GRB160806A

This page lists all entries on GRB160806A in GRBweb

Summary Fermi GBM GCN 19784 GCN 19785 GCN 19786 GCN 19789

Summary table
Variable Value Source
GRB_name_Fermi GRB160806584
T0 14:00:58.229 UTC Fermi_GBM
ra 274.4770° GCN_circulars,IPN Triangulation
decl 10.6070° GCN_circulars,IPN Triangulation
T90 1.664 s Fermi_GBM
T90_error 0.453 s Fermi_GBM
T90_start 14:00:58.229 UTC Fermi_GBM
fluence 1.65e-06 erg/cm² Fermi_GBM
fluence_error 2.79e-08 erg/cm² Fermi_GBM
T100 1.664 s
GBM_located False
mjd 57606.58400728009 Fermi_GBM
Fermi GBM table
GRB_name_Fermi GRB160806584
trigger_name bn160806584
ra 274.4771°
decl 10.6069°
pos_error 4.36e+00°
datum 2016-08-06
t_trigger 14:00:58.421 UTC
T90 1.664 s
T90_error 0.453 s
T90_start 14:00:58.229 UTC
fluence 1.65e-06 erg/cm²
fluence_error 2.79e-08 erg/cm²
flux_1024 1.12e+01 erg/cm²/s
flux_1024_error 4.39e-01 erg/cm²/s
flux_1024_time -1.28e-01 erg/cm²/s
flux_64 1.85e+01 erg/cm²/s
flux_64_error 2.10e+00 erg/cm²/s
GCN 19784 table
GRB_name GRB160806A
GCN_number 19784
Detection_method IPN Triangulation
t_trigger 14:01:00 UTC
ra 274.4770°
decl 10.6070°
Circular_text TITLE: GCN CIRCULAR NUMBER: 19784 SUBJECT: IPN Triangulation of GRB 160806A DATE: 16/08/09 12:59:49 GMT FROM: Anna Kozlova at Ioffe Institute K. Hurley, on behalf of the IPN, I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin, on behalf of the HEND-Odyssey GRB team, A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa, and A. Goldstein, on behalf of the Fermi GBM team, S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer, on behalf of the Swift-BAT team, A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, and W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr, on behalf of the GRS-Odyssey GRB team, report: A short-duration GRB 160806A has been detected by Fermi (GBM), Konus-Wind, INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), and Swift (BAT) at about 50460 s UT (14:01:00). The burst was outside the coded field of view of the BAT. We have triangulated it to a preliminary, 3 sigma error box whose coordinates are: --------------------------------------------- RA(2000), deg Dec(2000), deg --------------------------------------------- Center: 274.477 (18h 17m 54s) +10.607 (+10d 36' 25") Corners: 275.105 (18h 20m 25s) +10.412 (+10d 24' 42") 274.010 (18h 16m 02s) +11.481 (+11d 28' 52") 273.846 (18h 15m 23s) +10.795 (+10d 47' 42") 274.941 (18h 19m 46s) +9.712 ( +9d 42' 45") --------------------------------------------- The error box area is 3308 sq. arcmin, and its maximum dimension is 1.99 deg (the minimum one is 36 arcmin). The Sun distance was about 130 deg. This box may be improved. A triangulation map is posted at http://www.ioffe.ru/LEA/GRBs/GRB160806_T50460/IPN/ The Konus-Wind time history and spectrum will be given in a forthcoming GCN Circular.
GCN 19785 table
GRB_name GRB160806A
GCN_number 19785
Detection_method Konus-Wind Det
t_trigger 14:01:00.639 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 19785 SUBJECT: Konus-Wind observation of GRB 160806A DATE: 16/08/09 13:29:03 GMT FROM: Anna Kozlova at Ioffe Institute A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline on behalf of the Konus-Wind team, report: The short-duration GRB 160806A (IPN triangulation: Hurley et al., GCN 19784) triggered Konus-Wind at T0=50460.639 s UT (14:01:00.639). The burst light curve shows a single pulse which starts at ~T0-0.5 s and has a total duration of ~1.0 s. The emission is seen up to ~8 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB160806_T50460/ As observed by Konus-Wind, the burst had a fluence of 1.16(-0.23,+0.49)x10^-6 erg/cm2, and a 16-ms peak flux, measured from T0-0.026 s, of 5.98(-3.46,+4.98)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The spectrum of the burst (measured from T0 to T0+0.256 s) is well fit in the 20 keV - 8 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -1.00 (-0.51,+0.80) and Ep = 219 (-76,+395) keV (chi2 = 43/33 dof). Fitting by a GRB (Band) model yields alpha = -0.63 (-0.65,+1.00), Ep = 171 (-59,+154) keV, and an upper limit on the high energy photon index: beta < -1.8 (chi2 = 40/32 dof) All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 19786 table
GRB_name GRB160806A
GCN_number 19786
Detection_method Fermi GBM Det
t_trigger 14:00:58.420 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 19786 SUBJECT: GRB 160806A: Fermi GBM observation DATE: 16/08/09 15:54:06 GMT FROM: Peter Veres at UAH P Veres (UAH) and C Meegan (UAH) report on behalf of the Fermi GBM Team: "At 14:00:58.42 UT on 6 August 2016, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 160806A (trigger 492184862 / 160806584) which was also detected by the Konus-Wind (Kozlova et al., GCN 19785) and located by the Interplanetary Network (Hurley et al., GCN 19784). The GBM on-ground location is consistent with the IPN position. The angle from the Fermi LAT boresight at the GBM trigger time is 112 degrees. This burst was also independently detected by INTEGRAL SPI-ACS. The GBM light curve consists of a single symmetric pulse with a duration (T90) of about 1.7 s (50-300 keV). The time-averaged spectrum from T0 to T0+2 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.58 +/- 0.14 and the cutoff energy, parameterized as Epeak, is 142 +/- 11 keV. The event fluence (10-1000 keV) in this time interval is (1.35 +/- 0.07)E-6 erg/cm^2. The 64 ms peak photon flux measured starting from T0+0.13 s in the 10-1000 keV band is 17.6 +/- 2.0 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 122 +/- 15 keV, alpha = -0.41 +/- 0.20 and beta = -2.64 +/- 0.38. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 19789 table
GRB_name GRB160806A
GCN_number 19789
Detection_method INTEGRAL
Circular_text TITLE: GCN CIRCULAR NUMBER: 19789 SUBJECT: INTEGRAL/SPI-ACS and IBIS_VETO search for prompt gamma-ray counterpart of IceCube-160806A DATE: 16/08/10 16:40:10 GMT FROM: Volodymyr Savchenko at ISDC,U of Geneve V. Savchenko (APC, Paris, France) , C. Ferrigno (ISDC, University of Geneva, CH), P. Ubertini, A. Bazzano, L. Natalucci (IAPS-Roma, Italy), S. Mereghetti (IASF-Milano, Italy), P. Laurent (CEA, Saclay, France), E. Kuulkers (ESAC/ESA, Madrid, Spain) Using INTEGRAL/SPI-ACS and INTEGRAL/IBIS VETO we have performed a search for prompt gamma-ray counterpart of cosmic neutrino candidate IceCube-160806A (Cowen 2016, GCN 19787). At the time of the event (2016-08-06T12:21:33 UTC, hereafter T0), INTEGRAL IBIS was operating in the nominal mode. INTEGRAL/SPI was finishing the annealing cycle: at this stage of the procedure it has no effect on SPI-ACS. The spacecraft was pointing in the direction of Norma Arm Region, and the neutrino localization was at 110 deg angle with respect to the pointing axis. This orientation enables high response of both SPI-ACS and IBIS_VETO. The nearest confirmed GRB (GRB160806A), was triggered by INTEGRAL/SPI-ACS at 2016-08-06 14:00:57, 1h 40m after the event. This GRB is also detected in the IBIS_VETO light curve. SPI-ACS and IBIS_VETO (bottom) light-curves around the time of the neutrino candidate event can be found at: http://isdc.unige.ch/~savchenk/IceCube-160806A/ The count rate data around the event reveals variability, including smooth background instabilities as well as burst-like events. Several burst-like excesses can be seen, most prominent ones at T0+50s, T-150s, T0-2000s, and T0-10000s. Ratio of SPI-ACS to IBIS_VETO rates for these events is compatible with a gamma-ray source from the direction of IceCube-160806A. However, we note that these flares are coincident with GOES proton background flares. Although we can not exclude cosmic origin of some of these bursts, judging from long-lasting background instability near the region of interest, as well as the activity observed by GOES, we are inclined to conclude that these bursts are associated with background variability introduced by solar activity. We estimate a 3-sigma upper limit on fluence in 75-2000 keV energy range in the interval ±1000 s around the IceCube trigger of 3.3x10^-7 erg/cm^2 for a burst with duration less than 1 s with a characteristic short GRB spectrum (an exponentially cut off power law with alpha=-0.5 and Ep=500 keV). For a typical long GRB spectrum (the Band function with alpha=-1, beta=-2.5, and Ep=250 keV), the corresponding limiting peak flux is ~2.2x10^-7 erg/cm^2/s at 1 s time scale in 75-2000 keV energy range. The SPI-ACS light curves, binned at 50 ms, are derived from 91 independent detectors with different lower energy thresholds (mainly between 50 keV and 150 keV) and an upper threshold at about 100 MeV. The IBIS_VETO light curves, binned at 8 s, are derived from 16 independent detectors with lower energy thresholds near 80 keV and an upper threshold at about 50 MeV. Two groups of detector rates are recorded independently: bottom and lateral IBIS VETO. The response of the bottom IBIS VETO peaks in the direction opposite to satellite pointing axis, where the response of SPI-ACS is suppressed. Due to solar angle constrains, INTEGRAL can not perform pointed observation of the location of IceCube-160806A until September 22, so no pointed follow-up will be scheduled.