//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10496 SUBJECT: GRB 100316D: Swift detection of a burst DATE: 10/03/16 12:56:50 GMT FROM: Scott Barthelmy at NASA/GSFC M. Stamatikos (OSU/NASA/GSFC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester), S. Campana (INAF-OAB), A. de Ugarte Postigo (INAF-OAB), P. A. Evans (U Leicester), J. M. Gelbord (PSU), C. Guidorzi (U Ferrara), S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), R. Margutti (Univ Bicocca&OAB), F. E. Marshall (NASA/GSFC), S. R. Oates (UCL-MSSL), C. Pagani (U Leicester), K. L. Page (U Leicester), D. M. Palmer (LANL), P. Romano (INAF-IASFPA), B. Sbarufatti (INAF-OAB/IASFPA), R. L. C. Starling (U Leicester) and T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team: At 12:44:50 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 100316D trigger=416135). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 107.615, -56.278 which is RA(J2000) = 07h 10m 28s Dec(J2000) = -56d 16' 40" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). This is an image trigger, but there is a possibility that there is a low-level peak about 100 sec long. The XRT began observing the field at 12:47:08.1 UT, 137.7 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 107.6291, -56.2567 which is equivalent to: RA(J2000) = 07h 10m 30.98s Dec(J2000) = -56d 15' 24.1" with an uncertainty of 5.0 arcseconds (radius, 90% containment). This location is 81 arcseconds from the BAT onboard position, within the BAT error circle. No event data are yet available to determine the column density using X-ray spectroscopy. The initial flux in the 2.5 s image was 2.38e-09 erg cm-2 s-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 148 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. Because part of the 2.7'x2.7' sub-image was not received, the overlap with the XRT error circle is uncertain. The coverage of the XRT error circle by the 8'x8' region for the list of sources generated on-board is uncertain because the large number of sources filled the available telemetry. No correction has been made for the expected extinction corresponding to E(B-V) of 0.12. Burst Advocate for this burst is M. Stamatikos (Michael.Stamatikos-1 AT nasa.gov). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/too.html.) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10505 SUBJECT: GRB 100316D: Swift XRT refined analysis DATE: 10/03/16 18:32:59 GMT FROM: Rhaana Starling at U of Leicester R.L.C. Starling, P.A. Evans (U. Leicester) and M. Stamatikos (OSU/NASA/GSFC) report on behalf of the Swift-XRT team: We have analysed the first orbit of Swift XRT data for GRB 100316D (Stamatikos et al. GCN Circ. 10496), comprising 593 s of exposure from 143 s to 737 s after the BAT trigger. The data are solely in Windowed Timing (WT) mode. The light curve over this time decays very slowly and can be modelled with a power-law with a decay index of alpha=0.13+/-0.03. A spectrum formed from these data can be fitted with an absorbed power-law with a photon spectral index of 1.42 (+/-0.04). The best-fitting absorption column is 5.9 (+/-0.3) x 10^21 cm^-2, in excess of the Galactic value of 7.0 x 10^20 cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 6.6 x 10^-11 (8.7 x 10^-11) erg cm^-2 count^-1. If the decay contines with alpha=0.13, the predicted count rate at T+24h is 16 count s^-1 or an observed (unabsorbed) 0.3-10 keV flux of 1.1 (1.4) x10^-9 erg cm-2 s-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00416135. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10511 SUBJECT: GRB 100316D: Swift-BAT refined analysis DATE: 10/03/16 23:16:32 GMT FROM: Scott Barthelmy at NASA/GSFC T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-60 to T+243 sec from the telemetry downlinks, we report further analysis of BAT GRB 100316D (trigger #416135) (Stamatikos, et al., GCN Circ. 10496). The BAT ground-calculated position is RA, Dec = 107.599, -56.275 deg, which is RA(J2000) = 07h 10m 23.8s Dec(J2000) = -56d 16' 28.9" with an uncertainty of 3.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 85%. The mask-weighted light curve is relatively flat. The emission started before T-80 sec when the location came into the BAT FoV during a Swift planned-target slew. Using the event-by-event data, the lightcurve conitinue through the 64-sec integration of the image trigger and out to at least T+240 sec. Using the on-board mask-weighted lightcurve, the lightcurve continues out to at least T+740 sec where the data ends. The time-averaged spectrum using just the T+0.0 to T+64.0 sec image-trigger interval is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 2.29 +- 0.41. The fluence in the 15-150 keV band is 3.0 +- 0.8 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T+0.00 sec in the 15-150 keV band is 0.1 +- 0.0 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/416135/BA/ We note that this lightcurve is very non-typical for a GRB and that the spectrum is soft. This is similar both in the temporal and spectral properties to the GRB060218-SN2006aj burst (Camapana, et al.; Nature, v224, p1008, Figure 1). In the 060218 burst, the BAT lightcurve was flat from T-50 to T+300 sec. The X-ray temporal decay (Starling, GCN Circ 10505) is shallow as it was in SN2006aj (Campana, Fig 1). We further note that the 5 arcsec XRT error circle (GCN 10496) covers the edge of an extended object (a pair of unresolved stars or a galaxy) in DSS. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10512 SUBJECT: GRB 100316D: VLT/X-shooter observations DATE: 10/03/17 03:05:25 GMT FROM: Paolo D'Avanzo at INAF-OAB S.D. Vergani (GEPI-Obs. Paris), P. D'Avanzo (INAF-OAB), A.J. Levan (Univ. Warwick), S. Covino (INAF-OAB), D. Malesani, J. Hjorth (DARK/NBI), L.A. Antonelli (INAF-OAR) report on behalf of a larger collaboration: We observed the field of GRB 100316D (Stamatikos et al., GCN 10496) with the VLT equipped with the X-shooter spectrograph. Observations started on 2010 Mar 17 at 00:58 UT (~ 12 hours after the GRB). In the 100s acquisition image, we detect an object inside the XRT error circle, at the following position (J2000): RA: 07:10:30.77 Dec: -56:15:20.7 (+/- 0.5"). The object has a magnitude R~21 (calibrated against USNO-B1.0) and is very close (~3.5") to the DSS galaxy reported by Sakamoto et al. (GCN 10511). In the X-shooter spectrum of this source we detect several bright emission lines. Among these we have [OII], Hdelta, Hgamma, Hbeta, [OIII], Halpha all at a common redshift of 0.059. At present, we cannot say if this object (that might be a region of the nearby galaxy) is related with GRB 100316D. Further analysis and observations are in progress. We caution that the above analysis (particularly the wavelength solution) is preliminary. Reduction with updated calibrations is underway. We would like to thank the ESO staff for their kind assistance, in particular Thomas Rivinius, Alvaro Alvarez and Andres Pino //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10513 SUBJECT: GRB 100316D: Gemini/GMOS and VLT/X-shooter observations DATE: 10/03/17 04:37:46 GMT FROM: Paolo D'Avanzo at INAF-OAB S.D. Vergani (GEPI-Obs. Paris), A.J. Levan (Univ. Warwick), P. D'Avanzo (INAF-OAB), S. Covino (INAF-OAB), D. Malesani, J. Hjorth (DARK/NBI), N.R. Tanvir (Univ. Leicester), L.A. Antonelli (INAF-OAR) report on behalf of a larger collaboration: We carried out further observations of the field of GRB 100316D (Stamatikos et al., GCN 10496) with the Gemini telescope equipped with GMOS in imaging mode (~ 12 hours after the GRB). Inside the XRT error circle we detect two discrete, compact objects, both of which lie on the stellar field of the DSS galaxy (Sakamoto et al. GCN 10511; Vergani et al. GCN 10512): Object A: RA (J2000): 07:10:30.77 Dec (J2000): -56:15:20.7 Object B: RA (J2000): 07:10:30.48 Dec (J2000): -56:15:22.3 Both position have errors of approximately 0.5" in each axis. We note that object "A" is the same reported by Vergani et al. (GCN 10512). We obtained a VLT/X-shooter spectrum of source "B", which exhibits the same emission lines reported by Vergani et al. (GCN 10512) for object "A" at the same redshift of z=0.059. Likely, object "A" and "B" are regions of the nearby DSS galaxy. A finding chart is available at the following web page: http://www.astro.ku.dk/~malesani/GRB/100316D/GRB100316D_finder.png We caution that the above analysis (particularly the wavelength solution) is preliminary. Reduction with updated calibrations is underway. We would like to thank the Gemini staff for their kind assistance, in particular Rodrigo Carrasco. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10514 SUBJECT: GRB 100316D: GROND Detection of the Optical/NIR Afterglow Candidate DATE: 10/03/17 04:47:13 GMT FROM: Adria C. Updike at Clemson U Paulo Afonso (MPE Garching), Adria Updike (Clemson University), Marco Nardini, Robert Filgas, Abdullah Yoldas, and Jochen Greiner (MPE Garching) report on behalf of the GROND team: We observed the field of GRB 100316D (Swift trigger 416135; Stamatikos et al., GCN 10496) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m ESO/MPI telescope at La Silla Observatory (Chile). Observations started at 00:28 UT on March 17, 11.66 hours after the GRB trigger, and are continuing. They were performed at an average seeing of 1" and at an average airmass of 1.1. We detect what appears to be a bright point on the edge of the extended object noted by Sakamoto et al. (GCN 10511) within the XRT error circle. This is consistent with the source identified by Vergani et al. (GCN 10512). The source is detected in all bands, suggesting a redshift < 3.5. We cannot yet determine if this source is related to the GRB. Further observations are required to establish variability, and to check whether the optical bands show similarities to GRB 060218 - SN 2006aj as reported by Sakamoto et al. (GCN 10511) for the gamma ray and x-ray bands. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10517 SUBJECT: Tentative redshift of GRB100316D from X-ray data DATE: 10/03/17 06:37:22 GMT FROM: Sergio Campana at INAF-OAB S. Campana (INAF-OAB) reports on behalf of the Swift-XRT team: Swift XRT observed GRB 100316D (Stamatikos et al. 2010, GCN10496) in Windowed Timing (WT) mode in the 144-737 s time interval. During this interval the light curve decays very slowly (decay index alpha=-0.13, Starling et al. 2010, GCN 10505). In addition, the 1.5-10 keV to 0.3-1.5 keV hardness ratio remains constant (reduced chi2=0.91 with 97 degrees of freedom, dof). Motivated by the high count rate (around 30 c s^-1, but far from the pile up limit) and by the constant spectral shape we tried to estimate the GRB redshift from the X-ray data. We assume a Galactic column density of 7x10^20 cm^-2 (Kalberla et al. 2005, A&A 440 775) and fit the WT spectrum taken from the Leicester pages (http://www.swift.ac.uk/xrt_spectra/00416135/) with an absorbed (phabs*zphabs) cutoff power law model (the cutoff power law model provides much better results in terms of column density evaluation with respect to a simple power law model when small spectral variations are present). Given the high count rate we selected single pixel events only. The resulting fit is good (reduced chi2=1.2, 333 dof). The redshift is constrained to lie within the 90% confidence level (delta chi2=4.61) of 0.014 R.L.C. Starling, P.A. Evans (U. Leicester) and M. Stamatikos (OSU/NASA/GSFC) report on behalf of the Swift XRT team: We have now analysed the first 3 orbits of Swift XRT data for GRB 100316D (trigger=416135, Stamatikos et al. GCN Circ. 10496), comprising 8 s of Windowed Timing (WT) settling mode data, 593 s of WT mode data and 3.7 ks of Photon Counting (PC) mode data. The early light curve is flat and can be modelled with a power-law decay with a decay index of alpha=0.13+/-0.03 as described in Starling et al. (GCN Circ. 10505). This now breaks at some time after T+750 s to a steeper decay of alpha=2.0 +0.3/-0.1. Using 1967 s of XRT Photon Counting mode data and 1 U-band UVOT image, we find an astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 107.62763, -56.25547 which is equivalent to: RA (J2000): 07h 10m 30.63s Dec (J2000): -56d 15' 19.7" with an uncertainty of 3.7 arcsec (radius, 90% confidence). This position may be improved as more data are received. The latest position can be viewed at http://www.swift.ac.uk/xrt_positions. Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). We note that this position is 1.5 arcsec from the optical/nIR candidate 'Object A' reported in the VLT/X-Shooter and Gemini/GMOS observations by Vergani et al. (GCN Circ. 10513) and GROND observations reported by Afonso et al. (GCN Circ. 10514), and 2.9 arcsec from the candidate 'Object B' reported in GCN Circ. 10513. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10520 SUBJECT: GRB 100316D: Swift/UVOT Observations DATE: 10/03/17 16:54:15 GMT FROM: Samantha Oates at MSSL S. R. Oates (MSSL-UCL), M. De Pasquale (MSSL-UCL) and M. Stamatikos (OSU/NASA/GSFC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 100316D 148s after the BAT trigger (Stamatikos et al., GCN Circ. 10496). Coincident with the refined Swift XRT error circle (Starling et al. GCN Circ. 10519), we detect the DSS galaxy, which hosts the sources A and B (Vergani et al. GCN Circ. 10512, 10513), but we are unable to resolve it. Our photometry, performed on 3ks of data in the 7 UVOT filters, shows no change larger than 1 sigma in the flux of this DSS galaxy. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10523 SUBJECT: GRB 100316D: Further Gemini observations DATE: 10/03/18 02:55:05 GMT FROM: Andrew Levan at U.of Leicester A.J. Levan (U. Warwick), N.R. Tanvir (U. Leicester), P. D'Avanzo (INAF-OAB), S.D. Vergani (GEPI-Obs. Paris), D. Malesani (DARK/NBI) report for a larger collaboration. "We re-observed the location of GRB 100316D (Stamatikos et al. GCN 10496; Starling et al. GCN 10519) using Gemini/GMOS in the r-band. Observations began at 23:55 UT, approximately 36 hours after the GRB, and 24 hours after our first epoch (Vergani et al. GCN 10513). The seeing in the second epoch is slightly worse than the first (0.9" versus 0.7") and so the resulting images are slightly shallower. No obvious objects within the refined XRT error circle (Starling et al. GCN 10519) show significant (>3 sigma) evidence for variation. However, we do note the presence of a previously unreported compact source that is within the X-ray error circle, but is close to the nucleus of the galaxy, at RA(J2000) = 07:10:30.54 Dec(J2000) = -56:15:20.0 This source is brighter than those previously discussed in GCN 10513 (R~20) but again, given the difficulty of performing accurate photometry against a bright and varying background of the host, we can't as yet make any firm statements about variability. We note, it is of course possible that a brightening supernova component and fading afterglow are conspiring to mask variability between these two epochs, and further observations are planned. We thank the staff of Gemini, in particular Rodrigo Carrasco for their help in executing these observations." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10524 SUBJECT: GRB 100316D: Pre-burst emission measured by BAT DATE: 10/03/18 21:13:59 GMT FROM: Takanori Sakamoto at NASA/GSFC T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL), M. Stamatikos (GSFC/OSU) (i.e. the Swift-BAT team): Using the BAT hard X-ray survey data (Detector Plane Histogram data), we have processed the BAT survey data for pre- and post-trigger periods using the batsurvey script and have extracted the flux at the location of the GRB. While Swift was pointing at GRB 100316C from T-2650 s to T-80 s, the GRB 100316D location was in the FOV of BAT. At 12:43, Swift slewed to a pre-planned target (1E 1048.1-5937), and triggered on GRB 100316D. After re-pointing to the location of GRB 100316D, Swift slewed away from GRB 100316D at T+750 s due to an observational constraint. GRB 100316D came back into the FOV of BAT at T+5050 s (a pre-planned observation of 1E 1048.1-5937). The BAT light curve in the 14-195 keV band around the trigger time is available at: -Light curve from T-6000 sec to T+6000 sec: http://gcn.gsfc.nasa.gov/other/GRB100316D_bat_lc.gif -Zoom-in light curve from T-2000 sec to T+1000 sec: http://gcn.gsfc.nasa.gov/other/GRB100316D_bat_lc_zoomin.gif The light curve produced by the BAT event-by-event data is overlaid with the survey light curve in the figure. There is a probable early low-level emission starting from T-1500 s. The emission then rises at T-500 s, peaks at T-100 s, and decays with an exponential decay constant of ~750 s. The emission continues through the slew at T+750 s. The emission is no longer detected by BAT after T+5050 s. As pointed out in Sakamoto et al. (GCN Circ. 10511), the BAT light curve profile of GRB 100316D is very similar to the GRB 060218-SN2006aj burst (Camapana, et al.; Nature, v224, p1008). The BAT light curve of GRB 060218 shows a rise at T-300 s, a peak at T+450 s, and an exponential decay constant of ~500 s, with a duration of ~2000 sec. GRB 100316D was detected in Swift-BAT from ~T-500 sec to at least ~T+800 sec, hence the lower limit on the duration of GRB 100316D is ~1300 sec. The fluence in the 15-150 keV band measured with the available 955 seconds of event data is 3.4 x 10^-6 erg/cm2. This corresponds to an isotropic equivalent energy (Eiso) of 3.1x10^49 ergs in the 15.88 keV - 158.85 keV band at the GRB rest frame assuming a redshift z=0.059 of a potential source and a galaxy inside the XRT error circle (Vergani et al. GCN Circ. 10512, 10513). This unusually long duration in concert with a soft spectrum and a low Eiso (Eiso of GRB 060218 was 6.2x10^49 ergs) strengthens the similarity between GRBs 100316D and 060218. Although the lack of a clear optical counterpart to GRB 100316D at this stage is distinctly different than GRB 060218, the prompt emission characteristics are very much like supernova-associated GRB 060218. Hence, we suggest additional follow-up observations especially in the IR that may confirm the presence of a host supernova. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10525 SUBJECT: GRB 100316D: Possible Supernova DATE: 10/03/19 12:32:17 GMT FROM: Andrew Levan at U.of Leicester K. Wiersema (U. Leicester), P. D'Avanzo (INAF-OAB), A.J. Levan (U. Warwick), N.R. Tanvir (U. Leicester), D. Malesani (DARK/NBI), S. Covino (INAF-OAB) report for a larger collaboration: "We obtained a third epoch of observations of the localization of GRB 100316D (Stamatikos et al. GCN 10496; Starling et al. GCN 10519) using Gemini South and GMOS. Observations began at 23:48 UT on March 18, and were obtained in the r-band under excellent seeing (0.5"). Image subtraction reveals that the source previously identified by Levan et al (GCN 10523), has brightened between the two observations by ~0.3 magnitudes. We suggest that this object represents the rising supernova associated with GRB 100316D. Images of the field, and the subtraction can be found at http://www.star.le.ac.uk/~anl/100316D Further observations are planned. We thank the staff of Gemini for their help in executing these observations" //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10533 SUBJECT: GRB 100316D: ATCA radio observations DATE: 10/03/20 15:52:22 GMT FROM: Alicia Soderberg at Harvard/CfA Mark Wieringa (CSIRO), Alicia Soderberg (Harvard/CfA), and Phil Edwards (CSIRO) report: "We observed the field of GRB 100316D (Stamatikos et al. GCN 10496) with the Australia Telescope Compact Array beginning on Mar 18.35 for 3.5 hrs. Data were collected at central frequencies of 5.4 and 9.0 GHz with 2 GHz bandwidth each. We do not detect any radio sources within the refined XRT error circle (Starling et al. GCN 10519). We place upper limits of 104 microJy at 5.4 GHz and 165 microJy at 9.0 GHz (4 sigma). At the redshift of the host galaxy (z=0.059; Vergani et al. GCN 10512), these limits imply a radio spectral luminosity below 8e+27 erg/s/Hz which is a factor of 2 to 10 lower than the radio afterglow luminosities observed for nearby long-duration GRBs 980425 (Kulkarni et al. 1998), 031203 (Soderberg et al. 2004), and 060218 (Soderberg et al. 2006) on comparable timescales. Further observations are planned." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10541 SUBJECT: GRB 100316D: Spectroscopic Discovery of a Supernova from Magellan DATE: 10/03/22 22:19:26 GMT FROM: Ryan Chornock at UC Berkeley R. Chornock, A. M. Soderberg, R. J. Foley, E. Berger, A. Frebel, P. Challis (Harvard/CfA), J. D. Simon, and S. Sheppard (Carnegie) report: We have been obtaining nightly spectra of GRB 100316D (Stamatikos et al., GCN 10496) with the MagE, LDSS3, and IMACS spectrographs on the twin 6.5-m Magellan telescopes, starting on 2010 March 18.0 UT, approximately 1.5 days after the BAT trigger. All spectra included the variable point source found by Levan et al. (GCN 10523) and Wiersema et al. (GCN 10525) within the slit aperture. All spectra show superposed high-equivalent-width nebular emission lines at z=0.059, in agreement with Vergani et al. (GCN 10512). Our earliest spectra show a very blue continuum with a few weak stellar features indicative of some starlight from a young stellar population falling within our spectroscopic aperture, but no other obvious features. By the time of our most recent MagE spectrum, from March 22.0 UT (T0+5.5 days), a few broad undulations in the continuum have developed, although contamination from the galaxy light and possibly an afterglow remains significant. The strongest feature has a flux peak near 7850 Angs (in the rest frame) and a minimum near 7280 Angs. An additional local minimum in the continuum is located near 5700 Angs with a broad maximum located to the red of that. The appearance of undulations in the spectrum near the expected locations of supernova features from a comparison with SN 1998bw at early times (while no such undulations appear in our earliest spectra) leads us to conclude that we have spectroscopically determined that the transient source which was detected photometrically (Wiersema et al., GCN 10525) is a supernova. A plot of an early and a recent spectrum compared to SN 1998bw can be found here: http://www.cfa.harvard.edu/~eberger/grb100316d-mage.pdf //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10543 SUBJECT: Emerging Supernova in the Afterglow of GRB 100316D DATE: 10/03/24 13:37:52 GMT FROM: Filomena Bufano at INAF-Osb Astro di Padova F. Bufano, S. Benetti, E. Cappellaro, INAF Osservatorio Astronomico di Padova (INAF-OAPd); S. Covino, INAF Osservatorio Astronomico di Brera (INAF-OABr); S. Vergani, P.Goldoni, GEPI (Observatoire de Paris) - APC (Université Paris 7); M. Della Valle, INAF Osservatorio di Capodimonte; E. Pian, INAF Osservatorio Astronomico di Trieste; S. Campana, G.Tagliaferri, INAF-OABr; D.Malesani, J. Fynbo, Dark Cosmology Centre; M. Turatto, INAF Osservatorio Astronomico di Catania; F.Patat, European Southern Observatory (ESO) and P. Mazzali, INAF-OAPd report on behalf of a larger colaboration that a high-dispersion optical spectrum (range 350-900 nm, resolution 0.02 nm) of the afterglow associated to GRB 100316D (cf. GCN 10496) was obtained with the VLT telescope (+XShooter) at ESO-Paranal on March 23.04 UT. The spectrum of the source located at R.A.=07:10:31.8 and Decl.=-56:15:20.2, J2000.0 (as measured on the XShooter acquisition image) shows very broad bumps with peaks measured at about 430nm and 670nm reminiscent of an emerging broad line type Ic supernova (in agreement with Chornock et al, GCN 10541). Indeed, above 600 nm the spectrum of this source shows some similarities with that of SN 1998bw (Patat et al. 2001, ApJ, 555, 900) taken 7 days after outburst. There are however major differences with the spectrum of this transient, showing a significant flux deficiency in the range 450-550nm in comparison with SN 1998bw . [GCN OPS NOTE(24mar10): Per author's request, the parenthetical comment "(in agreement with Chornock et al, GCN 10541)" was added.] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10547 SUBJECT: GROND observations of GRB100316D/SN2010bh DATE: 10/03/26 22:58:43 GMT FROM: Arne Rau at MPE Arne Rau, Marco Nardini (both MPE Garching), Adria Updike (Clemson University), Robert Filgas, Jochen Greiner, Thomas Kruehler (all MPE Garching), and Sylvio Klose (TLS Tautenburg) report on behalf of the GROND team: We report on additional observations of the field of GRB 100316D (Swift trigger 416135; Stamatikos et al., GCN 10496) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPI/ESO telescope at La Silla Observatory (Chile). Observations started on 17 March 2010 at 00:27 UT, 11.7 hours after the burst (Afonso et al., GCN Circular #10514). The field was observed during additional 16 epochs and observations are continuing. Image subtraction revealed the supernova SN2010bh reported by Wiersema et al. (GCN Circular #10525), Chornock et al. (GCN Circular #10541), and Bufano et al. (GCN Circular #10543) to emerge approx. 5 days post-burst and to reach an AB magnitude of r ~ 18.8 +/- 0.2 at 7.5 days post-burst. The observed light curve evolution of SN2010bh is similar to that of SN1998bw (Galama et al. 1998), the supernova associated with GRB980425, shifted to the redshift of GRB100316D (z=0.059; Vergani et al., GCN Circular #10512). The optical luminosity is comparable to SN1998bw, except in the g-band, where the flux is suppressed by approx. 30%. This likely corresponds to the significant flux deficiency in the range 450-550nm reported from the X-Shooter spectrum (Bufano et al., GCN Circular #10543).