GRB171120A

This page lists all entries on GRB171120A in GRBweb

Summary Fermi GBM IPN Swift Fermi LAT GCN 22133 GCN 22135 GCN 22136 GCN 22137 GCN 22138 GCN 22139 GCN 22140 GCN 22141 GCN 22142 GCN 22143 GCN 22144 GCN 22145 GCN 22149 GCN 22209

Summary table
Variable Value Source
GRB_name_Fermi GRB171120556
T0 13:20:00.683 UTC GCN_circulars,Konus-Wind Det
ra 163.7905° Swift
decl 22.4587° Swift
pos_error 2.07e-04° Swift
T90 44.062 s Fermi_GBM
T90_error 0.383 s Fermi_GBM
T90_start 13:20:02.375 UTC Fermi_GBM
fluence 1.61e-05 erg/cm² Fermi_GBM
fluence_error 3.30e-08 erg/cm² Fermi_GBM
T100 65.317 s
GBM_located False
mjd 58077.55556346065 GCN_circulars,Konus-Wind Det
Fermi GBM table
GRB_name_Fermi GRB171120556
trigger_name bn171120556
ra 163.7908°
decl 22.4583°
pos_error 2.55e+00°
datum 2017-11-20
t_trigger 13:20:02.372 UTC
T90 44.062 s
T90_error 0.383 s
T90_start 13:20:02.375 UTC
fluence 1.61e-05 erg/cm²
fluence_error 3.30e-08 erg/cm²
flux_1024 3.57e+01 erg/cm²/s
flux_1024_error 5.06e-01 erg/cm²/s
flux_1024_time 9.60e-02 erg/cm²/s
flux_64 5.78e+01 erg/cm²/s
flux_64_error 2.37e+00 erg/cm²/s
IPN table
GRB_name GRB171120A
ra 163.7875°
decl 22.4500°
pos_error 5.00e-02°
Swift table
GRB_name GRB171120A
t_trigger 13:20:02 UTC
ra 163.7905°
decl 22.4587°
pos_error 2.07e-04°
T90 64.0 s
fluence 8.60e-06 erg/cm²
Fermi LAT table
GRB_name_Fermi GRB171120556
GRB_name GRB171120A
MET 532876807.0
datum 2017-11-20
t_trigger 13:20:02 UTC
ra 163.8400°
decl 22.4000°
pos_error 1.70e-01°
GCN 22133 table
GRB_name GRB171120A
GCN_number 22133
Detection_method Swift Det
t_trigger 13:20:02 UTC
ra 163.7870°
decl 22.4500°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22133 SUBJECT: GRB 171120A: Swift detection of a burst DATE: 17/11/20 13:34:57 GMT FROM: Kim Page at U.of Leicester A. Tohuvavohu (PSU), A. D'Ai (INAF-IASFPA), A. Deich (PSU), P. A. Evans (U Leicester), J.D. Gropp (PSU), A. Y. Lien (GSFC/UMBC) and K. L. Page (U Leicester) report on behalf of the Swift Team: At 13:20:02 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 171120A (trigger=791201). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 163.787, +22.450 which is RA(J2000) = 10h 55m 09s Dec(J2000) = +22d 26' 58" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a multi-peaked structure with a duration of about 60 sec. The peak count rate was ~17000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 13:21:31.0 UT, 88.5 seconds after the BAT trigger. Using promptly downlinked data we find a bright, uncatalogued X-ray source with an enhanced position: RA, Dec 163.7911, 22.4584 which is equivalent to: RA(J2000) = 10h 55m 09.87s Dec(J2000) = +22d 27' 30.3" with an uncertainty of 2.5 arcseconds (radius, 90% containment). This location is 33 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. A power-law fit to a spectrum formed from promptly downlinked event data does not constrain the column density. The initial flux in the 2.5 s image was 2.00e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 98 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 0.02. Burst Advocate for this burst is A. Tohuvavohu (aaronb AT swift.psu.edu). 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 22135 table
GRB_name GRB171120A
GCN_number 22135
Detection_method Swift-XRT Det
ra 163.7904°
decl 22.4587°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22135 SUBJECT: GRB 171120A: Enhanced Swift-XRT position DATE: 17/11/20 19:15:06 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 2976 s of XRT Photon Counting mode data and 7 UVOT images for GRB 171120A, 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 = 163.79042, +22.45869 which is equivalent to: RA (J2000): 10h 55m 9.70s Dec (J2000): +22d 27' 31.3" 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 22136 table
GRB_name GRB171120A
GCN_number 22136
Detection_method Fermi LAT Det
t_trigger 13:20:02 UTC
ra 163.8400°
decl 22.4000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22136 SUBJECT: GRB 171120A: Fermi-LAT detection DATE: 17/11/20 20:39:29 GMT FROM: Giacomo Vianello at SLAC F. Longo (University and INFN, Trieste), G. Vianello (Stanford), D. Kocevski (NASA/GSFC) and M.Arimoto (Waseda University) report on behalf of the Fermi-LAT collaboration: At 13:20:02 on November 20, 2017, Fermi-LAT detected high-energy emission from GRB 171120A,which was also detected by Swift-BAT (Tohuvavohu et al., GCN 22133) and by Fermi-GBM (trigger 532876807/171120556). The best LAT on-ground location is found to be RA, Dec = 163.84, 22.40 deg (J2000) with an error radius of 0.17 deg (90% containment, statistical error only). This was 24 deg from the LAT boresight at the time of the trigger. The LAT on-ground position is consistent with the Swift-XRT localization (Evans et al., GCN 22135). More than 30 photons above 100 MeV are observed within ~ 6.5 ks seconds of the trigger. The highest-energy photon is a 3.4 GeV event which is observed ~4.8 ks seconds after the GBM trigger. The Fermi-LAT point of contact for this burst is: Francesco Longo (francesco.longo@ts.infn.it). 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 22137 table
GRB_name GRB171120A
GCN_number 22137
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 22137 SUBJECT: GRB 171120A: Swift-XRT refined Analysis DATE: 17/11/20 21:49:56 GMT FROM: Phil Evans at U of Leicester K.L. Page (U. Leicester), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), A. Tohuvavohu (PSU), S. J. LaPorte (PSU), J.A. Kennea (PSU), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester) and report on behalf of the Swift-XRT team: report on behalf of the Swift-XRT team: We have analysed 8.2 ks of XRT data for GRB 171120A, from 78 s to 22.5 ks after the BAT trigger. The data comprise 337 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 late-time light curve (from T0+3.9 ks) can be modelled with a power-law decay with a decay index of alpha=0.41 (+/-0.09). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.78 (+0.15, -0.14). The best-fitting absorption column is 2.34 (+0.28, -0.26) x 10^22 cm^-2, in excess of the Galactic value of 1.2 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.92 (+/-0.18) and a best-fitting absorption column of 2.4 (+/-0.3) x 10^22 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 6.6 x 10^-11 (1.4 x 10^-10) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 2.4 (+/-0.3) x 10^22 cm^-2 Galactic foreground: 1.2 x 10^20 cm^-2 Excess significance: 12.8 sigma Photon index: 1.92 (+/-0.18) If the light curve continues to decay with a power-law decay index of 0.41, the count rate at T+24 hours will be 0.059 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.9 x 10^-12 (8.3 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/00791201. This circular is an official product of the Swift-XRT team.
GCN 22138 table
GRB_name GRB171120A
GCN_number 22138
Detection_method Fermi GBM Det
t_trigger 13:20:02.370 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 22138 SUBJECT: GRB 171120A: Fermi GBM Detection DATE: 17/11/21 00:44:27 GMT FROM: Matthew Stanbro at UAH/Fermi M. Stanbro, C. Meegan, (UAH) and A von Kienlin (MPE) report on behalf of the Fermi GBM Team: "At 13:20:02.37 UT on 20 November 2017, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 171120A (trigger 532876807 / 171120556) which was also detected by the Swift/BAT (A. Tohuvavohu et al. 2017, GCN 22133) and Fermi LAT (F. Longo et al. 2017, GCN 22136). 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 GBM light curve consists of 2 pulses with a duration (T90) of about 44 s (50-300 keV). The time-averaged spectrum from T0+0.002 s to T0+44.897 s is best fit by a Band function with Epeak = 141 +/- 12 keV, alpha = -0.91 +/- 0.06, and beta = -2.16 +/- 0.09. The event fluence (10-1000 keV) in this time interval is (1.80 +/- 0.05)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+0.10 s in the 10-1000 keV band is 35.69 +/- 0.51 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 22139 table
GRB_name GRB171120A
GCN_number 22139
Detection_method Swift-BAT Det
ra 163.7740°
decl 22.4610°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22139 SUBJECT: GRB 171120A: Swift-BAT refined analysis DATE: 17/11/21 04:19:31 GMT FROM: Amy Lien at GSFC M. Stamatikos (OSU), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), A. Tohuvavohu (PSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-240 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 171120A (trigger #791201) (Tohuvavohu et al., GCN Circ. 22133). The BAT ground-calculated position is RA, Dec = 163.774, 22.461 deg which is RA(J2000) = 10h 55m 05.8s Dec(J2000) = +22d 27' 38.2" with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment). The partial coding was 14%. The mask-weighted light curve shows a multi-peaked structure that starts at ~T-15 s and ends at ~T+65 s. The two main peaks occur at ~T0 and ~T+40 s, respectively. T90 (15-350 keV) is 64 +- 16 sec (estimated error including systematics). The time-averaged spectrum from T-15.53 to T+64.47 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 1.06 +- 0.28, and Epeak of 86.0 +- 19.0 keV (chi squared 55.57 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 8.6 +- 0.3 x 10^-6 erg/cm2 and the 1-sec peak flux measured from T+39.97 sec in the 15-150 keV band is 11.4 +- 0.5 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.67 +- 0.06 (chi squared 70.86 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/791201/BA/
GCN 22140 table
GRB_name GRB171120A
GCN_number 22140
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 22140 SUBJECT: GRB 171120A: MITSuME Akeno optical upper limits DATE: 17/11/21 10:18:12 GMT FROM: Katsuhiro L. Murata at Nagoya U H. Mamiya, R. Itoh, K. L. Murata, T. Yoshii, Y. Tachibana, S. Harita, K. Morita, T. Ozawa, K. Shiraishi, Y. Yatsu, and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration: We searched for the optical counterpart of GRB 171120A (A. Tohuvavohu et al., GCN Circular #22133) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation started on 2017-11-20 15:38:32.17 UT. We did not find any new point source within enhanced XRT circle (P.A. Evans al., GCN Circular #22135) in all three bands. We obtained following limits for the magnitudes. T0+[hour] MID-UT T-EXP[sec] g' Rc Ic ------------------------------------------------------------------------------------------------------ ~3.26 18:40:07.63 9960 >21.5 >20.7 >19.8 ------------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used GSC2.3 catalog for flux calibration.
GCN 22141 table
GRB_name GRB171120A
GCN_number 22141
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22141 SUBJECT: GRB171120A: GWAC-F60A upper limit DATE: 17/11/21 11:39:32 GMT FROM: L.P. Xin at NAOC L. P. Xin, W. L. Dong, P. P. Zhang, X. H. Han, J. Y. Wei, E. W. Liang, X. G. Wang, Y. J. Xiao, Y. G. Yang, X. M. Lu, L. Huang, H. B. Cai, X. M. Meng, Y. L. Qiu, Y. Xu, Y. J. Xiao, Y. T. Zheng, R. S. Zhang, J. Wang, C. Wu, J. S. Deng, D. W. Xu, T. Damien and H. L. Li report: We observed GRB 171120A (Tohuvavohu et al., GCN 22133) with GWAC-F60A 60cm optical telescope at 19:06:58 UT, Nov. 20th 2017, about 5.75 hours after the burst. No any new source was not detected in the XRT error circle (Evens et al., GCN 22135) in our 15*300 sec stacked R-band image down to the 3 sigma limit of about 19.5 mag at the mid time of 6.25 hours after the burst. The brightness was calibrated by USNO B1.0 R2 catalogues. GWAC-F60A is operated by Guangxi university and NAOC, CAS, at Xinglong observatory, China. The message may be cited.
GCN 22142 table
GRB_name GRB171120A
GCN_number 22142
Detection_method Konus-Wind Det
t_trigger 13:20:00.683 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 22142 SUBJECT: Konus-Wind observation of GRB 171120A DATE: 17/11/21 12:48:30 GMT FROM: Dmitry Frederiks at Ioffe Institute D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline, on behalf of the Konus-Wind team, report: The long GRB 171120A (Swift/BAT detection: Tohuvavohu et al., GCN 22133; Stamatikos et al., GCN 22139; Fermi-LAT detection: Longo et al., GCN 22136; Fermi-GBM detection: Stanbro et al., GCN 22138) triggered Konus-Wind at T0=48000.683 s UT (13:20:00.683). The KW light curve shows two separate emission episodes. A total duration of the burst is ~44 s. The emission is seen up to ~10 MeV. As observed by Konus-Wind, the burst had a fluence of 1.7(-0.3,+0.5)x10^-5 erg/cm2 and a 64-ms peak energy flux, measured from T0+1.644, of (1.29 ± 0.13)x10^-5 erg/cm2 (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum (measured from T0 to T0+49.408 s) is best fit in the 20 keV - 15 MeV range by a cutoff power-law (CPL) function with the following model parameters: the photon index alpha = -1.59(-0.19,+0.23), and the peak energy Ep = 200(-56,+183) keV, chi2 = 84/98 dof. Fitting this spectrum with the GRB (Band) function yields the same alpha and Ep, and an upper limit on beta of -2.0. The spectrum near the peak count rate (measured from T0+0.128 to T0+0.256 s) is best fit in the 20 keV - 15 MeV range by the CPL function with the following model parameters: the photon index alpha = -0.33(-0.30,+0.35), and the peak energy Ep = 305(-41,+53) keV, chi2 = 39/36 dof. Fitting this spectrum with the GRB (Band) function yields similar alpha and Ep, and an upper limit on beta of -2.7. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB171120_T48000/ All the quoted errors are estimated at the 90% confidence level. All the presented results are preliminary.
GCN 22143 table
GRB_name GRB171120A
GCN_number 22143
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 22143 SUBJECT: GRB 171120A: AstroSat CZTI detection DATE: 17/11/21 21:06:13 GMT FROM: Vidushi Sharma at IUCAA V. Sharma and D. Bhattacharya (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the Astrosat CZTI collaboration: Analysis of Astrosat CZTI data showed the detection of GRB 171120A, which was also detected by Swift-BAT (Tohuvavohu et al., GCN 22133), Fermi-GBM (trigger 532876807/171120556) and Fermi-LAT (Longo F. et al., GCN 22136). The source was clearly detected in the 40-200 keV energy range. The light curve of the CZT detector shows a single peak of emission at 13:20:02 UT. The measured peak count rate is 367.4 cts/s above the background in combined data of four quadrants, with a total of 634 cts. The local mean background count rate was 307.6 cts/s. Using cumulative rates, we measure a T90 of 6.8 s. It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The Veto light curve shows a strong peak coincident with the peak in the CZT detector and a weaker second peak ~39 s later. 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 22144 table
GRB_name GRB171120A
GCN_number 22144
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 22144 SUBJECT: GRB 171120A: Swift/UVOT Upper Limits DATE: 17/11/21 21:21:20 GMT FROM: Jeffrey Gropp at PSU J. D. Gropp (PSU) and A. Tohuvavohu (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 171120A 99 s after the BAT trigger (Tohuvavohu et al., GCN Circ. 22133). No optical afterglow consistent with the refined XRT position (Evans et al. GCN Circ. 22135) 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 99 249 147 >19.9 u_FC 311 561 246 >19.7 white 99 5989 560 >21.1 v 640 6399 413 >19.1 b 566 5784 413 >20.9 u 311 11713 811 >20.7 w1 5174 11532 1082 >21.0 m2 9724 10624 886 >21.0 w2 4559 6194 393 >21.0 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.02 in the direction of the burst (Schlegel et al. 1998).
GCN 22145 table
GRB_name GRB171120A
GCN_number 22145
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 22145 SUBJECT: GRB 171120A: Xinglong-2.16m optical upper limit DATE: 17/11/22 04:24:59 GMT FROM: Dong Xu at NAOC/CAS Z.P. Zhu, H.X. Feng, D. Xu (NAOC), Y. Zhao, F. Xiao (NAOC), S.B. Qian (YNAO), Y.D. Hu (IAA-CSIC) report We observed the field of GRB 171120A (Tohuvavohu et al., GCN 22133) using the 2.16-m telescope located at Xinglong, Hebei, China, equipped with BFOSC. We obtained 1x600s and 2x900s R-band frames, starting at 18:54:02 UT on 2017-11-20, i.e., 5.57 hr after the BAT trigger. No optical source was detected in the stacked image at the XRT position (Evens et al., GCN 22135), down to the limiting magnitude of R~21.5 mag at the median time of 5.95 hr post-burst, calibrated with the SDSS field.
GCN 22149 table
GRB_name GRB171120A
GCN_number 22149
Detection_method Insight-HXMT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 22149 SUBJECT: GRB 171120A: Insight-HXMT detection DATE: 17/11/23 15:03:23 GMT FROM: Zhengwei Li at IHEP Z. W. Li, J. Y. Liao, C. K. Li, X. B. Li, S. L. Xiong, C. Z. Liu, X. F. Li, Z. Chang, X. F. Lu, J. L. Zhao, A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin, Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song, H. Y. Wang, M. Wu, Y. P. Xu, S. N. Zhang (IHEP), report on behalf of the Insight-HXMT team: During the commissioning phase, at 2017-11-20T13:20:02.00 (T0), Insight-HXMT detected GRB 171120A (trigger ID: HEB171120555) in a routine search of the data, which was also observed by Swift/BAT (A. Tohuvavohu et al, GCN Circ.22133), Swift/XRT(P.A. Evans et al, GCN Circ.22135),Fermi/GBM(M.Stanbro et al, GCN Circ.22138), Fermi/LAT(F. Longo et al, GCN Circ.22136), Konus-Windan(D.Frederiks et al, GCN Circ.22142) and AstroSat/CZTI (V.Sharma et al, GCN Circ.22143). The Insight-HXMT light curve consists of two pulses with a duration (T90) of 39.9s measured from T0+0.5s. The 200-ms peak rate, measured from T0+0.6s, is 6895.7 cnts/sec. The total counts from this burst is 5746.9 counts. URL_LC: http://www.hxmt.org/images/GRB/HEB171120555_lc.jpg All measurements above are made with the CsI detectors operating in the regular mode with the energy range of about 80-800 keV (record energy). Only gamma-rays with energy greater than about 200 keV can penetrate the spacecraft and leave signals in the CsI detectors installed inside of the telescope. The time-averaged spectrum from T0-0.2 to T0+1.0 s is adequately fit by a Power Law model with spectral index = -1.96 +/- 0.07 . The energy fluence is (6.20 +/- 0.33) E-06 erg/cm^2 in 200 - 5000 keV in this time interval. The analysis results presented above are preliminary; final results will be published elsewhere. Insight-HXMT is the first Chinese space X-ray telescope, which was funded jointly by the China National Space Administration (CNSA) and the Chinese Academy of Sciences (CAS). More information about it could be found at: http://www.hxmt.org/index.php/enhome .
GCN 22209 table
GRB_name GRB171120A
GCN_number 22209
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 22209 SUBJECT: GRB 171120A CALET Gamma-Ray Burst Monitor detection DATE: 17/12/08 00:27:12 GMT FROM: Takanori Sakamoto at AGU Y. Yamada, A. Yoshida, T. Sakamoto, Y. Kawakubo, M. Moriyama, A. Tezuka, S. Matsukawa (AGU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), 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), A. V. Penacchioni, P. S. Marrocchesi (U of Siena) and the CALET collaboration: The long-duration GRB 171120A (Tohuvavohu et al., GCN circ. 22133; Longo et al., GCN circ. 22136; Frederiks et al., GCN circ. 22142; Sharma et al., GCN circ. 22143; Li et al., GCN circ. 22149) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 13:20:02 on 20 November 2017. The burst signal was seen by the all CGBM instruments. The light curve of the SGM shows two largely separated episodes. The first episode starts at T0, peaks at T+1 sec and ends at T+4 sec. The second episode starts T+38 sec, peaks at T+40 sec and ends at T+46 sec. The T90 duration measured by the SGM data is 44.4 +- 0.9 sec (40-1000 keV). The light curve is available at http://cgbm.calet.jp/cgbm_trigger/flight/1195219087/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at the Waseda University.