GRB150118B

This page lists all entries on GRB150118B in GRBweb

Summary Fermi GBM IPN Fermi LAT GCN 17307 GCN 17308 GCN 17342 GCN 17344

Summary table
Variable Value Source
GRB_name_Fermi GRB150118409
T0 9:48:17 UTC GCN_circulars,Fermi LAT Det
ra 240.2400° Fermi_LAT
decl -35.7500° Fermi_LAT
pos_error 5.00e-01° Fermi_LAT
T90 40.193 s Fermi_GBM
T90_error 0.572 s Fermi_GBM
T90_start 9:48:25.454 UTC Fermi_GBM
fluence 1.41e-04 erg/cm² Fermi_GBM
fluence_error 1.10e-07 erg/cm² Fermi_GBM
T100 48.647 s
GBM_located False
mjd 57040.408530092594 GCN_circulars,Fermi LAT Det
Fermi GBM table
GRB_name_Fermi GRB150118409
trigger_name bn150118409
ra 240.2400°
decl -35.7500°
pos_error 2.47e+00°
datum 2015-01-18
t_trigger 9:48:17.774 UTC
T90 40.193 s
T90_error 0.572 s
T90_start 9:48:25.454 UTC
fluence 1.41e-04 erg/cm²
fluence_error 1.10e-07 erg/cm²
flux_1024 4.07e+01 erg/cm²/s
flux_1024_error 4.13e-01 erg/cm²/s
flux_1024_time 4.58e+01 erg/cm²/s
flux_64 4.62e+01 erg/cm²/s
flux_64_error 1.75e+00 erg/cm²/s
IPN table
GRB_name GRB150118B
ra 240.2417°
decl -35.7500°
pos_error 5.00e-01°
Fermi LAT table
GRB_name_Fermi GRB150118409
GRB_name GRB150118B
MET 443267300.76
datum 2015-01-18
t_trigger 9:48:17.760 UTC
ra 240.2400°
decl -35.7500°
pos_error 5.00e-01°
GCN 17307 table
GRB_name GRB150118B
GCN_number 17307
Detection_method Fermi LAT Det
t_trigger 9:48:17 UTC
ra 240.2400°
decl -35.7500°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17307 SUBJECT: GRB 150118B: Fermi-LAT detection DATE: 15/01/18 23:05:42 GMT FROM: Daniel Kocevski at GSFC D. Kocevski (NASA/GSFC), J. Racusin (NASA/GSFC), S. Zhu (UMD) and M. Arimoto (Tokyo Tech) report on behalf of the Fermi-LAT team: At 09:48:17 UT on Jan 18th, 2015, Fermi-LAT detected high-energy emission from GRB 150118B, which was also detected by Fermi-GBM (trigger 443267300/150118409). The best LAT on-ground location is found to be RA, Dec = 240.24, -35.75 (J2000) with an error radius of 0.5 deg (90% containment, statistical error only). This was ~60 deg from the LAT boresight at the time of the trigger and triggered an autonomous repoint of the spacecraft, although the source was occulted by the Earth within 150s of the GBM trigger and didn't re-enter the LAT field of view until T0+2500s The data from the Fermi-LAT show an increase in the event rate after the GBM trigger that is temporally correlated with the GBM emission. The detection above 100 MeV is primarily driven by a single 2 GeV event which is observed within 5 degrees of the GBM position and ~50 seconds after the GBM trigger. Using the LAT Low Energy (LLE) data selection, which is sensitive to > 30 MeV, an increase in the event rate at > 8 sigma significance above background was observed approximately coincident with the time of the GBM emission. The Fermi-LAT point of contact for this burst is Makoto Arimoto (arimoto@hp.phys.titech.ac.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 17308 table
GRB_name GRB150118B
GCN_number 17308
Detection_method Fermi GBM Det
t_trigger 9:48:17.770 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 17308 SUBJECT: GRB 150118B: Fermi GBM Detection DATE: 15/01/18 23:44:36 GMT FROM: Matthew Stanbro at UAH/Fermi Matthew Stanbro (UAH) reports on behalf of the Fermi GBM Team: "At 09:48:17.77 UT on 18 January 2015, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 150118B (trigger 443267300 / 150118409) which was also detected by the Fermi-LAT (Kocevski et al. 2015, GCN 17307) The GBM on-ground location is consistent with the LAT position. The trigger caused GBM to generate an Autonomous Repoint of Fermi. The GBM light curve consists of several episodes with a duration (T90) of about 40 s (50-300 keV). The time-averaged spectrum from T0-4.608 s to T0+49.665 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.89 +/- 0.01 and the cutoff energy, parameterized as Epeak, is 755 +/- 14 keV The event fluence (10-1000 keV) in this time interval is (1.5 +/- 0.007)E-04 erg/cm^2. The 1-sec peak photon flux measured starting from T0+45.8 s in the 8-1000 keV band is 40.7 +/- 0.4 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 17342 table
GRB_name GRB150118B
GCN_number 17342
Detection_method IPN Triangulation
t_trigger 9:48:18 UTC
ra 242.0080°
decl -36.0200°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17342 SUBJECT: IPN Triangulation of GRB 150118B (long/intense) DATE: 15/01/21 21:12:38 GMT FROM: Dmitry Svinkin at Ioffe Institute K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team, I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin, on behalf of the HEND-Odyssey GRB team, S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, V. Connaughton, M. S. Briggs, C. Meegan, and 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: The long-duration, bright GRB 150118B (Kocevski et al., GCN Circ. 17307) has been observed by Fermi (GBM trigger 443267300; Stanbro GCN Circ. 17308), Konus-Wind, INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), MESSENGER (GRNS), and Swift (BAT), so far, at about 35298 s UT (09:48:18). 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: 242.008 (16h 08m 02s) -36.020 (-36d 01' 12") Corners: 242.375 (16h 09m 30s) -34.181 (-34d 10' 51") 241.798 (16h 07m 12s) -36.507 (-36d 30' 24") 241.669 (16h 06m 40s) -37.699 (-37d 41' 55") 242.219 (16h 08m 53s) -35.520 (-35d 31' 13") --------------------------------------------- The error box area is 1139 sq. arcmin, and its maximum dimension is 3.56 deg (the minimum one is 8.3 arcmin). The Sun distance was 52 deg. The box is long because all annuli intersect at grazing incidence due to conjunction of the spacecraft involved in the triangulation. The Fermi (LAT) position (Kocevski et al., GCN Circ. 17307) is outside of the box at 1.5 deg from its center. This box may be improved. A triangulation map is posted at http://www.ioffe.ru/LEA/GRBs/GRB150118_T35302/IPN/ The Konus-Wind time history and spectrum will be given in forthcoming GCN Circular.
GCN 17344 table
GRB_name GRB150118B
GCN_number 17344
Detection_method Konus-Wind Det
t_trigger 9:48:22.394 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 17344 SUBJECT: Konus-Wind observation of GRB 150118B DATE: 15/01/22 11:30:17 GMT FROM: Dmitry Frederiks at Ioffe Institute S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A.Lysenko, and T. Cline on behalf of the Konus-Wind team, report: The long-duration, hard-spectrum, intense GRB 150118B (Fermi-LAT detection: Kocevski et al., GCN 17307; Fermi-GBM detection: Stanbro, GCN 17308; IPN triangulation: Hurley et al., GCN 17342) triggered Konus-Wind at T0=35302.394 s UT (09:48:22.394). The light curve shows multiple emission episodes from ~T0-8 s to ~T0+60 s. The emission is seen up to ~10 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB150118_T35302/ As observed by Konus-Wind, the burst had a fluence of 1.87(-0.15,+0.14)x10^-4 erg/cm2, and a 64-ms peak flux, measured from T0+39.680 s, of 1.88(-0.18,+0.20)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum (measured from T0 to T0+58.368 s) is best fit in the 20 keV - 15 MeV range by the cutoff power law with the following model parameters: the photon index alpha = -0.98(-0.04,+0.04), and the peak energy Ep = 695(-42,+47) keV, chi2 = 103/97 dof. Fitting this spectrum with the Band model yields the same values of alpha and Ep with an upper limit on beta of -2.8 The spectrum near the peak count rate (measured from T0+35.328 to T0+41.984 s) is best fit in the 20 keV - 15 MeV range by the cutoff power law with the following model parameters: the photon index alpha = -0.84(-0.08,+0.08), and the peak energy Ep = 614(-55,+64) keV, chi2 = 115/98 dof. All the quoted errors are at the 90% sigma confidence level. All the quoted values are preliminary.