//////////////////////////////////////////////////////////////////////// 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: 10412 SUBJECT: GRB 100213B: Swift detection of a burst DATE: 10/02/13 23:12:15 GMT FROM: Scott Barthelmy at NASA/GSFC L. Vetere (PSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), D. N. Burrows (PSU), J. M. Gelbord (PSU), D. Grupe (PSU), 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), F. E. Marshall (NASA/GSFC), C. Pagani (PSU), D. M. Palmer (LANL), T. Sakamoto (NASA/UMBC), M. H. Siegel (PSU), M. C. Stroh (PSU) and T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team: At 22:58:34 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 100213B (trigger=412220). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 124.338, +43.455 which is RA(J2000) = 08h 17m 21s Dec(J2000) = +43d 27' 19" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a FRED-like pulse structure with a duration of about 30 sec. The peak count rate was ~1000 counts/sec (15-350 keV), at ~2 sec after the trigger. The XRT began observing the field at 23:01:03.7 UT, 149.5 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 124.2858, +43.4473 which is equivalent to: RA(J2000) = 08h 17m 08.59s Dec(J2000) = +43d 26' 50.2" with an uncertainty of 5.2 arcseconds (radius, 90% containment). 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 1.75e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 77 seconds with the White filter starting 157 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 100% of the XRT error circle. The 3-sigma upper limit is about 20.5 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 0.08. Burst Advocate for this burst is L. Vetere (vetere 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: 10413 SUBJECT: GRB 100213B: NOT optical observations DATE: 10/02/14 00:44:21 GMT FROM: Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst D. Malesani (DARK/NBI), N.R. Tanvir (Univ. Leicester), D. Xu (WIS, DARK/NBI), G. Leloudas (DARK/NBI), P. Jakobsson (Univ. Iceland), A. Somero, and S. Katajainen (Tuorla Obs.), report on behalf of a larger collaboration: We observed the field of GRB 100213B (Vetere et al., GCN 10412) with the NOT equipped with ALFOSC. Due to adverse weather, we could only obtain one 5-min R-band exposure, starting on Feb 13.970 UT (19 min after the GRB). We find an object with R ~ 21.5 located just outside the edge of the XRT error circle, at coordinates RA = 08:17:07.97, Dec = +43:26:54.6. This location is 8 arcsec away of the X-ray position, which has a reported error radius of 5.2" (Vetere et al., GCN 10412). The object seems elongated in our image. However, it is not visible in the SDSS data of this field, and may therefore be the afterglow of GRB 100213B. Inside the XRT error circle, there is also a possible source close to our image detection limit (R ~ 22.2), at coordinates RA = 08:17:08.48, Dec = +43:26:50.3 (0.8" uncertainty). Given the low S/N, the reality of this source cannot be confirmed. Further observations are encouraged. The NOT may attempt again later tonight depending on the weather conditions. //////////////////////////////////////////////////////////////////////// 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: 10416 SUBJECT: GRB 100213B: Swift XRT refined analysis DATE: 10/02/14 05:07:53 GMT FROM: Loredana Vetere at PSU L. Vetere (PSU) reports on behalf of the Swift-XRT team: We have analysed 1.7 ks of XRT data for GRB 100213B (Vetere et al. GCN Circ. 10412), from 155 s to 5.7 ks after the BAT trigger. The data comprise 500 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. Using 1.2ks of XRT Photon Counting mode data we find a refined XRT position: RA, Dec = 124.28384, 43.44683 which is equivalent to: RA (J2000): 08h 17m 08.12s Dec (J2000): +43d 26' 48.6" with an uncertainty of 4.9 arcsec (radius, 90% confidence). The light curve can be modelled with a power-law decay with a decay index of alpha=2.06 (+0.10, -0.08). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.47 (+/-0.12). The best-fitting absorption column is 1.3 (+0.4, -0.3) x 10^21 cm^-2, in excess of the Galactic value of 5.9 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 4.9 x 10^-11 (5.6 x 10^-11) erg cm^-2 count^-1. If the light curve continues to decay with a power-law decay index of 2.06, the count rate at T+24 hours will be 6.9 x 10^-5 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.4 x 10^-15 (3.9 x 10^-15) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00412220. This circular is an official product of the Swift-XRT team.//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10417 SUBJECT: GRB 100213B: Swift-BAT refined analysis DATE: 10/02/14 05:56:33 GMT FROM: Scott Barthelmy at NASA/GSFC S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), 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), T. N. Ukwatta (GWU), L. Vetere (PSU) (i.e. the Swift-BAT team): Using the data set from T-61 to T+242 sec from recent telemetry downlinks, we report further analysis of BAT GRB 100213B (trigger #412220) (Vetere, et al., GCN Circ. 10412). The BAT ground-calculated position is RA, Dec = 124.320, 43.464 deg which is RA(J2000) = 08h 17m 16.8s Dec(J2000) = +43d 27' 51.7" with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment). The partial coding was 56%. The mask-weighted light curve shows a FRED-like pulse starting at ~T-5 sec, peaking at ~T+5 sec, and ending at ~T+150 sec. Because the burst goes out of the BAT FOV at T+250 sec (due to an observing constraint), we can not tell if there if any detectable activity past T+250 sec. T90 (15-350 keV) is 48.0 +- 16.0 sec (estimated error including systematics). The time-averaged spectrum from T-12.7 to T+35.3 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 1.13 +- 0.61, and Epeak of 39.1 +- 8.8 keV (chi squared 58.8 for 56 d.o.f.). The 1-sec peak flux measured from T+10.76 sec in the 15-150 keV band is 0.5 +- 0.2 ph/cm2/sec. A fit to a simple power law gives a photon index of 2.04 +- 0.13 (chi squared 67.0 for 57 d.o.f.). 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/412220/BA/ //////////////////////////////////////////////////////////////////////// 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: 10419 SUBJECT: GRB 100213B: PAIRITEL NIR Upper Limits DATE: 10/02/14 08:57:49 GMT FROM: Adam Morgan at U.C. Berkeley A. N. Morgan, B. E. Cobb, C. R. Klein, J. S. Bloom (UC Berkeley), report: We observed the field of GRB 100213B (Vetere et al., GCN 10412) with the 1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began under good weather conditions at 2010-02-14 02:53:48 UT, ~3.92 hours after the Swift trigger. In mosaics (effective exposure time of ~2387 seconds) taken simultaneously in the J, H, and Ks filters, we do not detect any sources within the XRT error circle, nor at the potential NOT position (Malesani et al., GCN 10413). The preliminary photometry yields: post_burst t_mid(h) exp(s) filt U. Limit (3 sig) 4.44 2387 J > 19.2 4.44 2387 H > 18.2 4.44 2387 Ks > 17.1 Observations are ongoing. All magnitudes given in the Vega system, calibrated to 2MASS. No correction for Galactic extinction has been made to the above reported values. //////////////////////////////////////////////////////////////////////// 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: 10421 SUBJECT: GRB 100213B: Swift/UVOT Upper Limits DATE: 10/02/14 12:39:59 GMT FROM: Peter Curran at MSSL P.A. Curran (MSSL-UCL) and L. Vetere (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 100213B 158 s after the BAT trigger (Vetere et al., GCN 10412). No optical afterglow consistent with the XRT position (Vetere et al., GCN 10416) or the NOT R-band position (Malesani et al., GCN 10413) 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 initial exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag -------------------------------------------------- white 158 4654 273 >21.17 v 3430 5065 393 >19.64 b 4250 5722 233 >20.38 u 4044 5679 393 >20.38 w1 3840 5475 393 >20.31 m2 3634 5269 393 >21.10 w2 4660 4860 197 >20.00 The values quoted above are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.08 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10422 SUBJECT: GRB 100213B: Gemini-N Observations DATE: 10/02/14 13:52:00 GMT FROM: Antonino Cucchiara at PSU A. Cucchiara (PSU), R. Chornock (Harvard),D. B. Fox (PSU), E. Berger (Harvard), report on behalf of a larger collaboration: "We observed the field of GRB 100213B (Vetere et al., GCN 10412) with GMOS on the Gemini-North 8-m telescope starting on 2010 Feb 14.24 (~7 hours after the burst). Inside the refined XRT error circle (GCN #10416) we detect no new sources in a 2 min r-band acquisition image. Outside the XRT error circle we clearly detect the source reported by Malesani et al. (GCN #10413). We then obtain 2x1200s spectra on this source at central wavelength 8000A. We detect [OII]3727, H-beta and [OIII]5007 at the common redshift of z =0.604. At this point is not clear whether this object is related to GRB 100213B. We thank the Gemini staff for performing this observation, in particular Tom Geballe." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10423 SUBJECT: GRB 100213B: Enhanced Swift-XRT position DATE: 10/02/14 17:42:01 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team. Using 819 s of XRT Photon Counting mode data and 1 UVOT image for GRB 100213B, 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 = 124.28226, +43.44773 which is equivalent to: RA (J2000): 08h 17m 7.74s Dec (J2000): +43d 26' 51.8" with an uncertainty of 3.5 arcsec (radius, 90% confidence). This position is 3.7" from the object reported by Malesani et al. (GCN Circ. 10413) and Cucchiara et al (GCN Circ. 10422). Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// 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: 10426 SUBJECT: GRB 100213B: GRT Optical Observation DATE: 10/02/15 20:34:15 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 100213B detected by Swift (trigger #412220; Vetere et al., GCN Circ. 10412) with the 14-inch Goddard Robotic Telescope (GRT) located at the Goddard Geophysical and Astronomical Observatory (http://cddisa.gsfc.nasa.gov/ggao/). Total 59 images of 60 sec exposures were taken in the R filter starting from February 13 23:55:15 (UT) about 0.94 hours after the trigger and stopped on February 14 01:50:46 (UT). We do not detect the optical afterglow both in the individual images and the combined image inside the XRT position (Evans, GCN #10423). The estimated three sigma upper limit of the combined image (total exposure of 3540 sec) is ~18.7 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. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10454 SUBJECT: GRB 100213B: Mondy optical observations DATE: 10/02/26 02:54:05 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Klunko (ISTP), A. Volnova (SAI MSU), A. Pozanenko (IKI) on behalf of larger GRB follow up collaboration report: We observed the field of GRB 100213B (Vetere et al., GCN 10412) with AZT-33IK telescope of Sayan observatory (Mondy) starting Feb. 14 (UT) 14:54:31. We do not detect any sources in enhanced XRT error circle (Evans, GCN 10423). The upper limit (3 sigma) of stacked image is based on USNO-B1.0 nearby stars: T0+ Filter, Exposure, mag. (mid, d) (s) 0.6801 R 94x30 > 20.80 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 10913 SUBJECT: GRB 100213B: Detection of Fading Optical Afterglow DATE: 10/06/30 23:03:00 GMT FROM: Jules Halpern at Columbia U. Y. Li, J. Weston, X. Fernandez, A. Brown, J. H. Yoon, A. P. S. Crotts, and J. P. Halpern (Columbia U.) report on behalf of the graduate Observational Astronomy class: "We obtained R-band images of the field of Swift GRB 100213B (Vetere et al., GCN 10412) on two consecutive, photometric nights using the MDM 1.3m telescope, for total exposure times of 30 and 40 minutes, respectively. Within 3.8" of the enhanced Swift XRT afterglow position (of 90% confidence radius 3.5", Evans, GCN 10423), we find a fading object at (J2000) R.A. = 08h 17m 07.94s, Decl. = +43d 26' 54.94" with positional uncertainty ~0.5", and the following magnitudes: ---------------------------------------------------------- Date(UT) Mid-time(UT) t-t0(hr) Exp(min) R(mag) ---------------------------------------------------------- Feb. 14 03:44 4.8 30 22.00+/-0.14 Feb. 15 03:35 28.6 40 23.01+/-0.24 ---------------------------------------------------------- Magnitudes are referenced to Landolt (1992) standard stars, and are not corrected for Galactic extinction. The position of the afterglow coincides with the R ~ 21.5 object detected by Malesani et al. (GCN 10413) 19 minutes after the GRB, and whose redshift z = 0.604 was measured by Cucchiara et al. (GCN 10422). We conclude that the observed variability and positional coincidence with an emission-line object establishes the optical afterglow and host galaxy redshift of GRB 100213B. Further observations of the host galaxy are encouraged. MDM images of the field are posted at http://www.astro.columbia.edu/~jules/grb/100213b/ This message may be cited."