//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10746 SUBJECT: GRB 100513A: Swift detection of a burst DATE: 10/05/13 02:23:42 GMT FROM: David Palmer at LANL W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU), H. A. Krimm (CRESST/GSFC/USRA), R. Margutti (INAF-OAB), C. B. Markwardt (CRESST/GSFC/UMD), D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU), T. N. Ukwatta (GSFC/GWU) and L. Vetere (PSU) report on behalf of the Swift Team: At 02:07:08 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 100513A (trigger=421814). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 169.580, +3.605 which is RA(J2000) = 11h 18m 19s Dec(J2000) = +03d 36' 19" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a multi-peaked structure with a duration of about 50 sec. The peak count rate was ~1000 counts/sec (15-350 keV), at ~5 sec after the trigger. The XRT began observing the field at 02:09:15.5 UT, 126.8 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued, fading X-ray source with an enhanced position: RA, Dec 169.6119, 3.6272 which is equivalent to: RA(J2000) = 11h 18m 26.86s Dec(J2000) = +03d 37' 38.1" with an uncertainty of 2.5 arcseconds (radius, 90% containment). This location is 139 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received; the latest position is available at http://www.swift.ac.uk/sper. We cannot determine whether the source is fading at the present time. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density consistent with the Galactic value of 4.19e+20 cm^-2 (Kalberla et al. 2005). UVOT took a finding chart exposure of 150 seconds with the White filter starting 130 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The XRT position is outside of the 2.7'x2.7' sub-image. 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 expected extinction corresponding to E(B-V) of 0.05. Burst Advocate for this burst is W. H. Baumgartner (wayne AT milkyway.gsfc.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: 10747 SUBJECT: GRB 100513A: PAIRITEL NIR afterglow candidate DATE: 10/05/13 03:48:19 GMT FROM: Adam Morgan at U.C. Berkeley A. N. Morgan, D. A. Perley, C. R. Klein, and J. S. Bloom (UC Berkeley) report: We observed the location of GRB 100513A (Baumgartner et al., GCN 10746) with the 1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began at 2010-05-13 03:03:07 UT, ~0.77 hours after the Swift Trigger, after sunset. In mosaics (effective exposure time of 0.92 hours) taken simultaneously in the J, H, and Ks filters, we detect a NIR source within the XRT error circle at a location: 11:18:26.8, +03:37:40 (J2000) The preliminary photometry yields: post burst t_mid (hr) exp.(s) filt mag m_err 0.93 772 J 17.7 0.1 All magnitudes are given in the Vega system, calibrated to 2MASS. No correction for Galactic extinction has been made to the above reported values. [GCN OPS NOTE(13may10): Per author's request, the Palmer reference was change to the Baumgartner reference.] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10748 SUBJECT: GRB 100513A: SARA-N Upper Limit DATE: 10/05/13 05:26:18 GMT FROM: Adria C. Updike at Clemson U Adria C. Updike, Dieter H. Hartmann (Clemson University) and Tomomi Otani (FIT) report: We observed the field of GRB 100513A (Baumgartner et al., GCN 10746) beginning 1 hour and 55 minutes after the burst with the SARA-North 0.9m telescope located at KPNO. We do not detect the afterglow candidate (Morgan et al., 10747) in 4 minutes of stacked exposures in each of the R and I bands to a limiting magnitude of 19.5 in R and 19 in I (as compared to the USNO B1.0 catalog). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10749 SUBJECT: GRB 100513A: PAIRITEL continued observations and confirmation of fading DATE: 10/05/13 06:36:33 GMT FROM: Adam Morgan at U.C. Berkeley A. N. Morgan, D. A. Perley, C. R. Klein, and J. S. Bloom (UC Berkeley) report: We continued to observe the location of GRB 100513A (Baumgartner et al., GCN 10746) with the 1.3m PAIRITEL located at Mt. Hopkins, Arizona. The candidate afterglow (Morgan et al., GCN 10747) is detected in all three filters (J, H, and Ks) in the first epoch. The source fades between epochs, confirming that this is indeed the afterglow of GRB 100513A. The preliminary photometry yields: post burst t_mid (hr) exp.(s) filt mag m_err 0.99 1030 J 17.8 0.1 0.99 1030 H 17.2 0.1 0.99 1030 Ks 16.4 0.2 1.68 1685 J 18.0 0.1 1.68 1685 H 17.6 0.1 2.72 2855 J 18.4 0.2 All magnitudes are given in the Vega system, calibrated to 2MASS. No correction for Galactic extinction has been made to the above reported values. [GCN OPS NOTE(13may10): Per author's request, the Palmer reference was change to the Baumgartner reference.] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10750 SUBJECT: GRB 100513A: Lick observations and R-band dropout DATE: 10/05/13 07:03:07 GMT FROM: Daniel Perley at U.C. Berkeley D. A. Perley, C. R. Klein, and A. N. Morgan (UC Berkeley) report: We began observing the location of the afterglow of GRB 100513A (Baumgartner et al., GCN 10746) at 04:06 UT using the Nickel 40-inch telescope at Lick Observatory. A total of fourteen 300-second images were acquired in the R-band under clear sky conditions. A co-add of the first 9 images (midpoint 04:35 UT) reveals a faint point source at the position reported by Morgan et al (GCN 10747). The source is near the detection limit of the co-add and is not detected in individual images. Photometry of the object relative to three nearby SDSS stars (converted to Rc via the Lupton transformation equation) gives the following magnitude: R = 21.39 +/- 0.25 (t_mid = 2.46 hours) We note that this is significantly fainter than expected from the preliminary JHK magnitudes of Morgan et al (GCN 10749). The IR spectral index is relatively flat (beta~0.5), suggesting little host extinction. Assuming no extinction in addition to the Galactic value, a direct power-law extrapolation of the JHK data to R-band over-predicts the observed flux by >2 magnitudes, strongly suggesting an R-band dropout and likely redshift of 4.6 < z < 6.0. We note also that the X-ray column is consistent with no absorption beyond Galactic (Baumgartner et al.), consistent with a high-redshift origin. We encourage I/z/Y-band follow-up to better constrain the redshift and dust extinction. Spectroscopic observations are planned. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10751 SUBJECT: GRB 100513A: Enhanced Swift-XRT position DATE: 10/05/13 07:12:23 GMT FROM: Phil Evans at U of Leicester P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) report on behalf of the Swift-XRT team. Using 3728 s of XRT Photon Counting mode data and 5 UVOT images for GRB 100513A, 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 = 169.61169, +3.62774 which is equivalent to: RA (J2000): 11h 18m 26.81s Dec (J2000): +03d 37' 39.9" with an uncertainty of 1.7 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). This circular was automatically generated, and is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10752 SUBJECT: GRB 100513A: Gemini/GMOS Spectroscopic Redshift DATE: 10/05/13 07:39:53 GMT FROM: S. Bradley Cenko at Caltech S. B. Cenko, D. A. Perley, A. N. Morgan, C. R. Klein, J. S. Bloom, N. R. Butler, and B. E. Cobb (UC Berkeley) report on behalf of a larger collaboration: We have obtained an optical spectrum of the afterglow (Morgan et al., GCN 10747) of GRB 100513A (Baumgartner et al., GCN 10746) with the Gemini Multi-Object Spectrograph mounted on the 8 m Gemini North telescope. Observations began at 6:13 UT on 13 May (~ 4.1 hours after the GRB) and cover the wavelength range from 6000-10000 A. The spectrum exhibits a strong break at approximately 7000 A which we associate with a damped Ly-alpha system at z ~ 4.8. We identify a series of narrow absorption features redward of Ly-alpha, including O I 1302, Si II 1304, C II 1334, C II* 1335, Si IV 1393, 1402, Si II 1526, and C IV 1548, 1550 all at a common redshift of z = 4.772. The presence of C II*, along with Ly-alpha forest continuum emission blueward of 7000 A, strongly suggest this is the redshift of the GRB host galaxy. The presence of the Ly-alpha break at 7000 A further explains the relatively faint R-band afterglow observed by Perley et al (GCN 10750; also Updike et al., GCN 10748). We wish to thank the entire Gemini staff, in particular Richard McDermid, for the prompt execution of these observations. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10753 SUBJECT: GRB 100513A: Swift-BAT refined analysis DATE: 10/05/13 11:16:24 GMT FROM: Scott Barthelmy at NASA/GSFC T. N. Ukwatta (GWU), 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), T. Sakamoto (GSFC/UMBC), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC) (i.e. the Swift-BAT team): Using the data set from T-240 to T+962 sec from recent telemetry downlinks, we report further analysis of BAT GRB 100513A (trigger #421814) (Baumgartner, et al., GCN Circ. 10746). The BAT ground-calculated position is RA, Dec = 169.606, 3.617 deg, which is RA(J2000) = 11h 18m 25.5s Dec(J2000) = +03d 37' 00.4" with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment). The partial coding was 90%. The mask-weighted light curve shows multiple overlapping peaks starting at ~T-40 sec, peaking around T_zero, and ending at ~T+60 sec with a weak tail extending out to around T+180 sec. T90 (15-350 keV) is 84 +- 21 sec (estimated error including systematics). The time-averaged spectrum from T-64.1 to T+44.6 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.62 +- 0.14. The fluence in the 15-150 keV band is 1.4 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+1.09 sec in the 15-150 keV band is 0.6 +- 0.1 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/421814/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10754 SUBJECT: GRB 100513A: Swift XRT refined analysis DATE: 10/05/13 14:32:45 GMT FROM: Vanessa Mangano at INAF-IASFPA V. Mangano (INAF IASF Pa), B. Sbarufatti (INAF IASF Pa, INAF OAB) report on behalf the Swift XRT team: We have analysed the first four orbits of XRT data of GRB 100513A (Baumgartner et al. in GCN Circ. 10746), consisting of 154 s exposure in Windowed Timing mode (from T+130 s to T+284 s) and 9 ks exposure in Photon Counting mode (from T+285 s to T+19 ks). The UVOT-enhanced XRT position was given by Evans et al. in GCN Circ. 10751. After an initial flaring activity the light curve can be modelled with a power-law decay with an index of alpha=3.3 +/- 0.15 followed by a break at 714 +/- 40 s to an alpha=0.78 +/- 0.04. A spectrum formed from the WT[PC] mode data can be fitted with an absorbed power-law with a photon spectral index of 2.0+/-0.2 [2.3+/-0.2]. The best-fitting absorption column at the estimated redshift z=4.8 (Cenko et al. in GCN Circ. 10752) is 1.9 +/- 1.1 x 10^22 cm^-2, in excess of the Galactic value of 4.2 x 10^20 cm^-2 (Kalberla et al. 2005). Uncertainties are given at 90% c.l. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from these spectra is 3.4 x 10^-11 (4.3 x 10^-11) erg cm^-2 count^-1. If the light curve continues to decay with a power-law decay index of 0.78, the count rate at T+24 hours will be 0.004 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.4 x 10^-13 (1.7 x 10^-13) erg cm^2-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00421814. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10755 SUBJECT: GRB 100513A, RIMOTS optical upper limits DATE: 10/05/13 15:06:18 GMT FROM: Kazuhiro Noda at Miyazaki U K.Noda, N.Ohmori, A.Daikyuji, Y.Nisioka, M.Yamauchi (University of Miyazaki) We have observed the field covering the error circle of GRB GRB100513A (Swift trigger 421814, GCN 10746(Baumgartner et al.), GCN 10746(Morgan et al.), GCN 10751(Evans et al.)) with the unfiltered CCD camera on the 30-cm telescope at University of Miyazaki. The observation was started 12:52:15 UT, about 10.7 hr after the Swift trigger time. We have compared our data of 30 sec exposures with the USNO-A2.0 catalog, There is no new source at the reported position. (GCN 10746(Baumgartner et al.), GCN 10746(Morgan et al.), GCN 10751(Evans et al.)) the upper limits are as follows: -------------------------------------------------------------- Start(UT) End(UT) Num. of frames Limit (mag.) -------------------------------------------------------------- 12:52:15 12:52:45 1 14.05 12:52:15 13:51:11 42 16.78 --------------------------------------------------------------- //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10756 SUBJECT: GRB 100513A: Swift/UVOT upper limits DATE: 10/05/13 16:01:19 GMT FROM: Erik Hoversten at Swift/Penn State E. A. Hoversten (PSU) and W. H. Baumgartner (GSFC/UMBC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 100513A 130s after the BAT trigger (Baumgartner et al., GCN 10746). We do not detect any source at the enhanced Swift XRT position (Evans et al., GCN 10751) nor at the position of the PAIRITEL NIR detection (Morgan et al., GCN 10747). UVOT magnitude 3-sigma upper limits are reported in the following table: Filter T_start T_stop Exp(s) Mag (3-sigma upper limit) ------------------------------------------------------------- white 130 1707 411 > 21.29 v 618 1757 136 > 19.02 b 544 1683 116 > 19.89 u 289 1658 343 > 20.22 uvw1 667 1462 97 > 19.33 uvm2 5000 5200 196 > 19.59 uvw2 6026 6226 196 > 20.03 The quoted upper limits have not been corrected for the expected Galactic extinction along the line of sight of E_(B-V) = 0.05 mag (Schlegel et al. 1998). All photometry is on the UVOT photometric system described in Poole et al. (2008, MNRAS, 383, 627). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10757 SUBJECT: GRB 100513A: Faulkes Telescope South observations DATE: 10/05/13 16:15:41 GMT FROM: Cristiano Guidorzi at Ferrara U,Italy C. Guidorzi (U. Ferrara) & A. Gomboc (U. Ljubljana) report on behalf of a large collaboration: On 2010 May 13 at 11:44:17 UT the 2-m Faulkes Telescope South began observing the Swift GRB 100513A (Baumgartner et al., GCN Circ. 10746) using the i' filter, corresponding to 9.6 hr after the burst trigger time. We clearly detect the NIR afterglow (Morgan et al. GCN Circ. 10747, 10749) with the following magnitude: Mid time from Total Exp Filter Magnitude trigger (hr) (s) ------------------------------------------------- 9.89 6x300 i' 21.3 +- 0.2 ------------------------------------------------- Magnitude has been calibrated from nearby SDSS stars. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10758 SUBJECT: GRB 100513A: Faulkes Telescope South observations DATE: 10/05/14 15:32:58 GMT FROM: Cristiano Guidorzi at Ferrara U,Italy C. Guidorzi (U. Ferrara) & A. Gomboc (U. Ljubljana) report on behalf of a large collaboration: On 2010 May 13 at 11:44:17 UT the 2-m Faulkes Telescope South began observing the Swift GRB 100513A (Baumgartner et al., GCN Circ. 10746) using the i' filter, corresponding to 9.6 hr after the burst trigger time. We clearly detect the NIR afterglow (Morgan et al. GCN Circ. 10747, 10749) with the following magnitude: Mid time from Total Exp Filter Magnitude trigger (hr) (s) ------------------------------------------------- 9.89 6x300 i' 21.3 +- 0.2 ------------------------------------------------- Magnitude has been calibrated from nearby SDSS stars. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10768 SUBJECT: GRB 100513A: EVLA radio observation DATE: 10/05/16 22:59:55 GMT FROM: Poonam Chandra at Royal Mil. College Canada Poonam Chandra (RMC) and Dale A=2E Frail (NRAO) report on behalf of a larger collaboration: We observed GRB 100513A (Baumgartner et al. GCN 10746) with the Expanded Very Large Array (EVLA) on May 14.02 UT at a center frequency of 8.46 GHz. We do not detect any radio source anywhere within the refined XRT error circle (Evans et al., GCN 10751) to a 3-sigma limit of 60 uJy. The peak flux at the PAIRITEL afterglow position (Morgan et al., GCN 10747) is -43+/-20 uJy. The EVLA is still undergoing active commissioning and we caution that these results should be considered preliminary=2E The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities=2C Inc. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10774 SUBJECT: GRB 100513A: MITSuME Akeno Optical Observation DATE: 10/05/18 13:50:13 GMT FROM: Yoichi Yatsu at Tokyo Tech. Y.Yatsu, H. Nakajima, T. Enomoto, K. Kawakami, K. Tokoyoda, Shimokawabe, and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration: We observed the field of GRB100513A (Baumgartner et al. GCNC 10746) with the three color (g', Rc and Ic) CCD camera attached to the MITSuME 50 cm optical telescope at Akeno, Japan. The observation started at 2010-05-13 11:07:42 UT. On the combined images, we could not find the optical counterpart in the XRT error circle (GCN 10746) in the three bands. The 3-sigma upper limits based on the GSC2.3 catalog are listed below: Start(UT) -- END(UT) Total EXP[sec] g' Rc Ic ---------------------------------------------------------------- 11:07:42.1 -- 11:32:45.1 540.0 >18.9 >18.8 >18.3 14:23:16.8 -- 14:50:38.0 960.0 >17.8 >18.0 >17.4 14:50:46.5 -- 15:36:25.0 2220.0 > 19.1 > 19.0 > 18.4 ---------------------------------------------------------------- //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10820 SUBJECT: GRB 100513A: CrAO optical observations DATE: 10/06/01 20:26:58 GMT FROM: Alexei Pozanenko at IKI, Moscow V. Rumyantsev (CrAO), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We observed the field of the Swift GRB 100513A (Baumgartner et al. GCN 10746) with Shajn telescope of CrAO in R-filter between May, 13 (UT) 18:43 -- 20:38, and in I-filter on May, 14 (UT) 19:47 -- 20:57 and on May, 16 (UT) 18:28 -- 20:20. The afterglow (Morgan et al. GCN 10747) is clearly detected on May, 13,14 and not detected on May 16. The afterglow coordinates are (J2000) RA = 11 18 26.85 Dec = +03 37 40.3 with uncertainty of 0.3 arcsec. The photometry of stacked images based on USNO-B1.0 star 0936-0206849 (RA(J2000) = 11:18:37.91 Dec(J2000)= +03:37:43.1) assuming R=18.59 I=17.88 is following: T0+ Filter, Exposure, mag. Upper Limit (mid, d) (s) 0.7313 R 104x60 23.03 +/- 0.12 24.3 1.7573 I 64x60 21.59 +/- 0.07 23.6 3.7202 I 91x60 >23.5 23.5 The combined images can be found at http://grb.rssi.ru/GRB100513A/ Using above photometry combined with reported earlier (R = 21.39 at 2.46 hours, GCN 10750; J-filter photometry in GCNs 10747, 10749; i'=21.3 at 9.89 hours, GCN 10757) one can suggest taht power law index of decay light curve in J, R and I- bandpass is compatible and equal to ~0.7 in the first day. The break of power law can be assumed in I-band between first and third days with power law decay index > 2.