//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10411 SUBJECT: GRB 100213A: Swift detection of a burst DATE: 10/02/13 22:44:16 GMT FROM: Scott Barthelmy at NASA/GSFC D. Grupe (PSU), S. D. Barthelmy (GSFC), D. N. Burrows (PSU), C. Guidorzi (U Ferrara), S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), C. B. Markwardt (CRESST/GSFC/UMD), D. M. Palmer (LANL), T. Sakamoto (NASA/UMBC), B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU), M. C. Stroh (PSU), T. N. Ukwatta (GSFC/GWU) and L. Vetere (PSU) report on behalf of the Swift Team: At 22:27:48 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 100213A (trigger=412217). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 349.428, +43.383 which is RA(J2000) = 23h 17m 43s Dec(J2000) = +43d 23' 00" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows two main spikes with a total duration of about 4 sec (we can not reject a short burst). The peak count rate was ~6000 counts/sec (15-350 keV), at ~2 sec after the trigger. The XRT began observing the field at 22:29:00.8 UT, 72.7 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source with an enhanced position: RA, Dec 349.3917, 43.3796 which is equivalent to: RA(J2000) = 23h 17m 34.01s Dec(J2000) = +43d 22' 46.4" with an uncertainty of 3.2 arcseconds (radius, 90% containment). This location is 95 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 1.11e+21 cm^-2 (Kalberla et al. 2005). UVOT took a finding chart exposure of 150 seconds with the White filter starting 76 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 16% of the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. 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 0.31. Burst Advocate for this burst is D. Grupe (grupe AT astro.psu.edu). 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: 10414 SUBJECT: GRB 100213A: Swift XRT refined analysis DATE: 10/02/14 05:02:10 GMT FROM: Dirk Grupe at PSU/Swift-XRT D. Grupe (PSU) reports on behalf of the Swift-XRT team: We have analyzed 274 s of XRT data for GRB 100213A (Grupe et al. GCN Circ. 10411), from 86 s to 361 s after the BAT trigger. The data are entirely in Photon Counting (PC) mode. At this point only data of the first orbit are available. Further observations have been delayed due to the detection of GRB 100213B (Vetere et al., GCN Circ. 10412). Therefore no prediction of the future light curve is possible at this time. A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.04 (+0.45, -0.56) with the absorption column density fixed to the Galactic value of 1.1 x 10^21 cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.5 x 10^-11 (5.9 x 10^-11) erg cm^-2 count^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00412217. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10415 SUBJECT: GRB 100213A: SARA observations DATE: 10/02/14 05:05:29 GMT FROM: Adria C. Updike at Clemson U Adria C. Updike (Clemson University), Gary D. Henson (ETSU), and Dieter H. Hartmann (Clemson University) report: We observed the field of GRB 100213A (Grupe et al., GCN 10411) with the 0.9m SARA telescope located on Kitt Peak in Arizona beginning 4 hours and 11 minutes after the trigger at high airmass under good conditions. In 20 minutes of stacked exposures, we detect no new sources in the XRT error circle down to a limiting magnitude of R ~ 20 (as compared to USNO B1.0 field stars). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10418 SUBJECT: GRB 100213A: Enhanced Swift-XRT position DATE: 10/02/14 08:36:03 GMT FROM: Phil Evans at U of Leicester A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester) report on behalf of the Swift-XRT team. Using 273 s of XRT Photon Counting mode data and 1 UVOT images for GRB 100213A, 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 = 349.39183, +43.37892 which is equivalent to: RA (J2000): 23h 17m 34.04s Dec (J2000): +43d 22' 44.1" with an uncertainty of 2.2 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: 10420 SUBJECT: GRB 100213A: Swift/UVOT Upper Limits DATE: 10/02/14 12:39:40 GMT FROM: Peter Curran at MSSL P.A. Curran (MSSL-UCL) and D. Grupe (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 100213A 77s after the BAT trigger (Grupe et al., GCN 10411). No optical afterglow consistent with the XRT position (Beardmore et al., GCN 10418) is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627) for the first exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag ------------------------------------------------ white 77 227 147 >20.20 v 59 68 9 >17.19 u 289 366 75 >19.7 The values quoted above are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.31 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10424 SUBJECT: GRB 100213A: Swift-BAT refined analysis DATE: 10/02/15 14:25:12 GMT FROM: Scott Barthelmy at NASA/GSFC S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), D. Grupe (PSU), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL), T. Sakamoto (GSFC/UMBC), J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-61 to T+242 sec from telemetry downlinks, we report further analysis of BAT GRB 100213A (trigger #412217) (Grupe, et al., GCN Circ. 10411). The BAT ground-calculated position is RA, Dec = 349.379, 43.370 deg which is RA(J2000) = 23h 17m 31.0s Dec(J2000) = +43d 22' 13.1" with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment). The partial coding was 59%. The mask-weighted light curve shows four spikes between ~T-0.7 and ~T+2.5 sec plus a low level tail out to ~T+40 sec. T90 (15-350 keV) is 2.4 +- 0.4 sec (estimated error including systematics). The time-averaged spectrum from T-0.7 to T+2.2 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.34 +- 0.15. The fluence in the 15-150 keV band is 2.7 +- 0.3 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T+1.01 sec in the 15-150 keV band is 2.1 +- 0.2 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/412217/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10425 SUBJECT: GRB 100213A: GRT Optical Observation DATE: 10/02/15 20:29:56 GMT FROM: Takanori Sakamoto at NASA/GSFC T. Sakamoto (UMBC/GSFC), D. Donato (ORAU/GSFC), N. Gehrels (GSFC), T. Okajima (JHU/GSFC), Y. Urata (NCU), C.A. Wallace (FGCU) We observed the field of GRB 100213A detected by Swift (trigger #412217; Grupe et al., GCN Circ. 10411) with the 14-inch Goddard Robotic Telescope (GRT) located at the Goddard Geophysical and Astronomical Observatory (http://cddisa.gsfc.nasa.gov/ggao/). Total 49 images of 60 sec exposures were taken in the R filter starting from February 13 23:42:02 (UT) about 1.2 hours after the trigger and stopped on February 14 01:28:00 (UT). We do not detect the optical afterglow both in the individual images and the combined image inside the XRT position (Beardmore et al., GCN #10418). The estimated three sigma upper limit of the combined image (total exposure of 1800 sec; excluding bad quality images) is ~17.5 mag using the USNO-B1 catalog. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10427 SUBJECT: GRB 100213A: Swift-BAT lag analysis indicates probably SHB DATE: 10/02/16 19:05:36 GMT FROM: Scott Barthelmy at NASA/GSFC J. P. Norris (U. Denver), S. D. Barthelmy (GSFC), N. Gehrels (GSFC), and D. Grupe (PSU) report: Temporal analysis of BAT data for GRB 100213A suggests that the burst is likely a member of the short, hard class: Structures in the burst's most intense pulse complex are as short as ~ 10-25 ms, typical of most short bursts. Spectral lag analysis of this most intense pulse complex indicate a lag between BAT channels 4 (100-350 keV) and 2 (25-50 keV) of ~ 5 ms +- 15 ms. For the whole event, the lag between these same channels is ~ 15 ms +- 15 ms. A Bayesian Block analysis reveals no significant emission after the T90 duration of 2.4 s (reported in GCN circ. 10424, Barthelmy et al.) for ~ 400 s following the BAT trigger time. This is inconsistent only at the 2-sigma level with the finding in Circ 10424 that there was "low level emission out to T+40 sec", and we further note that this emission is only in the 15-25 keV band. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10446 SUBJECT: GRB 100213B R band observations DATE: 10/02/22 18:00:16 GMT FROM: Janos Kelemen at Konkoly Obs/Hungary GRB 100213B R band observations J. Kelemen (kelemen at konkoly.hu) on behalf of the GRB OT observing program at the Konkoly Observatory. On 15 february 2010 19:56:20 UT we observed the field of GRB 100213B detected by Swift (trigger #412220; Vetere et al., GCN 10412) with a 60/90 cm Schmidt telescope located at the Mountain Station of the Konkoly Observatory using R filter. The total exposure of the coadded images were 2700 s. We examined both the XRT position and the position reported D. Malesani et al. GCN 10413. No new object brighter than 21.3 +/- 0.2 was found. Time Mag Error. Flag. [s] [R] [1-sigma] ------------------------------------- 161866 21.30 0.2 Upper Limit ------------------------------------- This message can be cited.