GRB130327B

This page lists all entries on GRB130327B in GRBweb

Summary Fermi GBM IPN Fermi LAT GCN 14344 GCN 14346 GCN 14347 GCN 14348 GCN 14353 GCN 14357 GCN 14398

Summary table
Variable Value Source
GRB_name_Fermi GRB130327350
T0 8:24:04 UTC Fermi_LAT
ra 217.8749° Fermi_LAT
decl -69.4034° Fermi_LAT
pos_error 1.14e-03° Fermi_LAT
T90 31.233 s Fermi_GBM
T90_error 0.724 s Fermi_GBM
T90_start 8:24:06.099 UTC Fermi_GBM
fluence 5.20e-05 erg/cm² Fermi_GBM
fluence_error 8.06e-08 erg/cm² Fermi_GBM
T100 33.332 s
GBM_located False
mjd 56378.3500462963 Fermi_LAT
Fermi GBM table
GRB_name_Fermi GRB130327350
trigger_name bn130327350
ra 218.0900°
decl -69.5100°
pos_error 2.64e+00°
datum 2013-03-27
t_trigger 8:24:04.051 UTC
T90 31.233 s
T90_error 0.724 s
T90_start 8:24:06.099 UTC
fluence 5.20e-05 erg/cm²
fluence_error 8.06e-08 erg/cm²
flux_1024 1.26e+01 erg/cm²/s
flux_1024_error 3.23e-01 erg/cm²/s
flux_1024_time 3.25e+01 erg/cm²/s
flux_64 1.68e+01 erg/cm²/s
flux_64_error 1.31e+00 erg/cm²/s
IPN table
GRB_name GRB130327B
ra 218.0917°
decl -69.5167°
pos_error 1.67e-01°
Fermi LAT table
GRB_name_Fermi GRB130327350
GRB_name GRB130327B
MET 386065447.0
datum 2013-03-27
t_trigger 8:24:04 UTC
ra 217.8749°
decl -69.4034°
pos_error 1.14e-03°
GCN 14344 table
GRB_name GRB130327B
GCN_number 14344
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 14344 SUBJECT: GRB 130327B: gamma-ray detection by AGILE DATE: 13/03/27 23:24:56 GMT FROM: Ettore Del Monte at IASF/INAF F. Longo (University of Trieste and INFN Trieste), A. Giuliani (INAF/IASF Milan), M. Marisaldi (INAF/IASF Bologna), E. Del Monte (INAF/IAPS Rome), F. Lazzarotto, I. Donnarumma, Y. Evangelista, M. Feroci, L. Pacciani, P. Soffitta, E. Costa, I. Lapshov, M. Rapisarda (INAF/IAPS Rome), G. Barbiellini, (INFN Trieste), 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), M. Tavani, V. Vittorini, A. Argan, G. Piano, S. Sabatini, M. Cardillo (INAF/IASF Rome), G. Pucella (ENEA Frascati), A. Pellizzoni, A. Trois (INAF/OA Cagliari), M. Pilia (ASTRON), S. Vercellone (INAF/IASF Palermo), P. W. Cattaneo, A. Rappoldi (INFN Pavia), P. Picozza, A. Morselli, E. Striani, (INFN Roma-2), M. Prest, E. Vallazza (Universita' dell'Insubria), P. Lipari, D. Zanello (INFN Roma-1), P. Giommi, C. Pittori, F. Lucarelli, P. Santolamazza, F. Verrecchia (ASDC) and G. Valentini (ASI), on behalf of the AGILE Team, report: The AGILE Gamma Ray Imaging Detector (GRID) detected emission from GRB 130327B, localised by Fermi/GBM (http://gcn.gsfc.nasa.gov/other/386065447.fermi). The GRB occurred at approximately 28 deg off-axis in the field of view of the AGILE/GRID. A preliminary analysis of the AGILE/GRID data in temporal coincidence with the GRB shows a significant excess of gamma-ray events above 80 MeV at the location of the event. Most of the events detected by the AGILE/GRID have times between ~ t0 + 9 sec and t0 + 14 sec where t0 is 27 March 2013 at 08:24:04.05 UT. The GRB was also detected also by the AGILE/MCAL, operating in the energy range 0.5 - 100 MeV. A more detailed analysis of the AGILE data is in progress. More observations of this interesting burst are strongly encouraged. This message may be cited.
GCN 14346 table
GRB_name GRB130327B
GCN_number 14346
Detection_method Fermi GBM Det
t_trigger 8:24:04.050 UTC
ra 214.9000°
decl -74.6000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14346 SUBJECT: GRB 130327B: Fermi GBM detection DATE: 13/03/28 03:35:36 GMT FROM: Vandiver Chaplin at UAH/Fermi-GBM V.Chaplin (UAH) and G. Fitzpatrick (UCD) report on behalf of the Fermi GBM Team: "At 08:24:04.05 UT on 27 March 2013, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 130327B (trigger 386065447 / 130327350), which was also detected by several instruments on-board the AGILE spacecraft (Del Monte et al. GCN 14344). The on-ground calculated location, using the GBM trigger data, is RA = 214.9, DEC = -74.6 degrees, with an uncertainty of 1 degree (radius, 1-sigma containment, statistical only; there is additionally a systematic error which is currently estimated to be 2 to 3 degrees). The angle from the Fermi LAT boresight at the GBM trigger time was 47 degrees. The Fermi Observatory executed a maneuver following this trigger and tracked the burst location for the next 2.5 hours, subject to Earth-angle constraints. The GBM light curve consists of multiple spikes on top of a gradual rise and decay. The main emission occurs between T0 and T0+35 seconds. The total duration (T90) is about 62 s (50-300 keV). The time-averaged spectrum from T0-0.8 s to T0+33 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.57 +/- 0.02 and the cutoff energy, parameterized as Epeak, is 341 +/- 6.3 keV. The spectrum also fits a Band function with Epeak = 334 +/- 7 keV, alpha = -0.56 +/- 0.02, and beta = -3.4 +/- 0.4. The event fluence (10-1000 keV) in this time interval is (5.176 +/- 0.057)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+32.4 s in the 8-1000 keV band is 12.7 +/- 0.3 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 14347 table
GRB_name GRB130327B
GCN_number 14347
Detection_method Fermi LAT Det
t_trigger 8:24:04 UTC
ra 218.0900°
decl -69.5100°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14347 SUBJECT: GRB 130327B: Fermi-LAT detection of a burst DATE: 13/03/28 04:29:54 GMT FROM: Masanori Ohno at Hiroshima U M. Ohno (Hiroshima U.), J. McEnery (NASA/GSFC), G. Vianello (Stanford), J.L. Racusin (NASA/GSFC) and E. Troja (CRESST) report on behalf of the Fermi-LAT team: At 08:24:04 on March 27th, 2013, Fermi LAT detected high energy emission from GRB 130327B, which was also detected by Fermi-GBM (trigger 386065447 / 130327350 ; Chaplin and Fitzpatrick GCN 14346) and by AGILE (Del Monte et al. GCN 14344). The best LAT on-ground location is found to be RA, DEC 218.09, -69.51 (J2000) with an error radius of 0.17 deg (68% containment, statistical error only), this was about 50 deg from the LAT boresight at the time of the trigger and triggered an autonomous repoint of the spacecraft. The data from the Fermi LAT show a significant increase in the event rate within 5 degree of the GBM location after the GBM trigger that is spatially and temporally correlated with the GBM emission with high significance. More than 20 photons above 100 MeV are observed within 100 seconds. A Swift TOO observation has been requested. The Fermi LAT point of contact for this burst is Julie McEnery ( julie.mcenery@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. [GCN OPS NOTE(28mar13): Per author's request, the date in the first sentence was changed from "28" to "27".]
GCN 14348 table
GRB_name GRB130327B
GCN_number 14348
Detection_method Konus-Wind Det
t_trigger 8:24:07.662 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 14348 SUBJECT: Konus-Wind observation of GRB 130327B DATE: 13/03/28 09:37:10 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 GRB 130327B (AGILE detection: Longo et al., GCN 14344; Fermi-GBM detection: Chaplin and Fitzpatrick, GCN 14346; Fermi-LAT detection: Ohno et al., GCN 14347) triggered Konus-Wind at T0=30247.662s UT (08:24:07.662) The light curve shows a multi-peaked structure with a total duration of ~35 s. The emission is seen up to 12 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB130327_T30247/ As observed by Konus-Wind, the burst had a fluence of (5.6 0.5)x10-5 erg/cm2, and a 64-ms peak flux, measured from T0+4.352s, of (4.9 0.5)x10-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum (measured from T0 to T0+40.704 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 = -0.59 0.08, the high energy photon index beta = -2.65 0.25, the peak energy Ep = 278 18 keV, chi2 = 122/97 dof. The spectrum at the maximum count rate (measured from T0 to T0+7.936 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 = -0.62 0.13, the high energy photon index beta = -2.6 0.4, the peak energy Ep = 314 39 keV, chi2 = 97.6/92 dof. All the quoted results are preliminary.
GCN 14353 table
GRB_name GRB130327B
GCN_number 14353
Detection_method Swift-XRT Other
ra 217.8749°
decl -69.4035°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14353 SUBJECT: Swift/XRT observation of GRB 130327B DATE: 13/03/29 13:16:30 GMT FROM: Hans Krimm at NASA-GSFC H. A. Krimm (CRESST/GSFC/USRA) and V. Mangano (INAF-IASFPA) for the Swift team: We have analysed 7.9 ks of XRT data for the AGILE/Konus/Fermi-detected burst: GRB 130327B (Longo et al, GCN 14344; Chaplin & Fitzpatrick, GCN 14346; Ohno et al, GCN 14347; Golenetskii et al, GCN 14348), from 110.1 ks to 128.6 ks after the Fermi/GBM trigger. The data are entirely in Photon Counting (PC) mode. An X-ray source is detected within the Fermi/LAT error circle. The refined XRT position is RA, Dec = 217.87488, -69.40345 which is equivalent to: RA (J2000): 14 31 29.97 Dec(J2000): -69 24 12.4 with an uncertainty of 4.1 arcsec (radius, 90% confidence). This position is 459 arcsec from the Fermi/LAT position. We cannot determine at the present time whether the source is fading. The count rate level is 4 x 10^-3 counts/s. Further Swift observations have been scheduled.
GCN 14357 table
GRB_name GRB130327B
GCN_number 14357
Detection_method Suzaku WAM Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 14357 SUBJECT: GRB 130327B: Suzaku WAM observation of the prompt emission DATE: 13/04/01 12:17:36 GMT FROM: Makoto Tashiro at Saitama U/Swift Y. Ishida, M. Tashiro, Y. Terada, T. Yasuda, H. Ueno, S. Sugimoto (Saitama U.), K. Yamaoka (Nagoya U.), M. Ohno, T. Kawano, K. Takaki, R. Nakamura, Y. Fukazawa (Hiroshima U.), M. Yamauchi, M. Akiyama, N. Ohmori, E. Mochinaga (Univ. of Miyazaki), 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 long GRB 130327B (Chaplin et al GCN14346) was detected by the the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 08:24:04.751 UT (=T0). The observed light curve shows double-peaked structure starting at T0-1s, ending at T0+33s with a duration (T90) of about 30 seconds. The fluence in 100 - 1000 keV was 3.29(+0.15/-0.21)x10^-5 erg/cm^2. The 1-s peak flux measured from T0+23s was 2.23 photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-1s to T0+33s is well fitted by a power-law with exponential cutoff model : dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with alpha 0.89(+0.46/-0.56), and Epeak 484(+64/-50) keV (chi^2 / d.o.f. = 11.1/13). All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are included. The light curves for this burst will be available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html
GCN 14398 table
GRB_name GRB130327B
GCN_number 14398
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 14398 SUBJECT: GRB 130327B: Swift/XRT source is not the afterglow DATE: 13/04/19 20:11:29 GMT FROM: Hans Krimm at NASA-GSFC H. A. Krimm (CRESST/GSFC/USRA) and E. Troja (NASA/GSFC/CRESST) for the Swift team: Swift carried out an additional 4.6 ksec observation of the field containing GRB 130327B (e.g. Longo et al, GCN 14344; Ohno et al, GCN 14347), starting at 2013-04-18 12:43:13 UT, approximately 22 days after the burst. The source reported in Krimm & Mangano (GCN 14353) as a possible afterglow to GRB 130327B is still detected at a rate of 0.002 0.001 cts/s (0.3-10 keV), which is statistically consistent with the rate reported in GCN 14353. Since we would expect a GRB afterglow to have faded over this time period, we conclude that the XRT source is not associated with GRB 130327B, and is instead a background source, possibly an AGN. No further Swift observations are planned.