GRB100814A

This page lists all entries on GRB100814A in GRBweb

Summary Fermi GBM IPN Swift GCN 11086 GCN 11087 GCN 11088 GCN 11089 GCN 11090 GCN 11091 GCN 11092 GCN 11093 GCN 11094 GCN 11095 GCN 11096 GCN 11097 GCN 11098 GCN 11099 GCN 11100 GCN 11107 GCN 11118 GCN 11119 GCN 11121 GCN 11122 GCN 11129 GCN 11131 GCN 11133 GCN 11134 GCN 11153

Summary table
Variable Value Source
GRB_name_Fermi GRB100814160
T0 3:50:08.809 UTC Fermi_GBM
ra 22.4734° Swift
decl -17.9954° Swift
pos_error 7.77e-05° Swift
T90 150.53 s Fermi_GBM
T90_error 1.619 s Fermi_GBM
T90_start 3:50:09.385 UTC Fermi_GBM
fluence 1.49e-05 erg/cm² Fermi_GBM
fluence_error 9.47e-08 erg/cm² Fermi_GBM
redshift 1.4400
T100 176.691 s
GBM_located False
mjd 55422.15982417824 Fermi_GBM
Fermi GBM table
GRB_name_Fermi GRB100814160
trigger_name bn100814160
ra 22.4721°
decl -17.9964°
pos_error 2.80e+00°
datum 2010-08-14
t_trigger 3:50:08.809 UTC
T90 150.53 s
T90_error 1.619 s
T90_start 3:50:09.385 UTC
fluence 1.49e-05 erg/cm²
fluence_error 9.47e-08 erg/cm²
flux_1024 4.60e+00 erg/cm²/s
flux_1024_error 2.81e-01 erg/cm²/s
flux_1024_time 6.78e+00 erg/cm²/s
flux_64 6.94e+00 erg/cm²/s
flux_64_error 1.41e+00 erg/cm²/s
IPN table
GRB_name GRB100814A
ra 22.4792°
decl -17.9833°
pos_error 5.00e-02°
redshift 1.4400
Swift table
GRB_name GRB100814A
t_trigger 3:50:11 UTC
ra 22.4734°
decl -17.9954°
pos_error 7.77e-05°
T90 174.5 s
fluence 9.00e-06 erg/cm²
redshift 1.4400
GCN 11086 table
GRB_name GRB100814A
GCN_number 11086
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 11086 SUBJECT: GRB 100814A: ROTSE-III Detection of Optical Counterpart DATE: 10/08/14 04:14:34 GMT FROM: Brad Schaefer at LSU B. E. Schaefer (Louisiana State), E.S. Rykoff (UCSB), W. Rujopakarn (Steward), S. B. Pandey (U Mich), W. Zheng (U Mich), report on behalf of the ROTSE collaboration: ROTSE-IIIc, located at the H.E.S.S. site at Mt. Gamsberg, Namibia, responded to GRB 100814A (Swift trigger 431605). The first image was at 03:55:01.1 UT, 289.8 s after the burst (4.1 s after the GCN notice time). The unfiltered images are calibrated relative to USNO A2.0. We detect a new object, not visible in the DSS (second epoch), nor in our first set of observations with coordinates: 01:29:53.67 -17:59:41.58 (J2000), with positional uncertainty of 1" or better start UT mag mlim(of image) ---------------------------------- 03:55:11.3 17.4 8.0 A jpeg image is available at http://www.rotse.net/images/gsq431605_3c011-020_key.jpg Note that the object marked 29 is the candidate in question. Continuing observations are in progress.
GCN 11087 table
GRB_name GRB100814A
GCN_number 11087
Detection_method Swift Det
t_trigger 3:50:11 UTC
ra 22.4810°
decl -17.9860°
Circular_text TITLE: GCN CIRCULAR NUMBER: 11087 SUBJECT: GRB 100814A: Swift detection of a burst with an optical afterglow DATE: 10/08/14 04:22:40 GMT FROM: David Palmer at LANL A. P. Beardmore (U Leicester), J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU), N. P. M. Kuin (UCL-MSSL), O. M. Littlejohns (U Leicester), C. B. Markwardt (NASA/GSFC), K. L. Page (U Leicester), D. M. Palmer (LANL), C. J. Saxton (UCL-MSSL), R. L. C. Starling (U Leicester), E. Troja (NASA/GSFC/ORAU) and T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team: At 03:50:11 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 100814A (trigger=431605). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 22.481, -17.986 which is RA(J2000) = 01h 29m 55s Dec(J2000) = -17d 59' 07" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed three separate peaks over a total interval of at least 150 sec. The peak count rate was ~6000 counts/sec (15-350 keV), at ~6 sec after the trigger. The XRT began observing the field at 03:51:38.6 UT, 87.4 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source located at RA, Dec 22.47220, -17.99643 which is equivalent to: RA(J2000) = 01h 29m 53.33s Dec(J2000) = -17d 59' 47.1" with an uncertainty of 3.8 arcseconds (radius, 90% containment). This location is 48 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. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density consistent with the Galactic value of 1.75e+20 cm^-2 (Kalberla et al. 2005). The initial flux in the 2.5 s image was 6.18e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 250 seconds with the U filter starting 153 seconds after the BAT trigger. A bright optical afterglow candidate was found at RA=22.4749, dec=-17.9932 which is RA = 01h 29m 53.98s Dec=-17d 59m 35.5s (J2000). The estimated magnitude is U=16.8 . Burst Advocate for this burst is C. J. Saxton (cjs2 AT mssl.ucl.ac.uk). 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.)
GCN 11088 table
GRB_name GRB100814A
GCN_number 11088
Detection_method Swift-UVOT Det
ra 22.4731°
decl -17.9954°
Circular_text TITLE: GCN CIRCULAR NUMBER: 11088 SUBJECT: GRB 100814A: Swift UVOT observations of the optical afterglow DATE: 10/08/14 04:49:29 GMT FROM: Caryl Gronwall at PSU/Swift-UVOT C. Gronwall (PSU) and C. J. Saxton (MSSL) report on behalf of the Swift/UVOT team: In response to GRB 100814A (Swift/BAT trigger 431605) at 03:50:11 UT, UVOT took a finding chart exposure of 250 seconds with the U filter starting 153 seconds after the BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 01:29:53.54 = 22.47309 DEC(J2000) = -17:59:43.5 = -17.99541 with a 90%-confidence error radius of about 0.75 arc sec. This position is 4.7 arc sec. from the center of the XRT error circle. This position supersedes the position given in (Beardmore et al., GCN Circ. 11087) and is consistent with the optical afterglow position from ROTSE (Schaefer et al., GCN Circ. 11086). The estimated magnitude is 16.76 with a 1-sigma error of about 0.14. No correction has been made for the expected extinction corresponding to E(B-V) of 0.02.
GCN 11089 table
GRB_name GRB100814A
GCN_number 11089
Detection_method Other
redshift 1.4400
Circular_text TITLE: GCN CIRCULAR NUMBER: 11089 SUBJECT: GRB100814A: Magellan Echellette Observations DATE: 10/08/14 05:09:50 GMT FROM: Hsiao-Wen Chen at U Chicago John O'Meara (Saint Michael's College), Hsiao-Wen Chen (UChicago), Jason X. Prochaska (UC Santa Cruz) report on behalf of a larger collaboration: "We observed the afterglow of GRB100814A reported by Schaefer et al. (GCN 11086) and confirmed by Gronwall et al. (GCN 11088) using the MagE echellette spectrograph on the Magellan Clay Telescope. The observations started at UT 04:46 on August 14, 2010, ~ one hour after the inital trigger. We obtained a 900s exposure. Our preliminary reduction shows that the afterglow spectrum displays absorption transitions due to AlIII, FeII, and MgII at redshift z=1.44, which we tentatively identify as the host redsdhift of the GRB. Further analysis is underway. This message may be cited."
GCN 11090 table
GRB_name GRB100814A
GCN_number 11090
Detection_method Optical
ra 22.4317°
decl -18.0107°
Circular_text TITLE: GCN CIRCULAR NUMBER: 11090 SUBJECT: GRB 100814A: IAC80 R-band observations DATE: 10/08/14 05:52:08 GMT FROM: Javier Gorosabel at IAA-CSIC J. Gorosabel (IAA-CSIC), S. Rodriguez LLano (IAC), A.J. Castro-Tirado (IAA-CSIC), report on behalf of a larger collaboration: "Following the detection of GRB 100814A by Swift (Beardmore et al. GCNC 11087) we have acquired a series of R-band images with the 0.82-m IAC80 telescope at Observatory of Teide, Tenerife, Spain. The first exposure started on Aug 14.1788 UT (~27.3 minutes post burst). The optical afterglow (Schaefer et al. GCNC 11086; Gronwall et al. GCN 11088) is detected with a preliminary magnitude of R~18.7, assuming a magnitude of R=16.87 for the USNO-B1.0 star placed at RA(J2000)=01:29:43.606, DEC(J2000)=-18:00:38.61."
GCN 11091 table
GRB_name GRB100814A
GCN_number 11091
Detection_method GROND
redshift 1.4400
Circular_text TITLE: GCN CIRCULAR NUMBER: 11091 SUBJECT: GRB 100814A: GROND Detection of the Optical/NIR Afterglow DATE: 10/08/14 11:20:51 GMT FROM: Patricia Schady at MPE/Swift R. Filgas, P. Schady and J. Greiner (MPE Garching) report on behalf of the GROND team: We observed the field of GRB 100814A (Swift trigger 431605; Beardmore et al., GCN #11087) 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 at 03:57 UT, 7 minutes after the GRB trigger at 03:50 UT, and are continuing. They were performed at an average seeing of 1.2" and at an average airmass of 2. We detect a single point source in all GROND optical (g'r'i'z') and NIR bands (JHK) at a position consistent with the coordinates provided by Schaefer et al. (GCN #11086) and Gronwall et al. (GCN #11088), and consistent with the spectroscopic redshift of z=1.44 (O'Meara et al. GCN #11089). The afterglow decays as a power law with a best-fit index of alpha ~ 0.5, decaying from r' = 18.0 +/- 0.1 at T+25 minutes down to r' = 19.5 +/- 0.1 (all in AB system) by the end of our observations, at T+6 hours. Analysis is on going. Given magnitudes are calibrated against USNO zeropoints and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E(B-V)=0.02 in the direction of the burst (Schlegel et al. 1998).
GCN 11092 table
GRB_name GRB100814A
GCN_number 11092
Detection_method Swift-XRT Det
ra 22.4731°
decl -17.9950°
Circular_text TITLE: GCN CIRCULAR NUMBER: 11092 SUBJECT: GRB 100814A: Enhanced Swift-XRT position DATE: 10/08/14 12:17:34 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 5031 s of XRT Photon Counting mode data and 6 UVOT images for GRB 100814A, 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 = 22.47308, -17.99503 which is equivalent to: RA (J2000): 01h 29m 53.54s Dec (J2000): -17d 59' 42.1" with an uncertainty of 1.5 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.
GCN 11093 table
GRB_name GRB100814A
GCN_number 11093
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 11093 SUBJECT: GRB 100814A: CQUEAN r- and i-band Observation DATE: 10/08/14 12:59:28 GMT FROM: Myungshin Im at Seoul Nat U Myungshin Im, Won-Kee Park (CEOU/Seoul National Univ), Soojong Pak, Hyeongju Jeong, Eunbin Kim, and Jinyoung Kim (Kyunghee University) We observed GRB 100814A (Beardmore et al. GCN 11087) with the SDSS r- and i-filters during the commissioning run of CQUEAN (the Camera for QUasars in the Early uNiverse) on the 2.1m telescope at the McDonald Observatory. The observation started at 2010 August 14, 08:57:54 UT, about 5 hours after the BAT trigger. A series of 180 secs exposures were taken, and we confirm the afterglow at the location reported by Schaefer et al. (GCN 11086) and Gorosabel et al.(GCN 11090). A preliminary photometry from a single frame with the mid-point time of 09:00:24 UT is r ~ 19.10 +- 0.03 AB mag (subject to systematic error in the zero point determination), consistent with the value reported by Filgas et al. (GCN 11091). The photometric calibration is based on a standard star observation on the same night (BD+17 4708). We thank the staffs of the McDonalnd Observatory, Peter S. Odoms and John Kuehne for their assistance of the CQUEAN commissioning run.
GCN 11094 table
GRB_name GRB100814A
GCN_number 11094
Detection_method Swift-BAT Det
ra 22.4790°
decl -17.9900°
Circular_text TITLE: GCN CIRCULAR NUMBER: 11094 SUBJECT: GRB 100814A, Swift-BAT refined analysis DATE: 10/08/14 13:16:56 GMT FROM: Takanori Sakamoto at NASA/GSFC H. A. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL), A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 100814A (trigger #431605) (Beardmore, et al., GCN Circ. 11087). The BAT ground-calculated position is RA, Dec = 22.479, -17.990 deg which is RA(J2000) = 01h 29m 55.0s Dec(J2000) = -17d 59' 25.7" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 90%. The mask-weighted light curve shows three FRED-like spikes starting around T-4 sec, T+60 sec and T+140 sec. Those spikes peak around T+5 sec, T+70 sec and T+145 sec. The low level emission is visible up to T+235 sec. T90 (15-350 keV) is 174.5 +- 9.4 sec (estimated error including systematics). The time-averaged spectrum from T-3 to T+235 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.47 +- 0.04. The fluence in the 15-150 keV band is 9.0 +- 0.2 x 10^-06 erg/cm2. The 1-sec peak photon flux measured from T-0.06 sec in the 15-150 keV band is 2.5 +- 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/431605/BA/
GCN 11095 table
GRB_name GRB100814A
GCN_number 11095
Detection_method Swift-UVOT Det
ra 22.4734°
decl -17.9954°
Circular_text TITLE: GCN CIRCULAR NUMBER: 11095 SUBJECT: Swift/UVOT observations of GRB100814A DATE: 10/08/14 15:26:23 GMT FROM: Patricia Schady at MPE/Swift M. De Pasquale (MSSL-UCL) and C.J. Saxton (MSSL-UCL) report on the behalf of the Swift UVOT team: The Swift/UVOT began settled observations of the field of GRB 100814A 153 s after the BAT trigger (Beardmore et al. 2010, GCN Circ. 11087) with a finding chart in the u filter. We detect the optical afterglow in all filters except uvw2. The refined UVOT position is RA (J2000) = 01h 29m 53.61s = 22.47338 Dec (J2000) = -17d 59m 43.6s = -17.99545 with an estimated uncertainty of 0.6 arcsec (radius, 90% confidence, statistical + systematic). This is about 1.5 arcsec north of the UVOT-enhanced XRT position (Beardmore et al. 2010, GCN Circ. 11092). Preliminary magnitudes, and 3-sigma upper limits for detecting a source in the finding charts and in co-added images are Filter T_start T_stop Exp(s) Mag Err --------------------------------------------------------------------- u (fc) 153 403 246 16.80 0.06 v 458 627 39 17.91 0.32 b 408 721 53 21.22 0.20 u 153 701 285 16.84 0.06 uvw1 507 676 39 17.33 0.20 uvm2 483 651 39 17.86 0.31 uvw2 434 602 39 >18.52 3-sigma UL white 3858 4211 344 18.63 0.07 ----------------------------------------------------------- The quoted magnitudes and upper limits have not been corrected for the expected Galactic extinction along the line of sight corresponding to a reddening of E_{B-V} = 0.02 mag (Schlegel, et al., 1998, ApJS, 500, 525). All photometry is on the UVOT photometry system described in Poole et al. (2008, MNRAS, 383, 627).
GCN 11096 table
GRB_name GRB100814A
GCN_number 11096
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 11096 SUBJECT: GRB 100814A: Swift-XRT refined analysis DATE: 10/08/14 20:34:14 GMT FROM: Andy Beardmore at U Leicester A. P. Beardmore (U Leicester) and C. J. Saxton (MSSL-UCL) report on behalf of the Swift-XRT team: We have analysed 6.0 ks of XRT data for GRB 100814A (Beardmore et al. GCN Circ. 11087), from 76 s to 28.6 ks after the BAT trigger. The data comprise 721 s in Windowed Timing (WT) mode (the first 9 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Beardmore et al. (GCN. Circ 11092). The X-ray light curve initially rises by a factor of ~2 in count rate, reaching a broad peak at approximately T+160 s after the trigger, on top of which are superimposed three small flares at T+146, 176 and 220 s, respectively. At T+295 s the light curve falls with a steep decay of alpha=5.7 (+0.4, -0.3), then breaks to a shallow decay at T+517 s, after which it decays with an index of 0.47 (+0.03, -0.04). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.68 (+0.04, -0.03). The best-fitting absorption column is 5.0 (+/-0.8) x 10^20 cm^-2, in excess of the Galactic value of 1.8 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index of 1.90 (+0.11, -0.10) and a best-fitting absorption column of 3.1 (+2.2, -1.4) x 10^20 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.8 x 10^-11 (4.2 x 10^-11) erg cm^-2 count^-1. If the light curve continues to decay with a power-law decay index of 0.47, the count rate at T+24 hours will be 0.18 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.0 x 10^-12 (7.7 x 10^-12) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00431605. This circular is an official product of the Swift-XRT team.
GCN 11097 table
GRB_name GRB100814A
GCN_number 11097
Detection_method Swift-UVOT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 11097 SUBJECT: Swift/UVOT Observations of GRB100814A - a clearer table. DATE: 10/08/15 09:33:27 GMT FROM: Massimiliano de Pasquale at MSSL-UCL M. De Pasquale (MSSL-UCL) and C.J. Saxton (MSSL-UCL) report on the behalf of the Swift UVOT team: In the GCN circ 11095 (Swift/UVOT observations of GRB100814A) the table containing the information on epochs and magnitudes could not be read well because of a formatting problem. In the following, we rewrite the table with a clearer look. We apologize for any inconvenience it might have caused. Filter T_start T_stop Exp(s) Mag Err ---------------------------------------------------------- u (fc) 153 403 246 16.80 0.06 v 458 627 39 17.91 0.32 b 408 721 53 21.22 0.20 u 153 701 285 16.84 0.06 uvw1 507 676 39 17.33 0.20 uvm2 483 651 39 17.86 0.31 uvw2 434 602 39 >18.52 3-sigma UL white 3858 4211 344 18.63 0.07 ---------------------------------------------------------- [GCN OPS NOTE(15aug10): Per author's request, the "B" in the Subject line was changed to "A".]
GCN 11098 table
GRB_name GRB100814A
GCN_number 11098
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 11098 SUBJECT: GRB 100814A: Submm observations from APEX DATE: 10/08/15 12:02:52 GMT FROM: Antonio Deugarte at IAA-CSIC A. de Ugarte Postigo (INAF-OAB, DARK/NBI), C. de Breuck, A.J. Castro-Tirado (IAA-CSIC), G. Siringo, F.M. Montenegro-Montes, M. Martinez (APEX), A. Hacar (OAN), T. Stanke, A. Lundgren, M. Dumke (ESO) report on behalf of a larger collaboration: "We have observed the field of GRB 100418A (Beardmore et al. GCNC 11087) using LABOCA/APEX at Chajnantor (Chile) in the 345 GHz band. Observations began on 15th August at 05:39 UT (25.8 hours after the burst onset). In a preliminary analysis we do not detect any new source at the position of the afterglow (Schaefer et al. GCNC 11086, De Pasquale et al. GCNC 11095) down to a 3-sigma limit of 5.4 mJy. The formal flux density at the position of the afterglow is 4.6+/-1.8 mJy."
GCN 11099 table
GRB_name GRB100814A
GCN_number 11099
Detection_method Fermi GBM Det
t_trigger 3:50:08.810 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 11099 SUBJECT: GRB 100814A: Fermi GBM observation DATE: 10/08/15 12:23:54 GMT FROM: Andreas von Kienlin at MPE A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team: "At 03:50:08.81 UT on 14 August 2010, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 100814A (trigger 303450610 / 100814160), which was also detected by the Swift-BAT (Beardmore et al. 2008, GCN 11087) The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight is 87.2 degrees. The GBM light curve consists of several pulses with a duration (T90) of about 149 +/- 1 s (50-300 keV). The time-averaged spectrum from T0+0.003 s to T0+157.57 s is best fit by a Band function with Epeak = 106.4 +13.9/-12.6 keV, alpha = -0.64 +0.14/-0.12, and beta = -2.02 +0.09/-0.12 (Castor C-STAT 807 for 484 d.o.f.). The event fluence (10-1000 keV) in this time interval is (1.98 +/- 0.06)E-05 erg/cm^2. The 1.024-sec peak photon flux measured starting from T0+6.784 s in the 10-1000 keV band is 4.5 +/- 0.2 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 11100 table
GRB_name GRB100814A
GCN_number 11100
Detection_method correction
Circular_text TITLE: GCN CIRCULAR NUMBER: 11100 SUBJECT: Swift/UVOT observations of GRB100814A - title correction to GCN 11097 DATE: 10/08/15 17:31:14 GMT FROM: Massimiliano de Pasquale at MSSL-UCL M. De Pasquale (MSSL/UCL) and C. J. Saxton (MSSL/UCL) on behalf of the Swift/UVOT team report: In the title of the GCN circular 11097 we mention "GRB100814B." It should have been "GRB100814A". Apologies for the mistake.
GCN 11107 table
GRB_name GRB100814A
GCN_number 11107
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 11107 SUBJECT: GRB100814A - interesting UVOT lightcurve. DATE: 10/08/16 15:52:03 GMT FROM: Massimiliano de Pasquale at MSSL-UCL M. De Pasquale, C. J. Saxton, and S. R. Oates (MSSL/UCL) report, on behalf of the Swift/UVOT team: Swift GRB 100814A (Beardmore et al. GCN circ 11087) shows an interesting optical/UV lightcurve, with a flux rise detected by UVOT between approximately 10,000 and 100,000 seconds after the trigger. At about 40 hours after the trigger, the afterglow was still of magnitude ~ 19 in the u and v filters. Ground based observatories are encouraged to follow up this event.
GCN 11118 table
GRB_name GRB100814A
GCN_number 11118
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 11118 SUBJECT: GRB 100814A : Lulin optical observation DATE: 10/08/17 08:03:26 GMT FROM: Yuji Urata at Nat. Central U. Y. Urata (NCU) and K.Y Huang (ASIAA) on behalf of EAFON report; "We observed the GRB 100814A optical afterglow (Beardmore et al. GCN 11087) using Lulin One-meter Telescope (LOT) with g', r', i' and z'-band filters. The observation started at 2010 August 16 19:09 about 2.65 days after the trigger. All of images show the optical afterglow clearly. The brightness of the afterglow calibrated against USNO-B1 stars in the field is R~19.2. The afterglow decays only ~0.5 magnitude from our previous observation at August 14 (0.7 days after the burst). This interesting feature is also notified by Pasquale (# 11107). Further observation is scheduled."
GCN 11119 table
GRB_name GRB100814A
GCN_number 11119
Detection_method Konus-Wind Det
t_trigger 3:50:11.288 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 11119 SUBJECT: Konus-Wind observation of GRB 100814A DATE: 10/08/17 08:48:16 GMT FROM: Dmitry Frederiks at Ioffe Institute S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, report: The long GRB 100814A (Swift-BAT trigger=431605; Beardmore et al., GCN 11087; Krimm et al., GCN 11094) triggered Konus-Wind at T0=13811.288s UT (03:50:11.288) The burst light curve consists of several pulses with a total duration of ~150 s. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB100814_T13811/ As observed by Konus-Wind the burst had a fluence of (1.2 +/- 0.2)x10-5 erg/cm2, and a 256-ms peak flux measured from T0+1.024s of (0.75 +/- 0.25)x10-6 erg/cm2/s (both in the 20 keV - 2 MeV energy range). The time-integrated spectrum of the burst (from T0 to T0+155.904 s) is best fit in the 20 keV - 2 MeV range by a power law with exponential cutoff model, for which alpha = -0.4(-0.3, +0.4), and Ep = 128(-17, +23) keV (chi2 = 59/58 dof). The spectrum at the maximum count rate (measured from T0 to T0+8.848 s) is best fit in the 20 keV - 2 MeV range by a power law with exponential cutoff model, for which alpha = 0.55 +/- 0.30, and Ep = 147(-10, +12) keV (chi2 = 55/58 dof). All the quoted results are preliminary. All the quoted errors are at the 90% confidence level.
GCN 11121 table
GRB_name GRB100814A
GCN_number 11121
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 11121 SUBJECT: GRB 100814A: NOT optical observations DATE: 10/08/17 09:33:24 GMT FROM: Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst D. Malesani, J.P.U. Fynbo (DARK/NBI), D. Xu (Weizmann Inst.), P. Jakobsson (Univ. Iceland), L. Buchhave, T. Hansen (NBI), report on behalf of a larger collaboration: We observed the optical afterglow of GRB 100814A (Schaefer et al., GCN 11086; Beardmore et al., GCN 11087) with the NOT equipped with ALFOSC. Observations were carried out in the R band, with a mean time August 17.13 UT (2.97 days after the burst). The optical afterglow is well detected, with R=19.5 compared to several USNO stars in the field. The error is about 0.3 mag, completely due to the scatter in the calibration stars. [GCN OPS NOTE(17aug10): Per author's request, TH was added to the author list.]
GCN 11122 table
GRB_name GRB100814A
GCN_number 11122
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 11122 SUBJECT: GRB 100814A : Liverpool Telescope Observations DATE: 10/08/17 10:52:58 GMT FROM: Zach Cano at ARI/John Moores Liverpool Z. Cano (Liverpool JMU), C. Guidorzi (U.Ferrara) report on behalf of a larger collaboration: We observed the optical afterglow of GRB 100814A (Schaefer et al., GCN 11086; Beardmore et al., GCN 11087) with the 2m Liverpool Telescope, starting at 22:16:09 UT on the 16th of August 2010, in filters r and i. We clearly detect the afterglow in both filters with the following magnitudes: ====================================== Filter T-To (days) Mag -------------------------------------- R 2.96 19.75 +/- 0.02 I 2.93 18.32 +/- 0.04 ====================================== The photometric calibration is performed against USNO-B1 objects 0720-0016107 (R2=19.58) and 0719-0016667 (I=17.27). Our detection is consistent with the values reported by Malesani et al. (GCN 11121). Observations are ongoing.
GCN 11129 table
GRB_name GRB100814A
GCN_number 11129
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 11129 SUBJECT: GRB 100814A: optical observations DATE: 10/08/18 17:23:27 GMT FROM: Alexei Pozanenko at IKI, Moscow L. Elenin, I. Molotov (ISON), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We observed the field of the Swift GRB 100814A (Beardmore et al. GCN 11087) with 0.45-m telescope f ISON-NM observatory on Aug. 17 (UT) 10:07:17 - 10:48:07. The afterglow (Schaefer et al. GCN 11086; Beardmore et al. GCN 11087) is well detected. Preliminary photometry of unfiltered image against USNO-B1.0 field stars (R) is following T-T0, filter, exposure, OT (day) 3.2689 W 300x7 19.79 +/- 0.05 the photometry error is statistical only.
GCN 11131 table
GRB_name GRB100814A
GCN_number 11131
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 11131 SUBJECT: EVLA radio afterglow detection of GRB 100814A DATE: 10/08/19 23:45:19 GMT FROM: Poonam Chandra at Royal Mil. College Canada Poonam Chandra (RMC), Dale A. Frail (NRAO) and S. Bradley Cenko (Berkeley) report on behalf of a larger collaboration: "We observed the localization of GRB 100814A (Beardmore et al. GCN 11087) with the Expanded Very Large Array (EVLA) on August 18.38 UT at a C band wide receiver (receiver frequency range 4-8 GHz). We detect the radio afterglow of the GRB at the Swift-XRT position (Beardmore et al. GCN 11092) at 4.5 and 7.9 GHz frequencies. The flux densities at 4.5 and 7.9 GHz bands are 198+/-29 uJy and 453+/-23 uJy, respectively. The EVLA is still undergoing active commissioning and we caution that these results should be considered preliminary. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc."
GCN 11133 table
GRB_name GRB100814A
GCN_number 11133
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 11133 SUBJECT: GRB 100814A: ISON-NM optical observations DATE: 10/08/22 07:30:05 GMT FROM: Leonid Elenin at ISON L. Elenin, I. Molotov (ISON), A. Volnova (SAI MSU), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We continue observation of the Swift GRB 100814A (Beardmore et al. GCN 11087) with 0.45-m telescope of ISON-NM observatory on Aug. 20 (UT) 08:42:06 - 09:33:14 and Aug. 21 (UT) 09:45:22 - 11:04:41. The afterglow (Schaefer et al. GCN 11086; Beardmore et al. GCN 11087) is well detected on stacked images for both epochs. Preliminary photometry of unfiltered image against USNO-B1.0 star 0720-0016107, assuming R=19.73 is following: T-T0, filter, exposure, OT (day) 6.2205 W 300x10 21.66 +/- 0.23 7.2734 W 300x15 22.50 +/- 0.30 The photometry errors are statistical only. The images of GRB100814A is available at: http://spaceobs.org/images/GRB1000814A-3epoch.jpg
GCN 11134 table
GRB_name GRB100814A
GCN_number 11134
Detection_method Suzaku WAM Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 11134 SUBJECT: GRB 100814A: Suzaku WAM observation of the prompt emission DATE: 10/08/23 01:12:09 GMT FROM: Yusuke Nishioka at Miyazaki U. Y. Nishioka, N. Ohmori, A. Daikyuji, M. Yamauchi (Univ. of Miyazaki), T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.), N. Vasquez (Tokyo Tech.) K. Yamaoka (Aoyama Gakuin U.), S. Sugita (Nagoya U.), Y. Terada, M. Tashiro, W. Iwakiri, K. Takahara, T. Yasuda (Saitama U.), M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. E. Nakagawa, T. Tamagawa (RIKEN), Y. Urata, P. Tsai (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo), S. Hong (Nihon U.), on behalf of the Suzaku WAM team, report: The long GRB 100814A (Swift/BAT trigger #431605 ; Krimm et al., GCN 11094; Fermi/GBM trigger #303450610 ; von Kienlin et al., GCN 11099) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 03:50:08.51 UT (=T0). The observed light curve shows a multi-peaked structure starting at T0-1.5s, ending at T0+19.5s, followed by a weaker emission seen up to T0+150.5s with a duration (T90) of about 110 seconds. The fluence in 100 - 1000 keV was 7.14(+1.03/-1.37) x 10^-6 erg/cm^2. The 1-s peak flux measured from T0+0.5s was 2.00(-0.48,+0.40) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-1.5s to T0+150.5s is well fitted by a single power-law with a photon index of 3.18(+1.03/-0.7) (chi^2/d.o.f = 13.32/15). All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are not included. The light curves for this burst are available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html -- ------------------------------------ $B5\:jBg3X(B $B9)3X8&5f2J(B $B1~MQJ*M}3X@l96(B $B=$;N2]Dx(B $B#2G/(B $B@>2,!!M42p(B yusuke613@astro.miyazaki-u.ac.jp ------------------------------------
GCN 11153 table
GRB_name GRB100814A
GCN_number 11153
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 11153 SUBJECT: GRB 100814A: Maidanak optical observations DATE: 10/08/27 20:30:05 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Volnova (SAI MSU), A. Pozanenko (IKI), O. Vozyakova (SAI MSU), B. Satovski (Astrotel), M. Im (Seoul National Univ), M. Ibrahimov (MAO) report on behalf of larger GRB follow-up collaboration: We observed the field of the Swift GRB 100814A (Beardmore et al. GCN 11087) with AZT-22 telescope of Maidanak observatory. Several images in R were obtained starting on Aug. 14 (UT) 22:56:44. We clearly the afterglow (Schaefer et al. GCN 11086; Beardmore et al. GCN 11087). The photometry of stacked image against USNO-B1.0 field stars is following t-T0, Filter, Exposure, OT, Upper limit (3 sigma) (mid, d) (s) 0.81185 R 30*60 18.75+/-0.01 23.4 the photometry error is statistical only.