GRB161202A

This page lists all entries on GRB161202A in GRBweb

Summary IPN Swift Fermi LAT GCN 20227 GCN 20228 GCN 20229 GCN 20230 GCN 20231 GCN 20232 GCN 20233 GCN 20234 GCN 20235 GCN 20238 GCN 20318

Summary table
Variable Value Source
GRB_name_Fermi GRB161202970
T0 23:11:48.822 UTC GCN_circulars,Konus-Wind Det
ra 356.9027° Swift
decl 19.6465° Swift
pos_error 1.81e-04° Swift
fluence 8.60e-06 erg/cm² Swift
GBM_located False
mjd 57724.966537291664 GCN_circulars,Konus-Wind Det
IPN table
GRB_name GRB161202A
ra 356.8958°
decl 19.6333°
pos_error 5.00e-02°
Swift table
GRB_name GRB161202A
t_trigger 23:12:52 UTC
ra 356.9027°
decl 19.6465°
pos_error 1.81e-04°
fluence 8.60e-06 erg/cm²
Fermi LAT table
GRB_name_Fermi GRB161202970
GRB_name GRB161202A
MET 502413395.0
datum 2016-12-02
t_trigger 23:16:31 UTC
ra 356.9027°
decl 19.6465°
pos_error 4.40e-04°
GCN 20227 table
GRB_name GRB161202A
GCN_number 20227
Detection_method Swift Det
t_trigger 23:12:52 UTC
ra 356.8950°
decl 19.6400°
Circular_text TITLE: GCN CIRCULAR NUMBER: 20227 SUBJECT: GRB 161202A: Swift detection of a burst DATE: 16/12/02 23:29:05 GMT FROM: Scott Barthelmy at NASA/GSFC B. Sbarufatti (INAF-OAB/PSU), S. D. Barthelmy (GSFC), D. N. Burrows (PSU), S. B. Cenko (GSFC), J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC), C. Gronwall (PSU), N. P. M. Kuin (UCL-MSSL), F. E. Marshall (NASA/GSFC) and M. H. Siegel (PSU) report on behalf of the Swift Team: At 23:12:52 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 161202A (trigger=725036). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 356.895, +19.640, which is RA(J2000) = 23h 47m 35s Dec(J2000) = +19d 38' 23" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows many peaks with a total duration of about 70 sec. The peak count rate was ~10,000 counts/sec (15-350 keV), at ~7 sec after the trigger. The XRT began observing the field at 23:14:06.7 UT, 74.1 seconds after the BAT trigger. Using promptly downlinked data we find a bright, fading, uncatalogued X-ray source with an enhanced position: RA, Dec 356.9031, 19.6477 which is equivalent to: RA(J2000) = 23h 47m 36.74s Dec(J2000) = +19d 38' 51.7" with an uncertainty of 2.4 arcseconds (radius, 90% containment). This location is 39 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. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density in excess of the Galactic value (6.00 x 10^20 cm^-2, Willingale et al. 2013), with an excess column of 9.9 (+6.04/-4.79) x 10^21 cm^-2 (90% confidence). The initial flux in the 2.5 s image was 2.18e-09 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 0.09. Burst Advocate for this burst is B. Sbarufatti (boris.sbarufatti AT brera.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 20228 table
GRB_name GRB161202A
GCN_number 20228
Detection_method Swift-XRT Det
ra 356.9027°
decl 19.6465°
Circular_text TITLE: GCN CIRCULAR NUMBER: 20228 SUBJECT: GRB 161202A: Enhanced Swift-XRT position DATE: 16/12/03 06:58:32 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 4140 s of XRT Photon Counting mode data and 6 UVOT images for GRB 161202A, 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 = 356.90269, +19.64648 which is equivalent to: RA (J2000): 23h 47m 36.65s Dec (J2000): +19d 38' 47.3" with an uncertainty of 1.6 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 20229 table
GRB_name GRB161202A
GCN_number 20229
Detection_method Fermi LAT Det
t_trigger 23:12:52.700 UTC
ra 356.9500°
decl 19.4900°
Circular_text TITLE: GCN CIRCULAR NUMBER: 20229 SUBJECT: GRB 161202A: Fermi-LAT detection DATE: 16/12/03 09:38:30 GMT FROM: Giacomo Vianello at SLAC G.Vianello (Stanford), F.Longo (University and INFN, Trieste) report on behalf of the Fermi-LAT team: On December, 02, 2016 Fermi-LAT detected high-energy emission from GRB 161202A, which was also detected by Swift (GCN 20227). The best LAT on-ground location is found to be RA, Dec = 356.95, 19.49 (J2000) with an error radius of 0.13 deg (90 % containment, statistical error only), which is fully compatible with the enhanced Swift/XRT position reported in GCN 20228. This was outside the field of view of the LAT at the time of the trigger t0 = 23:12:52.7. The location of the GRB was observed however between t0 + 1680 s and t0 + 3500 s. During this time interval, the data from the Fermi-LAT show a significant increase in the event rate correlated with the trigger with high significance. 5 photons were detected above 100 MeV. The highest-energy photon is a 4 GeV event which is observed 2000 seconds after the GBM trigger. The Fermi-LAT point of contact for this burst is Giacomo Vianello (giacomov@stanford.edu). 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 20230 table
GRB_name GRB161202A
GCN_number 20230
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 20230 SUBJECT: GRB 161202A: MITSuME Okayama upper limits DATE: 16/12/03 16:14:06 GMT FROM: Daisuke Kuroda at OAO/NAOJ D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ), S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto) and N. Kawai(Tokyo Tech) report on behalf of MITSuME and OISTER collaboration: We observed the field of GRB 161202A (Sbarufatti et al., GCNC 20227) with the optical three color (g', Rc and Ic) CCD camera attached to the MITSuME 50cm telescope of Okayama Astrophysical Observatory. The observation started on 2016-12-03 09:13:55 UT (~10.0 h after the burst). We did not find any new point source within the enhanced XRT circle (Evans et al., GCNC 20228) in all the three bands. Three sigma upper limits of the OT are listed below. We used SDSS-DR8 catalog for flux calibration. #T0+[day] MID-UT T-EXP[sec] g' Rc Ic ----------------------------------------------------- 0.53482 12:03:00 11580.0 >20.6 >20.2 >19.8 ----------------------------------------------------- T0+ : Elapsed time after the burst [day] T-EXP: Total Exposure time [sec]
GCN 20231 table
GRB_name GRB161202A
GCN_number 20231
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 20231 SUBJECT: GRB 161202A: Swift-XRT refined Analysis DATE: 16/12/03 16:46:45 GMT FROM: Phil Evans at U of Leicester D.N. Burrows (PSU), T.G.R. Roegiers (PSU), S.L. Gibson (U. Leicester), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA) and B. Sbarufatti report on behalf of the Swift-XRT team: We have analysed 8.5 ks of XRT data for GRB 161202A (Sbarufatti et al. GCN Circ. 20227), from 66 s to 52.1 ks after the BAT trigger. The data comprise 160 s in Windowed Timing (WT) mode (the first 5 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. 20228). The light curve can be modelled with a series of power-law decays. The initial decay index is alpha=2.53 (+0.41, -0.24). At T+217 s the decay flattens to an alpha of 0.83 (+/-0.09) before breaking again at T+8090 s to a final decay with index alpha=1.44 (+0.35, -0.14). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.79 (+0.18, -0.17). The best-fitting absorption column is 9.4 (+1.9, -1.7) x 10^21 cm^-2, in excess of the Galactic value of 6.0 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 2.79 (+0.24, -0.23) and a best-fitting absorption column of 1.39 (+0.22, -0.20) x 10^22 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.7 x 10^-11 (1.7 x 10^-10) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.39 (+0.22, -0.20) x 10^22 cm^-2 Galactic foreground: 6.0 x 10^20 cm^-2 Excess significance: 11.1 sigma Photon index: 2.79 (+0.24, -0.23) 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 7.4 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.7 x 10^-13 (1.3 x 10^-12) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00725036. This circular is an official product of the Swift-XRT team.
GCN 20232 table
GRB_name GRB161202A
GCN_number 20232
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 20232 SUBJECT: GRB 161202A: Swift/UVOT Upper Limits DATE: 16/12/03 19:45:55 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel (PSU) and B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 161202A 83 s after the BAT trigger (Sbarufatti et al., GCN Circ. 20227). No optical afterglow consistent with the XRT position (Evans et al. GCN Circ. 20228) 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 83 232 147 >21.2 white 83 4066 344 >21.5 v 4277 4477 197 >19.4 b 3661 11907 862 >20.8 u 295 10303 1027 >20.5 w1 4688 6144 217 >19.6 w2 4071 4271 197 >19.6 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.09 in the direction of the burst (Schlegel et al. 1998).
GCN 20233 table
GRB_name GRB161202A
GCN_number 20233
Detection_method Swift-BAT Det
ra 356.9040°
decl 19.6520°
Circular_text TITLE: GCN CIRCULAR NUMBER: 20233 SUBJECT: GRB 161202A: Swift-BAT refined analysis DATE: 16/12/04 02:10:37 GMT FROM: Amy Lien at GSFC J. R. Cummings (CPI), S. D. Barthelmy (GSFC), N. Gehrels (GSFC), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), B. Sbarufatti (INAF-OAB/PSU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-240 to T+962 sec from the recent telemetry downlink, we report further analysis of BAT GRB 161202A (trigger #725036) (Sbarufatti, et al., GCN Circ. 20227). The BAT ground-calculated position is RA, Dec = 356.904, 19.652 deg which is RA(J2000) = 23h 47m 36.9s Dec(J2000) = +19d 39' 06.3" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 86%. The first peaks of the burst occurred before it came into the BAT field of view at ~T-67 s. The mask-weighted light curve shows more than ten pulses that last till ~T+80 s. The time-averaged spectrum from T-63.41 to T+65.79 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.55 +- 0.05. The fluence in the 15-150 keV band is 8.6 +- 0.3 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+2.11 sec in the 15-150 keV band is 5.9 +- 0.3 ph/cm2/sec. 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/725036/BA/
GCN 20234 table
GRB_name GRB161202A
GCN_number 20234
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 20234 SUBJECT: GRB 161202A: RATIR Optical and NIR Observations DATE: 16/12/04 17:03:08 GMT FROM: Eleonora Troja at GSFC Eleonora Troja (GSFC), Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (STScI), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UVI), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), José A. de Diego (UNAM), Leonid Georgiev (UNAM), Jesús González (UNAM), Carlos Román-Zúñiga (UNAM), Neil Gehrels (GSFC), Harvey Moseley (GSFC), John Capone (UMD), V. Zach Golkhou (ASU), and Vicki Toy (UMD) report: We observed the field of GRB 161202A (Sbarufatti, et al., GCN 20227; Vianello & Longo, GCN 20229) with the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio Astronómico Nacional on Sierra San Pedro Mártir from 2016/12 4.08 to 2016/12 4.31 UTC (26.70 to 32.11 hours after the BAT trigger), obtaining a total of 3.34 hours exposure in the r and i bands and 1.45 hours exposure in the Z, Y, J, and H bands. For a source within the Swift-XRT error circle (Burrows, et al., GCN 20231) in comparison with the SDSS DR9 and 2MASS catalogs, we obtain the following upper limits (3-sigma): r > 24.0 i > 23.9 Z > 23.1 Y > 22.8 J > 22.4 H > 22.0 These magnitudes are in the AB system and are not corrected for Galactic extinction in the direction of the GRB. We thank the staff of the Observatorio Astronómico Nacional in San Pedro Mártir.
GCN 20235 table
GRB_name GRB161202A
GCN_number 20235
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 20235 SUBJECT: GRB 161202A: Astrosat CZTI detection DATE: 16/12/05 07:58:12 GMT FROM: Vidushi Sharma at IUCAA V. Sharma, V. Bhalerao and D. Bhattacharya (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 a long duration GRB161202A (Swift detection: B. Sbarufatti et al., GCN Circ. 20227) in the 40-200 keV energy range. The light curve shows a multiple peak structure with main peak at 23:11:50 UT, 62 secs before the Swift BAT trigger(consistent with GCN 20233). The measured peak count rate is 230.75 counts/sec above the background in combined data of four quadrants, with a total of 1432.98 counts. The local mean background count rate was 345.25 counts/sec. Using cumulative rates, we measure a T90 of 75.25 sec. 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 20238 table
GRB_name GRB161202A
GCN_number 20238
Detection_method Konus-Wind Det
t_trigger 23:11:48.822 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 20238 SUBJECT: Konus-Wind observation of GRB 161202A DATE: 16/12/06 16:44:29 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 long-duration GRB 161202A (Swift-BAT detection and observation: Sbarufatti et al., GCN Circ. 20227, Cummings et al., GCN Circ. 20233; Fermi-LAT detection: Vianello & Longo, GCN Circ. 20229) triggered Konus-Wind at T0=83508.822 s UT (23:11:48.822). The burst light curve shows a multipeaked structure started at ~T0-57.1 s with a total duration of ~181.0 s. The emission is seen up to ~2 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB161202_T83508/ As observed by Konus-Wind, the burst had a fluence of 2.90(-0.40,+0.73)x10^-5 erg/cm2, and a 64-ms peak flux, measured from T0+3.920 s, of 3.03(-0.80,+0.80)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum of the burst (measured from T0 to T0+139.520 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 = -1.43(-0.25,+0.30) and Ep = 222(-63,+201) keV (chi2 = 65/62 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high-energy photon index: beta < -1.9 (chi2 = 65/61 dof) The spectrum near the maximum count rate (measured from T0+0.256 to T0+8.448 s) is best fit in the 20 keV - 2 MeV range by the power law with exponential cutoff model: with alpha = -0.67(-0.21,+0.24) and Ep = 203(-20,+26) keV (chi2 = 76/62 dof). Fitting by the GRB (Band) model yields the same alpha and Ep, and an upper limit on the high-energy photon index: beta < -2.5 (chi2 = 76/61 dof) All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 20318 table
GRB_name GRB161202A
GCN_number 20318
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 20318 SUBJECT: GRB 161202A: 15 GHz upper limits from AMI DATE: 16/12/21 09:35:10 GMT FROM: Kunal Mooley at Oxford U K. P. Mooley (Hintze Fellow, Oxford), T. D. Staley, R. P. Fender (Oxford), G. E. Anderson (Curtin), T. Cantwell (Manchester), D. Titterington, S. H. Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), K. Grainge, A. Scaife (Manchester) The AMI Large Array robotically triggered on the Swift alert for GRB 161202A (Sbarufatti et al., GCN 20227) as part of the 4pisky program, and subsequent follow up observations were obtained up to 10 days post-burst. Although the data from the first epoch were lost due to technical problems, our observations at 15 GHz on 2016 Dec 03.93 and Dec 05.77 (UT) do not reveal any radio source at the XRT location (Evans et al., GCN 20228), with 3sigma upper limits of 200 uJy and 121 uJy respectively. We thank the AMI staff for scheduling these observations. The AMI-GRB database is a log of all GRB follow up observations with the AMI, and is available at http://4pisky.org/ami-grb/.