GRB130504C

This page lists all entries on GRB130504C in GRBweb

Summary Fermi GBM IPN Fermi LAT GCN 14574 GCN 14583 GCN 14584 GCN 14587 GCN 14588 GCN 14601 GCN 14603

Summary table
Variable Value Source
GRB_name_Fermi GRB130504978
T0 23:28:57 UTC Fermi_LAT
ra 91.6304° Fermi_LAT
decl 3.8339° Fermi_LAT
pos_error 1.00e-03° Fermi_LAT
T90 73.217 s Fermi_GBM
T90_error 2.111 s Fermi_GBM
T90_start 23:29:06.222 UTC Fermi_GBM
fluence 1.29e-04 erg/cm² Fermi_GBM
fluence_error 2.32e-07 erg/cm² Fermi_GBM
T100 82.439 s
GBM_located False
mjd 56416.9784375 Fermi_LAT
Fermi GBM table
GRB_name_Fermi GRB130504978
trigger_name bn130504978
ra 91.6304°
decl 3.8339°
pos_error 2.48e+00°
datum 2013-05-04
t_trigger 23:28:57.518 UTC
T90 73.217 s
T90_error 2.111 s
T90_start 23:29:06.222 UTC
fluence 1.29e-04 erg/cm²
fluence_error 2.32e-07 erg/cm²
flux_1024 4.33e+01 erg/cm²/s
flux_1024_error 5.25e-01 erg/cm²/s
flux_1024_time 3.08e+01 erg/cm²/s
flux_64 5.34e+01 erg/cm²/s
flux_64_error 2.16e+00 erg/cm²/s
IPN table
GRB_name GRB130504C
ra 91.7167°
decl 3.8500°
pos_error 3.00e-01°
Fermi LAT table
GRB_name_Fermi GRB130504979
GRB_name GRB130504C
MET 389402940.0
datum 2013-05-04
t_trigger 23:28:57 UTC
ra 91.6304°
decl 3.8339°
pos_error 1.00e-03°
GCN 14574 table
GRB_name GRB130504C
GCN_number 14574
Detection_method Fermi LAT Det
t_trigger 23:30:15 UTC
ra 91.7150°
decl 3.8460°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14574 SUBJECT: GRB 130504C: Fermi-LAT detection of a burst DATE: 13/05/05 16:40:11 GMT FROM: Daniel Kocevski at SLAC D. Kocevski (NASA/GSFC), M. Ohno (Hiroshima U.), J. Racusin (NASA/GSFC), G. Vianello (Stanford), V. Vasileiou (LUPM), and E. Troja (CRESST) report on behalf of the Fermi-LAT team: At 23:30:15 UT on 04 May 2013, Fermi LAT detected high energy emission from GRB 130504C, which was also detected by Fermi-GBM (trigger 389402940 / 130504979). The GBM detection triggered an autonomous repoint of the spacecraft. The best LAT on-ground location is found to be RA=91.715, DEC=3.846 (J2000) with an error radius of 0.155 deg (68% containment, statistical error only). The burst was about 40 deg from the LAT boresight at the time of the trigger and the spacecraft slew brought the source within the LAT field of view for the next 2200 seconds. The data from the Fermi LAT show long lasting emission with >70 photons above 100 MeV observed out to 1000s seconds with a TS of >70. Multi-peaked emission lasting roughly 40 seconds can be seen using the non-standard LAT Low Energy (LLE) with a significance of ~26 sigma. The highest energy LAT photon has an energy of ~5 GeV arriving 251 seconds after the trigger. A Swift TOO request has been submitted. A GBM circular is forthcoming. The Fermi LAT point of contact for this burst is Daniel Kocevski (daniel.kocevski@nasa.gov). 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. Daniel Kocevski NASA Goddard Space Flight Center www.kocevski.com 510.316.3208
GCN 14583 table
GRB_name GRB130504C
GCN_number 14583
Detection_method Fermi GBM Det
t_trigger 23:28:57.518 UTC
ra 90.7100°
decl 4.4500°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14583 SUBJECT: GRB 130504C: Fermi GBM detection DATE: 13/05/05 23:54:40 GMT FROM: Michael Burgess at UAH J. Michael Burgess (UAH), Valerie Connaughton (UAH) and Shaolin Xiong (UAH) report on behalf of the Fermi GBM Team: "At 23:28:57.518 UT on 04 May 2013, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 130504C (trigger 389402940 / 130504978). High peak flux from the GRB caused GBM to issue a repoint request that reoriented the satellite to place the GRB near the LAT boresight for 2.5 hours, subject to Earth limb contraints. The on-ground calculated location, using the GBM trigger data, is RA = 90.71, DEC = 4.45 (J2000 degrees, equivalent to 06 h 02 m, 4 d 27 '), with an uncertainty of 1.0 degrees (radius, 1-sigma containment, statistical only; there is additionally a systematic error which is currently estimated to be 2 to 3 degrees). This location is consistent with the LAT location. The angle from the Fermi LAT boresight is 47 degrees. This burst was also independently detected by INTEGRAL SPI-ACS. The GBM light curve consists of about 5 peaks associated with the GRB and 1 peak associated with a solar flare about 100 seconds prior to T0. The duration (T90) of the GRB is about 74 s (50-300 keV). The time-averaged spectrum from T0-2.0 s to T0+120.0 s is adequately fit by a Band function with Epeak = 637 +/- 34 keV, alpha = -1.23 +/- 0.01, and beta = -2.28 +/- 0.08 The event fluence (10-1000 keV) in this time interval is (1.34 +/- 0.01)E-04 erg/cm^2. The 1-sec peak photon flux measured starting from T0+30.8 s in the 10-1000 keV band is 43 +/- 0.5 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 14584 table
GRB_name GRB130504C
GCN_number 14584
Detection_method Swift-XRT Other
ra 91.6305°
decl 3.8339°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14584 SUBJECT: GRB 130504C: Swift-XRT observations DATE: 13/05/06 00:33:18 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo, A. Melandri (INAF-OAB) report on behalf of the Swift team: We have analysed 1.3 ks of Swift-XRT data for the Fermi 130504C (Kocevski GCN Circ. 14574; Burgess et al. GCN Circ. 14583), from 65.6 ks to 70.1 ks after the LAT trigger. The data are all in Photon Counting (PC) mode. We detect an uncatalogued X-ray source inside the LAT error circle (Kocevski GCN Circ. 14574), at the following position: RA, Dec=91.63047, 3.83388 which is equivalent to: RA (J2000): 06 06 31.3 Dec (J2000): +03 50 01.96 with an uncertainty of 4.8 arcsec (radius, 90% confidence). The count rate at this position is (4.4 +/- 0.7) x 10^-2 cts/s. At the present stage, it is not possible to determine whether the source is fading.
GCN 14587 table
GRB_name GRB130504C
GCN_number 14587
Detection_method Konus-Wind Det
t_trigger 23:29:04.491 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 14587 SUBJECT: Konus-Wind observation of GRB 130504C DATE: 13/05/06 11:08:40 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-duration intense GRB 130504C (Fermi-LAT detection: Kocevski et al., GCN 14574; Fermi-GBM detection: Burgess et al., GCN 14583) triggered Konus-Wind at T0=84544.491s UT (23:29:04.491) The light curve shows multiple partly overlapped peaks from ~T0-15 s to ~T0+105s. The emission is seen up to 12 MeV. A possible hard precursor is seen in the 360-1400 keV light curve at ~T0-50s, but its attribution to GRB 130504C is yet unclear. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB130504_T84544/ As observed by Konus-Wind, the burst had a fluence of (2.0 0.1)x10-4 erg/cm2, and a 64-ms peak flux, measured from T0+21.440s, of (2.6 0.2)x10-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum (measured from T0 to T0+105.216 s) is best fit in the 20 keV - 15 MeV range by the GRB (Band) function with the following model parameters: the low-energy photon index alpha = -1.32 0.04, the high energy photon index beta = -2.15 0.1, the peak energy Ep = 452 49 keV, chi2 = 110/97 dof. The spectrum at the maximum count rate (measured from T0+21.248 to T0+23.296 s) is best fit in the 20 keV - 15 MeV range by the GRB (Band) function with the following model parameters: the low-energy photon index alpha = -0.74 0.12, the high energy photon index beta = -1.93 0.06, the peak energy Ep = 251 38 keV, chi2 = 61/66 dof. All the quoted results are preliminary.
GCN 14588 table
GRB_name GRB130504C
GCN_number 14588
Detection_method Swift-XRT Other
ra 91.6304°
decl 3.8339°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14588 SUBJECT: GRB 130504C: further Swift-XRT observations DATE: 13/05/06 14:14:28 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo, A. Melandri (INAF-OAB), P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team: We have analysed 7.7 ks of XRT data for the Fermi-LAT-detected burst: GRB 130504C, from 65.6 ks to 93.3 ks after the Fermi-LAT trigger. The data are entirely in Photon Counting (PC) mode. The X-ray source reported by D'Avanzo et al. (GCN Circ. 14584) displays behaviour consistent with fading. We propose it as the X-ray afterglow of GRB 130504C. The refined XRT position is RA, Dec = 91.63038, +3.8339 which is equivalent to: RA (J2000): 06 06 31.29 Dec(J2000): +03 50 02.0 with an uncertainty of 3.6 arcsec (radius, 90% confidence). The light curve can be modelled with a power-law decay with a decay index of alpha=1.3 (+/-1.0). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.8 (+/-0.3). The best-fitting absorption column is 5.1 (+2.0, -1.6) x 10^21 cm^-2, in excess of the Galactic value of 2.5 x 10^21 cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 5.0 x 10^-11 (7.9 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 5.1 (+2.0, -1.6) x 10^21 cm^-2 Galactic foreground: 2.5 x 10^21 cm^-2 Excess significance: 2.7 sigma Photon index: 1.8 (+/-0.3) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00020267. This circular is an official product of the Swift-XRT team. [GCN OPS NOTE(06may13): Per author's request, the extra "further" was removed from the ubject-line.]
GCN 14601 table
GRB_name GRB130504C
GCN_number 14601
Detection_method Suzaku WAM Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 14601 SUBJECT: GRB 130504C: Suzaku WAM observation of the prompt emission DATE: 13/05/08 04:31:01 GMT FROM: Makoto Tashiro at Saitama U/Swift T. Yasuda, M. Tashiro, Y. Terada, Y. Ishida, H. Ueno, S. Sugimoto (Saitama U.), M. Ohno, K. Takaki, T. Kawano, R. Nakamura, S. Furui, Y. Fukazawa (Hiroshima U.), M. Yamauchi, N. Ohmori, M. Akiyama (Univ. of Miyazaki), K. Yamaoka (Nagoya U.), S. Sugita (Ehime U.), Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA), W. Iwakiri (RIKEN), Y. Hanabata (ICRR), Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo) on behalf of the Suzaku WAM team, report: The bright, long GRB 130504C (GCN 14574; Fermi-LAT detection : Kocevski et al.) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 23:29:00.540 UT (=T0). The observed light curve shows a multi-peaked structure starting at T0-9 s, ending at T0+110 s with a duration (T90) of about 67 seconds. The fluence in 100 - 1000 keV was 9.11 (+0.14/-0.51) x10^-5 erg/cm^2. The 1-s peak flux measured from T0+ 27 s was 15.9 (+0.3/-4.0) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-9 s to T0+110 s is well fitted by a GRB Band model as follows. the low-energy photon index alpha: -1.59 (+0.17/-0.12), the high-energy photon index beta: -2.43 (+0.17/-0.33), and the peak energy Epeak: 845 (+227/-159) keV (chi^2/d.o.f = 77.0/50). Due to the brightness of this burst, a 1% systematic error was added for low energy channels. All the quoted errors are at statistical 90% confidence level. 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
GCN 14603 table
GRB_name GRB130504C
GCN_number 14603
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 14603 SUBJECT: GRB 130504C: Swift-XRT afterglow confirmation DATE: 13/05/08 15:13:43 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo (INAF-OAB), A.Y. Lien (NASA-GSFC), P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team: We have analysed 12.3 ks of XRT data for the Fermi-LAT-detected burst GRB 130504C (Kocevski et al. GCn Circ 14574), from 65.6 ks to 278.7 ks after the Fermi-LAT trigger. The data are entirely in Photon Counting (PC) mode. The X-ray source reported by D'Avanzo et al. (GCN Circ. 14584, 14588) displays a fading behaviour. The overall light curve can be modelled with a power-law decay with a decay index of alpha=1.39 (+0.32, -0.25). We confirm it as the X-ray afterglow of GRB 130504C. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00020267.