GRB161004B

This page lists all entries on GRB161004B in GRBweb

Summary Fermi GBM IPN Swift GCN 19987 GCN 19988 GCN 19991 GCN 19994 GCN 19995 GCN 19996 GCN 19997 GCN 19998 GCN 20003 GCN 20005

Summary table
Variable Value Source
GRB_name_Fermi GRB161004964
T0 23:07:54.317 UTC GCN_circulars,Konus-Wind Det
ra 112.1512° Swift
decl -39.8979° Swift
pos_error 1.81e-04° Swift
T90 12.8 s Fermi_GBM
T90_error 0.572 s Fermi_GBM
T90_start 23:07:56.067 UTC Fermi_GBM
fluence 1.73e-05 erg/cm² Fermi_GBM
fluence_error 2.87e-08 erg/cm² Fermi_GBM
T100 20.583 s
GBM_located False
mjd 57665.96382311342 GCN_circulars,Konus-Wind Det
Fermi GBM table
GRB_name_Fermi GRB161004964
trigger_name bn161004964
ra 112.1571°
decl -39.8950°
pos_error 2.49e+00°
datum 2016-10-04
t_trigger 23:07:54.787 UTC
T90 12.8 s
T90_error 0.572 s
T90_start 23:07:56.067 UTC
fluence 1.73e-05 erg/cm²
fluence_error 2.87e-08 erg/cm²
flux_1024 1.58e+01 erg/cm²/s
flux_1024_error 4.21e-01 erg/cm²/s
flux_1024_time 4.67e+00 erg/cm²/s
flux_64 1.90e+01 erg/cm²/s
flux_64_error 1.88e+00 erg/cm²/s
IPN table
GRB_name GRB161004B
ra 112.1583°
decl -39.9000°
pos_error 5.00e-02°
Swift table
GRB_name GRB161004B
t_trigger 23:07:59 UTC
ra 112.1512°
decl -39.8979°
pos_error 1.81e-04°
T90 15.9 s
fluence 8.80e-06 erg/cm²
GCN 19987 table
GRB_name GRB161004B
GCN_number 19987
Detection_method Swift Det
t_trigger 23:07:59 UTC
ra 112.1570°
decl -39.8950°
Circular_text TITLE: GCN CIRCULAR NUMBER: 19987 SUBJECT: GRB 161004B: Swift detection of a burst DATE: 16/10/04 23:18:17 GMT FROM: David Palmer at LANL A. D'Ai (INAF-IASFPA), V. D'Elia (ASDC), F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL) and B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team: At 23:07:59 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 161004B (trigger=715246). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 112.157, -39.895 which is RA(J2000) = 07h 28m 38s Dec(J2000) = -39d 53' 40" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single FRED peak with substructure and a duration of about 20 sec. The peak count rate was ~12000 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began observing the field at 23:09:12.7 UT, 73.4 seconds after the BAT trigger. Using promptly downlinked data we find a bright, uncatalogued X-ray source located at RA, Dec 112.15290, -39.89858 which is equivalent to: RA(J2000) = 07h 28m 36.70s Dec(J2000) = -39d 53' 54.9" with an uncertainty of 3.6 arcseconds (radius, 90% containment). This location is 17 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. We cannot determine whether the source is fading at the present time. No spectrum from the promptly downlinked event data is yet available to determine the column density. The initial flux in the 2.5 s image was 5.23e-10 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 82 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT 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 0.54. Burst Advocate for this burst is A. D'Ai (antonino.dai AT ifc.inaf.it). 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 19988 table
GRB_name GRB161004B
GCN_number 19988
Detection_method Swift-XRT Other
ra 112.1514°
decl -39.8976°
Circular_text TITLE: GCN CIRCULAR NUMBER: 19988 SUBJECT: GRB 161004B: Prompt enhanced Swift-XRT position DATE: 16/10/04 23:53:05 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Using promptly downlinked XRT event data for GRB 161004B, we find an enhanced XRT position of the afterglow: RA, Dec: 112.1514, -39.8976 which is equivalent to: RA (J2000) = 07 28 36.34 Dec (J2000) = -39 53 51.5 with an uncertainty of 2.0 arcseconds (radius, 90% confidence). Analysis of the promptly available data is online at http://www.swift.ac.uk/sper/715246. Position enhancement is is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular is an official product of the Swift-XRT team.
GCN 19991 table
GRB_name GRB161004B
GCN_number 19991
Detection_method Swift-XRT Det
ra 112.1513°
decl -39.8979°
Circular_text TITLE: GCN CIRCULAR NUMBER: 19991 SUBJECT: GRB 161004B: Enhanced Swift-XRT position DATE: 16/10/05 11:55:09 GMT FROM: Phil Evans at U of Leicester P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) report on behalf of the Swift-XRT team. Using 3535 s of XRT Photon Counting mode data and 5 UVOT images for GRB 161004B, 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 = 112.15126, -39.89791 which is equivalent to: RA (J2000): 07h 28m 36.30s Dec (J2000): -39d 53' 52.5" 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, MNRAS, 397, 1177). This circular was automatically generated, and is an official product of the Swift-XRT team.
GCN 19994 table
GRB_name GRB161004B
GCN_number 19994
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 19994 SUBJECT: GRB 161004B: Swift-XRT refined Analysis DATE: 16/10/05 12:53:00 GMT FROM: Phil Evans at U of Leicester V. D'Elia (ASDC), D.N. Burrows (PSU), T.G.R. Roegiers (PSU), L.M. McCauley (PSU), P.A. Evans (U. Leicester), S.L. Gibson (U. Leicester), J.P. Osborne (U. Leicester), A. Melandri (INAF-OAB) and A. D'Ai report on behalf of the Swift-XRT team: We have analysed 7.1 ks of XRT data for GRB 161004B (D'Ai et al. GCN Circ. 19987), from 63 s to 28.2 ks after the BAT trigger. The data comprise 77 s in Windowed Timing (WT) mode (the first 9 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Evans et al. (GCN Circ. 19988). The light curve can be modelled with an initial power-law decay with an index of alpha=0.89 (+/-0.05), followed by a break at T+2716 s to an alpha of 1.44 (+0.30, -0.22). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.99 (+0.19, -0.18). The best-fitting absorption column is 1.14 (+0.21, -0.19) x 10^22 cm^-2, in excess of the Galactic value of 3.5 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 5.1 x 10^-11 (9.7 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.14 (+0.21, -0.19) x 10^22 cm^-2 Galactic foreground: 3.5 x 10^21 cm^-2 Excess significance: 7.1 sigma Photon index: 1.99 (+0.19, -0.18) If the light curve continues to decay with a power-law decay index of 1.44, the count rate at T+24 hours will be 2.1 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x 10^-13 (2.0 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00715246. This circular is an official product of the Swift-XRT team.
GCN 19995 table
GRB_name GRB161004B
GCN_number 19995
Detection_method Swift-BAT Det
ra 112.1560°
decl -39.8960°
Circular_text TITLE: GCN CIRCULAR NUMBER: 19995 SUBJECT: GRB 161004B: Swift-BAT refined analysis DATE: 16/10/05 13:02:02 GMT FROM: Takanori Sakamoto at AGU T. Sakamoto (AGU), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC), A. D'Ai (INAF-IASFPA), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (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 161004B (trigger #715246) (D'Ai, et al., GCN Circ. 19987). The BAT ground-calculated position is RA, Dec = 112.156, -39.896 deg which is RA(J2000) = 07h 28m 37.4s Dec(J2000) = -39d 53' 47.3" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 75%. The mask-weighted light curve shows two overlapping peaks starting at T-10 sec, peaking at T+1 sec and ending at T+40 sec. T90 (15-350 keV) is 15.9 +- 0.7 sec (estimated error including systematics). The time-averaged spectrum from T-5.16 to T+27.31 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 1.21 +- 0.13, and Epeak of 177 +- 73 keV (chi squared 35.21 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 8.8 +- 0.2 x 10^-6 erg/cm2 and the 1-sec peak flux measured from T+0.36 sec in the 15-150 keV band is 10.1 +- 0.4 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.47 +- 0.03 (chi squared 47.75 for 57 d.o.f.). 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/715246/BA/
GCN 19996 table
GRB_name GRB161004B
GCN_number 19996
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 19996 SUBJECT: GRB161004B: AstroSat CZTI detection DATE: 16/10/05 14:56:42 GMT FROM: Dipankar Bhattacharya at IUCAA V. Kumar, V. Sharma, D. Bhattacharya and V. Bhalerao (IUCAA), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: Analysis of AstroSat CZTI data showed clear detection of GRB161004B (Swift BAT detection: D.Palmer et al., GCN Circ. 19987) in the 40-200 keV energy range. The light curve shows a single peak at 23:07:59.0 UT, coincident with the Swift Trigger. The measured peak count rate is 187.3 counts/sec above the background in combined data of four quadrants, with a total of 1393.0 counts. The local mean background count rate was 313.7 counts/sec. Using cumulative rates, we measure a T90 of 13.1 secs. CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.
GCN 19997 table
GRB_name GRB161004B
GCN_number 19997
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 19997 SUBJECT: GRB 161004B: Swift/UVOT Upper Limits DATE: 16/10/05 16:23:52 GMT FROM: Frank Marshall at GSFC F. E. Marshall (NASA/GSFC) and A. D'Ai (INAF-IASFPA) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 161004B 82 s after the BAT trigger (D'Ai et al., GCN Circ. 19987). No optical afterglow consistent with the XRT position (Evans et al., GCN Circ. 19991) is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 82 232 147 >20.8 u_FC 294 544 246 >19.6 white 82 1886 431 >21.2 v 624 1937 156 >19.5 b 550 1862 136 >19.6 u 294 1836 363 >19.6 w1 674 1812 136 >18.9 m2 5622 5747 123 >18.8 w2 600 1736 136 >18.7 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.54 in the direction of the burst (Schlegel et al. 1998).
GCN 19998 table
GRB_name GRB161004B
GCN_number 19998
Detection_method Fermi GBM Det
t_trigger 23:07:54.790 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 19998 SUBJECT: GRB 161004B: Fermi GBM detection DATE: 16/10/05 16:51:33 GMT FROM: Rachel Hamburg at UAH R. Hamburg (UAH) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 23:07:54.79 UT on 04 October 2016, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 161004B (trigger 497315278 / 161004964) which was also detected by the Swift BAT (D'Ai et al. 2016, GCN 19987) The GBM on-ground location is consistent with the Swift position. The trigger resulted in an Autonomous Repoint Request (ARR) by the GBM Flight Software owing to the high peak flux of the GRB. This ARR was accepted and the spacecraft slewed to the GBM in-flight location. The initial angle from the Fermi LAT boresight to the Swift location is 69 degrees. The GBM light curve consists of a single peak with a duration (T90) of about 14 s (50-300 keV). The time-averaged spectrum from T0-0.0 s to T0+18.4 s is best fit by a Band function with Epeak = 132 +/- 6 keV, alpha = -0.75 +/- 0.04, and beta = -2.4 +/- 0.1. The event fluence (10-1000 keV) in this time interval is (1.877 +/- 0.039)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+4.7 s in the 10-1000 keV band is 15.4 +/- 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 20003 table
GRB_name GRB161004B
GCN_number 20003
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 20003 SUBJECT: GRB 161004B: CALET Gamma-Ray Burst Monitor detection DATE: 16/10/06 13:51:35 GMT FROM: Takanori Sakamoto at AGU Y. Yamada, A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama (AGU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA), I. Takahashi (IPMU), Y. Asaoka, S. Ozawa, S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR), M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena) and the CALET collaboration: The long-duration GRB 161004B (D'Ai et al., GCN Circ. 19987; Kumar et al., GCN Circ. 19996; Hamburg et al., GCN Circ. 19998; INTEGRAL-SPI/ACS trigger #7590) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 23:07:52.64 on 4 October 2016. The burst signal was seen by the SGM instrument. The light curve of the SGM shows a single peak starting at T0, peaking at T+7 sec and ending at T+15 sec. The T90 duration measured by the SGM data is 11.1 +- 0.9 sec (40-450 keV). The light curve is available at http://cgbm.calet.jp/cgbm_trigger/flight/1159657616/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at the Waseda University.
GCN 20005 table
GRB_name GRB161004B
GCN_number 20005
Detection_method Konus-Wind Det
t_trigger 23:07:54.317 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 20005 SUBJECT: Konus-Wind observation of GRB 161004B DATE: 16/10/06 16:02:46 GMT FROM: Anastasia Tsvetkova at Ioffe Institute A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks, P. Oleynik, M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB 161004B (Swift-BAT trigger #715246: D'Ai et al., GCN 19987; Sakamoto et al., GCN 19995; Fermi GBM detection: Hamburg & Meegan, GCN 19998; CALET Gamma-Ray Burst Monitor detection: Yamada et al., GCN 20003) triggered Konus-Wind at T0=83274.317 s UT (23:07:54.317). The burst light curve shows a single pulse with a total duration of ~18 s. The emission is seen up to ~2 MeV. As observed by Konus-Wind, the burst had a fluence of 1.71(-0.07,+0.08)x10^-5 erg/cm2, and a 64-ms peak energy flux, measured from T0+4.144 s, of 3.43(-0.80,+0.80)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum of the burst (measured from T0 to T0+15.616 s) is best fit in the 20 keV - 2 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -1.05(-0.09,+0.09), and Ep = 175(-12,+14) keV (chi2 = 56/58 dof). Fitting by the GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -3.14 (chi2 = 56/57 dof). The spectrum near the peak count rate (measured from T0 to T0+7.424 s) is best fit in the 20 keV - 2 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -0.71(-0.10,+0.11), and Ep = 210(-13,+15) keV (chi2 = 67/58 dof). Fitting by the GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -3.12 (chi2 = 67/57 dof). The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB161004_T83274/ All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.