GRB100621A

This page lists all entries on GRB100621A in GRBweb

Summary IPN Swift GCN 10870 GCN 10871 GCN 10872 GCN 10873 GCN 10874 GCN 10875 GCN 10876 GCN 10877 GCN 10878 GCN 10880 GCN 10881 GCN 10882

Summary table
Variable Value Source
T0 3:03:32 UTC GCN_circulars,Swift Det
ra 315.3046° Swift
decl -51.1064° Swift
pos_error 1.81e-04° Swift
T90 63.6 s Swift
T90_start 3:03:32 UTC Swift
fluence 2.10e-05 erg/cm² Swift
redshift 0.5420 GCN_circulars,Optical
T100 63.6 s
GBM_located False
mjd 55368.1274537037 GCN_circulars,Swift Det
IPN table
GRB_name GRB100621A
ra 315.3083°
decl -51.0833°
pos_error 5.00e-02°
redshift 0.5420
Swift table
GRB_name GRB100621A
t_trigger 3:03:32 UTC
ra 315.3046°
decl -51.1064°
pos_error 1.81e-04°
T90 63.6 s
fluence 2.10e-05 erg/cm²
redshift 0.5420
GCN 10870 table
GRB_name GRB100621A
GCN_number 10870
Detection_method Swift Det
t_trigger 3:03:32 UTC
ra 315.3080°
decl -51.0860°
Circular_text TITLE: GCN CIRCULAR NUMBER: 10870 SUBJECT: GRB 100621A: Swift detection of a burst DATE: 10/06/21 03:16:45 GMT FROM: Scott Barthelmy at NASA/GSFC T. N. Ukwatta (GSFC/GWU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), V. D'Elia (ASDC), N. Gehrels (NASA/GSFC), J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC), C. B. Markwardt (CRESST/GSFC/UMD), M. H. Siegel (PSU), M. Stamatikos (OSU/NASA/GSFC), M. A. Stark (PSU) and G. Stratta (ASDC) report on behalf of the Swift Team: At 03:03:32 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 100621A (trigger=425151). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 315.308, -51.086 which is RA(J2000) = 21h 01m 14s Dec(J2000) = -51d 05' 10" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a triple-peaked structure with a duration of about 100 sec. The peak count rate was ~25,000 counts/sec (15-350 keV), at ~25 sec after the trigger. The XRT began observing the field at 03:04:48.8 UT, 76.0 seconds after the BAT trigger. XRT found a bright, uncatalogued X-ray source located at RA, Dec 315.3004, -51.1063 which is equivalent to: RA(J2000) = 21h 01m 12.09s Dec(J2000) = -51d 06' 22.6" with an uncertainty of 5.0 arcseconds (radius, 90% containment). This location is 73 arcseconds from the BAT onboard position, within the BAT error circle. No event data are yet available to determine the column density using X-ray spectroscopy. The initial flux in the 0.1 s image was 7.49e-08 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 84 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 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 0.03. Burst Advocate for this burst is T. N. Ukwatta (tilan.ukwatta AT gmail.com). 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 10871 table
GRB_name GRB100621A
GCN_number 10871
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 10871 SUBJECT: GRB 100621A: ROTSE-III Optical Limits DATE: 10/06/21 03:40:05 GMT FROM: Shashi Bhushan Pandey at ROTSE S. B. Pandey (U Mich), W. Rujopakarn (Steward), T. Guver (U Arizona), 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 100621A (Swift trigger 425151; Ukwatta T. N., GCN 10870), producing images beginning 5.0 s after the GCN notice time. An automated response took the first image at 03:04:05.0 UT, 32.2 s after the burst, and during the gamma-ray emission, under fair conditions. We took 10 5-sec, 10 20-sec and 10 60-sec exposures. These unfiltered images are calibrated relative to USNO A2.0 (R). Imaging is on going. Comparison to the DSS (second epoch) reveals no new sources within the 3-sigma Swift/BAT error circle or the XRT error circle; the field is not crowded. Individual images have limiting magnitudes ranging from 16.1-17.3; we set the following specific limits. start UT end UT t_exp(s) mlim t_start-tGRB(s) Coadd? -------------------------------------------------------------------- 03:04:05.0 03:04:10.0 5 16.1 32.2 N 03:05:30.0 03:09:13.0 200 18.4 232.2 Y
GCN 10872 table
GRB_name GRB100621A
GCN_number 10872
Detection_method Swift-XRT Other
ra 315.3052°
decl -51.1060°
Circular_text TITLE: GCN CIRCULAR NUMBER: 10872 SUBJECT: GRB 100621A: Prompt enhanced Swift-XRT position DATE: 10/06/21 03:56:48 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Using 0 s of promptly downlinked XRT event data for GRB 100621A, we find an enhanced XRT position of the afterglow: RA, Dec: 315.3052, -51.1060 which is equivalent to: RA (J2000) = 21 01 13.24 Dec (J2000) = -51 06 21.7 with an uncertainty of 2.0 arc sec (radius, 90% confidence). Analysis of the promptly available data is online at http://www.swift.ac.uk/sper/425151. Position enhancement is 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.
GCN 10873 table
GRB_name GRB100621A
GCN_number 10873
Detection_method Swift-XRT Det
ra 315.3047°
decl -51.1062°
Circular_text TITLE: GCN CIRCULAR NUMBER: 10873 SUBJECT: GRB 100621A: Enhanced Swift-XRT position DATE: 10/06/21 09:33:26 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 3262 s of XRT Photon Counting mode data and 4 UVOT images for GRB 100621A, 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 = 315.30466, -51.10624 which is equivalent to: RA (J2000): 21h 01m 13.12s Dec (J2000): -51d 06' 22.5" 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.
GCN 10874 table
GRB_name GRB100621A
GCN_number 10874
Detection_method GROND
Circular_text TITLE: GCN CIRCULAR NUMBER: 10874 SUBJECT: GRB 100621A: GROND observation of bright NIR afterglow DATE: 10/06/21 09:56:56 GMT FROM: Jochen Greiner at MPI Adria Updike (Clemson Univ.), Ana Nicuesa (Tautenburg Obs.), Marco Nardini, Thomas Kruehler and Jochen Greiner (all MPE Garching) report on behalf of the GROND team: We observed the field of GRB 100621A (Swift trigger 425151; Ukwatta et al., GCN #10870) 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 03:07 UT on June 21st, 4 minutes after the GRB trigger, and continued for 3 hours. They were performed at an average seeing of 1.5" under clear sky conditions. In stacked images of 6 min total integration time in g'r'i'z' and 8 min in JHK, centered at 03:20 UT, we detect a bright, uncatalogued NIR source within the Swift/XRT error circle (Evans et al. GCN #10872) at the following coordinates: RA (2000.0) = 21h 01m 13.08s DEC (2000.0) = -51d 06' 22.5" with an error of +-0.3". This coincides with the enhanced XRT position (Evans et al. 2010, GCN #10873). In the first hour the source faded by about 1 mag in the JHK bands, thus we identify this object as the GRB afterglow of GRB 100621A. Our preliminary photometry centered at 03:45 UT is (in AB magnitudes): g' = 22.7+-0.4 r' = 21.6+-0.1 i' = 20.5+-0.1 z' = 19.7+-0.1 J = 17.3+-0.1 H = 16.3+-0.1, and K = 15.8+-0.1 These magnitudes were derived by calibrating the images against the GROND zeropoints and 2MASS field stars and are not corrected for the Galactic foreground extinction corresponding to a reddening of E_(B-V)= 0.03 in the direction of the burst (Schlegel et al. 1998). We note that there are indications of this source in the DSS2 images. Also, there is no fading in the g' band, suggesting that this is the underlying host galaxy at a redshift smaller than about 3. The extremely red colour then is likely due to severe intrinsic dust extinction. We encourage spectroscopic observations.
GCN 10875 table
GRB_name GRB100621A
GCN_number 10875
Detection_method Swift-BAT Det
ra 315.3090°
decl -51.1020°
Circular_text TITLE: GCN CIRCULAR NUMBER: 10875 SUBJECT: GRB 100621A: Swift-BAT refined analysis DATE: 10/06/21 13:10:27 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 100621A (trigger #425151) (Ukwatta, et al., GCN Circ. 10870). The BAT ground-calculated position is RA, Dec = 315.309, -51.102 deg, which is RA(J2000) = 21h 01m 14.1s Dec(J2000) = -51d 06' 08.8" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 97%. The mask-weighted light curve shows three main overlapping peaks starting at ~T-8 sec, with the main peak at ~T+25 sec, and ending at ~T+220 sec. T90 (15-350 keV) is 63.6 +- 1.7 sec (estimated error including systematics). The time-averaged spectrum from T-6 to T+204 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.90 +- 0.03. The fluence in the 15-150 keV band is 2.1 +- 0.0 x 10^-5 erg/cm2. The 1-sec peak photon flux measured from T+24.46 sec in the 15-150 keV band is 12.8 +- 0.3 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/425151/BA/
GCN 10876 table
GRB_name GRB100621A
GCN_number 10876
Detection_method Optical
redshift 0.5420
Circular_text TITLE: GCN CIRCULAR NUMBER: 10876 SUBJECT: GRB 100621A: VLT/X-shooter redshift DATE: 10/06/21 14:00:38 GMT FROM: Bo Milvang-Jensen at Dark Cosmology Centre,NBI,U. Copenhagen B. Milvang-Jensen (DARK/NBI), P. Goldoni (APC/Univ. Paris 7 and SAp/CEA), N. R. Tanvir, K. Wiersema (Univ. Leicester), D. Malesani (DARK/NBI), A. de Ugarte Postigo (INAF-OAB), V. D'Elia (INAF-OAR and ASDC), S. D. Vergani (GEPI/Obs. Paris and APC/Univ. Paris 7), J. P. U. Fynbo (DARK/NBI), L. Kaper (Univ. Amsterdam), J. Sollerman (Univ. Stockholm), on behalf of the X-shooter GRB collaboration, and A. Updike (Clemson Univ.), J. Greiner, T. Kruehler (MPE Garching), on behalf of the GROND team, report: We observed the optical afterglow of GRB 100621A (Ukwatta et al., GCN 10870; Updike et al., GCN 10874) with the ESO VLT equipped with the X-shooter spectrograph. The afterglow was detected in the I-band acquisition image. Four spectra lasting 10 minutes each were obtained, covering the spectral range 3000-25000 AA, starting on 2010 June 21, at 10:09 UT (7.1 hr after the GRB); the observations were done during twilight. Preliminary inspection of the spectrum reveals emission features which we interpret as due to [O II] 3727, Hbeta and the [O III] doublet from the underlying host galaxy, at a common redshift z = 0.542. The [O II] line is very weak. This, together with the low redshift and the optically faint and red afterglow supports high extinction internal to the host (Updike et al., GCN 10874). We caution that the data reduction was carried out using archival calibration files. We acknowledge a particularly helpful and attentive support from the ESO staff in Paranal: M. Olivares, T. Rivinius, C. Ledoux, C. Martayan, and the visiting astronomers: F. Ferraro, B. Lanzoni.
GCN 10877 table
GRB_name GRB100621A
GCN_number 10877
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 10877 SUBJECT: GRB 100621A: Swift XRT refined analysis DATE: 10/06/21 14:10:13 GMT FROM: Giulia Stratta at ASDC G. Stratta (ASDC), V. D'Elia (ASDC) and T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift-XRT team: We have analysed 3.6 ks of XRT data for GRB 100621A (Ukwatta et al. GCN Circ. 10870), from 79 s to 7.0 ks after the BAT trigger. The data comprise 322 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Evans et al. (GCN. Circ 10872). The light curve can be modelled with a series of power-law decays. The initial decay index is alpha=3.41 (+0.11, -0.18). At T+153 s the decay steepens to an alpha of 4.34 (+0.20, -0.12) before breaking again at T+389 s to a final decay with index alpha=0.55 (+0.13, -0.07). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.73 (+0.07, -0.06). The best-fitting absorption column is 6.11 (+0.27, -0.26) x 10^21 cm^-2, in excess of the Galactic value of 2.9 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index of 2.15 (+0.17, -0.16) and a best-fitting absorption column of 6.6 (+1.0, -0.9) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 5.0 x 10^-11 (1.0 x 10^-10) erg cm^-2 count^-1. If the light curve continues to decay with a power-law decay index of 0.55, the count rate at T+24 hours will be 0.23 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x 10^-11 (2.4 x 10^-11) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00425151. This circular is an official product of the Swift-XRT team.
GCN 10878 table
GRB_name GRB100621A
GCN_number 10878
Detection_method Swift-UVOT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 10878 SUBJECT: GRB 100621A: Swift/UVOT observations DATE: 10/06/21 14:30:51 GMT FROM: Samantha Oates at MSSL S. R. Oates (MSSL-UCL) and T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 100621A 85s after the BAT trigger (Ukwatta et al., GCN 10870). We detect a source at the enhanced Swift XRT position (Evans et al. GCN 10873) and at the location of the GROND source (Updike et al. GCN 10874). This source is also observed in the DSS and observed to be constant during the first 7000s and is thus likely to be the host galaxy, which is also suggested by Updike et al. (GCN 10874). The magnitudes and 3-sigma upper limits for the finding chart exposures (FC) and summed images for this possible host galaxy are: Filter T_start T_stop Exp(s) Magnitude/3-sigma upper limit ------------------------------------------------------------- white (FC) 85 234 147 20.87 +/- 0.35 white 576 7093 519 20.46 +/- 0.15 u (FC) 297 546 246 > 20.18 u 700 6683 360 > 20.14 v 626 6067 391 19.49 +/- 0.31 b 552 6888 372 20.27 +/- 0.28 uvw1 1107 6478 352 19.64 +/- 0.25 uvm2 6073 6273 197 > 19.66 uvw2 5663 5863 197 19.60 +/- 0.28 ------------------------------------------------------------- The quoted upper limits have not been corrected for the expected Galactic extinction along the line of sight of E_(B-V) = 0.03 mag. All photometry is on the UVOT photometric system described in Poole et al. (2008, MNRAS, 383, 627).
GCN 10880 table
GRB_name GRB100621A
GCN_number 10880
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 10880 SUBJECT: GRB 100621A MOA-II optical limit DATE: 10/06/22 01:04:15 GMT FROM: Takashi Sako at Nagoya U./MOA D. Suzuki, F. Hayashi, S.Kobara, T. Sako, H. Naito, K. Omori (STE Lab, Nagoya Univ.) on behalf of the MOA Collaboration report: We searched for an optical afterglow of GRB 100621A (GCN 10870, T. N. Ukwatta et al.) starting from 09:02 UT on 2010 June 21st (6 hours after the burst) with the MOA-II 1.8m telescope at Mt.John observatory in New Zealand. In a single image of a 300sec exposure with a wide-band Red filter (center wavelength ~ 750nm and FWHM ~ 250nm), we did not find any object within the error circle of the Swift XRT source position (GCN 10873). A 3 sigma upper limit is set in the I magnitude at 22.23 mag. This photometry was done by using the DoPhot and calibrated against the USNO-B1.0 catalog stars, and not corrected for the Galactic extinction.
GCN 10881 table
GRB_name GRB100621A
GCN_number 10881
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 10881 SUBJECT: GRB 100621A: IRSF/SIRIUS NIR Observation DATE: 10/06/22 15:37:21 GMT FROM: Hiroyuki Naito at Nagoya U H. Naito, T. Sako, D. Suzuki, S. Kobara and K. Omori (Nagoya Univ.) on behalf of the MOA Collaboration, T. Nagayama, M. Kurita (Nagoya Univ.) and N. Oi (The Graduate University for Advanced Studies/NAOJ) on behalf of the IRSF Collabration report: We searched for a NIR afterglow of GRB 100621A (Ukwatta et al., GCN 10870) starting from 04:02 to 04:51 UT on 2010 June 21 with the SIRIUS on the IRSF 1.4m telescope at SAAO in South Africa. In images of a 300 sec exposure with J, H and Ks filter, we detected an new source within the error circle of the enhanced Swift XRT position (Evans et al., GCN 10873) and at the location of the GROND source (Updike et al., GCN 10874) . The estimated magnitudes are the followings. --------------------------------------------------------------- Mid time from Total Exp. J-mag* H-mag* K-mag* trigger (min) (s) --------------------------------------------------------------- 61.41 300 16.56 15.22 14.18 67.61 300 16.24 14.63 13.84 73.84 300 15.27 13.78 12.63 80.14 300 15.07 13.57 12.40 86.36 300 14.93 13.45 12.23 92.56 300 14.90 13.45 12.32 98.81 300 14.93 13.47 12.34 105.0 300 15.04 13.55 12.36 --------------------------------------------------------------- *Typical error is ~ 0.1 mag This photometry was done by using the DoPhot and calibrated against the 2MASS catalog stars, and not corrected for the Galactic extinction. The source was brightened up by >1mag during our observation period while the other field stars were reasonably stable.
GCN 10882 table
GRB_name GRB100621A
GCN_number 10882
Detection_method Konus-Wind Det
t_trigger 3:03:33.352 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 10882 SUBJECT: Konus-Wind observation of GRB 100621A DATE: 10/06/23 10:22:55 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 100621A (Swift-BAT trigger=425151; Ukwatta et al., GCN 10870; Ukwatta et al., GCN 10875) triggered Konus-Wind at T0=11013.352s UT (03:03:33.352) The burst light curve shows multiple overlapping peaks with a total duration of ~80 s. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB100621_T11013/ As observed by Konus-Wind the burst had a fluence of 3.6(+/-0.4)x10-5 erg/cm2, and a 256-ms peak flux measured from T0+26.880s of 1.70(+/-0.13)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+73.984 s) is best fit in the 20 keV - 2 MeV range by the GRB (Band) model, for which: the low-energy photon index alpha = -1.70 (+/-0.13), the high energy photon index beta = -2.45 ( <-2.3 ), the peak energy Ep = 95(-13, +18)keV (chi2 = 65/57 dof). The spectrum at the maximum count rate (measured from T0+24.832 to T0+33.024 s) is best fit in the 20 keV - 2 MeV range by the GRB (Band) model, for which: the low-energy photon index alpha = -1.15 (-0.2/+0.3), the high energy photon index beta = -2.8 (-0.7/+0.3), the peak energy Ep = 83(+/-9)keV (chi2 = 64/57 dof). Assuming z=0.542 (Milvang-Jensen et al., GCN 10876) and a standard cosmology model with H_0 = 70 km/s/Mpc, Omega_M = 0.27, Omega_Lambda = 0.73, the isotropic energy release E_iso = 2.8(+/-0.3)x10^52 erg, the peak luminosity (L_iso)_max = (2.04+/-0.16)x10^51 erg/s. All the quoted results are preliminary. All the quoted errors are at the 90% confidence level.