar disk, Neutron star", "Supernova, Neutron star", "Black hole, Magnetar" ] }, "answerKey": "A" }, { "id": "atel_13320", "message": "Title: Fermi-LAT detection of enhanced gamma-ray activity from the FSRQ PKS 0208-512\nAuthors: R. Angioni (SSDC/INFN) on behalf of the Fermi-LAT collaboration\nDate: 1 Dec 2019; 00:28 UT\nProvenance: Roberto Angioni (r.angioni90@gmail.com)\nSubjects: Gamma Ray, >GeV, AGN, Quasar\nDescription: Referred to by ATel #: 13352, 13558\nThe Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed enhanced gamma-ray flaring activity from a source positionally consistent with the flat-spectrum radio quasar PKS 0208-512, also known as 4FGL J0210.7-5101 (The Fermi-LAT collaboration 2019, arXiv:1902.10045), with coordinates R.A. = 32.692502 deg, Decl. = -51.017192 deg (J2000; Johnston et al. 1995, AJ, 110, 880), and redshift z=0.999 (Wisotzki et al. 2000, A&A, 358, 77). \nPreliminary analysis indicates that this source was in an elevated gamma-ray emission state on 29 November 2019, with a daily averaged gamma-ray flux (E>100MeV) of (1.1+/-0.2) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). The latter corresponds to a flux increase of a factor of 13 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL). This is comparable to the previous highest LAT daily flux ever observed for this source in May 2011 (ATel #3338). The corresponding photon index is 2.1+/-0.1, and is significantly smaller than the 4FGL value of 2.35+/-0.01. A ~22 GeV photon with a probability greater than 99% of being emitted by PKS 0208-512 has also been detected. \nBecause Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. This source is part of the \"LAT Monitored Sources\" and consequently, a preliminary estimation of the daily gamma-ray flux observed by Fermi-LAT will be publicly available ( http://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/ ). We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is W. Collmar (wec@mpe.mpg.de). \nThe Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Quasar", "Minor body", "Star and stellar system" ] }, "answerKey": "B" }, { "id": "atel_13400", "message": "Title: A VLA Radio Detection of Supernova SN2020oi\nAuthors: A. Horesh, I. Sfaradi (HUJI)\nDate: 11 Jan 2020; 21:34 UT\nProvenance: Assaf Horesh (assafh@mail.huji.ac.il)\nSubjects: Radio, Supernovae, Transient\nDescription: Referred to by ATel #: 13401, 13448\nWe report the detection of radio emission from the nearby supernova in M100, SN2020oi (TNS report 58241; ATel #13393; ATel #13391; ATel #13398; TNS AstroNote 2020-8; TNS AstroNote 2020-9). \n \nThe Jansky Very Large Array (VLA) undertook a second public observation of SN2020oi on 2020 January 11. The observation was conducted at 44 GHz (Q-band) in the D configuration. We performed an analysis of the data using the 3C286 as a flux calibrator and J1215+1654 as a gain calibrator. \n \nA single point source is detected in the VLA image at RA=12:22:54.917 Dec=15:49:25.01 (consistent with the position of SN2020oi) at a flux level of ~5 mJy. This confirms the possible detection we previously reported at a lower frequency of 8 GHz in an image with a lower spatial resolution (ATel #13398). \n \nWe encourage further high cadence multi frequency radio observations with the VLA and other facilities. \n \nWe thank the VLA and NRAO staff for scheduling and performing this public observation.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Star and stellar system", "Exoplanet", "Near-Earth object" ] }, "answerKey": "B" }, { "id": "atel_13450", "message": "Title: Photometric History for the Past Century of ASASSN-V J060000.76-310027.83 (J060000)\nAuthors: Bradley E. Schaefer (Louisiana State Univ.)\nDate: 5 Feb 2020; 17:37 UT\nProvenance: Bradley E. Schaefer (schaefer@lsu.edu)\nSubjects: Optical, Star, Transient, Variables\nDescription: The ASAS-SN Team (ATel #13346) reported their discovery of an ordinary early-K star (ATel #13349, #13361), constant in magnitude from 2013 Oct 24 until 2019 Oct 24 (ATel #13346), that displayed an exponentially increasing fade into a 0.8 mag dip in brightness with a minimum on 2019 Dec 11 (ATel #13357).\nI examined roughly a hundred archival photographic plates at Harvard College Observatory, with the significant detections spanning from 1922-1948. Except for three plates from late 1937, all the plates have an average magnitude of B=14.94, with an RMS scatter of 0.12 mag, consistent with the usual photometric accuracy of measurement. From 1937, I measured B=15.3 for Sep 13, B=15.3 for Nov 5, and B>15.3 for Nov 24. With three solid measures that the star was significantly faint by around 0.4 mag for over a month, I conclude that J060000 had a dip in brightness in late 1937, much like the 2019/2020 dip.\nThe original Palomar Sky Survey 103a-O plate is closely in the B system, when calibrated with measured image radii from 16 nearby stars of similar B magnitude. I measure B=14.90 ± 0.28 for 1956 Mar 9.\nThree all-sky surveys, with public on-line light curves, are showing J060000 to be constant to within the measurement uncertainty as shown by nearby comparison stars. ASAS has 437 magnitudes from 2001 to 2009, with V=13.65. SuperWASP has 11292 magnitudes from 2006 to 2008, with a mean magnitude of 13.96 for a bandpass from 400 to 700 nm. ASAS-SN has 1159 magnitudes from 2013-2018 with V=13.64, plus 1359 magnitudes from 2017 to 2019 Sep with g=14.21.\nThe 314 individual magnitudes for the APASS survey used 7 filters on 17 nights from 2011-2014. The RMS scatter of the magnitudes for J060000 are consistent with the stated photometric uncertainties and with the RMS scatters of nearby comparison stars, so J060000 appears constant. I calculate B=14.88, V=13.63, g'=14.23, r'=13.09, i'=12.65, and Z=12.44.\nAfter AAVSO Alert Notice 691, many observers contributed 3484 B, V, R, and I magnitudes from 2019 Dec 20 to 2020 Feb 1. The light curve shows two local minima, with these second and third dips being of larger amplitude in blue light and smaller amplitude in red light. The minimum of 2020 Jan 2 has B=15.40, V=14.05, and I=12.48, while the minimum of 2020 Jan 27 has B=15.55, V=14.11, R=13.18, and I=12.51. For the maximum between these dips (around 2020 Jan 9), B=15.13, V=13.83, R=13.03, and I=12.35.\nFor a scenario with the dips being caused by some occulting dust cloud, we can calculate R = A_V/E(B-V): (1) From the normal un-dimmed state to the bottom of the third dip, A_V=14.11-13.63=0.48, while the B-V changed from 14.88-13.63=1.25 to 15.55-14.11=1.44 for E(B-V)=0.19. This gives R=2.5. (2) From the baseline to the maximum between the dips, R=4.0. (3) For the dust adding extinction from the maximum between dips to the bottom of the third dip, R=2.0.\nI conclude: (1) J060000 had a dip in late 1937 that was much like the current episode of dips. (2) Other than the two dip episodes, J060000 is constant (to within typically 0.04 mag or less), with no trends, flares, or oscillations for the last century. (3) The 2019/2020 episode is chromatic (the dips are much deeper in blue than red light), with brightnesses varying as expected for occultation by dust clouds. (4) The R value for the dust varies from 2.0 to 4.0, implying some segregation of dust by size. (5) The only known class of star displaying rare, irregular, and chromatic dips on ordinary main sequence stars, with no infrared excess, is the 'dipper' class, with the Boyajian Star (KIC 8462852) as the prototype.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Neutron star", "Star and stellar system", "Stellar evolution" ] }, "answerKey": "C" }, { "id": "atel_13525", "message": "Title: A high-resolution, high S/N, optical HARPS public spectrum of Betelgeuse during minimum\nAuthors: Luca Sbordone (ESO, Chile), Claudia Paladini (ESO, Chile), Juanita Antilen (Universidad de Chile), Silvina Cardenas (IAFE, Argentina), Giada Casali (INAF-Arcetri, Italy), Avinash Chaturvedi (ESO, Germany), Lorenza Della Bruna (Stockholm University, Sweden), Ana I. Ennis (Instituto de Astrofisica de La Plata, Argentina), Keila Y. Ertini (Instituto de Astrofisica de La Plata, Argentina), Iskra Georgieva (Chalmers University of Technology, Sweden), Aishwarya Girdhar (ESO, Germany), Johanna Hartke (ESO, Chile), Edoardo Iani (ESO, Germany), Heidi Korhonen (ESO, Chile), Francesca Lucertini (Universidad de Andres Bello, Chile), Alonso Luna (Universidad de Andres Bello, Chile), Paula A. Miquelarena Hollger (ICATE, Argentina), Chiara Mazzucchelli (ESO, Chile), Camila Navarrete (ESO, Chile), Raphael A. P. Oliveira (Universidade de Sao Paulo, Brazil), Anna Pala (ESO, Germany), Thallis Pessi (Universidade Federal de Santa Maria, Brazil)), Ana C. Posses (Universidad Diego Portales, Chile), Cinthya Rodriguez (Instituto de Astrofisica de La Plata, Argentina), Linda Schmidtobreick (ESO, Chile), Peter Scicluna (ESO, Chile), Mattia Sirressi (Stockholm University, Sweden), Luis C. Vasconcelos Filho (Valongo Observatory, Brazil), Markus Wittkowski (ESO, Germany), John J. Yana Galarza (Universidade de Sao Paulo, Brazil)\nDate: 26 Feb 2020; 20:48 UT\nProvenance: Linda Schmidtobreick (lschmidt@eso.org)\nSubjects: Optical, Star\nDescription: On February 12, 2020, approx. 01:32 UT, within the framework of the ESO La Silla Observing School 2020 (https://www.eso.org/sci/meetings/2020/lasilla_school2020.html), four 10s exposure HARPS (HAM mode) spectra of Betelgeuse were obtained, covering the spectral range 378nm to 691nm, at R=115,000 and with a S/N of exceeding 500 per pixel at 640nm after coadding. Betelgeuse is one of brightest stars in the sky, and has been undergoing a dimming event (see https://www.eso.org/public/news/eso2003/). The spectrum is characterised by prominent TiO bands, the main opacity sources in the optical range and one of the candidate's dust precursors. TiO forms when the star cools, and the bands can absorb a large fraction of the visible light. The epoch of our observation falls into the broad minimum of the lightcurve when Betelgeuse reached V=1.614mag (Guinan et al. 2020, ATel #13512). The raw and reduced spectra are public and can be retrieved from the ESO archive (http://archive.eso.org/cms/data-portal.html). They have been obtained under Program/run ID 60.A-9501(C) and OB ID 1000032052. The authors of this communication are the students and tutors of the La Silla Observing School 2020.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system", "Pulsar", "Variable star", "Stellar evolution" ] }, "answerKey": "A" }, { "id": "atel_13575", "message": "Title: 4 - 11 GHz detection of Swift J1818.0-1607 with the Breakthrough Listen Instrument at the Robert C. Byrd Green Bank Telescope\nAuthors: Vishal Gajjar (UCB); Karen Perez (Columbia); Andrew Siemion (UCB); Dave MacMahon (UCB); Matt Lebofsky (UCB); Steve Croft (UCB); Danny Price (Swinburn); and Breakthrough Listen team\nDate: 21 Mar 2020; 16:51 UT\nProvenance: Vishal Gajjar (vishalg@berkeley.edu)\nSubjects: Radio, Neutron Star, Soft Gamma-ray Repeater, Star, Pulsar, Magnetar\nDescription: Referred to by ATel #: 13577, 13579, 13580, 13587, 13649, 13966, 14001\nWe report a detection of Swift J1818.0-1607 across 4 to 12 GHz (C and X-bands) using the Robert C. Byrd Green Bank Telescope (GBT) and the Breakthrough Listen digital backend (MacMahon et al. 2018, PASP, 130, 044502). The Breakthrough Listen Initiative is conducting a wide ranging search for observational indicators of extraterrestrial civilizations (technosignatures), including observations of a variety of exotic objects such as magnetars (Lacki et al 2020 in prep). \nOn UT 2020 March 12, 21:16:47 the Swift Burst Alert Telescope reported outburst activity from SGR Swift J1818.0-1607 (GCN circular 27373). Following up on this activity, NICER reported a coherent periodic feature with 0.733417(4) Hz periodicity and suggested the source to be an active magnetar. Several radio follow-up campaigns (ATels #13553, #13554, #13559, #13560, #13562, #13569) detected radio pulsation from the source below 3 GHz. \nUsing the GBT, we carried out a 600 second observation on UT 2020 March 14, 12:22:47 at 6 GHz with 4 GHz instantaneous bandwidth (C-band), immediately followed by another 600 second scan at UT 13:07:57 at 9.3 GHz with 3.7 GHz of instantaneous bandwidth (X-band). Observations were recorded as GUPPI-formatted baseband voltages (Lebofsky et al. 2019, PASP, 131, 124505). Data were processed with a bespoke GPU-accelerated pipeline to convert voltages to high temporal resolution SIGPROC formatted filterbank products, and voltages were preserved. We used the periodicity of 0.7334110 Hz reported by Enoto et al. (ATel #13551) and DM of 703 pc-cm-3 (Rajwade et al. ATel #13554) to produce folded profiles at both bands. Data affected by RFI were flagged using PSRCHIVE tools. \nAt C-band, we found a prominent profile with integrated S/N of around 16. Based on the radiometer equation we estimate that the approximate peak flux density of the detection is around 0.04 mJy. We only included the lower 2 GHz of C-band for the integrated profile. Upon closer inspection, we noticed that this average profile actually consists of a few intermittent, prominent, and bright bursts instead of regular weaker single pulses (see linked figure). At X-band, we did not find a significant profile. A separate search for single pulses was undertaken for both the C-band and X-band data, using the technique described by Gajjar et al (2018, ApJ, 283, 2). \nThe preliminary analysis detected 29 single pulses across 4 - 8 GHz with S/N ranging between 6.2 to 146, corresponding to peak flux densities of 21 to 500 mJy. \nWe also report a marginal detection of a weak burst across 8 - 11 GHz from these observations with a S/N of around 7.2 at the DM of 703 pc-cm^-3. This corresponds to a peak flux density of around 40 mJy. \nWe report a wide variety of single pulses with multiple sub-pulse components and varying pulse widths (see linked figures), similar to other radio magnetars (Pearlman et al. 2018, ApJ, 886, 17; Maan et al 2019, ApJ, 882, 9; etc). A leading theory for Fast Radio Bursts (FRBs) is that they originate from magnetars; however, most FRB searches have been undertaken at lower frequencies (< 3 GHz). Our detections suggest that many FRBs are likely to be active above 4 GHz, given flatter spectral indices of radio emission from magnetars. Detection of bright single pulses further supports these claims. \nThese observations suggest that Swift J1818.0-1607 is still active and we encourage further follow-up observations. \nWe thank the GBT staff for all their help during these observations. \nWe are releasing all of our data taken during these observations to the community. Links to download these data and detection figures are available at the following location. \nDetection Plots and Data Download", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Neutron star", "Black hole", "Nova", "Galaxy" ] }, "answerKey": "A" }, { "id": "atel_13625", "message": "Title: The obscured pulsar IGR J18179-1621 entered a bright state\nAuthors: P. Esposito (IUSS-PV), G. L. Israel (INAF-OAR), N. Rea, A. Borghese, F. Coti Zelati (ICE-CSIC, IEEC), on behalf of a larger collaboration\nDate: 10 Apr 2020; 09:43 UT\nProvenance: Paolo Esposito (paoloesp@iasf-milano.inaf.it)\nSubjects: X-ray, Binary, Neutron Star, Pulsar\nDescription: Referred to by ATel #: 13737\nXMM-Newton observed serendipitously the position of IGR J18179-1621 (Bozzo et al. 2012, A&A, 545, A83; Li et al. 2012, MNRAS, 426, L16; Nowak et al. 2012, ApJ, 757,143) on 2020 March 15 and again on 2020 April 4. The XMM-Newton monitoring campaign is aimed at observing the outburst evolution of the new magnetar Swift J1818-1607 (Esposito et al. 2020, astro-ph/2004.04083).\nIGR J18179-1621 was discovered in 2012 with INTEGRAL during an outburst that lasted few weeks. A Swift/XRT monitoring led to the discovery of strong pulsations at 11.82 s (Halpern 2012, ATel #3949) and showed a flux decreasing from 2.9e-10 erg/cm^2/s on 2012 February 29 to 8e-12 erg/cm^2/s in about 19 days (Bozzo et al. 2012). The source was suggested to be an accreting high-mass X-ray binary.\nIn the first XMM-Newton observation (22.1 ks exposure time; 2020 March 15), IGR J18179-1621 fell in an off-axis portion of the EPIC MOS2 CCD camera. Using the SAS tool EUPPER and the exposure map, we set a 3 sigma upper limit on its count rate of 0.0041 counts/s. Using the WebPIMMS and adopting the spectrum below, we find an upper limit on the observed flux of approximately 3e-13 erg/cm^2/s in the 2-10 keV band.\nIn the second observation (27.7 ks exposure time; 2020 April 4), the source was clearly detected in the EPIC pn and MOS2 cameras. Its spectrum can be modelled as a hard power law modified for the interstellar absorption with photon index -0.6 +/- 0.2 and absorption (20 +/- 3)e22 cm^-2. The observed 2-10 keV flux was (2.1 +/- 0.1)e-11 erg/cm^2/s. A strong periodic flux modulation is detected at 11.8268(1) s. The high time resolution XMM-Newton data show a double peak profile with two slightly asymmetric peaks. All uncertainties are at 1 sigma confidence level.\nThe brightening of a factor larger than 50 in about 20 days may indicate either that the source is entering a new outburst, or that it is on the decay path from an outburst that peaked after 2020 March 15 and has a time scale of weeks. Multi-band observations of the source are encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium, Neutron star", "Binary system, Supernova", "Binary system, Neutron star", "Binary system, Pulsar" ] }, "answerKey": "C" }, { "id": "atel_13700", "message": "Title: LJT Spectroscopic Classification of PTSS-20hk (AT2020iic) as a Type Ibn Supernova\nAuthors: Jujia Zhang(YNAO), Zhijian Xu, Bin Li (PMO), Wenxiong Li (THU), Hanjie Tan(NCU), Xiaofeng Wang(THU), Haibin Zhao(PMO), Lifan Wang (PMO/TAMU)\nDate: 3 May 2020; 08:47 UT\nProvenance: Ju-Jia Zhang (jujia@ynao.ac.cn)\nSubjects: Optical, Supernovae\nDescription: We obtained an optical spectrum (range 350-870 nm) of PTSS-20hk (AT2020iic), discovered by PTSS, on UT 2020 May 02.7 with the Li-Jiang 2.4 m telescope (LJT+YFOSC) at the Li-Jiang Observatory of Yunnan Observatories. The blue spectrum is dominated by the emission of He I 5876. The emission of He I 5016 is also presented in the spectrum. These look like the typical feature of SNe Ibn at a relatively early phase. Cross-correlation with the comparison tool GELATO (Harutyunyan et al. 2008, A&A, 488, 383, https://gelato.tng.iac.es) shows that it matches with SN Ibn 2005la at t = +17.5 days after the maximum.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Repeater", "Magnetar", "Variable star" ] }, "answerKey": "A" }, { "id": "atel_13770", "message": "Title: Search for counterpart to IceCube-200530A with ANTARES\nAuthors: Alexis Coleiro (APC/Universite de Paris) and Damien Dornic (CPPM/CNRS) on behalf of the ANTARES Collaboration\nDate: 31 May 2020; 08:07 UT\nProvenance: Antoine Kouchner (kouchner@apc.univ-paris-diderot.fr)\nSubjects: >GeV, TeV, Neutrinos, Transient\nDescription: Using data from the ANTARES detector, we have performed a follow-up analysis of the recently reported single track-like event IceCube-200530A (GCN 27865< https://gcn.gsfc.nasa.gov/gcn3/27865.gcn3>). The original reconstructed origin was on the edge of the ANTARES field of view for upward going events (-0.04 degrees below Its horizon). \n \nNo muon neutrino candidate events were recorded in a 3 deg cone centered on the location of the IceCube event coordinates (accounting for the reported uncertainties) during a +/- 1h time-window centered on the IceCube event time. \n \nThis leads to a preliminary conservative 90% confidence level upper limit on the muon-neutrino fluence from a point source of about 80 GeV.cm^-2 over the energy range 6 TeV – 6 PeV (the range corresponding to 5-95% of the detectable flux) for an E^-2 power-law spectrum, and about 110 GeV.cm^-2 (1 TeV - 560 TeV) for an E^-2.5 spectrum. A search over an extended time window of +/- 1 day has also yielded no detection (34% visibility). \n \nANTARES is the largest undersea neutrino detector (Mediterranean Sea) and it is primarily sensitive to astrophysical neutrinos in the TeV-PeV energy range. At 10 TeV, the median angular resolution for muon neutrinos is about 0.5 degrees. In the range 1-100 TeV ANTARES has a competitive sensitivity to this position in the sky.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Stellar evolution", "Neutron star", "Magnetar" ] }, "answerKey": "C" }, { "id": "atel_13860", "message": "Title: Fermi-LAT detection of renewed gamma-ray activity from the FSRQ TXS 0025+197\nAuthors: Isabella Mereu (INFN Perugia) on behalf of the Fermi Large Area Telescope Collaboration\nDate: 10 Jul 2020; 21:35 UT\nProvenance: Isabella Mereu (mereuisabella@gmail.com)\nSubjects: Gamma Ray, >GeV, Request for Observations, AGN, Blazar\nDescription: Referred to by ATel #: 13910\nThe Large Area Telescope (LAT) on board the Fermi Gamma-ray Space Telescope has observed an increasing gamma-ray flux from a source positionally coincident with the flat spectrum radio quasar TXS 0025+197 (Douglas et al. 1996 AJ, 111, 1945), at RA: 7.12424 deg, Dec.: 20.00742 deg (J2000, Beasley et al. 2002 ApJS, 141, 13). TXS 0025+197, also known as 4FGL J0028.4+2001, has a redshift of 1.5517+/-0.0004 (Alam et al. 2015, ApJS, 219, 12). \nPreliminary analysis indicates that this source was in an elevated gamma-ray emission state on July 9, 2020, with the emission of two E > 10 GeV photons (E = 11.8 GeV; time : 2020-07-09 04:12:56.731; E = 13.6 GeV; time : 2020-07-09 18:36:53.725, with association probability > 99%) and with a daily averaged gamma-ray flux (E>100MeV) of (1.0 +/- 0.2) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). The latter corresponds to a flux increase of a factor of 80 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL, Abdollahi et al. 2020). The corresponding photon index is 1.87 +/- 0.11, and significantly smaller than the 4FGL value of 2.44 +/- 0.07. The peak 6-hour integrated gamma-ray flux (E>100 MeV) of (1.5+/-0.4) X 10^-6 photons cm^-2 s^-1 was reached by TXS 0025+197 in the interval 06:00-12:00 UT, with corresponding photon spectral index of 1.83+/-0.18. Previous bright gamma-ray activity from this object was reported in August 2019 (ATel #13032) and October 2018 (ATel #12084) . This source is one of the \"LAT Monitored Sources\"(https://fermi.gsfc.nasa.gov/ssc/data/access/lat/msl_lc/source/TXS_0025p197). \nSince Fermi normally operates in an all-sky scanning mode, regular monitoring of this source will continue. In consideration of the ongoing activity of this source we strongly encourage multiwavelength observations. The Fermi LAT contact persons are S. Buson (sara.buson@gmail.com) and R. Angioni (r.angioni90@gmail.com). \nThe Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan, and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Black hole", "Supernova", "Galaxy" ] }, "answerKey": "B" }, { "id": "atel_13925", "message": "Title: The blazar AO 0235+16 in high optical state\nAuthors: V. M. Larionov, T. S. Grishina (St. Petersburg University)\nDate: 8 Aug 2020; 14:45 UT\nProvenance: V. Larionov (vlar@astro.spbu.ru)\nSubjects: Optical, Blazar, Quasar\nDescription: We perform optical photometric and polarimetric monitoring of a sample of gamma-bright blazars using 0.7-m AZT-8 telescope (Crimean Astrophysical Observatory), within the frames of GASP/WEBT project. We report that the blazar AO 0235+16 (z=0.94) reached R=16.55 in the night of 2020 August 07, TJD 59069.53. That is the highest brightness level of AO0235+16 for the last 3 observing seasons, as compared to the quiescence level of 18-19 mag. R band light curve for AO 0235+16 can be seen on our web-page. The polarization degree during last nights varies between 3 and 11%. Current high activity state of this blazar deserves close attention in all wavelengths.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Globular cluster", "Black hole, Quasar", "Black hole, Galaxy", "Black hole, Accreting object" ] }, "answerKey": "B" }, { "id": "atel_14050", "message": "Title: BL Lac at Brightest NIR Light\nAuthors: L. Carrasco, G. Escobedo, A. Porras, E. Recillas, V. Chavushyan, Y. D. Mayya (INAOE, Mexico)\nDate: 29 Sep 2020; 18:05 UT\nProvenance: LUIS CARRASCO (carrasco@inaoep.mx)\nSubjects: Radio, Infra-Red, Optical, Gamma Ray, AGN, Black Hole, Quasar\nDescription: We report on a recent NIR flare of BL Lac, associated with the Gamma ray source 2FGLJ2202.8+4216 (z = 0.0686). On September 6th,2020 (JD, 2459098.89) we obtained NIR photometry for this object and found it with enhanced fluxes, corresponding to: J = 10.356 +/- 0.02, H = 9.503 +/- 0.02 and Ks = 8.619 +/- 0.03. Our previous photometry for this object on JD2458881.6 yielded fainter fluxes by a factor of 2.2. The present flare has reached the brightest flux levels since we started monitoring this object on JD 2454358. Our observations are carried out with the 2.1m telescope of the Guillermo Haro Observatory operated by the National Institute for Astrophysics, Optics and Electronics (Mexico), equipped with the instrument CANICA a NIR camera. We strongly encourage further multiwavelength coverage.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Stellar evolution, Quasar", "Star and stellar system, Black hole, Quasar", "Active galactic nucleus, Black hole, Accreting object", "Active galactic nucleus, Black hole, Quasar" ] }, "answerKey": "D" }, { "id": "atel_14150", "message": "Title: Spectroscopic classification of AT2020yky as a nova in M31\nAuthors: Monika Soraisam (NCSA/UIUC), Kevin McKinnon, Rafael Nunez, Puragra Guhathakurta, Stephanie Figuereo (UCSC), Chien-Hsiu Lee (NOIR Lab), Sarah DeSantis (Steward), Tim Marquez (UCSB), Kareem El-Badry (UCB)\nDate: 5 Nov 2020; 03:07 UT\nProvenance: Monika Soraisam (soraisam@illinois.edu)\nSubjects: Optical, Cataclysmic Variable, Nova\nDescription: Referred to by ATel #: 14212\nWe report the spectroscopic observation of AT2020yky/ZTF20acoqrpm (RA 0h42m20.17s, DEC +41d14m28.16s) from the SALVATION project. The source was flagged from the ZTF public alert stream as a transient candidate in M31 by the ANTARES broker (https://antares.noirlab.edu/loci/ANT2020aevgxui) on 2020 Nov 2 UT (see also https://wis-tns.weizmann.ac.il/object/2020yky). \nOn 2020 Nov 3 UT, we obtained the spectrum of this source with the Kast double spectrograph on the Shane 3 m telescope at Lick Observatory. The spectrum shows Balmer emission lines, with the FWHM of the H-alpha line around 1400 km/s, as well as O I with a P Cygni profile. The source is thus likely a nova in M31. \nWe thank the staff of Lick Observatory for their help in executing our ToO observation.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Star and stellar system", "Supernova", "Nova", "Neutron star" ] }, "answerKey": "C" }, { "id": "atel_14280", "message": "Title: Continued Swift observations of the flat spectrum radio quasar PKS 1127-14\nAuthors: Filippo D'Ammando (INAF-IRA Bologna)\nDate: 18 Dec 2020; 18:07 UT\nProvenance: Filippo D'Ammando (dammando@ira.inaf.it)\nSubjects: Optical, Ultra-Violet, X-ray, AGN, Black Hole, Blazar, Quasar\nDescription: Referred to by ATel #: 15385\nFollowing the initial Swift observations of the flat spectrum radio quasar PKS 1127-14 at redshift z = 1.184 (Wilkes 1986, MNRAS, 218, 331), after the gamma-ray flare detected by Fermi-LAT, and performed on 2020 December 13 (ATel #14265), further Swift observations were obtained on December 15 and 17. \nSwift-XRT data were taken in Photon Counting mode for a net exposure of about 1.6 ksec and 1.9 ksec on December 15 and 17, respectively. The X-ray spectrum (0.3-10 keV) observed on 2020 December 15 and 17 can be fit by an absorbed power law model with a HI column density consistent with the Galactic value in the direction of the source (n_H = 3.5 x 10^20 cm^-2, Ben Bekhti N. et al., 2016, A&A, 594, A116) and a photon index of 1.1 +/- 0.2 and 1.2 +/- 0.2, comparable within the uncertainties to the photon index observed on December 13. The corresponding (observed) 0.3-10 keV fluxes are (9.3+/-0.9) x10^-12 erg cm^-2 s^-1 and (8.4 +/- 0.7) x10^-12 erg cm^-2 s^-1, respectively, indicating a flux level only slightly lower than the flux on December 13, but still high. \nSimultaneous Swift-UVOT observations were performed on 2020 December 15 and 17. The measured magnitudes in optical and UV bands show a brightness level similar to what is observed on December 13 (see table below). \nBand | 2020-12-15 | 2020-12-17 \n---|---|--- \nV | 16.75 +/- 0.11 | 16.71 +/- 0.09 \nB | 17.13 +/- 0.08 | 17.02 +/- 0.07 \nU | 16.05 +/- 0.05 | 16.04 +/- 0.06 \nW1 | 15.84 +/- 0.07 | 15.77 +/- 0.07 \nM2 | 15.92 +/- 0.08 | 15.95 +/- 0.07 \nW2 | 16.18 +/- 0.07 | 16.15 +/- 0.07 \nIn consideration of the ongoing activity of this source, confirmed also by the Swift observations, we encourage further multi-wavelength observations. \nWe would like to thank the Swift Team for making these observations possible, in particular B. Sbarufatti as the Swift Observatory Duty Scientist.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Pulsar", "Minor body", "Magnetar", "Quasar" ] }, "answerKey": "D" }, { "id": "atel_14350", "message": "Title: Swift follow-up observations of BL Lacertae during a new flaring activity\nAuthors: Filippo D'Ammando (INAF-IRA Bologna)\nDate: 26 Jan 2021; 17:38 UT\nProvenance: Filippo D'Ammando (dammando@ira.inaf.it)\nSubjects: Optical, Ultra-Violet, X-ray, AGN, Black Hole, Blazar, Quasar\nDescription: Referred to by ATel #: 14467\nAfter the recent optical and gamma-ray flaring activity of the blazar BL Lacertae (ATel #14318, #14328, #14330, #14334), significant variability in brightness has been observed in X-rays by NICER during 2021 January 18-22 (ATel #14342). Following this activity, Swift target of opportunity observations were performed on 2021 January 25. \nSwift-XRT data were taken in Photon Counting mode for a net exposure of about 1.0 ksec. Preliminary analysis has been performed fitting the 0.3-10 keV X-ray spectra with an absorbed power-law with a photon index of 2.25 +/- 0.11 and the Galactic absorption corresponding to a hydrogen column density of n_H = 2.7 x 10^21 cm^-2, in agreement with the value obtained by the analysis of the joint NICER and NuSTAR spectrum obtained on 2020 October 11-12 (ATel #14096). The X-ray (0.3-10 keV) flux observed (i.e. not corrected for Galactic extinction) is (1.4+/-0.1) x10^-10 erg cm^-2 s^-1, a factor of 2.5 lower than the historical maximum observed in X-rays on 2020 October 6 (ATel #14069) but higher than all other fluxes observed for this source so far (ATel #14065). \nSwift-UVOT observations performed on 2021 January 25 found BL Lacertae at a similar brightness level with respect to the values observed on 2020 October 5 and 6 in the optical filters, and approximately 0.4-0.5 magnitude less bright in the UV filters. The observed magnitudes are V = 12.39 +/- 0.04, B = 13.19 +/- 0.05, U = 12.67 +/- 0.05, W1 = 13.26 +/- 0.06, M2 = 13.91 +/- 0.06, and W2 = 13.91 +/- 0.06. \nIn consideration of the ongoing activity of this source, confirmed also by the Swift observations, we encourage further multi-wavelength observations. \nWe would like to thank the Swift Team for making these observations possible, in particular K. L. Page, as the Swift Observatory Duty Scientist.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Pulsar", "Minor body", "Accreting object" ] }, "answerKey": "A" }, { "id": "atel_14475", "message": "Title: Palomar Gattini-IR classification of a new highly reddened symbiotic star in outburst\nAuthors: K. De (Caltech), D. Stern (JPL), L. Hillenbrand (Caltech), M. M. Kasliwal (Caltech), M. Hankins (Arkansas Tech), J. Jencson (Arizona), J. Sokoloski (Columbia), M. Ashley (UNSW), A. Babul (Columbia), V. Karambelkar (Caltech), R. M. Lau (ISAS/JAXA), A. Moore (ANU), E. O. Ofek (Weizmann), M. Sharma (Columbia), J. Soon (ANU), R. Soria (NAOC), T. Travouillon (ANU) on behalf of the Palomar Gattini-IR team\nDate: 19 Mar 2021; 19:59 UT\nProvenance: Kishalay De (kde@astro.caltech.edu)\nSubjects: Infra-Red, Optical, Cataclysmic Variable, Star, Transient, Variables\nDescription: We report the classification of a highly reddened transient detected by the Palomar Gattini-IR survey (Moore & Kasliwal 2019; De et al. 2020). The source was identified as part of an ongoing campaign to find large amplitude Galactic plane transients (De et al. 2021). \n \nThe source PGIR 20djo was first saved as a nova candidate in April 2020 at a magnitude of J = 13.1 +/- 0.2 Vega mag, and at coordinates \n \nRA = 19:03:56.2; Dec = +09:01:58.5 \n \nfollowing a brightness increase of ~ 1.5 mag from the template image. Low amplitude variability is detected dating back to the start of the survey in 2019. The source is coincident with a red source in PS1 images, with a r-band magnitude of ~ 20 mag. The source did not brighten subsequently during 2020. \n \nThe source re-appeared significantly brighter after solar conjunction in 2021 as a magnitude of J = 11.3 Vega mag, assigned for follow-up and reported to the Transient Name Server as AT 2019aajn. The 2021 brightening was also detected in ZTF data (Bellm et al. 2019; Masci et al. 2019) as ZTF18aaywchl, which shows a long lived outburst starting as early as 2018. The source was also reported in ATel #14376 as DDE 175, and is characterized by a red color of g - J ~ 7 mags. \n \nWe obtained an optical spectrum of the source with the Double Spectrograph on the Palomar 200-inch telescope. The spectrum shows a very red continuum superimposed with strong Balmer emission lines, and emission lines of He II, O I, Fe II and Ca II. We also detect likely absorption features of TiO near 8500 - 9000 Angstroms. Overall, the spectrum and light curve is consistent with a new reddened symbiotic star in outburst. \n \nWe encourage follow-up in all bands, in particular, the near-infrared given the highly reddened nature of the source.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Binary system", "Star and stellar system, Pulsar", "Star and stellar system, Interstellar medium", "Star and stellar system, Binary system" ] }, "answerKey": "D" }, { "id": "atel_14550", "message": "Title: Swift Bulge Survey: Follow-up observations of the transient source Swift J174038.1-273712\nAuthors: Rivera Sandoval, L. E., Heinke, C. O. (U. Alberta), Maccarone, T. (TTU), Shaw, A.(U. Nevada, Reno), Sivakoff, G. (U. Alberta) on behalf of the SBS team \nDate: 15 Apr 2021; 03:51 UT\nProvenance: Liliana Rivera Sandoval (lriveras@ualberta.ca)\nSubjects: X-ray, Transient\nDescription: Referred to by ATel #: 14552, 14626\nWe report Neil Gehrels Swift Observatory follow-up observations of the recently discovered transient source Swift J174038.1-273712 (Atel #14536, #14545), towards the Galactic bulge. The transient has decayed by less than a factor of 2 over 5 days, suggesting that it has already peaked in Lx, but that it is not rapidly decaying. \nObservations were obtained on 2021-04-14 with a total exposure time of 635s. Fitting the X-ray spectrum of the source with an absorbed power-law where N_H is fixed to the Galactic value of 5.5E21 cm^-2 and using the Cash statistics, we have obtained a power-law photon index of 1.5(+/-0.3) and a X-ray flux of 1.9(+0.4/-0.3)*1E-11 erg/s/cm^2 in the 0.5-10 keV band. There are too few counts in the Swift spectrum to fit the absorbed (blackbody+thermally comptonized continuum) model indicated by the NICER data. This flux is slightly fainter than the 0.5-10 keV flux measured by Swift [3.2(+2.3/-1.1)*1E-11 erg/s/cm^2, Atel #14536] at about 2021-04-08 20:06 (the 2021-04-09 date reported by Atel #14536 was the last time of the Bulge survey fields). Approximately 19 hours later, the flux measured by NICER [1.5(+/-0.2)*1E-11 erg/s/cm^2 0.5-10 keV, Atel #14545] is consistent with the Swift flux from 2021-04-14. It is possible that NICER's absolute flux could be slightly incorrect, as it is not an imaging instrument and this is a faint source in a crowded field. It is unclear whether this transient may have had a relatively bright outburst that peaked before our initial observations, but INTEGRAL data of this region may constrain this scenario.\nNeither 2021-04-14 UVOT observations of the field in the UVM2 filter, nor archival UVOT images in the same filter, reveal any source at the position of Swift J174038.1-273712. Further Swift observations are planned.\nWe thank the Swift team for scheduling our ToO request.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Nova, Variable star", "Accreting object, Variable star", "Accreting object, Interstellar medium", "Accreting object, Nova" ] }, "answerKey": "B" }, { "id": "atel_14610", "message": "Title: Non-detection of optical counterpart of Chandra Fast X-ray Transient FXT 210423 by Xinglong 2.16m telescope\nAuthors: L. P. Xin (NAOC), J. Wang (GXU/NAOC), J. Y. Wei (NAOC)\nDate: 7 May 2021; 08:24 UT\nProvenance: Weikang Zheng (zwk@umich.edu)\nSubjects: Optical, X-ray, Transient\nDescription: Referred to by ATel #: 14735\nThe field of FXT 210423 (Lin et al., ATel #14599) has been observed by NAOC 2.16m telescope at Xinglong observatory, China. The observations started at 12:44:10 UT. 4* 300 sec I-band images were obtained. The limiting magnitude is 20.0 mag in the single images and 20.5 mag in stacked image. There is no any sources at the location of FXT 210423 (Lin et al., ATel #14599). We thank the 2.16m operator assistants and duty astronomer for this observation.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus", "Quasar", "Variable star", "Supernova" ] }, "answerKey": "C" }, { "id": "atel_14670", "message": "Title: Correction to ATel 14663 and the recent time evolution of the X-ray flux from 4U 1705-32\nAuthors: H. Negoro, M. Nakajima (Nihon U.), W. Iwakiri (Chuo U.), M. Ishikawa (JAXA), K. Kobayashi, K. Asakura, K. Seino (Nihon U.), T. Mihara, T. Tamagawa, M. Matsuoka (RIKEN), T. Sakamoto, M. Serino, S. Sugita, K. Komachi, A. Yoshida (AGU), Y. Tsuboi, H. Kawai, Y. Okamoto, S. Kitakoga (Chuo U.), M. Shidatsu (Ehime U.), N. Kawai, M. Niwano, R. Hosokawa (Tokyo Tech), S. Nakahira, Y. Sugawara, S. Ueno, H. Tomida, M. Tominaga, T. Nagatsuka (JAXA), Y. Ueda, S. Yamada, S. Ogawa, K. Setoguchi, T. Yoshitake, Y. Goto, R. Uematsu (Kyoto U.), H. Tsunemi (Osaka U.), M. Yamauchi, Y. Nonaka, T. Sato, R. Hatsuda, R. Fukuoka (Miyazaki U.), T. Kawamuro (UDP/NAOJ), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC) report on behalf of the MAXI team:\nDate: 30 May 2021; 14:34 UT\nProvenance: Hitoshi Negoro (negoro@phys.cst.nihon-u.ac.jp)\nSubjects: Neutron Star, Transient\nDescription: We further report on the time evolution of the X-ray flux from the low-mass X-ray binary 4U 1705-32, which brightened rapidly on May 24 (Negoro et al. ATel #14663, Bult et al. ATel #14669). MAXI/GSC data show that the 4-10 keV X-ray flux started decreasing prior to the 2-4 keV X-ray flux on May 25, implying a soft state transition (#14663), and the 2-4 keV X-ray flux rapidly decreased on May 27. The 2-10 keV flux was below the 1-day detection of about 5 mCrab (1-sigma) on May 28 as reported by Bult et al. (ATel #14669). At 23:49 on May 29, the MAXI/GSC nova alert system triggered on the source again, and we confirmed the 4-10 keV flux increased to about 30 mCrab. The 2-4 keV flux is not significantly detected, yet. \n \nAll the months written in ATel #14663 should be May, not March. We apologize for any inconvenience caused by our mistake.\nMAXI trigger information on 4U 1705-32", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Pulsar", "Interstellar medium", "Neutron star", "Black hole" ] }, "answerKey": "C" }, { "id": "atel_14760", "message": "Title: OHP spectroscopic observations of AT2021, candidate Nova in M31\nAuthors: M. Dennefeld (IAP/Paris and Sorbonne University), J. Schmitt, St. Favard, J. Hornstein (OHP and Osu-Pytheas) and C. Adami (LAM)\nDate: 6 Jul 2021; 23:39 UT\nProvenance: Michel Dennefeld (dennefel@iap.fr)\nSubjects: Optical, Nova\nDescription: We observed at Haute-Provence Observatory (OHP, CNRS, France) the candidate Nova in M31, PNV 00424717 +4118173 = AT 2021scc (Hornoch et al., ATel 14753) on July 6th, 01h50UT, with the new spectro-imager Mistral during its last test runs at the 1.93m telescope. The wavelength coverage was 410-810nm and the spectral resolution 0.05nm per pixel (4 pixels for a 2\" slit). The continuum is well detected on the two 900sec exposures obtained in good observing conditions, but the only emission line seen is Halpha at about -100km/s. Halpha displays a clear PCygni profile, indicating an expansion velocity of about -550 km/s. As the object seemed to be brighter on the acquisition image than on the finding chart of Hornoch et al., it might still be in an early phase and would deserve further observations.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Magnetar", "Circumstellar disk", "Stellar evolution", "Nova" ] }, "answerKey": "D" }, { "id": "atel_14820", "message": "Title: BL Lac reaches a new optical all-time maximum\nAuthors: Lukas Kunkel, Adrian Scherbantin, Karl Mannheim (all Universitaet Wuerzburg), Fiona Kaplan, Niels Bader, Erik Heidemann, Felix Hemrich, Ben Horst, Alexander Lessing, Jonas Ludwig, Felix Molz, David Reinhart, Korbinian Rosenlehner, Kilian Schoch, Remco Steineke, Lukas Waller, Nils Zottmann, Martin Feige, Christian Lorey (all Friedrich-Koenig-Gymnasium / Hans-Haffner-Sternwarte), Dominik Elsaesser (TU Dortmund)\nDate: 31 Jul 2021; 07:18 UT\nProvenance: Dominik Elsaesser (dominik.elsaesser@tu-dortmund.de)\nSubjects: Optical, AGN, Blazar\nDescription: Referred to by ATel #: 14826, 14839, 14854\nSince BL Lac's major brightness outburst in the summer of 2020, we have observed a flare from this object roughly every three to three and a half months, each time reaching an even greater maximum brightness in the optical spectral range. \nThe current outbreak began in early July 2021 (ATel #14751, ATel #14773) and has been observed in different wavelength bands (ATel #14774, ATel #14777, ATel #14782, ATel #14783). \nTonight we measured a rapid increase in optical brightness (R-Band) from 11.433 ± 0.004 mag (21:30 UTC - JD 2459426.3956) to 11.315 ± 0.003 mag (22:12 UTC - JD 2459426.4252). Over the next hour and a half, the brightness then slowly increased (with fluctuations) to 11.271 ± 0.003 mag (23.50 UTC - JD 2459426.4930), which is a new all-time high state for this AGN, as far as our coverage is concerned. By dawn in Hettstadt, the brightness slowly decreased to 11.444 ± 0.008 mag (02:44 UTC - JD 2459426.6142). \n \nWe are using Bessel filters and for the aperture photometry we are using the specifications of the GASP list of WEBT (https://www.oato.inaf.it/blazars/webt/gasp/fc/2200fc.html). \n \nWe strongly encourage further observations of this record optical flare. \n \nThese measurements are carried out as part of the long-term AGN monitoring program of the Naturwissenschaftliches Labor fuer Schueler am Friedrich-Koenig-Gymnasium (FKG), the Universitaet Wuerzburg, and TU Dortmund with the 0.5m CDK-astrograph at the school and university observatory Hans-Haffner-Sternwarte in D-97265 Hettstadt (Germany). \n\nNATUR­WISSEN­SCHAFT­LICHES LABOR FÜR SCHÜLER AM FKG E.V.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Binary system", "Star and stellar system", "Active galactic nucleus" ] }, "answerKey": "D" }, { "id": "atel_14910", "message": "Title: Further Infrared Spectroscopy of RS Oph on day +34 reveals Coronal Line Emission\nAuthors: C. E. Woodward (U. Minnesota), D. P.K. Banerjee (PRL, India), A. Evans (Keele U., UK), S. Starrfield (Arizona State U.), R. M. Wagner (Ohio State U.), R. D. Gehrz (U. Minnesota)\nDate: 12 Sep 2021; 19:37 UT\nProvenance: C.E. Woodward (chickw024@gmail.com)\nSubjects: Infra-Red, Nova\nDescription: Low resolution (R = 1200) near-infrared (0.70 to 2.54 micron) spectroscopy of RS Oph (ATEL#14909, #14908, #14906, #14901, #14883, #14881 among others) obtained with SpeX (Rayner et al. 2003, PASP 115, 362) in short crossed-dispersed (SXD) mode on 2021 Sept 11.221 UT (approximately day +34 after eruption) on the NASA IRTF 3.2-m under good sky conditions (seeing 0.6 arcsec in the K-band) show that infrared coronal line emission (see Benjamin and Dinerstein 1990, AJ 100, 1588; Greenhouse et al. 1998, ApJ 352, 307) is now evident. In addition, the FWHM of the hydrogen emission lines are narrowing, and the red-wing asymmetries and saddle-shaped line profile peaks are disappearing (see ATEL#14866). The broad, blended emission complexes seen on day+12 (ATEL# 14866) now are resolving into individual line components, and multiple He II emission lines are now strong. Infrared coronal lines present, and representative observed fluxes (erg/s/cm2) include [S VIII] 0.9914 micron (2.8e-11), [S IX] 1.253 micron (3.4e-11), [Si X] 1.4305 micron (2.5e-11), [Si VI] 1.9650 micron, and [Si VII] 2.4833 micron (1.4e-11), with all wavelengths in vacuum. Also present is the line emission feature at 2.090 micron whose identification remains elusive. These latter detections substantiate reports of the detection of [Ne V] 0.3427 micron and coronal [FeX] 0.6375 micron lines by Munari et al. (ATEL#14895) just prior to the onset of the super-soft source (SSS) x-ray phase near 2021 September 04, as communicated by Page et al. (ATEL#14894) based on Neil Geherls SWIFT XRT observations. Currently, at the epoch of these latest SpeX observations discussed herein, the FWHM of the H emission lines (derived from the Br-series 19 to 9 lines in the H-band) exhibit an average velocity of 610 km/s. The observed fluxes (gaussian fit, erg/s/cm2) of Pa-β and Br-γ are 3.6e-10 and 6.5e-11, respectively while that of He I 10830 is 2.1e-9. Interestingly, the 12C16O band heads from 2.29 micron onwards, arising from the red giant secondary, are being detected very much earlier than in the 2006 outburst (they were not seen even on day 55; Evans et al. 2007, MNRAS 374, L1). We are examining whether the approximately 0.5 difference in the orbital phase of the red giant between the 2006 and 2021 eruptions (estimated using the ephemerides of Brandi et al. 2009, A&A 497, 815), could be responsible for the early appearance of the CO features in the current outburst. Clearly further infrared spectroscopic observations are encouraged. \nThe investigators are grateful to the NASA IRTF for providing the quick-access DDT opportunity (2021B996), and we thank the observatory staff for their assistance.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Repeater", "Supernova", "Nova", "Binary system" ] }, "answerKey": "C" }, { "id": "atel_15000", "message": "Title: NICER follow-up observations of the flaring blazar TXS 0646-176\nAuthors: Filippo D'Ammando (INAF-IRA Bologna) and Giulia Migliori (INAF-IRA Bologna)\nDate: 26 Oct 2021; 15:48 UT\nProvenance: Filippo D'Ammando (dammando@ira.inaf.it)\nSubjects: X-ray, AGN, Black Hole, Blazar, Quasar\nDescription: Following the recent gamma-ray flaring activity of the flat spectrum radio quasar TXS 0646-176 (ATel #14980, ATel #14981, ATel #14993), the source has been observed by NICER for a ToO request (NICER GO Cycle 3 ID: 4115, PI: D'Ammando) between 2021 October 19 21:08 UTC and October 25 05:53 UTC for an effective time of 61.5 ks. \nThe source is detected above the background across the energy interval 0.5-6.0 keV in the quick look data, with an average count rate of 2.0 counts/s. Variations of the count rate up to a factor of 2.5 has been observed across the observation, with possible short flares. \nPreliminary analysis shows that the NICER spectrum collected over the entire period in the 0.5-6.0 keV energy range can be described by an absorbed power-law model with a HI column density consistent with the Galactic value in the direction of the source (n_H = 2.37 x 10^21 cm^-2, Ben Bekhti et al., 2016, A&A, 594, A116) and a photon index of 1.22 +/- 0.01. The corresponding (observed) 0.3-10 keV flux is (7.9 +/- 0.1)e-12 erg cm^-2 s^-1. The photon index is similar to the ones reported for the X-ray observations carried out by Swift-XRT (ATel #14987) and SRG/eROSITA (ATel #14991) on 2021 October 18 and 2021 October 14-15, respectively. The X-ray flux estimated by NICER over the period 2021 October 19-25 is slightly lower than the values recently observed by Swift-XRT and SRG/eROSITA. \nIn consideration of the ongoing activity of this source, confirmed also by optical observations performed by REM (ATel #14999), we encourage further multi-wavelength observations. \nWe thank the NICER PI, Keith Gendreau, and the operation team for the rapid approval and execution of the ToO request. NICER is a 0.2-12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Pulsar, Quasar", "Neutron star, Quasar", "Black hole, Quasar", "Stellar evolution, Quasar" ] }, "answerKey": "C" }, { "id": "atel_15120", "message": "Title: LJT spectroscopic classification of AT 2021aghl as a relatively young Type Ia supernova\nAuthors: Liping Li (Yunnan University); Jujia Zhang, Qian Zhai (YNAO); Xiaofeng Wang(THU)\nDate: 17 Dec 2021; 01:59 UT\nProvenance: Ju-Jia Zhang (jujia@ynao.ac.cn)\nSubjects: Optical, Supernovae\nDescription: We report an optical spectrum of AT 2021aghl (350-870nm) that was obtained on 2021 Dec. 16.75 UT with the Lijiang 2.4-m telescope (LJT +YFOSC) at LiJiang observatory of Yunnan Observatories. The spectrum is similar to that of a type Ia supernovae at a few days before the maximum light. Cross-correlation with the library of supernova spectra using the comparison tool SNID (Blondin and Tonry 2007, ApJ, 666, 1024) shows that it matches with SN 2003du at t = -9 days. Given a redshift of 0.045 derived by narrow H-alpha emission of the host galaxy, an expansion velocity of about 13000 km/s can be deduced from the Si II 635.5 absorption minimum.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Stellar evolution", "Galaxy", "Supernova", "Magnetar" ] }, "answerKey": "C" }, { "id": "atel_15225", "message": "Title: AT2019cuk/SDSSJ1430/ZTF18aarippg: High-cadence NICER and NuSTAR X-ray observations of the potential supermassive black hole binary with imminent merger (the tick-tock source)\nAuthors: Dheeraj Pasham (MIT), Andrew Fabian (U. Cambridge), Dom Walton (U. Hertfordshire), Keith Gendreau (NASA/GSFC), Zaven Arzoumanian (NASA/GSFC), Megan Masterson (MIT), Erin Kara (MIT), Ron Remillard (MIT)\nDate: 17 Feb 2022; 03:59 UT\nProvenance: Dheeraj Pasham (drreddy@mit.edu)\nSubjects: X-ray, AGN, Transient\nDescription: The nuclear optical transient AT2019cuk/SDSSJ1430+2303/ZTF18aarippg was identified by ZTF on 30 March 2019. Based on its optical modulations with apparently decreasing period and unusual optical emission line shifts over the last 2.5 years, it has been suggested to be a supermassive black hole (SMBH) binary that could merge within the next three years (Jiang et al. 2022). While the probability of finding such a system within <1 Gpc is very low, the scientific potential of studying a bonafide SMBH binary close to coalescence is large. \nNICER has been monitoring AT2019cuk since 19 Jan 2022 on a daily basis and has carried out multiple visits over a few days to coordinate with a 114 ks NuSTAR exposure. NICER is detecting the source in the 0.3-4.0 keV with background-subtracted count rates between 1.7 and 3.5 counts/sec. NuSTAR's 3-70 keV count rate was 0.07 cps with no obvious variability over the 220 ks observation period. \nThe NICER light curve so far has covered a baseline of 24 days and has a modulation roughly consistent with the ~30 d Swift/XRT modulation (Jiang et al. 2022). The overall flux gradually increased by a factor of 2, peaked at roughly 30 d since the last maximum seen in Swift/XRT data, and dropped back in the last week (see https://space.mit.edu/~dheeraj/cuk.html). Data over a much longer baseline will be needed to validate this potential period, since red noise variations can easily produce such apparently periodic modulations. \nX-ray spectral fits for an accretion disk with reflection can provide geometrical information about the observer's line of sight, which may vary systematically with time for this system. We fit the 7-70 keV NuSTAR spectrum with a power law modified by Galactic absorption (2.3e20 cm^-2). Extrapolating this model over the entire 0.3-70 keV band (0.3-4 keV NICER and 3-70 keV NuSTAR) shows several features in the data/model plot: 1) systematic residuals between 0.3-1 keV, 2) emission line reminiscent of a relativistically broadened Fe line between 4.5-7 keV, and 3) a Compton hump-like feature above 10 keV. We then jointly fit the combined spectrum with a model consisting of X-ray reflection (using relxill; Garcia et al. 2014) plus a more distant, partially covering warm absorber (using XSTAR; Kallman & Bautista 2001). This model gives a good fit (joint chi-square of 303/347 DoF), reflection is preferred, although is relatively weak, with a reflection fraction of R = 0.19(+0.12 -0.07); 90% uncertainties. Fits without reflection (i.e., AGN continuum and warm absorber) are worse by delta-chisq = 32 for 4 fewer DoF. The reflection is highly ionized, with log[xi] = 3.0(+0.2 -0.1), suggesting an accretion disk origin. We find an inner radius of Rin = 7+/-3 Rg and an inclination of i < 21 deg (assuming a fixed powerlaw emissivity with q=3). The ionized absorption has a column density and ionization parameter of Nh = 2.6(+0.8,-0.9)e22 cm^-2 and log[xi/(erg cm/s)]=1.56(+0.16 -0.26), fairly typical of AGN warm absorbers (e.g., Laha et al. 2014). The covering factor is Cf = 0.44 +/- 0.04. The intrinsic continuum also appears to be fairly typical, with Gamma = 1.76(+0.03 -0.10) and Ecut > 140 keV (Ricci et al. 2017). \nNICER will continue monitoring AT2019cuk on a daily basis for the next several months as part of a GO program. We encourage follow-up observations of this potentially very exciting target. A weekly updated schedule can be found here: https://heasarc.gsfc.nasa.gov/docs/nicer/schedule/nicer_sts_current.html. To coordinate multiwavelength observations please contact drreddy@mit.edu \nNICER carries out prompt follow-up observations of X-ray-bright extragalactic transients and tracks alerts from LIGO/VIRGO and other facilities. NICER is a 0.2-12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA. Jiang, N., Yang, H., Wang, T., et al. 2022, arXiv:2201.11633", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole", "Neutron star", "Pulsar", "Near-Earth object" ] }, "answerKey": "A" }, { "id": "atel_15275", "message": "Title: LJT spectroscopic classification of AT 2022erq as a young SN 2005gj-like supernova\nAuthors: Liping Li (Yunnan University); Qian Zhai, Jujia Zhang(YNAO); Xiaofeng Wang(THU)\nDate: 13 Mar 2022; 07:58 UT\nProvenance: Ju-Jia Zhang (jujia@ynao.ac.cn)\nSubjects: Optical, Supernovae\nDescription: We report an optical spectrum of AT 2022erq (350-870nm) obtained on 2022 Mar. 12.9 UT with the Lijiang 2.4-m telescope (LJT +YFOSC) at LiJiang observatory of Yunnan Observatories. The spectrum is similar to the Ia-csm/IIn event at the early phase, e.g., SN 2005gj = 12d after the explosion via Gelato (Harutyunyan et al. 2008) or SN 2005gj = -12d before the peak via SNID (Blondin & Tonry 2007). The photometric analysis matches the spectroscopic result. AT 2022erq was discovered at about 18.1 mag with ATLAS-cyan band on Mar. 11.6. The photometry obtained by LJT on Mar. 12.9 (g = 17.43 \\pm 0.02, r = 17.51\\pm 0.01, i = 17.62 \\pm 0.02) shows a fast-rising of this transient. Given the redshift z = 0.066 (from the H-Balmer emissions), the absolute magnitude of 2022erq is close to -20mag during LJT observation without reddening correction. The fast-rising and high luminosity consistent the light curve of SN 2005gj a few days before the peak.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Minor body", "Magnetar", "Supernova", "Repeater" ] }, "answerKey": "C" }, { "id": "atel_15375", "message": "Title: Fermi-LAT detection of renewed gamma-ray activity from the BL Lac S4 0954+65\nAuthors: B. Rani (KASI, S. Korea), J. Valverde (UMBC/NASA GSFC), and G. La Mura (LIP, Portugal), on behalf of the Fermi Large Area Telescope Collaboration\nDate: 11 May 2022; 20:00 UT\nProvenance: Janeth Valverde (valverde@llr.in2p3.fr)\nSubjects: Gamma Ray, >GeV, Request for Observations, AGN, Blazar\nDescription: Referred to by ATel #: 15380, 15399, 15517\nThe Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed renewed gamma-ray activity from a source positionally consistent with the BL Lac S4 0954+65, also known as 4FGL J0958.7+6534 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 149.696855 deg, Decl. = +65.565227 deg (J2000; Johnston et al., 1995, AJ, 110, 880), and redshift z=0.368 (Wills et al., 1992, ApJ, 398, 454). \nPreliminary analysis indicates that this source was in an elevated gamma-ray emission state on May 09, 2022, with a daily averaged gamma-ray flux (E>100MeV) of (1.8+/-0.2) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of more than 30 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL). This is the highest LAT daily flux ever observed for this source. The corresponding photon index is 2.01+/-0.08, smaller than the 4FGL value of 2.22+/-0.02. Two high-energy photons were detected from the source, with the maximum energy of 37 GeV. The flare triggered the Fermi-LAT Monitor alert system, which issued the GCN/Fermi_LAT_MON Notice (https://gcn.gsfc.nasa.gov/other/1652194322_fermi.txt). \nBecause Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue (https://fermi.gsfc.nasa.gov/ssc/data/access/lat/LightCurveRepository/source.html?source_name=4FGL_J0958.7+6534). We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is Felicia McBride (fe@femcbride.com). \nThe Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Black hole", "Nova, Black hole", "Interstellar medium, Black hole", "Magnetar, Black hole" ] }, "answerKey": "A" }, { "id": "atel_15450", "message": "Title: Swift Observations of the Extremely Luminous Quasar SMSS J114447.77-430859.3 \nAuthors: J. M. Miller (Univ. of Michigan), A. C. Fabian (Univ. of Cambridge)\nDate: 21 Jun 2022; 15:16 UT\nProvenance: Jon Miller (jonmm@umich.edu)\nSubjects: Ultra-Violet, X-ray, AGN, Black Hole\nDescription: Referred to by ATel #: 15452, 15510\nRecent observations with the SkyMapper Southern Survey (SMSS) identified SMSS J114447.77-430859.3 as the optically brightest unbeamed quasar at z > 0.4, and the most luminous known quasar of the last nine billion years of cosmic history (Onken et al. 2022). For a redshift of z = 0.83, optical data give a bolometric luminosity of L_bol = 4.7 +/- 1.0 E+47 erg/s, and suggest an Eddington ratio of 1.4 (mildly super-Eddington). \n \nSMSS J1144 was not detected in the ROSAT All-Sky Survey, and was not previously targeted with any modern imaging X-ray telescope. We therefore requested an observation with the Neil Gehrels Swift Observatory. A short observation was obtained on 21 June 2022, starting at 01:04:02 UTC. \n \nAn X-ray source is clearly detected that is coincident with SMSS J1144. Source events were extracted in a circular region with a radius of 24 arc seconds. Background events were extracted in a nearby region of the same size. A total of 39 source counts were recorded in 1068 seconds of exposure, compared to 3 background counts. Assuming an unabsorbed power-law spectrum with a power-law index of Gamma = 2.0, the corresponding count rate of 0.034 +/- 0.006 c/s gives a flux of F_X = 1.1 +/- 0.2 E-12 erg/cm^2/s (0.3-10.0 keV, observed frame). At the host redshift of z=0.83, this signals an luminosity of L_X = 3.9 +/- 0.7 E+45 erg/s. \n \nAn implied X-ray to bolometric luminosity ratio of L_X / L_bol ~ 0.008 is broadly consistent with other massive black holes accreting close to (or above) their Eddington limit. In this accretion regime, the hard X-ray corona in massive black holes appears to be largely quenched, similar to stellar-mass black holes in the \"high/soft\" state. Future observations with Chandra, XMM-Newton, and NuSTAR can determine the broadband X-ray spectrum of SMSS J1144. \n \nThe UVOT UVM2 filter has a central wavelength of 2246 A, and the smallest red leak of those aboard Swift. It therefore functions as the best measure of UV flux. A strong source is detected at the position of SMSS J1144. We measure a flux density of F_uvm2_nu = 1.63 +/- 0.03 E-14 erg/cm^2/s/A, a flux of F_uvm2 = 8.1 +/- 0.2 E-12 erg/cm^2/s, and a luminosity of L_uvm2= 2.9 +/- 0.1 E+46 erg/s. \n \nWe thank Brad Cenko, Jamie Kennea, Caryl Gronwall, and the Swift team for making this observation. \n \nReferences \n \nOnken, C., et al., 2022, PASA, submitted, arxiv:2206.04204", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object", "Quasar", "Neutron star", "Interstellar medium" ] }, "answerKey": "B" }, { "id": "atel_15510", "message": "Title: NuSTAR and Swift observations of SMSS J114447.770-430859.3\nAuthors: E. Kammoun (IRAP, Toulouse), J. M. Miller (Univ. of Michigan), A. C. Fabian (Univ. of Cambridge)\nDate: 11 Jul 2022; 09:10 UT\nProvenance: Elias Kammoun (ekammoun@irap.omp.eu )\nSubjects: X-ray, AGN, Black Hole, Quasar\nDescription: SMSS J114447.77-430859.3 (J1144) has been identified as the most luminous known non-jetted quasar in the last 9 Gyr of cosmic history (Onken et al. 2022), thanks to observations with the SkyMapper Southern Survey (SMSS). For a spectroscopic redshift of z = 0.83, optical data give a mass estimate of log (M_BH/M_sun) = 9.4 +/- 0.5 and a bolometric luminosity of L_bol = 4.7 +/- 1.0 E+47 erg/s. This suggests an Eddington ratio of 1.4 (mildly super-Eddington). J1144 was not detected with the ROSAT All-Sky Survey, and was not targeted by any of the modern X-ray observatories. A recent observation (ATel#15450, ATel#15452) with the Neil Gehrels Swift Observatory (Swift), allowed us to detect the source with an observed flux of F_obs = 1.5 +/- 0.5 E-12 erg/s/cm^2. We have recently observed the source with NuSTAR for a total of 60 ks starting 2022-06-28 20:35:13 UTC. The source is detected up to 30 keV in the observed frame (~55 keV, rest frame), with a net count rate of 0.023 count/s. No variability has been detected during the observation. We extracted the source spectrum using a 50 arc second (radius) region, and a separate background region of double this size. The spectra were re-binned to require a minimum signal-to-noise (S/N) ratio of 4. We fitted simultaneously the spectra obtained from each of the NuSTAR FPM detectors and the Swift XRT spectrum using an absorbed cutoff power law. In the XSPEC parlance the model can be written as follows: TBabs[1] * zTBabs[2] * zcutoffpl[3]. The first absorption component accounts for the Galactic absorption in our line of sight. The second component accounts for neutral absorption at the rest frame of the source. This results in a statistically acceptable fit of C-stat/dof = 126/125. The best fit equivalent hydrogen column density is 1.04_{-0.8}^{+1.1} E+22 cm^-2. The best-fit photon index, high-energy cutoff, and normalization are 1.6+/-0.3, 25_{-8}^{+24} keV, and 1.2_{-0.3}^{+0.6}E-3 photons/keV/cm^2/s, respectively. This is equivalent to an un-absorbed 2-10 keV luminosity of 4.9+/-0.6 E+45 erg/s. All uncertainties are reported at the 90% confidence range. We tested a model where we added a reflection component. However, this component was not required by the data. The NuSTAR observation confirmed the flux level of the source during the Swift observation that took place ~1 week earlier. A new Swift observation took place on 2022-07-04 05:36:00 (UTC), in which the source increased in flux by 50% which can be attributed to an increase in the intrinsic luminosity, reaching an F_obs = 2.36 +/- 0.76E-12 erg/s/cm^2. This is equivalent to an unabsorbed luminosity L = 8.5 +/- 2.1 erg/s in the 2-10 keV range. The soft X-ray spectra obtained by Swift show hints of absorption features, albeit with a low significance. Accounting for these features may alter the best-fit values of photon index and high-energy cutoff. However, a higher S/N spectrum in the soft X-rays is required in order to confirm the existence of such features and better constrain the spectral shape. We thank Fiona Harrison and the NuSTAR planning team for executing this observation. We also thank Swift for executing the ToO observations. References: Onken, C., et al., 2022, PASA, submitted, arxiv:2206.04204", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Quasar", "Neutron star, Quasar", "Globular cluster, Quasar", "Circumstellar disk, Quasar" ] }, "answerKey": "A" }, { "id": "atel_15600", "message": "Title: Detection of an optical outburst from Swift J1943.4+0228\nAuthors: Yuankun Wang (UW) and Eric C. Bellm (UW) on behalf of the Zwicky Transient Facility Collaboration\nDate: 8 Sep 2022; 20:34 UT\nProvenance: Eric Bellm (ecbellm@uw.edu)\nSubjects: Optical, Transient\nDescription: We report an optical brightening of the Galactic X-ray transient Swift J1942.4+0228 (Krimm et al. 2012, ATel #4049) with the Zwicky Transient Facility (ZTF; Bellm et al. 2019, Graham et. al 2019). ZTF detected the source (internally designated as ZTF22abcvwog) with image differencing at m_g ~ 19.3 +/- 0.05 on 2022-08-26.18. Forced photometry on the previous ZTF observation on 2022-08-24.2 showed the source at m_g ~21.1 +/- 0.2 and m_r ~20.3 +/- 0.09 either near quiescence or at early outburst. No source was detected in g-band images taken on 2022-08-22. No excess is apparent in the Swift-BAT daily lightcurves. \n \nThe source reached peak brightness during an apparent fast flare on 2022-08-30.2 at m_g ~ 18.67 +/- 0.03 and m_r ~ 18.60 +/- 0.02. The main profile of the outburst peaked earlier, on 2022-08-28.2 at m_r ~18.86 +/- 0.03. The source has begun to fade; the latest observations by ZTF on 2022-09-05.3 show the source at m_r ~ 19.67 +/- 0.12 and m_g ~ 19.73 +/- 0.13. Realtime public photometry may be obtained from alert brokers such as ANTARES, Lasair, or ALeRCE. \n \nBased on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Grant No. AST-2034437 and a collaboration including Caltech, IPAC, the Weizmann Institute for Science, the Oskar Klein Center at Stockholm University, the University of Maryland, Deutsches Elektronen-Synchrotron and Humboldt University, the TANGO Consortium of Taiwan, the University of Wisconsin at Milwaukee, Trinity College Dublin, Lawrence Livermore National Laboratories, and IN2P3, France. Operations are conducted by COO, IPAC, and UW. The ZTF forced-photometry service was funded under the Heising-Simons Foundation grant #12540303 (PI: Graham). We acknowledge further support from the NSF under grant AST-1812779 and the Heising-Simons Foundation under grant 2018-0908.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object, Black hole", "Nova, Black hole", "Neutron star, Black hole", "Variable star, Black hole" ] }, "answerKey": "C" }, { "id": "atel_15720", "message": "Title: Redshift of the candidate host galaxy of FRB 20220912A\nAuthors: Vikram Ravi, Viraj Karambelkar, Tomas Ahumada Mena, Christoffer Fremling (Caltech) on behalf of the DSA-110 team\nDate: 26 Oct 2022; 00:46 UT\nProvenance: Vikram Ravi (v.vikram.ravi@gmail.com)\nSubjects: Radio, Optical, Fast Radio Burst\nDescription: Referred to by ATel #: 15791, 15806\nWe report a spectroscopic redshift measurement of the candidate host galaxy of FRB 20220912A, PSO J347.2702+48.7066 (ATel #15679, ATel #15716). We obtained a low-resolution spectrum of this galaxy with the LRIS instrument on the Keck I telescope on 2022 October 19 UTC. A single 300s exposure was conducted. Several emission lines were detected at a redshift of 0.077, including H-alpha, H-beta, and strong lines of [OII], [OIII], [NII], and [SII].", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Accreting object, Active galactic nucleus", "Galaxy, Magnetar", "Galaxy, Active galactic nucleus", "Galaxy, Nova" ] }, "answerKey": "C" }, { "id": "atel_15825", "message": "Title: NICER, Swift and ZTF identify further X-ray and optical brightening of the ongoing changing-look AGN AT2021fxu\nAuthors: Yukta Ajay (IISER Tirupati), Dheeraj Pasham (MIT), Muryel Guolo (JHU)\nDate: 24 Dec 2022; 17:52 UT\nProvenance: Dheeraj Pasham (drreddy@mit.edu)\nSubjects: Optical, X-ray, AGN, Transient\nDescription: AT2021fxu/ZTF21aalxxzn/Gaia22dgm is an optical transient identified by the Zwicky Transient Facility on 13 February 2021 09:06:19 UT, classified as an AGN at a redshift of 0.1097 (Newsome et al., 2022). It had previously been cataloged by the BAT AGN Spectroscopic Survey as an AGN (2MASX J13471874+0210579/SWIFT J1347.7+0212) (Koss et al., 2017). A comparison of the optical spectra from the Sloan Digital Sky Survey (SDSS) in 2001 and the Faulkes Telescope North (FTN) in 2022 revealed the appearance of previously absent broad emission lines (BELs) in the recent FTN spectrum. This suggests a shift in the spectral class of the AGN, from Type-II to Type-I, indicative of a changing-look (CL) AGN. \nAT2021fxu showed an optical outburst in 2022, with an optical rise spanning 1 April 2022 to 27 May 2022, followed by an optical decline until 19 July 2022. During the optical decline, Swift/XRT and NICER carried out multiple observations of the source, and the X-ray spectra are consistent with a simple powerlaw model (powerlaw index ~1.8). No change in the neutral column density since 2011 implied that the spectral transition occurred due to a change in accretion rate, and not because of variable obscuration along our line-of-sight. Furthermore, the optical g- and r- magnitudes of the source remained approximately the same from 2000, until 2021, which confirmed that the optical outburst in 2022 coincided with the CL transition in the AGN, and that AT2021fxu is currently undergoing its spectral transition (see Ajay et al. 2022, RNAAS for more details). \nAfter a decay of ~0.34 and ~0.2 magnitudes in the optical g- and r- over about 2 months after the first optical peak (until July 2022), the source showed further optical brightening reaching a second optical peak in November 2022, which was 0.12 magnitudes brighter than the first peak in May 2022. This motivated us to obtain additional Swift and NICER observations. Swift/XRT recorded a mean background-subtracted countrate of (0.104+/-0.009) cps on 11 December 2022, and (0.063+/-0.010) cps on 20 December 2022. Modeling the 0.3-10keV XRT spectrum from 11 December 2022 with the same powerlaw model as before, viz, TBabs*zTBabs*zashift(powerlaw) in XSPEC, gave a best-fit powerlaw index of 1.93+/-0.21. The observed 0.3-10 keV luminosity and flux from that XRT spectrum were (1.02+/-0.09)e+44 ergs/s and (3.36+0.49-0.27)e-12 ergs/cm^2/s, respectively (68% confidence values), which are higher by a factor of about 1.5 as compared to the previously observed XRT values after the outburst in April-May 2022. Similarly, we fit the 0.3-2 keV NICER spectrum (1.25+/-0.02cps) recorded between 16-17 December 2022 with the same powerlaw model and obtained a best-fit powerlaw index of (2.15+0.13-0.07), and 1.5x10^20 /cm^2 as an upper limit on the neutral column. These values are consistent with their respective measurements from the outburst in April-May 2022. The observed NICER 0.3-10 keV luminosity and flux are (7.19+0.62-1.28)e+43 ergs/s and (2.31+0.06-0.21)e-12 ergs/cm^2/s (68% confidence values), respectively, lower than the XRT values recorded about 5 days prior to NICER in December 2022. \nThese values suggest that the source has shown an overall increase in the observed X-ray flux following the new outburst (November 2022), and is variable in X-rays, but the overall X-ray spectral shape has remained the same. Further NICER and Swift monitoring observations are planned. We encourage optical spectroscopy and radio observations of this ongoing CL AGN. \nReferences: Newsome M., Dgany Y., Arcavi I. et al. 2022, TNSCR, 2022-1320 \nKoss M., Trakhtenbrot B., Ricci C. et al. 2017 ApJ 850 74 \nAjay Y., Guolo M., Pasham D. 2022 Res. Notes AAS 6 274 (DOI 10.3847/2515-5172/acacf1)", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Neutron star", "Active galactic nucleus, Variable star", "Active galactic nucleus, Quasar", "Neutron star, Variable star" ] }, "answerKey": "B" }, { "id": "atel_15875", "message": "Title: Optical bands flaring of the blazar Ton 599 (4C +29.45)\nAuthors: Tushar Tripathi, P. U. Devanand, Alok C. Gupta, S. Kishore, K. Dogra, Krishna Mohana A., V. Dhiman (Aryabhatta Research Institute of Observational Science (ARIES), Manora Peak, Nainital 263001, India)\nDate: 29 Jan 2023; 13:01 UT\nProvenance: Dr. Alok C. Gupta (acgupta30@gmail.com)\nSubjects: Optical, AGN, Blazar\nDescription: Since January 2023, it has been noticed that the blazar Ton 599 (4C 29.45, 1156+295; RA (2000.0) = 11:59:32.07, DEC (2000.0) = +29:14:42.0) at z = 0.729 is currently displaying flux variations in the complete electromagnetic spectrum e.g. in gamma-rays (ATel #15853; #15859), X-ray (ATel #15854), optical (ATel #15870), and in radio (ATel #15873). Historically the blazar has shown large amplitude variations in optical bands e.g. in U = 17.08 mag to 12.67 mag, B = 18.28 mag to 12.73 mag, V = 17.38 mag to 12.85 mag, R = 18.04 mag to 12.24 mag, and I = 17.03 mag to 11.69 mag (Fan et al. 2006, PASJ, 58, 797). We are monitoring the source in optical bands and the VRI magnitudes obtained by us on January 26, 2023 is listed below. The observations are carried out using our 1.04m Sampurnanand Telescope (ST) of ARIES, Nainital, India. 2459971.305824861 13.7917 0.0026 V 2459971.319481759 13.2771 0.0023 R 2459971.300460729 12.6961 0.0025 I Here the first column represents JD, second column magnitude, third column error and the fourth column optical filter. If we compare the brightness of the source with the historical data, the source seems to be still in the optical pre-outburst state. There is a possibility to detect the source in an even brighter state in coming days. We will try to observe the source in the coming days whenever it is possible.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Pulsar", "Magnetar, Black hole", "Active galactic nucleus, Black hole", "Neutron star, Black hole" ] }, "answerKey": "C" }, { "id": "atel_15950", "message": "Title: SLX 1746-331 - corrected location for near-infrared counterpart\nAuthors: M. A.P. Torres (IAC/ULL), P. G. Jonker (SRON/Nijmegen), M. T. Reynolds (Michigan), D. Steeghs (Warwick)\nDate: 17 Mar 2023; 13:19 UT\nProvenance: Manuel Torres (mtorres@cfa.harvard.edu)\nSubjects: Infra-Red, Black Hole, Neutron Star, Transient\nDescription: ATels #1252 and #1633 reported the discovery of the variable near-infrared counterpart to SLX 1746-331 from observations taken during 2007 and 2008 with the PANIC camera mounted on the 6.5m Magellan Baade telescope at Las Campanas observatory. Joshi et al. 2023 (ATel #15949) have identified the optical counterpart to SLX 1746-331 from observations during the on-going 2023 outburst. Given that its location is in disagreement with that provided for the infrared counterpart (ATel #1252), we have reviewed the analysis of the PANIC data. We regret to inform that the coordinates of an unrelated field star were erroneously reported in ATel #1252 instead of the counterpart location. The correct coordinates for the near-infrared counterpart to SLX 1746-331 are R.A(J2000)=17:49:48.96 and Dec(J2000) = -33:12:17.1, with 0.1 arcsec uncertainty and in agreement with the optical counterpart coordinates.\nNote that the K-band variability reported in ATels #1252 and #1633 correspond to the true near-infrared counterpart and that this was correctly marked in the finding chart provided in ATel #1252. The finder is at present available at the BlackCAT catalogue (https://www.astro.puc.cl/BlackCAT/references.php).", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Black hole, Neutron star", "Active galactic nucleus, Neutron star", "Quasar, Neutron star", "Accreting object, Neutron star" ] }, "answerKey": "A" }, { "id": "atel_16000", "message": "Title: MAXI/GSC detection of an X-ray burst probably from XTE J1810-189\nAuthors: K. Kobayashi, H. Negoro, M. Nakajima, M. Tanaka, Y. Soejima, Y. Kudo (Nihon U.), T. Mihara, T. Kawamuro, S. Yamada, T. Tamagawa, N. Kawai, M. Matsuoka (RIKEN), T. Sakamoto, M. Serino, S. Sugita, H. Hiramatsu, H. Nishikawa, A. Yoshida (AGU), Y. Tsuboi, S. Urabe, S. Nawa, N. Nemoto (Chuo U.), M. Shidatsu (Ehime U.), M. Niwano, S. Sato, N. Higuchi (Tokyo Tech), S. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, T. Kurihara (JAXA), Y. Ueda, S. Ogawa, K. Setoguchi, T. Yoshitake, K. Inaba, Y. Nakatani (Kyoto U.), M. Yamauchi, Y. Hagiwara, Y. Umeki, Y. Otsuki (Miyazaki U.), K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU), M. Sugizaki (NAOC), and W. Iwakiri (Chiba U.) \nDate: 21 Apr 2023; 10:43 UT\nProvenance: Hitoshi Negoro (negoro@phys.cst.nihon-u.ac.jp)\nSubjects: X-ray, Neutron Star\nDescription: The MAXI/GSC detected an X-ray burst-like event in the scan transit at 20:09 UT on 2023 April 19. Assuming that the source flux was constant over the transient, We obtain the source position at \n(R.A., Dec) = (272.498 deg, -19.211 deg) = (18 09 59, -19 12 39) (J2000) \nwith a statistical 90% C.L. elliptical error region with long and short radii of 0.16 deg and 0.14 deg, respectively. The roll angle of the long axis from the north direction is 38.0 deg counterclockwise. There is an additional systematic uncertainty of 0.1 deg (90% containment radius). However, the X-ray flux rapidly increased and decreased in about 20 sec during about 50 sec scanning observation, which means that a strict error region is larger than the above estimation. The X-ray flux averaged over the scan was 358 +- 37 mCrab (4.0-10.0keV, 1 sigma error). A faint activity with 41 +- 16 mCrab is also recognized in the scan transit at 2:21 on April 20. \n \nThe error region includes the LMXB XTE J1810-189 discovered in 2008 (ATel #1424). An X-ray burst from XTE J1810-189 was observed in 2008 (ATel #1443, Weng et al. 2015, MNRAS, 450, 2915). If we assume that this burst source is XTE J1810-189 and effective are correction is applied, the peak flux of this burst is about 1 Crab. Though the peak flux is about half of a burst peak flux in 2008 (Weng et al. 2015), the burst duration and the double-peaked structure just like seen in the burst in 2008 suggest the source is XTE J1810-189. If the source is XTE J1810-189, this may be the beginning of renewed activity since 2013 (ATel #4752, #4804). We also tentatively name the source MAXI J1809-192. \nBurst information", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Supernova", "Neutron star", "Stellar evolution" ] }, "answerKey": "C" }, { "id": "atel_16075", "message": "Title: Fermi-LAT gamma-ray observations of SN 2023ixf\nAuthors: G. Marti-Devesa (University of Innsbruck), on behalf of the Fermi-LAT Collaboration\nDate: 6 Jun 2023; 13:26 UT\nProvenance: Teddy Cheung (Teddy.Cheung@nrl.navy.mil)\nSubjects: Gamma Ray, >GeV, Supernovae\nDescription: We report an analysis of SN 2023ixf with all-sky survey data from the Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope. The SN 2023ixf was initially reported by K. Itagaki in M101 on May 19 (T0 = 2023-05-19 17:27:15 UTC) and later classified as a Type II SN (Perley et al., AstroNote 2023-119). Since then, it has been monitored at several wavelengths (e.g. ATels #16045, #16047, #16049, #16052, #16073) and neutrino limits have been provided (ATels #16043, #16070). \nWe searched for emission from a new gamma-ray transient source. Preliminary analysis indicates no significant (> 5 sigma) new excess emission (> 100 MeV) at the optical position of SN 2023ixf (TNS). Assuming a power-law spectrum (photon index = 2.0, fixed) for a point source at the SN 2023ixf nominal position, the >100 MeV flux upper limit (95% confidence) is < 1.9e-8 ph cm^-2 s^-1 (< 2.6e-11 erg cm^-2 s^-1) for a 14-day integration time after its discovery (2023-05-19 17:27:15 to 2023-06-02 17:27:15 UTC). This corresponds to a luminosity limit of < 1.3e41 erg s^-1 for a distance of 6.4 Mpc. No signal with larger fluence is detected either on shorter time scales (from T0 to T0+1, T0+5, or T0+12 days). This limit is about one order of magnitude above the hard X-ray luminosity reported by NuSTAR, which has a power-law index of 1.3 (ATel #16049). \nSince Fermi normally operates in an all-sky scanning mode, regular monitoring of this region will continue. For this source the Fermi-LAT contact person is Guillem Marti-Devesa (guillem.marti-devesa@uibk.ac.at). \nThe Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Interstellar medium", "Active galactic nucleus", "Supernova", "Binary system" ] }, "answerKey": "C" }, { "id": "atel_16125", "message": "Title: NICER confirms the onset of a new outburst from MAXI J1807+132\nAuthors: Giulia Illiano (INAF OAR), Alessandro Papitto (INAF OAR), Filippo Ambrosino (INAF OAR), Arianna Miraval Zanon (ASI; INAF OAR), Andrea Sanna (Univ. of Cagliari)\nDate: 10 Jul 2023; 19:15 UT\nProvenance: Alessandro Papitto (alessandro.papitto@inaf.it)\nSubjects: X-ray, Neutron Star, Transient\nDescription: Referred to by ATel #: 16128, 16185\nOn 2023 July 2 (MJD 60127.3), the Las Cumbres Observatory Network of telescopes (LCO) reported the increase in the optical flux of the transient low-mass X-ray binary (LMXB) MAXI J1807+132 (ATel #16119). NICER promptly performed targeted follow-up observations accumulating more than 18 ks of exposure so far, from July 5 22:38 UTC to July 10 16:03 UTC.\nOn July 8, NICER detected a sudden increase in flux by a factor of ~100, with the source reaching ~90 counts per second in the 0.2-12 keV band, well above the background level. Since then, the source's flux has continued to increase, reaching ~220 counts per second in the latest observations. Assuming that the 0.5-10 keV spectrum can be described by an absorbed power-law with photon index Γ~2.1 absorbed by a column density of 1E21 cm^-2 (Jiménez-Ibarra et al. 2019), such a count rate translates into an unabsorbed flux of ~4.2E-10 erg/cm^2/s. Such a value is similar to the maximum ones reported during the last outburst observed from the source in 2019 (ATel #13139, 13173).\nWe also performed a preliminary timing analysis to search for coherent X-ray pulsations in the observations carried out after the flux increase. We found no evidence for pulsations, with a 3σ upper limit on the pulse amplitude of ~5.8%. \nDuring MAXI J1807+132 outburst in 2017 (ATel #10208) and 2019 (ATel #13097), several brightening episodes were detected (Jiménez-Ibarra et al. 2019; ATel #13173). Moreover, in 2019 NICER detected two Type I X-ray bursts confirming the source classification as a neutron star (ATel #13239). For all these reasons, additional multi-wavelength follow-up is encouraged.\nNICER monitoring of MAXI J1807+132 is still ongoing. NICER is a 0.2-12 keV X-ray telescope operating on the International Space Station. The NICER mission and portions of the NICER science team activities are funded by NASA.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Supernova", "Neutron star", "Minor body", "Globular cluster" ] }, "answerKey": "B" }, { "id": "atel_16175", "message": "Title: Fermi-LAT detection of enhanced gamma-ray activity from the radio source GB6 J1102+7019\nAuthors: Denis Bernard (LLR, Ecole Polytechnique & CNRS / IN2P3), on behalf of the Fermi Large Area Telescope Collaboration\nDate: 6 Aug 2023; 18:46 UT\nProvenance: Denis Bernard (Denis.bernard@in2p3.fr)\nSubjects: Gamma Ray, >GeV, Request for Observations, AGN, Blazar\nDescription: The Large Area Telescope (LAT), one of the two instruments on the Fermi Gamma-ray Space Telescope, has observed enhanced gamma-ray activity from a source positionally consistent with the radio source GB6 J1102+7019, also known as 4FGL J1101.3+7017 (The Fermi-LAT collaboration 2020, ApJS, 247, 33), with coordinates R.A. = 165.505638 deg, Decl. = +70.315908 deg (J2000; Jackson et al., 2007, MNRAS, 376, 371). \nPreliminary analysis indicates that this source was in an elevated gamma-ray emission state on August 4, 2023, with a daily averaged gamma-ray flux (E>100MeV) of (0.4 +/- 0.1) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 40 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL). The corresponding photon index is 2.5 +/- 0.2 and is smaller than but consistent with the 4FGL value of 2.7 +/- 0.4 within the uncertainties. About half of the signal was detected in the 18:00 - 24:00 UTC time range, with an averaged gamma-ray flux (E>100MeV) of (0.8 +/- 0.3) X 10^-6 photons cm^-2 s^-1 (statistical uncertainty only). This corresponds to a flux increase of a factor of 80 relative to the average flux reported in the fourth Fermi-LAT catalog (4FGL). \nBecause Fermi normally operates in an all-sky scanning mode, regular gamma-ray monitoring of this source will continue. We encourage multifrequency observations of this source. For this source, the Fermi-LAT contact person is Denis Bernard (denis.bernard@in2p3.fr). \nThe Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Active galactic nucleus, Repeater", "Active galactic nucleus, Pulsar", "Active galactic nucleus, Black hole", "Active galactic nucleus, Star and stellar system" ] }, "answerKey": "C" }, { "id": "atel_16250", "message": "Title: VLT/X-shooter classification of AT 2023tbf (GOTO23aky) as a dwarf nova\nAuthors: A. Saccardi (GEPI/Paris Obs.), L. Izzo (INAF/OACn and DARK/NBI), J. T. Palmerio (GEPI/Paris Obs. and IAP), D. B. Malesani (Radboud Univ. and DAWN/NBI), P. D'Avanzo (INAF-OABr), V. D’Elia (ASI-SSDC and INAF-OAR), M. Della Valle (INAF/OAC), D. H. Hartmann (Clemson Univ.), K. E. Heintz (DAWN/NBI), P. Jakobsson (U. of Iceland), L. Kaper (U. of Amsterdam), G. Leloudas (DTU Space), A. J. Levan (Radboud Univ.), A. Martin-Carrillo (UCD), B. Schneider (MIT), S. Schulze (OKC), A. de Ugarte Postigo (OCA), and K. Wiersema (U. of Hertfordshire)\nDate: 21 Sep 2023; 16:41 UT\nProvenance: Daniele Malesani (d.malesani@astro.ru.nl)\nSubjects: Optical, Gamma-Ray Burst, Nova\nDescription: We observed the transient AT 2023tbf (GOTO23aky; Gompertz et al., GCN 34738), spatially and temporally consistent with the Fermi GBM GRB 230918B (Fermi GBM team, GCN 34738). We used the ESO VLT UT3 (Melipal) equipped with the X-shooter spectrograph, starting on 2023 September 20.093 UT. Our data cover the wavelength range 3000-24800 Å and consist of 4 exposures of 600 s each.\nIn the acquisition image, taken on 2023 Sep 20.086 UT, we measure for the transient a magnitude r = 19.64 ± 0.05 AB (calibrated against a single nearby star from the SkyMapper catalog).\nA strong continuum is detected in the blue end of the spectrum, with a decreasing signal towards the VIS and NIR arms. The UVB shows several broad undulations, not seen in GRB afterglow spectra; in the VIS and NIR arms, the continuum is smoother.\nThe source shows narrow absorption from Ca H and K a z = 0, as well as broad features in correspondence of the Balmer lines, at least H-β to H-η, all at z = 0. No features are identified at z > 0\\. Comparison with template spectra (e.g. Morales-Rueda & Marsh, 2002, MNRAS, 332, 814) allows us to classify AT 2023tbf as a dwarf nova. We thus conclude that AT 2023tbf is not a GRB afterglow and is not associated with GRB 230918B.\nWe acknowledge excellent support from the observing staff at Paranal, in particular Ditte Slumstrup, Xavier Haubois, Francisco Caceres and Paulina Venegas.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Nova", "Accreting object", "Stellar evolution" ] }, "answerKey": "A" }, { "id": "atel_16325", "message": "Title: Spectroscopic Classification of AT2023uru with SOAR/Goodman\nAuthors: K. W. Davis, R. J. Foley (UCSC)\nDate: 6 Nov 2023; 22:31 UT\nProvenance: Ryan Foley (foley@ucsc.edu)\nSubjects: Optical, Supernovae\nDescription: We report the following the classification of AT2023uru from spectroscopic observations with the Goodman spectrograph on the SOAR telescope using the AEON queue, made on 2023 Oct 27 UT. The target was supplied by CRTS and identified using the target management platform YSE-PZ (Coulter et al., 2023, PASP, 135, 4501). The classification was performed with SNID (Blondin & Tonry, 2007, ApJ, 666, 1024). \n \n \n Name | IAU Name | RA (J2000) | Dec (J2000) | z | Type | Phase | Notes \n \n | AT2023uru | 00:23:16.008 | +24:57:17.36 | 0.060 | II |post-peak| (1) \n \nNotes: When the redshift is given to 2 decimal places, it is derived from the SN spectrum. Otherwise, the redshift is determined from the host galaxy. (1) We measure a H-alpha absorption velocity of -14,500 km/s. We thank the SOAR observatory staff for executing this observation.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Variable star", "Magnetar", "Supernova", "Globular cluster" ] }, "answerKey": "C" }, { "id": "atel_16400", "message": "Title: AGILE detection of gamma-ray rebrightening of the blazar PKS 1424-418\nAuthors: A. Bulgarelli (INAF/OAS-Bo), C. Pittori, F. Verrecchia (SSDC and INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), L. Foffano (INAF/IAPS), G. Panebianco (INAF/OAS-Bo), G. Piano (INAF/IAPS), V. Fioretti, N. Parmiggiani, A. Addis, L. Baroncelli, A. Di Piano, L. Castaldini, A. Ciabattoni (INAF/OAS-Bo), F. Lucarelli (SSDC and INAF/OAR), S. Vercellone (INAF/OA-Brera), M. Cardillo, A. Ursi, C. Casentini (INAF/IAPS), I. Donnarumma (ASI), F. Gianotti, M. Trifoglio (INAF/OAS-Bo), A. Giuliani, S. Mereghetti, P. Caraveo, F. Perotti (INAF/IASF-Mi), A. Chen (Wits University), A. Argan, E. Costa, E. Del Monte, Y. Evangelista, M. Feroci, I. Lapshov, E. Menegoni, L. Pacciani, P. Soffitta, V. Vittorini (INAF/IAPS), F. Lazzarotto (INAF/OAPD), G. Di Cocco, F. Fuschino, M. Galli, C. Labanti (INAF/OAS-Bo), M. Marisaldi (University of Bergen), A. Pellizzoni, M. Pilia, A. Trois (INAF/OA-Cagliari), G. Barbiellini (INFN Trieste), F. Longo (Univ. Trieste and INFN Trieste), E. Vallazza (INFN Milano Bicocca), A. Morselli, P. Picozza (INFN and Univ. Roma Tor Vergata), M. Prest (Univ. dell'Insubria), P. Lipari, D. Zanello (INFN and Univ. Roma Sapienza), P. W. Cattaneo, A. Rappoldi (INFN Pavia), A. Ferrari (Univ. Torino and CIFS), F. Paoletti (East Windsor RSD Hightstown and INAF/IAPS), L. A. Antonelli (INAF/OAR), P. Giommi, L. Salotti, G. Valentini, and F. D'Amico (ASI)\nDate: 11 Jan 2024; 17:24 UT\nProvenance: Andrea Bulgarelli (bulgarelli@iasfbo.inaf.it)\nSubjects: Gamma Ray, >GeV, AGN, Blazar, Transient\nDescription: Referred to by ATel #: 16406\nAGILE is currently detecting intense gamma-ray emission above 100 MeV from a region positionally consistent with the blazar PKS 1424-418 (z = 1.522, White et al., ApJ 327 561, 1988). Integrating from 2024-01-09 09:46:07 UT to 2024-01-11 09:46:07 UT, a preliminary maximum likelihood analysis shows a detection at 5.3 sigma, with a flux F = (3.3 +/- 1.1) x 10^-06 ph/cm^2/s (E>100 MeV). The average flux, detected by the AGILE-GRID during the previous 7 days, was F(>100 MeV) = (1.9 +/- 0.7) x 10^-6 photons/cm^2/s. \nPrevious flares of PKS 1424-418 in gamma-rays were reported by AGILE in ATels #15818, #15533 and #15527. \nThe AGILE-GRID detection was obtained while AGILE is observing in spinning mode, surveying a large fraction of the sky each day. The source can be monitored with the public mobile application \"AGILEScience\" developed by the AGILE Team, available for both Android and iOS devices. \nMultifrequency observations of the PKS 1424-418 region are strongly encouraged.", "choices": { "label": [ "A", "B", "C", "D" ], "text": [ "Quasar", "Circumstellar disk", "Stellar evolution", "Active galactic nucleus" ] }, "answerKey": "D" } ]