GRB100522A

This page lists all entries on GRB100522A in GRBweb

Summary Fermi GBM IPN Swift GCN 10784 GCN 10785 GCN 10786 GCN 10787 GCN 10788 GCN 10789 GCN 10790 GCN 10791 GCN 10793 GCN 10795 GCN 10796

Summary table
Variable Value Source
GRB_name_Fermi GRB100522157
T0 3:45:49.843 UTC GCN_circulars,Konus-Wind Det
ra 6.9865° Swift
decl 9.4017° Swift
pos_error 1.81e-04° Swift
T90 35.326 s Fermi_GBM
T90_error 0.715 s Fermi_GBM
T90_start 3:45:52.297 UTC Fermi_GBM
fluence 3.86e-06 erg/cm² Fermi_GBM
fluence_error 4.07e-08 erg/cm² Fermi_GBM
T100 37.78 s
GBM_located False
mjd 55338.156826886574 GCN_circulars,Konus-Wind Det
Fermi GBM table
GRB_name_Fermi GRB100522157
trigger_name bn100522157
ra 6.9867°
decl 9.4022°
pos_error 3.26e+00°
datum 2010-05-22
t_trigger 3:45:52.294 UTC
T90 35.326 s
T90_error 0.715 s
T90_start 3:45:52.297 UTC
fluence 3.86e-06 erg/cm²
fluence_error 4.07e-08 erg/cm²
flux_1024 1.11e+01 erg/cm²/s
flux_1024_error 2.49e-01 erg/cm²/s
flux_1024_time 1.92e-01 erg/cm²/s
flux_64 1.50e+01 erg/cm²/s
flux_64_error 9.48e-01 erg/cm²/s
IPN table
GRB_name GRB100522A
ra 306.9833°
decl 9.4167°
pos_error 5.00e-02°
Swift table
GRB_name GRB100522A
t_trigger 3:45:52 UTC
ra 6.9865°
decl 9.4017°
pos_error 1.81e-04°
T90 35.3 s
fluence 2.10e-06 erg/cm²
GCN 10784 table
GRB_name GRB100522A
GCN_number 10784
Detection_method Swift Det
t_trigger 3:45:52 UTC
ra 6.9830°
decl 9.4170°
Circular_text TITLE: GCN CIRCULAR NUMBER: 10784 SUBJECT: GRB 100522A: Swift detection of a burst DATE: 10/05/22 04:14:56 GMT FROM: David Palmer at LANL E. Troja (NASA/GSFC/ORAU), A. P. Beardmore (U Leicester), M. M. Chester (PSU), J. M. Gelbord (PSU), S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), C. Pagani (U Leicester), D. M. Palmer (LANL), R. L. C. Starling (U Leicester), T. N. Ukwatta (GSFC/GWU) and L. Vetere (PSU) report on behalf of the Swift Team: At 03:45:52 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 100522A (trigger=422783). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 6.983, +9.417 which is RA(J2000) = 00h 27m 56s Dec(J2000) = +09d 25' 03" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a multi-peaked structure with a first pair of peaks near T0 with a duration of about 5 sec and a second fainter and softer pair of peaks near T+30 s. The peak count rate was ~15,000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 03:46:57.7 UT, 65.4 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source with an enhanced position: RA, Dec 6.9867, 9.4023 which is equivalent to: RA(J2000) = 00h 27m 56.82s Dec(J2000) = +09d 24' 08.1" with an uncertainty of 2.2 arcseconds (radius, 90% containment). This location is 54 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 in excess of the Galactic value (3.98e+20 cm^-2, Kalberla et al. 2005), with an excess column of 2.7 (+2.46/-2.10) x 10^21 cm^-2 (90% confidence). The initial flux in the 2.5 s image was 2.40e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 73 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 at the XRT position is 18.5 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.06. Burst Advocate for this burst is E. Troja (eleonora.troja AT nasa.gov). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/too.html.)
GCN 10785 table
GRB_name GRB100522A
GCN_number 10785
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 10785 SUBJECT: GRB 100522A: BOOTES-2 optical limit DATE: 10/05/22 05:24:50 GMT FROM: Martin Jelinek at Inst.Astrophys.Andalucia,Granada M. Jelnek (IAA-CSIC Granada), P. Kubnek (IPL Valencia, IAA-CSIC) and A. J. Castro-Tirado (IAA-CSIC), on behalf of a larger collaboration, report: "The 0.6m TELMA robotic telescope at the BOOTES-2 astronomical station in Mlaga (Spain) reacted to the Swift GRB 100522A (Troja et al., GCNC10784), starting 10m25s after the trigger (15s after receiving the delayed trigger). A set of 10s unfiltered images was obtained, however the progressing twillight degraded the images (already taken at high airmass). The 120s coadded image with an exposure mean time 735s after the GRB provides a limit R>15.5 at the XRT position reported by Troja et al." This message can be quoted.
GCN 10786 table
GRB_name GRB100522A
GCN_number 10786
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 10786 SUBJECT: GRB 100522A: NIR observations from CAHA DATE: 10/05/22 06:14:40 GMT FROM: Antonio Deugarte at IAA-CSIC A. de Ugarte Postigo (OAB-INAF), A.J. Castro-Tirado (IAA-CSIC), A. Guijarro and M. Alises (CAHA) report on behalf of a larger collaboration: "We have observed the field of GRB 100522A (Troja et al. GCNC 10784) with the 3.5m CAHA telescope (+Omega2000) in J and Ks bands. The observations were obtained during twilight, with a very high background. In a preliminary analysis we do not detect any source within the XRT error circle in any of the images. The 3x60s combined J-band exposure, has a mean time 04:20:27 UT and a 3-sigma limiting magnitude of 17.9. The 4x60s combined K-band exposure has a mean time of 04:31:50 and a limiting magnitude of 16.3."
GCN 10787 table
GRB_name GRB100522A
GCN_number 10787
Detection_method Swift-XRT Det
ra 6.9866°
decl 9.4018°
Circular_text TITLE: GCN CIRCULAR NUMBER: 10787 SUBJECT: GRB 100522A: Enhanced Swift-XRT position DATE: 10/05/22 12:42:18 GMT FROM: Phil Evans at U of Leicester J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team. Using 3778 s of XRT Photon Counting mode data and 6 UVOT images for GRB 100522A, 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 = 6.98662, +9.40184 which is equivalent to: RA (J2000): 00h 27m 56.79s Dec (J2000): +09d 24' 06.6" 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 10788 table
GRB_name GRB100522A
GCN_number 10788
Detection_method Swift-BAT Det
ra 6.9900°
decl 9.3970°
Circular_text TITLE: GCN CIRCULAR NUMBER: 10788 SUBJECT: GRB 100522A, Swift-BAT refined analysis DATE: 10/05/22 13:31:13 GMT FROM: Hans Krimm 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), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU), E. Troja (NASA/GSFC/ORAU), J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-60 to T+243 sec from the recent telemetry downlink, we report further analysis of BAT GRB 100522A (trigger #422783) (Troja, et al., GCN Circ. 10784). The BAT ground-calculated position is RA, Dec = 6.990, +9.397 deg which is RA(J2000) = 00h 27m 57.6s Dec(J2000) = +09d 23' 50.1" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 71%. The mask-weighted light curve shows a complex structure. There are two main episodes of emission, starting at T-0.5 sec and T+25 sec, respectively. The first episode starts with a broad multi-peaked structure 2.5 sec long followed by three short (~0.3 sec long) peaks. Then the emission returns to background levels before rising in a second, less intense and softer two peak structure approximately 15 sec long. T90 (15-350 keV) is 35.3 +- 1.8 sec (estimated error including systematics). The time-averaged spectrum from T-0.5 to T+40.2 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.89 +- 0.08. The fluence in the 15-150 keV band is 2.1 +- 0.1 x 10-6 erg/cm2. The 1-sec peak photon flux measured from T+0.04 sec in the 15-150 keV band is 7.1 +- 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/422783/BA/
GCN 10789 table
GRB_name GRB100522A
GCN_number 10789
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 10789 SUBJECT: GRB 100522A: Swift XRT refined analysis DATE: 10/05/22 13:50:22 GMT FROM: Rhaana Starling at U of Leicester R.L.C. Starling, A.P. Beardmore (U. Leicester) and E. Troja (NASA/GSFC/ORAU) report on behalf of the Swift-XRT team: We have analysed 5.4 ks of XRT data for GRB 100522A (Troja et al. GCN Circ. 10784), from 56 s to 13.6 ks after the BAT trigger. The data comprise 87 s in Windowed Timing (WT) mode (the first 7 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 Osborne et al. (GCN. Circ 10787). The light curve can be modelled with a series of power-law decays. The initial decay index is alpha = 4.8 (+/-0.4). At T+130 s the decay flattens to an alpha of 0.53 (+0.04, -0.09) before breaking again at T+7830 s to a final decay with index alpha = 1.2 (+2.8, -0.4). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of Gamma = 2.82 (+0.32, -0.28). The best-fitting absorption column is 4.0 (+0.8, -0.7) x 10^21 cm^-2, in excess of the Galactic value of 4.0 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index of 2.14 (+0.30, -0.28) and a best-fitting absorption column of 4.0 (+1.2, -1.0) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.4 x 10^-11 (8.1 x 10^-11) erg cm^-2 count^-1. If the light curve continues to decay with a power-law decay index of 1.2, the count rate at T+24 hours will be 0.011 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.8 x 10^-13 (8.9 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00422783. This circular is an official product of the Swift-XRT team.
GCN 10790 table
GRB_name GRB100522A
GCN_number 10790
Detection_method Fermi GBM Det
t_trigger 3:45:52.290 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 10790 SUBJECT: GRB 100522A: Fermi GBM observation DATE: 10/05/22 17:12:54 GMT FROM: Sheila McBreen at MPE S. McBreen (UCD/MPE) reports on behalf of the Fermi GBM Team: "At 03:45:52.29 UT on 22 May 2010, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 100522A (trigger 296192754 / 100522157) which was also detected by the Swift-BAT (Troja et al. 2010, GCN 10784). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight is 81 degrees. The GBM light curve consists of two of pulses with substructure from T0 to T0+5 s followed by two softer pulses lasting from T0+25 s to about T0+40 sec. The burst has a duration (T90) of about 35.0 +/-1.5 s (50-300 keV). The time-averaged spectrum from T0-0.003 s to T0+40.385 s is adequately fit by a simple power law function with index -1.81 (+/-0.03)(CSTAT 544 for 481 d.o.f.). The event fluence (8-1000 keV) in this time interval is (5.2 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+0.25 s in the 8-1000 keV band is 11.0 +/- 0.3 ph/s/cm^2. A power law function with an exponential high energy cutoff fits the spectrum equally well (CSTAT 538 for 480 d.o.f). The power law index is -1.62 (+0.10/-0.09) and the cutoff energy, parameterized as Epeak, is 138 (+82/-32) keV. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 10791 table
GRB_name GRB100522A
GCN_number 10791
Detection_method Swift-UVOT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 10791 SUBJECT: Swift/UVOT observations of GRB100522A. DATE: 10/05/22 23:38:54 GMT FROM: Massimiliano de Pasquale at MSSL-UCL M. De Pasquale (MSS-UCL) and Eleonora Troja (NASA/GSFC/ORAU) report on behalf of the Swift/UVOT team: Swift/UVOT began settled observations of GRB100522A (Troja et al. GCN Circ. 10784) starting 73 seconds after trigger. No optical afterglow within the enhanced XRT position (Osborne et al. GCN Circ. 10787) is detected in the UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Poole et al. 2008, MNRAS, 383, 627) for the first finding chart (FC) exposure and subsequent summed exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag ----------------------------------------------------------- white 73 223 147 >20.1 (FC) white 73 7223 569 >20.9 v 614 6199 352 >19.0 b 541 7018 352 >19.9 u 285 13630 1243 >20.1 uw1 663 12939 1242 >20.5 m2 639 7838 549 >20.2 w2 590 7429 363 >20.1 The values quoted above are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.06 in the direction of the burst (Schlegel et al. 1998).
GCN 10793 table
GRB_name GRB100522A
GCN_number 10793
Detection_method GROND
Circular_text TITLE: GCN CIRCULAR NUMBER: 10793 SUBJECT: GRB 100522A: GROND observations, upper limits DATE: 10/05/23 16:03:15 GMT FROM: Sylvio Klose at TLS Tautenburg P. Afonso (MPE Garching), S. Klose (TLS Tautenburg), and J. Greiner (MPE Garching), report on behalf of the GROND team: GROND (Greiner et al. 2008, PASP 120, 405), the 7-channel imager mounted at the 2.2m ESO/MPI telescope on La Silla, started follow-up observations of the Swift/Fermi burst GRB 100522A (Troja et al. 2010, GCN 10784; McBreen 2010, GCN 10790) on May 23 at 09:18 UT (about 29.5 hrs after the burst), and continued for about 1 hour. Within the enhanced XRT 1.5 arcsec error circle reported by Osborne et al. (GCN 10787) we do not find any afterglow candidate. Based on 50 min of total exposures in g'r'i'z' and 40 min in JHK, preliminary measured upper limits are (in the AB system, 3 sigma): g' > 24.8, r' > 24.4, i' > 23.6, z' > 23.3, J > 21.7, H > 20.9, K > 20.6, using GROND zeropoints and the 2MASS catalog.
GCN 10795 table
GRB_name GRB100522A
GCN_number 10795
Detection_method Suzaku WAM Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 10795 SUBJECT: GRB100522A: Suzaku WAM observation of the prompt emission DATE: 10/05/25 03:31:22 GMT FROM: Arata Daikyuji at Miyazaki U A. Daikyuji, N. Ohmori, Y. Nishioka, M. Yamauchi (Univ. of Miyazaki), K. Yamaoka (Aoyama Gakuin U.), S. Sugita (Nagoya U.), Y. Hanabata, T. Uehara, T. Takahashi, Y. Fukazawa (Hiroshima 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), N. Vasquez (Tokyo Tech.), Y. Urata, H. M. Lin (NCU), T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo), S. Hong (Nihon U.), on behalf of the Suzaku WAM team, report: The long GRB100522A (Swift/BAT trigger #422783 ; Troja et al., GCN 10784) was detected by the the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 2010-05-22 03:45:52 UT (=T0). The observed light curve shows a single peak starting at T0, ending at T0+4s with a duration (T90) of about 3 seconds. The WAM detected only the first bright peak observed by Swift/BAT (Barthelmy et al., GCN 10788) and Fermi/GBM(McBreen et al., GCN 10790). The fluence in 100 - 1000 keV was 1.39 (-0.18, +0.15) x10-6 erg/cm2. The 1-s peak flux measured from T0+1s was 1.50 (-0.27, +0.24) photons/cm2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0 to T0+4s is well fitted by a single power-law with a photon index of 2.26 (-0.18, +0.21) (chi2/d.o.f = 26.8/35). All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are not included. The light curves with 1-sec time resolution for this burst will be appeared at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html
GCN 10796 table
GRB_name GRB100522A
GCN_number 10796
Detection_method Konus-Wind Det
t_trigger 3:45:49.843 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 10796 SUBJECT: Konus-Wind observation of GRB 100522A DATE: 10/05/25 12:21:36 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 100522A (Swift-BAT trigger=422783; Troja et al., GCN 10784; Barthelmy et al., GCN 10788) triggered Konus-Wind at T0=13549.843s UT (03:45:49.843) The burst light curve shows a single pulse with a total duration of ~6 s. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB100522_T13549/ As observed by Konus-Wind the burst had a fluence of 1.7(-0.5, +0.3)x10-6 erg/cm2, and a 256-ms peak flux measured from T0-0.256s of 0.7(-0.2, +0.1)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+8.848 s) is best fit in the 20 keV - 2 MeV range by a single power-law model with a photon index of 2.9 (-/+0.5), chi2 = 78/69 dof. All the quoted results are preliminary. All the quoted errors are at the 90% confidence level.