GRB171103A

This page lists all entries on GRB171103A in GRBweb

Summary IPN Swift GCN 22095 GCN 22099 GCN 22100 GCN 22101 GCN 22103 GCN 22116

Summary table
Variable Value Source
T0 23:10:29.176 UTC GCN_circulars,Konus-Wind Det
ra 249.5100° Swift
decl -10.2060° Swift
pos_error 1.16e-02° Swift
T90 3.9 s Swift
T90_start 23:10:32 UTC Swift
fluence 3.80e-07 erg/cm² Swift
T100 6.724 s
GBM_located False
mjd 58060.96561546296 GCN_circulars,Konus-Wind Det
IPN table
GRB_name GRB171103A
ra 249.5375°
decl -10.2167°
pos_error 5.00e-02°
Swift table
GRB_name GRB171103A
t_trigger 23:10:32 UTC
ra 249.5100°
decl -10.2060°
pos_error 1.16e-02°
T90 3.9 s
fluence 3.80e-07 erg/cm²
GCN 22095 table
GRB_name GRB171103A
GCN_number 22095
Detection_method Swift Det
t_trigger 23:10:32 UTC
ra 249.5360°
decl -10.2150°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22095 SUBJECT: GRB 171103A: Swift detection of a short hard burst DATE: 17/11/03 23:23:43 GMT FROM: David Palmer at LANL T. N. Ukwatta (LANL), A. D'Ai (INAF-IASFPA), V. D'Elia (ASDC), Alex Deich (PSU), H. A. Krimm (NSF/USRA), N. P. M. Kuin (UCL-MSSL), D. M. Palmer (LANL), M. H. Siegel (PSU) and A. Tohuvavohu (PSU) report on behalf of the Swift Team: At 23:10:32 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 171103A (trigger=785850). Swift did not slew due to an observing constraint. The BAT on-board calculated location is RA, Dec 249.536, -10.215 which is RA(J2000) = 16h 38m 09s Dec(J2000) = -10d 12' 53" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single-peaked structure with a duration of less than 1 sec. The peak count rate was ~20000 counts/sec (15-350 keV), at ~0 sec after the trigger. Due to a Sun observing constraint, Swift cannot slew to the BAT position until 11:32 UT on 2018 January 15. There will thus be no XRT or UVOT data for this trigger before this time. Burst Advocate for this burst is T. N. Ukwatta (tilan.ukwatta AT gmail.com). 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 22099 table
GRB_name GRB171103A
GCN_number 22099
Detection_method Swift-BAT Det
ra 249.5100°
decl -10.2060°
Circular_text TITLE: GCN CIRCULAR NUMBER: 22099 SUBJECT: GRB 171103A: Swift-BAT refined analysis of a short GRB DATE: 17/11/04 21:58:58 GMT FROM: Amy Lien at GSFC D. M. Palmer (LANL), S. D. Barthelmy (GSFC), J. R. Cummings (CPI), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), J. P. Norris (BSU), T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 171103A (trigger #785850) (Ukwatta et al., GCN Circ. 22095). The BAT ground-calculated position is RA, Dec = 249.510, -10.206 deg which is RA(J2000) = 16h 38m 02.4s Dec(J2000) = -10d 12' 22.9" with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment). The partial coding was 65%. The mask-weighted light curve shows a complex multi-peak structure. It begins with three peaks from -0.8 sec to +0.3 sec. This is followed by low-level, slowly decaying emission out to ~T+20 sec and then a weaker peak at ~T+60 sec. The spacecraft slewed away from the burst location at ~T+600 sec due to a pre-planned slew. T90 (15-350 keV) is 3.90 +- 1.11 sec (estimated error including systematics). The time-averaged spectrum from T-0.37 to T+4.67 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.31 +- 0.18. The fluence in the 15-150 keV band is 3.8 +- 0.4 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T-0.37 sec in the 15-150 keV band is 3.6 +- 0.3 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The duration and hardness of this burst show it to be intermediate between the short and long burst populations. Using a 8-ms binned light curve, the lag analysis finds a lag of -0.5 +/- 4 ms for the 100-350 keV to 25-50 keV band, and -0.7 +/- 5 ms for the 50-100 keV to 15-25 keV band. These values are consistent with those of a short GRB. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/785850/BA/
GCN 22100 table
GRB_name GRB171103A
GCN_number 22100
Detection_method Fermi GBM Det
t_trigger 23:10:31.951 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 22100 SUBJECT: GRB 171103A: Fermi GBM observation DATE: 17/11/05 16:12:21 GMT FROM: Peter Veres at UAH P Veres (UAH) reports on behalf of the Fermi GBM Team: " GRB 171103A, detected by Swift (Ukwatta et al, GCN #22095) is clearly visible in the GBM data. It was not possible for GBM to trigger at this time because GBM was still in trigger mode for a transient that occurred 190 s earlier (171103963 / 531443246). The angle from the Fermi LAT boresight at the Swift trigger time is 102 degrees. The GBM light curve shows a single pulse with a duration (T90) of about 1.1 s (50-300 keV). The time-averaged spectrum for a 0.4 s interval starting from 23:10:31.951 UT is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.74 +/- 0.05 and the cutoff energy, parameterized as Epeak, is 2.1 +/- 0.2 MeV. The event fluence (10-1000 keV) in this time interval is (2.7 +/- 0.1)E-6 erg/cm^2. The 64-ms peak photon flux measured starting from 23:10:32.082 in the 10-1000 keV band is 30.3 +/- 2.0 ph/s/cm^2. "
GCN 22101 table
GRB_name GRB171103A
GCN_number 22101
Detection_method Konus-Wind Det
t_trigger 23:10:29.176 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 22101 SUBJECT: Konus-Wind observation of GRB 171103A (short/hard) DATE: 17/11/05 20:11:39 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 short-duration, hard-spectrum, intense GRB 171103A (Swift detection of a short hard burst: Ukwatta et al., GCN 22095; Palmer et al., GCN 22099; Fermi GBM observation: Veres, GCN 22100) triggered Konus-Wind at T0=83429.176 s UT (23:10:29.176). The burst light curve shows a single pulse with a total duration of ~0.3 s. The emission is seen up to ~15 MeV. As observed by Konus-Wind, the burst had a fluence of 8.50(-1.47,+1.57)x10^-6 erg/cm2, and a 16-ms peak energy flux, measured from T0-0.030 s, of 7.12(-2.18,+2.26)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum of the burst (measured from T0 to T0+0.256 s) is best fit in the 20 keV - 15 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -0.76(-0.17,+0.20), and Ep = 2463(-690,+1054) keV (chi2 = 31/28 dof). Fitting by the GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -1.98 (chi2 = 31/27 dof). The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB171103_T83429/ All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 22103 table
GRB_name GRB171103A
GCN_number 22103
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 22103 SUBJECT: GRB 171103A: AstroSat CZTI detection DATE: 17/11/06 12:52:32 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 a short bright GRB 171103A, which was also detected by Swift-BAT (Ukwatta T. N. et al, GCN # 22095), Fermi-GBM (Veres P., GCN # 22100) and Konus-Wind (Tsvetkova A. et al, GCN # 22101). The source was clearly detected in the 40-200 keV energy range. The light curve shows single peak of emission with peak at 23:10:32.100 UT. The measured peak count rate is 1420.9 cts/s above the background in combined data of four quadrants, with a total of 2964 cts. The local mean background count rate was 349.1 cts/s. Using cumulative rates, we measure a T90 of 0.46 s. It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. 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 22116 table
GRB_name GRB171103A
GCN_number 22116
Detection_method Insight-HXMT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 22116 SUBJECT: GRB 171103A: Insight-HXMT observation DATE: 17/11/10 07:57:17 GMT FROM: Shaolin Xiong at IHEP G. Li, J. Y. Liao, S. L. Xiong, C. K. Li, X. B. Li, C. Z. Liu, X. F. Li, Z. W. Li, X. F. Lu, Z. Chang, J. L. Zhao, A. M. 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 2017-11-03T23:10:32.04 (T0), Insight-HXMT/HE detected GRB 171103A (trigger ID: HEB171103965) in a routine search of the data,which is also detected by Swift/BAT (Ukwatta et al.,GCN 22095), Fermi/GBM (Veres et al., GCN 22100), Konus-Wind (Tsvetkova et al.,GCN 22101) and AstroSat/CZTI (Sharma et al., GCN 22103). The Insight-HXMT light curve mainly consists of multi-pulses with a duration (T90) of 0.21 s measured from T0+0.033 s. The 10-ms peak rate, measured from T0+0.096 s, is 19946.0 cnts/sec. The total counts from this burst is 2915.7 counts. URL_LC: http://www.hxmt.org/images/GRB/HEB171103965_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+0.05 s to T0+0.30 s is adequately fit by a Power Law model with spectral index = -0.97 ± 0.07. The energy fluence is (4.1 ± 0.3)e-6 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 could be found at: http://www.hxmt.org/index.php/enhome .