GRB090510A

This page lists all entries on GRB090510A in GRBweb

Summary Fermi GBM IPN Swift Fermi LAT GCN 9331 GCN 9332 GCN 9334 GCN 9336 GCN 9337 GCN 9338 GCN 9339 GCN 9340 GCN 9341 GCN 9342 GCN 9343 GCN 9344 GCN 9345 GCN 9350 GCN 9351 GCN 9352 GCN 9353 GCN 9354 GCN 9355

Summary table
Variable Value Source
GRB_name_Fermi GRB090510016
T0 0:22:59 UTC Fermi_LAT
ra 333.5521° Swift
decl -26.5831° Swift
pos_error 7.90e-05° Swift
T90 0.96 s Fermi_GBM
T90_error 0.138 s Fermi_GBM
T90_start 0:22:59.923 UTC Fermi_GBM
fluence 3.37e-06 erg/cm² Fermi_GBM
fluence_error 4.06e-08 erg/cm² Fermi_GBM
redshift 0.9030 GCN_circulars,Optical
T100 1.883 s
GBM_located False
mjd 54961.01596064815 Fermi_LAT
Fermi GBM table
GRB_name_Fermi GRB090510016
trigger_name bn090510016
ra 333.6000°
decl -26.6000°
pos_error 2.66e+00°
datum 2009-05-10
t_trigger 0:22:59.971 UTC
T90 0.96 s
T90_error 0.138 s
T90_start 0:22:59.923 UTC
fluence 3.37e-06 erg/cm²
fluence_error 4.06e-08 erg/cm²
flux_1024 9.10e+00 erg/cm²/s
flux_1024_error 2.44e-01 erg/cm²/s
flux_1024_time -4.80e-02 erg/cm²/s
flux_64 4.10e+01 erg/cm²/s
flux_64_error 1.58e+00 erg/cm²/s
IPN table
GRB_name GRB090510A
ra 333.5542°
decl -26.6000°
pos_error 5.00e-02°
redshift 0.9030
Swift table
GRB_name GRB090510A
t_trigger 0:23:00 UTC
ra 333.5521°
decl -26.5831°
pos_error 7.90e-05°
T90 0.3 s
fluence 3.40e-07 erg/cm²
redshift 0.9030
Fermi LAT table
GRB_name_Fermi GRB090510016
GRB_name GRB090510A
MET 263607781.0
datum 2009-05-10
t_trigger 0:22:59 UTC
ra 333.5530°
decl -26.5841°
pos_error 1.11e-04°
GCN 9331 table
GRB_name GRB090510A
GCN_number 9331
Detection_method Swift Det
t_trigger 0:23:00 UTC
ra 333.5550°
decl -26.6060°
Circular_text TITLE: GCN CIRCULAR NUMBER: 9331 SUBJECT: GRB 090510: Swift detection of a short hard burst DATE: 09/05/10 00:41:41 GMT FROM: Scott Barthelmy at NASA/GSFC E. A. Hoversten (PSU), S. D. Barthelmy (GSFC), D. N. Burrows (PSU), M. M. Chester (PSU), D. Grupe (PSU), J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), N. P. M. Kuin (MSSL), D. M. Palmer (LANL) and T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team: At 00:23:00 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 090510 (trigger=351588). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 333.555, -26.606 which is RA(J2000) = 22h 14m 13s Dec(J2000) = -26d 36' 19" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a single spike with a duration of about 0.5 sec. The peak count rate was ~21000 counts/sec (15-350 keV), at 0 sec after the trigger. The XRT began observing the field at 00:24:34.6 UT, 94.1 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source located at RA, Dec 333.55195, -26.58345 which is equivalent to: RA(J2000) = 22h 14m 12.47s Dec(J2000) = -26d 35' 00.4" with an uncertainty of 3.8 arcseconds (radius, 90% containment). This location is 81 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 1.66e+20 cm^-2 (Kalberla et al. 2005). UVOT took a finding chart exposure of 150 seconds with the White filter starting 97 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image does not include the position of the XRT candidate. The 8'x8' region for the list of sources generated on-board covers the XRT position and 100% of the BAT 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 0.02. We note the existence of the galaxy 2dFGRS TGS176Z296 at a distance of 140 arcsec from the XRT position. Burst Advocate for this burst is E. A. Hoversten (hoversten 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.)
GCN 9332 table
GRB_name GRB090510A
GCN_number 9332
Detection_method Swift-UVOT Det
ra 333.5523°
decl -26.5829°
Circular_text TITLE: GCN CIRCULAR NUMBER: 9332 SUBJECT: GRB 090510: Swift/UVOT Detection of a Candidate Optical Afterglow DATE: 09/05/10 01:26:57 GMT FROM: Frank Marshall at GSFC F. E. Marshall (GSFC) and E. A. Hoversten (PSU) report on behalf of the Swift team: UVOT took a second finding chart exposure of 250 seconds with the U filter starting 309 seconds after the BAT trigger for GRB 090510 (Hoversten et al. GCN Circ. 9331). There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 22:14:12.54 = 333.55227 DEC(J2000) = -26:34:58.4 = -26.58290 with a 90%-confidence error radius of about 0.69 arc sec. This position is 0.7 arc sec. from the center of the XRT error circle. The estimated magnitude is 18.95 with a 1-sigma error of about 0.17. No information about variability is available at this time. No correction has been made for the expected extinction corresponding to E(B-V) of 0.02.
GCN 9334 table
GRB_name GRB090510A
GCN_number 9334
Detection_method Fermi LAT Det
t_trigger 0:23:01.220 UTC
ra 333.4000°
decl -26.7670°
Circular_text TITLE: GCN CIRCULAR NUMBER: 9334 SUBJECT: Fermi LAT detection of GRB 090510 DATE: 09/05/10 04:26:20 GMT FROM: Masanori Ohno at ISAS/JAXA Masanori Ohno(ISAS/JAXA), Veronique Pelassa(CNRS/IN2P3/LPTA) report on behalf of the Fermi LAT team: At 00:23:01.22 UT on 10 May 2009, the Fermi Large Area Telescope (LAT) triggered and located GRB 090510 (trigger 263607783 / 090510016). Emission was observed in the LAT up to GeV energy band with a detection significance of more than 5 sigma. The best LAT on-board localization is found to be (RA,Dec=333.400, -26.767) with an error radius of 7 arcmin (statistical only). This position is consistent with both Fermi/GBM and Swift/XRT position. Further analysis is ongoing. We suggest follow up observation for this burst. The points of contact for this burst is Masanori Ohno ohno@astro.isas.jaxa.jp The Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden. This message can be cited.
GCN 9336 table
GRB_name GRB090510A
GCN_number 9336
Detection_method Fermi GBM Det
t_trigger 0:22:59.970 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 9336 SUBJECT: GRB 090510: Fermi GBM detection DATE: 09/05/10 05:46:27 GMT FROM: Sylvain Guiriec at UAH S. Guiriec, V. Connaughton and M. Briggs (UAH) report on behalf of the Fermi GBM Team: "At 00:22:59.97 UT on 2009 May 10, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 090510 (trigger 263607781 / 090510016) which was also detected by the Swift-BAT (Hoversten et al. 2009, GCN 9331) and the Fermi-LAT (Ohno et al. 2009, GCN 9334). The GBM position is consistent with those reported by Swift and the LAT. The GBM triggered on a precursor lasting 30 ms followed 0.4 s later by an intense and hard emission period of 0.5 s and a tail lasting a further 0.5 s. The intense period has several narrow peaks and its integrated spectrum is well fit by a Band function with alpha = -0.80 +/- 0.03, beta = 2.6 +/- 0.3 and EPeak = 4.4 +/- 0.4 MeV. The peak flux on a 64 ms timescale between 8 keV and 40 MeV was measured 0.55 s after the trigger to be 80 ph.cm^-2.s^-1. The 8 keV to 40 MeV fluence in the 0.512 s long period of intense emission is (3.0 0.2) E-5 erg.cm^-2. The spectral analysis results presented above are preliminary; further analysis is on-going."
GCN 9337 table
GRB_name GRB090510A
GCN_number 9337
Detection_method Swift-BAT Det
ra 333.5520°
decl -26.5980°
Circular_text TITLE: GCN CIRCULAR NUMBER: 9337 SUBJECT: GRB 090510: Swift-BAT refined analysis DATE: 09/05/10 06:08:40 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), E. E. Fenimore (LANL), N. Gehrels (GSFC), E. A. Hoversten (PSU), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD), D. M. Palmer (LANL), A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC) (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 090510 (trigger #351588) (Hoversten, et al., GCN Circ. 9331). The BAT ground-calculated position is RA, Dec = 333.552, -26.598 deg, which is RA(J2000) = 22h 14m 12.6s Dec(J2000) = -26d 35' 51.1" with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment). The partial coding was 16%. The mask-weighted light curve shows a small precursor peak at ~T-0.54 sec (width ~ 30 msec). Then the main peak starts at ~T-0.05 sec, peaks at T+0.04 sec with a width of ~50 msec. Then come two smaller peaks at T+0.24 and T+0.32 sec, each about 40 msec in width. At the 3-sigma level, there is the possibility of low-level emission between T+110 sec to ~T+170 sec. T90 (15-350 keV) is 0.3 +- 0.1 sec (estimated error including systematics). The time-averaged spectrum from T+0.0 to T+0.4 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 0.98 +- 0.20. The fluence in the 15-150 keV band is 3.4 +- 0.4 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T-0.30 sec in the 15-150 keV band is 9.7 +- 1.1 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/351588/BA/
GCN 9338 table
GRB_name GRB090510A
GCN_number 9338
Detection_method correction
ra 333.5527°
decl -26.5841°
Circular_text TITLE: GCN CIRCULAR NUMBER: 9338 SUBJECT: GRB 090510: NOT afterglow confirmation DATE: 09/05/10 10:30:19 GMT FROM: Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst G. Olofsson, M. Ergon (Univ. Stockholm), D. Malesani, J.P.U. Fynbo (DARK/NBI), P. Jakobsson (Univ. Iceland), N.R. Tanvir, K. Wiersema (Univ. Leicester), A.J. Levan (Univ. Warwick), report on behalf of a larger collaboration: We observed the field of short Swift/Fermi GRB 090510 (Hoversten et al., GCN 9331; Ohno & Pelassa, GCN 9334; Guiriec et al., GCN 9336) with the Nordic Optical Telescope equipped with ALFOSC. Observations were carried out in twilight and at high airmass (~3). The candidate afterglow (Marshall & Hoversten, GCN 9332) is clearly detected in a stack of our images taken at a mean epoch May 10.215 UT (4.7 hr after the GRB). Calibrating against closeby USNO stars (R1 magnitudes), we get R ~ 21.2. Comparing this value with the magnitude reported by Marshall & Hoversten (GCN 9332) indicates fading, thus confirming that this object is the afterglow of GRB 090510. Astrometry of the field yields the following coordinates for the afterglow (0.4" error): RA(J2000) = 22:14:12.64 Dec(J2000) = -26:35:02.8 which is consistent with the UVOT position. We note the presence of a fainter source ~1" East of the afterglow. A finding chart is posted at the following URL: http://www.astro.ku.dk/~malesani/GRB/090510/090510_finder.png We acknowledge the observiers at the NOT for carrying out this difficult observation. [GCN OPS NOTE(10may09): The authors point out that there is a correction to the coordinates given above (see GCN Circ 9340).]
GCN 9339 table
GRB_name GRB090510A
GCN_number 9339
Detection_method Swift-XRT Det
ra 333.5527°
decl -26.5827°
Circular_text TITLE: GCN CIRCULAR NUMBER: 9339 SUBJECT: GRB 090510: Enhanced Swift-XRT position DATE: 09/05/10 10:59:39 GMT FROM: Phil Evans at U of Leicester M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team. Using 1675 s of XRT Photon Counting mode data and 1 UVOT images for GRB 090510, 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 = 333.55271, -26.58266 which is equivalent to: RA (J2000): 22h 14m 12.65s Dec (J2000): -26d 34' 57.6" with an uncertainty of 1.4 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, arXiv:0812.3662). This circular was automatically generated, and is an official product of the Swift-XRT team.
GCN 9340 table
GRB_name GRB090510A
GCN_number 9340
Detection_method correction
ra 333.5523°
decl -26.5831°
Circular_text TITLE: GCN CIRCULAR NUMBER: 9340 SUBJECT: GRB 090510: correction to coordinates in GCN 9338 DATE: 09/05/10 14:32:45 GMT FROM: Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst D. Malesani (DARK/NBI) reports: The coordinates of the afterglow reported in GCN 9338 (Olofsson et al.) are wrong. The correct ones (referenced to USNO-B1 stars, 0.3" error) are: RA(J2000) = 22:14:12.56 Dec(J2000) = -26:34:59.0 These coordinates are 0.7" away from the UVOT position (Marshall & Hoversten, GCN 9332) and indeed consistent within their quoted error. The object identified in the finding chart posted at http://www.astro.ku.dk/~malesani/GRB/090510/090510_finder.png is correctly the afterglow. I thank Frank Marshall for pointing out the mistake, and regret for any confusion that this may have created. No blame should go to the other co-authors of GCN 9338.
GCN 9341 table
GRB_name GRB090510A
GCN_number 9341
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 9341 SUBJECT: GRB 090510: Swift XRT refined analysis DATE: 09/05/10 15:41:02 GMT FROM: Dirk Grupe at PSU/Swift-XRT D. Grupe (PSU) and E. Hoversten (PSU) report on behalf of the Swift- XRT team: We have analysed XRT data for GRB090510 (Hoversten et al. GCN Circ. 9331) up to 25ks after the burst beginning 94.1 s after the BAT trigger. The data comprise 200 s in Windowed Timing (WT) mode and 9.7 ks in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Goad et al. (GCN. Circ 9339). The light curve can be modelled with a broken power-law decay with an index of alpha=0.77+/-0.05, followed by a break at T+1470+/-160 s to an alpha of 2.16 (+0.17, -0.14). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.57+/-0.08 with an absorption column consistent with the Galactic value of 1.66 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode spectrum is consistent with this result. If the light curve continues to decay with a power-law decay index of 2.16, the count rate at T+24 hours will be 1.3e-4 counts/s, corresponding to an observed 0.3-10 keV flux of 6.1 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/00351588. This circular is an official product of the Swift-XRT team.
GCN 9342 table
GRB_name GRB090510A
GCN_number 9342
Detection_method Swift-BAT Det
ra 333.5521°
decl -26.5831°
Circular_text TITLE: GCN CIRCULAR NUMBER: 9342 SUBJECT: GRB 090510: UVOT refined analysis DATE: 09/05/10 16:59:54 GMT FROM: Paul Kuin at MSSL N. P. M. Kuin (MSSL/UCL) and E.A. Hoversten (PSU) report on behalf of the Swift UVOT team. The Swift UltraViolet/Optical Telescope (UVOT) began observations of the short hard burst GRB 090510 (Swift BAT trigger number 351588; Hoversten et al. GCN Circ. 9331) on May 10, 2009, at 00:24:24 UT, 80 seconds after the BAT trigger with a settling exposure in the UVOT v filter. A new optical source was found by the UVOT (Marshall and Hoversten, GCN Circ. 9332) for which we have a refined position (based on matching the UVOT field sources to the USNO-B1 catalogue) of RA, DEC = 333.55208, -26.58311, which is equivalent to: RA = 22:14:12.5, DEC = -26:34:59.2, with an uncertainty of 1.5" (90% confidence). The refined UVOT position is offset 1.6" from the refined XRT position (Goad et al., GCN Circ. 9339) and is consistent with the revised NOT position (Malesani, GCN Circ. 9340) to within 0.2". GRB 090510 is detected in all UVOT filters, except perhaps in b, which implies that the redshift is less than about 1.5. The emission is seen to rise to a peak around 600s after the trigger. The initial magnitude observed in the UVOT filters are given below: Filter Tstart(s) Tstop(s) Exposure(s) Magnitude wh 97 247 147.4 19.63 +/- 0.17 wh 588 608 19.5 18.76 +/- 0.22 wh 1167 1526 58.3 19.16 +/- 0.20 v 80 1410 97.3 18.46 +/- 0.33 b 564 1502 97.2 >19.62 (2.2 sigma) u 712 1477 323.6 19.05 +/- 0.17 uvw1 687 1452 75.9 18.61 +/- 0.27 uvm2 662 1434 93.7s 18.10 +/- 0.22 uvw2 614 1552 115.4s 18.31 +/- 0.18 The values quoted above are on the UVOT Photometric System (Poole et al, 2008, MNRAS 383,627). They are not corrected for the expected galactic reddening of E(B-V) = 0.020 in the direction of the burst (Schlegel et al. 1998).
GCN 9343 table
GRB_name GRB090510A
GCN_number 9343
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 9343 SUBJECT: AGILE detection of GRB 090510 DATE: 09/05/10 19:38:52 GMT FROM: Marco Feroci at IASF/INAF F. Longo, E. Moretti, G. Barbiellini, E. Vallazza (INFN Trieste), A. Giuliani (INAF/IASF Milan), S. Cutini, C. Pittori (ASDC) M. Marisaldi, A. Bulgarelli, F. Gianotti, M. Trifoglio, G. Di Cocco, C. Labanti, F. Fuschino, M. Galli (INAF/IASF Bologna), A. Chen, S. Mereghetti, F. Perotti, P. Caraveo (INAF/IASF Milan), Y. Evangelista, E. Del Monte, M. Feroci, I. Donnarumma, L. Pacciani, P. Soffitta, E. Costa, F. Lazzarotto, I. Lapshov, M. Rapisarda(INAF/IASF Rome), A. Pellizzoni, M. Pilia (INAF/OA Cagliari), S. Vercellone (INAF/IASF Palermo), M. Tavani, G. Pucella, F. D'Ammando, V.Vittorini, A. Argan, A. Trois, G. Piano, S. Sabatini (INAF/IASF Rome), P. Picozza, A. Morselli (INFN Roma-2), M. Prest (Universita' dell'Insubria), P. Lipari, D. Zanello (INFN Roma-1), A. Rappoldi, P. Cattaneo (INFN Pavia) and P. Giommi, P. Santolamazza, F. Verrecchia (ASDC) and L. Salotti (ASI), on behalf of the AGILE Team, report: AGILE detected the remarkable short GRB 090510 (Hoversten et al. GCN #9331, Ohno et al. GCN #9334) at approximately 61 degrees off-axis. An analysis of AGILE-GRID data shows an above 5-sigma detection of gamma-ray emission above 100 MeV. The gamma-ray lightcurve above 100 MeV shows emission during both the prompt phase and during a "delayed" phase. Also the Mini-Calorimeter detected a very significant and structured event lasting ~200 msec with emission well above 3 MeV. The burst triggered also SuperAGILE, although outside the field of view. This is the first short GRB with emission above 100 MeV detected by AGILE.
GCN 9344 table
GRB_name GRB090510A
GCN_number 9344
Detection_method Konus-Wind Det
t_trigger 0:23:01.547 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 9344 SUBJECT: Konus-Wind observation of GRB 090510 DATE: 09/05/11 13:37:31 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, report: The short hard GRB 090510 (Swift-BAT trigger #351588: Hoversten et al., GCN 9331, Ukwatta et al., GCN 9337; Fermi-LAT trigger 263607783 / 090510016: Ohno & Pelassa, GCN 9334) triggered Konus-Wind at T0=1381.547 s UT (00:23:01.547). The burst light curve shows a multipeaked structure with a duration of ~0.4 s As observed by Konus-Wind the burst had a fluence of (2.42 +/- 0.37)x10^-5 erg/cm2, and a 16-ms peak flux measured from T0+0.002 s of (2.27 +/- 0.63)x10^-4 erg/cm2/s (both in the 20 keV - 15 MeV energy range). The spectrum of the most intense part (from T0 to T0+0.192 s; it comprises ~75% of the total counts) is well fitted (in the 20 keV - 15 MeV range) by GRB (Band) model for which: the low-energy photon index alpha = 0.11(-0.43, +0.48), the high energy photon index beta = -1.61(-0.34, +0.15), the peak energy E0 = 552(-249, +448) keV (chi2 = 28.6/31 dof). Since beta > -2 we can establish only the lower limit on the peak energy in the EF(E) spectrum: Ep > 912 keV. The emission is clearly seen up to the end of the Konus-Wind energy range at 15 MeV. All the quoted errors are at the 90% confidence level. We note that since beta > -2 the bolometric fluence might be substantially higher than the given value. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB090510_T01381/ [GCN OPS NOTE(11may09): The typo in the Subject-line was changed from "091005" to "090510".]
GCN 9345 table
GRB_name GRB090510A
GCN_number 9345
Detection_method correction
Circular_text TITLE: GCN CIRCULAR NUMBER: 9345 SUBJECT: GRB 090510: correction to GCN 9344 DATE: 09/05/11 13:54:52 GMT FROM: Valentin Pal'shin at Ioffe Inst V. Pal'shin on behalf of the Konus-Wind team, report: "...the peak energy E0 = 552(-249, +448) keV (chi2 = 28.6/31 dof)." in GCN 9344 should be read as: "...the e-folding energy E0 = 552(-249, +448) keV (chi2 = 28.6/31 dof)."
GCN 9350 table
GRB_name GRB090510A
GCN_number 9350
Detection_method Fermi LAT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 9350 SUBJECT: GRB 090510: Fermi-LAT follow-up analysis DATE: 09/05/11 21:33:14 GMT FROM: Nicola Omodei at INFN(Pisa)/GLAST N. Omodei (INFN Pisa), J. Granot (University of Hertfordshire), P. Meszaros (PSU), J. McEnery (GSFC), F. Piron (LPTA), S. Razzaque (NRL) H. Tajima (SLAC), V. Vasileiou (GSFC/UMBC), D. Williams (UCSC), report on behalf of the Fermi LAT Collaboration. A follow-up analysis of the short bright Fermi GRB 090510 (Ohno et al., GCN 9334, Guiriec et al., GCN 9336) has been performed by the Fermi-LAT team. Fermi LAT has detected more than 50 events above 100 MeV (>10 above 1 GeV) during the first second and more than 150 events above 100 MeV (>20 above 1 GeV) in the first minute after the GBM trigger. All these events are positionally consistent (within the 95% containment radius of the LAT point spread function) with the position reported by Swift (Goad et al. GCN 9339). They indicate extended emission above GeV energies, making this burst an absolute priority for follow-up searches, especially a redshift determination. The points of contact for this burst is: Masanori Ohno ohno@astro.isas.jaxa.jp The Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
GCN 9351 table
GRB_name GRB090510A
GCN_number 9351
Detection_method Swift-UVOT Other
ra 333.5522°
decl -26.5845°
Circular_text TITLE: GCN CIRCULAR NUMBER: 9351 SUBJECT: GRB 090510: Swift/UVOT host galaxy candidates DATE: 09/05/11 23:50:50 GMT FROM: Paul Kuin at MSSL N. P. M. Kuin (MSSL/UCL), S. Oates (MSSL/UCL), M. De Pasquale (MSL/UCL), E.A. Hoversten (PSU), and F. Marshall (GSFC) report on behalf of the Swift UVOT team. The Swift UltraViolet/Optical Telescope (UVOT) continued observations of the short hard burst GRB 090510 (Swift BAT trigger number 351588; Hoversten et al. GCN Circ. 9331) today. The summed image in the white filter taken between 92.7ks and 127.6 ks shows that the source has faded from the initial magnitude of wh = 18.76 mag at T+800 and is now possibly detected at 3.3 sigma at a magnitude of 22.9+/-0.3. Observations between T+2000s and T+100ks show a decay index of about 1. There are also two nearby sources at the 6 sigma level detectable, which we consider to be possible hosts of GRB 090510. The first, nearest, candidate is at position RA, DEC = 333.55220, -26.584525 (22h 14m 12.53s, -26d 35m 04.29s (J2000)), with a diameter of 2.3", and the second, more extended, candidate is found at position RA, DEC = 333.54963, -26.582294 (22h 14m 11.91s, -26d 34m 56.26s (J2000)), is more elongated with a diameter of about 3.1". The estimated positional accuracy is 0.7" for both sources. Both sources have a wh magnitude of 21.61 +/- 0.17. We encourage follow-up observations. We would like to make a correction: The UVOT positional error on GRB 090510 quoted in GCN 9342 was too large. The correct uncertainty in the GRB position was 0.61" (90% confidence radius).
GCN 9352 table
GRB_name GRB090510A
GCN_number 9352
Detection_method GROND
Circular_text TITLE: GCN CIRCULAR NUMBER: 9352 SUBJECT: GRB 090510: GROND observations DATE: 09/05/12 15:19:57 GMT FROM: Thomas Kruehler at MPE/MPI F. Olivares (MPE Garching), S. Klose (Tautenburg), T. Kruehler, J. Greiner (both MPE Garching) report on behalf of the GROND team: GROND, mounted at the 2.2m on La Silla, observed the field of GRB 090510, detected by Swift (Hoversten et al., GCN 9331), Fermi GBM (Guiriec et al., GCN 9336) and LAT (Ohno & Pelassa, GCN #9334), AGILE (Longo et al., GCN 9343) and Konus-Wind (Golenetskii et al., GCN 9344), in g'r'i'z'JHK starting at 6:34 UT on 10 May 2009. We detect the afterglow reported by Marshall & Hoversten (GCN #9332) and Olofsson et al. (GCN #9338) in the optical bands. At a midtime of 9.0 h after the burst, we measure the following AB magnitudes of the afterglow and upper limits in stacked images g' = 23.5 +/- 0.3 r' = 23.0 +/- 0.1 i' = 22.8 +/- 0.1 z' = 22.6 +/- 0.1 J > 21.8 H > 21.4 K > 20.7 calibrated against the GROND zeropoints and 2MASS field stars. We caution that the photometry might be contaminated by the nearby source mentioned by Olofsson et al. (GCN #9338). Together with the magnitude reported by NOT (Olofsson et al. GCN #9338), this implies a rapid early fading with an index of ~2 during this epoch, which is compatible to the X-ray afterglow at a similar time interval (Grupe & Hoversten, GCN #9341). A late flattening of the optical light curve is then indicated by the UVOT detection (Kuin et al. #GCN 9351).
GCN 9353 table
GRB_name GRB090510A
GCN_number 9353
Detection_method Optical
redshift 0.9030
Circular_text TITLE: GCN CIRCULAR NUMBER: 9353 SUBJECT: GRB090510: VLT/FORS2 spectroscopic redshift DATE: 09/05/12 17:42:34 GMT FROM: Arne Rau at MPE Arne Rau (MPE Garching), Sheila McBreen (UCD/MPE Garching), Thomas Kruehler, and Jochen Greiner (both MPE Garching) report: We present follow-up optical spectroscopy of the short Swift/Fermi GRB 090510 (Hoversten et al., GCN 9331; Ohno & Pelassa, GCN 9334; Guiriec et al., GCN 9336) using VLT/FORS2 (PI McBreen). Observations of the optical source consistent with position of the afterglow (Marshall & Hoversten, GCN 9332; Olofsson et al., GCN 9338; Olivares et al., GCN 9352) started on May 12 08:17UT. A total of three 30min exposures with the 300I grism were obtained, covering an approximate wavelength range of 6000-10000 Angstroms. Preliminary analysis of the spectra reveals two emission lines at 7093 and 9250 Angstroms, which we identify as [OII] and Hbeta at a common redshift of z=0.903 +/- 0.003. Furthermore, there are indications of a spectral break in the continuum around 7600 Angstroms, suggesting a possible 4000A break at the same redshift. The detection of emission lines and the possible 4000A break suggest the dominance of the underlying host galaxy over the afterglow at the time of our observations. It also confirms that host galaxies of short GRBs are not all old and dead ellipticals but instead drawn from the underlying field galaxy distribution (e.g., Berger 2009, ApJ, 690, 231). In the acquisition image the center of the host is 0.7" offset with respect to the NOT refined afterglow position, which corresponds to 5.5 kpc at a z=0.903. At a redshift of z=0.903, the isotropic equivalent energy of the burst is 3.8E52 erg in the 1 keV - 10 MeV rest frame (using the Fermi/GBM spectral parameters of Guiriec et al., GCN 9336). The peak energy of the best fit GBM Band function model is 8.4 +/- 0.8 MeV in the rest frame. We acknowledge excellent support from the ESO staff, in particular F. Selman and I. Condor.
GCN 9354 table
GRB_name GRB090510A
GCN_number 9354
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 9354 SUBJECT: GRB 090510, Radio limits DATE: 09/05/13 16:00:14 GMT FROM: Dale A. Frail at NRAO D. A. Frail (NRAO) and P. Chandra (RMC) report on behalf of a larger collaboration: "We have used the Very Large Array (VLA) to image a field toward the short, bright Fermi-LAT burst GRB 090510 (GCN # 9350, 9334). The VLA observed at a frequency of 8.46 GHz on three epochs, May 11.48, May 12.48 and May 13.52 UT. There is no radio source detected at the position of the optical afterglow (GCN #9340). Adding the data together for all three epochs, the 3-sigma limit is 84 uJy. No further observations are planned. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc."
GCN 9355 table
GRB_name GRB090510A
GCN_number 9355
Detection_method Suzaku WAM Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 9355 SUBJECT: GRB 090510: Suzaku WAM observation of the prompt emission DATE: 09/05/14 08:52:46 GMT FROM: Norisuke Ohmori at Miyazaki U N. Ohmori, K. Noda, E. Sonoda, M. Yamauchi, K. Kono, H. Hayashi, A. Daikyuji, Y. Nishioka (Univ. of Miyazaki), M. Ohno, M. Suzuki, M. Kokubun, T. Takahashi (ISAS/JAXA), K. Yamaoka, S. Sugita (Aoyama Gakuin U.), Y. E. Nakagawa, T. Tamagawa (RIKEN), S. Hong (Nihon U.), N. Vasquez (Tokyo Tech.), T. Uehara, Y. Hanabata, T. Takahashi, Y. Fukazawa (Hiroshima U.), W. Iwakiri, M. Tashiro, Y. Terada, A. Endo, K. Onda, T. Sugasahara (Saitama U.), Y. Urata (NCU), T. Enoto, K. Nakazawa, K. Makishima (Univ. of Tokyo), on behalf of the Suzaku WAM team, report: The short hard GRB 090510 detected by the Fermi-LAT (Swift/BAT trigger #351588; Hoversten et al., GCN 9331,Fermi-LAT trigger #263607783; Ohno et al., GCN 9334) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 00:23:00 UT (=T0). The observed light curve shows a multi-peaked structure starting at T0-0.1s, ending at T0+0.9s with a duration (T90) of about 0.33 seconds. The emissions was clearly detected at least up to 5 MeV. However, since the incident angle of this burst to the WAM is off-axis, we cannot perform a reliable spectral analysis at this moment. We are now improving our detector response from such an off-axis direction. 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