GRB191031D

This page lists all entries on GRB191031D in GRBweb

Summary IPN Swift GCN 26112 GCN 26114 GCN 26117 GCN 26118 GCN 26120 GCN 26121 GCN 26122 GCN 26123 GCN 26124 GCN 26125 GCN 26126 GCN 26128 GCN 26129 GCN 26133 GCN 26134 GCN 26147 GCN 26149 GCN 26150 GCN 26175 GCN 26240 GCN 26841

Summary table
Variable Value Source
T0 21:23:31 UTC GCN_circulars,Swift Det
ra 283.2895° Swift
decl 47.6441° Swift
pos_error 2.46e-04° Swift
T90 0.29 s Swift
T90_start 21:23:31 UTC Swift
fluence 4.10e-07 erg/cm² Swift
T100 0.29 s
GBM_located False
mjd 58787.891331018516 GCN_circulars,Swift Det
IPN table
GRB_name GRB191031D
ra 283.2750°
decl 47.6333°
pos_error 5.00e-02°
Swift table
GRB_name GRB191031D
t_trigger 21:23:31 UTC
ra 283.2895°
decl 47.6441°
pos_error 2.46e-04°
T90 0.29 s
fluence 4.10e-07 erg/cm²
GCN 26112 table
GRB_name GRB191031D
GCN_number 26112
Detection_method Swift Det
t_trigger 21:23:31 UTC
ra 283.2750°
decl 47.6390°
Circular_text TITLE: GCN CIRCULAR NUMBER: 26112 SUBJECT: GRB 191031D: Swift detection of a short hard burst DATE: 19/10/31 21:53:41 GMT FROM: Hans Krimm at NSF/NASA-GSFC V. D'Elia (SSDC), E. Ambrosi (INAF-IASFPA), A. D'Ai (INAF-IASFPA), J.D. Gropp (PSU), J. A. Kennea (PSU), N. J. Klingler (PSU), H. A. Krimm (NSF), D. M. Palmer (LANL) and A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift Observatory Team: At 21:23:31 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 191031D (trigger=932608). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 283.275, +47.639 which is RA(J2000) = 18h 53m 06s Dec(J2000) = +47d 38' 19" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single peak structure with a duration of about 0.4 sec. The peak count rate was ~18000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 21:24:59.8 UT, 88.8 seconds after the BAT trigger. Using promptly downlinked data we find a fading, uncatalogued X-ray source with an enhanced position: RA, Dec 283.2890, 47.6438 which is equivalent to: RA(J2000) = 18h 53m 09.37s Dec(J2000) = +47d 38' 37.7" with an uncertainty of 2.3 arcseconds (radius, 90% containment). This location is 38 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. UVOT took a finding chart exposure of 150 seconds with the White filter starting 92 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 0.08. This GRB was also detected by Fermi/GBM (trignum=191031891, GCN 26111), and the INTEGRAL/SPIACS event (trignum=8402). We note that the Fermi automated circular has misnamed this event GRB 191031C. Burst Advocate for this burst is V. D'Elia (delia AT ssdc.asi.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/)
GCN 26114 table
GRB_name GRB191031D
GCN_number 26114
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 26114 SUBJECT: Correction in name: GRB 191031D (not GRB 191031C) DATE: 19/10/31 22:21:14 GMT FROM: Bagrat Mailyan at UAH B. Mailyan (UAH) reports on behalf of the Fermi GBM Team: "The Fermi Gamma-ray Burst Monitor (GBM) trigger 594249816/191031891 at 21:23:31 UT on 31 Oct 2019, of GRB 191031C (GCN Circ. #26111) should be GRB 191031D. We apologize for any confusion caused.”
GCN 26117 table
GRB_name GRB191031D
GCN_number 26117
Detection_method Swift-XRT Det
ra 283.2895°
decl 47.6441°
Circular_text TITLE: GCN CIRCULAR NUMBER: 26117 SUBJECT: GRB 191031D: Enhanced Swift-XRT position DATE: 19/11/01 00:27:16 GMT FROM: Phil Evans at U of Leicester J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team. Using 722 s of XRT Photon Counting mode data and 1 UVOT images for GRB 191031D, 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 = 283.28951, +47.64407 which is equivalent to: RA (J2000): 18h 53m 9.48s Dec (J2000): +47d 38' 38.6" with an uncertainty of 1.9 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 26118 table
GRB_name GRB191031D
GCN_number 26118
Detection_method Fermi GBM Det
t_trigger 21:23:31.130 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 26118 SUBJECT: GRB 191031D: Fermi GBM detection DATE: 19/11/01 03:22:35 GMT FROM: Bagrat Mailyan at UAH B. Mailyan (UAH) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 21:23:31.13 UT on 31 October 2019, the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB 191031D (trigger 594249816/191031891) which was also detected by the Swift BAT and XRT (D'Elia et al. 2019, GCN 26112) The Fermi GBM Final Real-time Localization (GCN 26111) is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 64 degrees. The GBM light curve shows a short spike with a duration (T90) of about 0.256 s (50-300 keV). The time-averaged spectrum from T0-0.064 s to T0+0.32 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.42 +/- 0.04 and the cutoff energy, parameterized as Epeak, is 856 +/- 53 keV The event fluence (10-1000 keV) in this time interval is (4.36 +/- 0.09)E-06 erg/cm^2. The 64 ms peak photon flux measured starting from T0+0.128 s in the 10-1000 keV band is 48.7 +/- 1.59 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog: https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html For Fermi GBM data and info, please visit the official Fermi GBM Support Page: https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"
GCN 26120 table
GRB_name GRB191031D
GCN_number 26120
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 26120 SUBJECT: GRB 191031D: VLA 9.8 GHz upper limit DATE: 19/11/01 04:14:06 GMT FROM: Wen-fai Fong at Northwestern U T. Laskar (Bath), W. Fong, K. D. Alexander, G. Schroeder, K. Paterson (Northwestern) and E. Berger (Harvard) report: "We observed the position of the short-duration GRB 191031D (Fermi-GBM et al., GCN 26111; D'Elia et al., GCN 26112; Mailyan et al., GCN 26118) with the Karl G. Jansky Very Large Array (VLA) under Program 19B-217 (PI: Fong) beginning on 2019 Oct 31.992 UT (2.4 hr post-burst) at a mean frequency of 9.8 GHz. Based on preliminary analysis, in 1 hour of observations we do not detect any radio emission at or near the position of the XRT afterglow (Osborne et al., GCN 26117) to a 3-sigma limit of 15 microJy. Additional, detailed analysis is ongoing. We thank Amy Mioduszewski and the rest of the VLA staff for their assistance with rapidly approving and executing these observations. Further observations are planned."
GCN 26121 table
GRB_name GRB191031D
GCN_number 26121
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 26121 SUBJECT: GRB 191031D: RATIR Optical and NIR Observations DATE: 19/11/01 04:40:51 GMT FROM: Alan M Watson at UNAM 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), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), Jesús González (UNAM), Carlos Román-Zúñiga (UNAM), Harvey Moseley (GSFC), John Capone (UMD), V. Zach Golkhou (U. Wash.), and Vicki Toy (UMD) report: We observed the field of GRB 191031D (Fermi GBM Team, GCN Circ. 26111; D'Elia et al., GCN Circ. 26112) 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 2019/11 1.09 to 2019/11 1.12 UTC (4.65 to 5.49 hours after the BAT trigger), obtaining a total of 0.56 hours exposure in the r and i bands, 0.23 hours exposure in the Z and Y bands, and 0.06 hours exposures in the J and H bands. For a source within the Swift-XRT error circle, in comparison with the USNO-B1 and 2MASS catalogs, we obtain the following upper limits (3-sigma): r > 22.94 i > 23.17 Z > 21.50 Y > 21.40 J > 19.44 H > 19.33 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 26122 table
GRB_name GRB191031D
GCN_number 26122
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 26122 SUBJECT: GRB 191031D: COATLI Optical Observations DATE: 19/11/01 05:13:02 GMT FROM: Alan M Watson at UNAM Alan M. Watson (UNAM), Nat Butler (ASU), Rosa L. Becerra (UNAM), Diego González (UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Margarita Pereyra (UNAM), and Eleonora Troja (GSFC) report: We observed the field of GRB 191031A (D'Ai et al., GCN Circ. 26101; Fermi GBM Team, GCN Circ. 26102) with the COATLI 50-cm telescope and interim imager at the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir (http://coatli.astroscu.unam.mx) from 2019-11-01 02:47 UTC to 04:49 UTC (5.4 to 7.4 hours after the trigger), obtaining a total of 4530 seconds of exposure in the w filter. We do not detetect any uncataloged sources in the enhanced XRT error region (Osborne et al., GCN Circ. 26117) to a 3-sigma limit of w = 23.2. Our w magnitudes are calibrated against the Pan-STARRS1 catalog, are on an approximate AB system (Becerra et al., 2019, ApJ, 872, 118), and are not corrected for Galactic extinction in the direction of the GRB. We thank the COATLI technical team and the staff of the Observatorio Astronómico Nacional.
GCN 26123 table
GRB_name GRB191031D
GCN_number 26123
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 26123 SUBJECT: GRB 191031D: AGILE/MCAL observations DATE: 19/11/01 09:11:45 GMT FROM: Alessandro Ursi at INAF/IAPS A. Ursi (INAF/IAPS), F. Verrecchia (SSDC, and INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, C. Casentini, G. Piano (INAF/IAPS), F. Lucarelli, C. Pittori (SSDC, and INAF/OAR), A. Bulgarelli, V. Fioretti, N. Parmiggiani (INAF/OAS-Bologna), M. Pilia, A. Trois (INAF/OA-Cagliari), I. Donnarumma (ASI), F. Longo (Univ. Trieste and INFN Trieste), report on behalf of the AGILE Team: The AGILE Mini-CALorimeter (MCAL) detected the short GRB 191031D at T0 = 2019-10-31 21:23:28.17 +/- 0.01 s (UTC), already detected by Fermi/GBM (GCN #26111), Swift (D'Elia et al., 2019; GCN #26112), and INTEGRAL/SPIACS (trignum=8402). The event lasted about 0.2 s and released a total number of ~430 counts in the detector (in the 0.4-100 MeV energy range), above an average background rate of 544 counts / s. The light curve shows a single peak episode and can be found at http://www.agilescienceapp.it/notices/GRB_064997_499641808.174626.png. The AGILE-MCAL detector is a CsI detector with a 4 pi FoV, sensitive in the energy range 0.4-100 MeV. Additional analysis of AGILE data is in progress.
GCN 26124 table
GRB_name GRB191031D
GCN_number 26124
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 26124 SUBJECT: GRB 191031D: Swift-XRT refined Analysis DATE: 19/11/01 09:29:57 GMT FROM: Phil Evans at U of Leicester B. Sbarufatti (PSU), D.N. Burrows (PSU), J. D. Gropp (PSU), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester), M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) , M. Capalbi (INAF-IASFPA) and V. D'Elia report on behalf of the Swift-XRT team: We have analysed 6.2 ks of XRT data for GRB 191031D (D'Elia et al. GCN Circ. 26112), from 101 s to 17.5 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Osborne et al. (GCN Circ. 26117). The light curve can be modelled with a power-law decay with a decay index of alpha=2.04 (+0.22, -0.21). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.90 (+0.26, -0.16). The best-fitting absorption column is consistent with the Galactic value of 6.6 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.3 x 10^-11 (3.8 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 6.6 (+/-2.1) x 10^20 cm^-2 Galactic foreground: 6.6 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 1.90 (+0.26, -0.16) If the light curve continues to decay with a power-law decay index of 2.04, the count rate at T+24 hours will be 1.9 x 10^-6 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.2 x 10^-17 (7.1 x 10^-17) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00932608. This circular is an official product of the Swift-XRT team.
GCN 26125 table
GRB_name GRB191031D
GCN_number 26125
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 26125 SUBJECT: GRB 191031D: MITSuME Akeno optical upper limits DATE: 19/11/01 10:51:07 GMT FROM: Ogawa Futa at Tokyo Institute of Technology F. Ogawa, R. Adachi, K. L. Murata, M. Oeda, K.Shiraishi, K. Iida, M. Niwano, R. Hosokawa, S. Toma, Y. Yatsu, and N. Kawai (TokyoTech) report on behalf of the MITSuME collaboration: We searched for the optical counterpart of GRB 191031D (The Fermi GBM team, GCN Circular #26111, V. D'Elia et al., GCN Circular #26112, Bagrat Mailyan, #26114) 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 19/11/01 08:18:36 UT. We did not find any new point sources within the XRT circle (J.P. Osborne et al., GCN Circular #26117) in all three bands. We obtained the following 5-sigma limits for the magnitudes. T0+[hour] MID-UT T-EXP[sec] 5-sigma limits ------------------------------------------------------------------------------------------------ ~11.5 09:12:34 1680 g'>18.3, Rc>18.2, Ic>17.3 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used UCAC4 catalog for flux calibration. The magnitudes are expressed in the AB system.
GCN 26126 table
GRB_name GRB191031D
GCN_number 26126
Detection_method Konus-Wind Det
t_trigger 21:23:31.324 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 26126 SUBJECT: Konus-Wind observation of GRB 191031D DATE: 19/11/01 11:56:53 GMT FROM: Dmitry Frederiks at Ioffe Institute D. Frederiks, S. Golenetskii, R. Aptekar, A. Lysenko, A. Ridnaia, D. Svinkin, A. Tsvetkova, M. Ulanov, and T. Cline on behalf of the Konus-Wind team, report: The short-duration GRB 191031D (Swift detection: D'Elia et al., GCN Circ. 26112; Fermi GBM detection: Mailyan & Meegan, GCN Circ. 26118; AGILE/MCAL observations: Ursi et al., GCN Circ. 26123) triggered Konus-Wind at T0=77011.324 s UT (21:23:31.324). The burst light curve shows a mult-peaked pulse which started at ~T0-0.064 s and had a total duration of ~0.35 s. The emission is seen up to ~5 MeV. As observed by Konus-Wind, the burst had a fluence of 2.72(-0.27, +0.31)x10^-6 erg/cm2, and a 16-ms peak flux, measured from T0-0.016 s, of 1.95(-0.32,+0.38)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 = -0.27(-0.17,+0.20) and Ep = 370(-46,+58) keV (chi2 = 35/39 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.6 (chi2 =35/38 dof). The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB191031_T77011/ All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 26128 table
GRB_name GRB191031D
GCN_number 26128
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 26128 SUBJECT: GRB 191031D: Swift/UVOT Upper Limits DATE: 19/11/01 17:00:34 GMT FROM: Sam LaPorte at PSU GRB 191031D: Swift/UVOT Upper Limits J. D. Gropp (PSU) and V. D'Elia (SSDC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 191031D 93 s after the BAT trigger (D'Elia et al., GCN Circ. 26112). No optical afterglow consistent with the XRT position (Osborne et al. GCN Circ. 26117) 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 93 242 147 >20.8 u_FC 306 555 246 >20.2 white 93 6694 575 >21.1 v 636 5863 294 >19.9 b 561 6683 471 >20.4 u 306 6477 697 >20.3 w1 686 6273 452 >19.8 m2 661 6067 294 >19.6 w2 612 5658 294 >19.9 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.08 in the direction of the burst (Schlegel et al. 1998).
GCN 26129 table
GRB_name GRB191031D
GCN_number 26129
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 26129 SUBJECT: GRB 191031D: AstroSat CZTI detection DATE: 19/11/01 18:46:38 GMT FROM: Ramkrishna Gaikwad at IUCAA/AstroSat R. Gaikwad, S. Gupta, 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 GRB 191031D, which was also detected by Fermi GBM Real-time Localization (GCN #26111), Swift (D'Elia et al., GCN #26112), Swift-XRT (Osborne et al., GCN #26117), Fermi GBM (Mailyan et al., GCN #26118), VLA (Laskar T. et al., GCN #26120), RATIR (Butler N. et al., GCN #26121), COATLI (Watson A. M. et al., GCN #26122), AGILE/MCAL (Ursi A. et al., GCN #26123), MITSuME Akeno (Ogawa F. et al., GCN #26125) and Konus-Wind (Frederiks D. et al., GCN #26126). The source was clearly detected in the 40-200 keV energy range. The light curve showed single pulse of emission peaking at 2019-10-31 21:23:31.0 UT. The measured peak count rate associated with the burst is 628 cts/s above the background in the combined data of four quadrants, with a total of 393 cts. The local mean background count rate was 556 cts/s. Using cumulative rates, we measure a T90 of 0.35 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 26133 table
GRB_name GRB191031D
GCN_number 26133
Detection_method Swift-BAT Det
ra 283.2690°
decl 47.6450°
Circular_text TITLE: GCN CIRCULAR NUMBER: 26133 SUBJECT: GRB 191031D: Swift-BAT refined analysis DATE: 19/11/01 19:07:47 GMT FROM: Hans Krimm at NSF/NASA-GSFC T. Sakamoto (AGU), S. D. Barthelmy (GSFC), V. D'Elia (SSDC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), J. P. Norris (BSU), D. M. Palmer (LANL), M. Stamatikos (OSU), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-61 to T+242 sec from the recent telemetry downlink, we report further analysis of BAT GRB 191031D (trigger #932608) (D'Elia, et al., GCN Circ. 26112). The BAT ground-calculated position is RA, Dec = 283.269, 47.645 deg which is RA(J2000) = 18h 53m 04.5s Dec(J2000) = +47d 38' 40.9" with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment). The partial coding was 37%. The mask-weighted light curve shows a multi-peak structure from T-0.05 sec to T+0.3 sec with a harder first pulse and softer second pulse. There is no sign of extended emission. T90 (15-350 keV) is 0.29 +- 0.05 sec (estimated error including systematics). The time-averaged spectrum from T-0.03 to T+0.31 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 0.80 +- 0.15. The fluence in the 15-150 keV band is 4.1 +- 0.4 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T-0.36 sec in the 15-150 keV band is 4.3 +- 0.4 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The duration and hardness of GRB 191031D place it squarely within the distribution of short, hard bursts detected by BAT. Using the 4-ms binned light curve, the spectral lag of the burst is 0.2 ms +- 2 ms for the 50-100 keV to 15-25 keV bands, and 0.4 ms +- 3 ms for the 100-350 keV to 25-50 keV bands. These values are consistent with a short GRB. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/932608/BA/
GCN 26134 table
GRB_name GRB191031D
GCN_number 26134
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 26134 SUBJECT: GRB 191031D: MMT Binospec Optical Upper Limit DATE: 19/11/01 20:39:58 GMT FROM: Kerry Paterson at Northwestern K. Paterson, W. Fong, K. D. Alexander, G. Schroeder, A. Rouco Escorial (Northwestern) report: “We observed the field of the short-duration GRB 191031D (Fermi-GBM et al., GCN 26111; D'Elia et al., GCN 26112; Mailyan et al., GCN 26118) with Binospec mounted on the 6.5-m MMT on Mount Hopkins, Arizona, starting on 2019 November 1 at 01:44:13 UT, 4.31 hours after the burst. We obtained 15x120-sec of observations in the r-band in 1.05” seeing and clear conditions. We do not detect any optical source in or around the enhanced XRT position (Osborne et al. GCN 26117). We obtain a 3-sigma upper limit of r > 23.5 AB mag on the afterglow or any coincident host galaxy, not corrected for Galactic extinction. Photometry is calibrated to the USNO-B1.0 catalog. This limit is consistent with, and slightly deeper than the limit found by Butler et al. (GCN 26121). We note that the closest, clearly-extended source is 5.48 arcsec to the southwest. Further observations are planned. We thank the MMT staff, and in particular observer Michael Calkins, for their assistance with these observations.”
GCN 26147 table
GRB_name GRB191031D
GCN_number 26147
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 26147 SUBJECT: GRB 191031D: Gemini optical upper limit DATE: 19/11/02 19:25:43 GMT FROM: Eleonora Troja at NASA/GSFC/UMD S.Dichiara (UMD, NASA-GSFC) and E. Troja (UMD, NASA-GSFC) report on behalf of a larger collaboration: We observed the field of the short duration GRB 191031D (Fermi GBM Team, GCN Circ. 26111; D'Elia et al., GCN Circ. 26112) with the Gemini North 8-meter telescope located on Mauna Kea, beginning on 2019-11-02 04:43:08 UT, approximately 1.3 d post-burst. We obtained a series of 6x120s r-band images using the Gemini Multi-Object Spectrograph (GMOS). No credible counterpart is detected within the enhanced X-ray position (Osborne el al., GCN 26117) down to r > 25 AB mag, not corrected for Galactic extinction. We thank S. Stewart and the Gemini North staff for executing these observations.
GCN 26149 table
GRB_name GRB191031D
GCN_number 26149
Detection_method correction
Circular_text TITLE: GCN CIRCULAR NUMBER: 26149 SUBJECT: Konus-Wind observation of GRB 191031D: correction to GCN 26126 DATE: 19/11/03 11:15:05 GMT FROM: Dmitry Frederiks at Ioffe Institute D. Frederiks, on behalf of the Konus-Wind team: Reported in Frederiks et al. 2019 (GCN Circ. 26126), the KW spectral parameters and fluxes of short/hard GRB 191031D are incorrect due to wrong instrument calibrations used. The correct values are given below. As observed by Konus-Wind, the burst had a fluence of 5.72(-0.63,+0.69)x10^-6 erg/cm2, and a 16-ms peak flux, measured from T0-0.016 s, of 4.12(-0.72,+0.80)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 = -0.12(-0.18,+0.20) and Ep = 735(-92,+112) keV (chi2 = 32/39 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.9 (chi2 =32/38 dof). I apologize for possible inconvenience this may have caused.
GCN 26150 table
GRB_name GRB191031D
GCN_number 26150
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 26150 SUBJECT: GRB 191031D: Zwicky Transient Facility Follow-Up of a Swift Short GRB (Trigger 594249816/191031891) DATE: 19/11/03 19:13:26 GMT FROM: Tomas Ahumada at U. of Maryland Tomás Ahumada (UMD), Shreya Anand (Caltech), Michael W. Coughlin (Caltech), S. Bradley Cenko (NASA GSFC), Eric C. Bellm (UW), Leo P. Singer (NASA GSFC), Mansi M. Kasliwal (Caltech) on behalf of the ZTF and GROWTH collaborations We observed the localization region of the short GRB 191031D (trigger 594249816/191031891) detected by the Swift XRT, BAT and the Gamma-Ray Burst Monitor (GBM) on the Fermi satellite with the Palomar 48 inch telescope equipped with the 47 square degree Zwicky Transient Facility (ZTF) camera. These observations are part of the ZTF public survey and serendipitously covered the GRB localization. We obtained a series of g-band images beginning at 02:48:56.6 UT on 2019 Nov 01 (5.4 hours after the burst trigger time). This corresponds to ~68% of the probability enclosed in the GBM localization region and the totality of the Swift region. The images were processed through the ZTF reduction and image subtraction pipelines at IPAC to search for potential counterparts. No high-significance transients were identified by our pipeline in the area observed. The median 5 sigma upper limit for an isolated point source in our images was g > 20.8 mag for these observations. ZTF is a project led by PI S. R. Kulkarni at Caltech (see ATEL #11266 ), and includes IPAC; WIS, Israel; OKC, Sweden; JSI/UMd, USA; UW, USA; DESY, Germany; NRC, Taiwan; UW Milwaukee, USA and LANL USA. ZTF acknowledges the generous support of the NSF under AST MSIP Grant No 1440341. Alert distribution service provided by DIRAC@UW. Alert filtering is being undertaken by the GROWTH marshal system, supported by NSF PIRE grant 1545949.
GCN 26175 table
GRB_name GRB191031D
GCN_number 26175
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 26175 SUBJECT: GRB 191031D: Chandra upper limit DATE: 19/11/05 14:50:39 GMT FROM: Wen-fai Fong at Northwestern U A. Rouco Escorial, W. Fong, (Northwestern), E. Berger (Harvard), and R. Margutti (Northwestern) report: "We initiated observations of the location of the short-duration GRB191031D (Fermi-GBM et al., GCN 26111; D'Elia et al., GCN 26112; Mailyan et al., GCN 26118) with the Chandra X-ray Observatory on 2019 Nov 3.694 UT (mid-time of 16:39:42 UT), 2.8 days post-burst under Program 20500021 (ObsID 21302; PI: Berger). The effective exposure time is 19.8 ksec. We do not detect an X-ray source within the enhanced XRT position (Osborne et al., GCN 26117), and calculate a 3-sigma limit of <4.5e-4 cps in the 0.5-10 keV energy range using the method described by Gehrels (1986). Applying the best-fit XRT spectral parameters, we calculate an unabsorbed flux limit of <6.0e-15 erg/s/cm^2 in the 0.3-10 keV energy range. Relative to the XRT light curve starting from t~900 sec post-burst, this constrains the late-time X-ray power-law decline to be alpha<-0.75 (where F~t^alpha). We thank the Chandra staff for the rapid scheduling and execution of these observations."
GCN 26240 table
GRB_name GRB191031D
GCN_number 26240
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 26240 SUBJECT: GRB 191031D: CALET Gamma-Ray Burst Monitor detection DATE: 19/11/13 03:39:09 GMT FROM: Valentin Pal'shin at AGU Y. Shimizu (Kanagawa U), A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU), Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), Y. Asaoka, S. Torii (Waseda U), T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC), M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena), and the CALET collaboration: The short bright GRB 191031D (Swift detection: Ambrosi et al., GCN Circ. 26112, Sakamoto et al., GCN Circ. 26133; Fermi GBM detection: Mailyan and Meegan, GCN Circ. 26118; AGILE/MCAL observations: Ursi et al., GCN Circ. 26123; Konus-Wind observation: Frederiks et al., GCN Circ. 26126, 26149; AstroSat CZTI detection: Gaikwad et al., GCN Circ. 26129; https://gcn.gsfc.nasa.gov/other/191031D.gcn3) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 21:23:31.261 UTC on 31 October 2019. The burst signal was seen by all CGBM detectors. No real-time CGBM GCN notice was distributed about this trigger because the real-time communication from the ISS was off (loss of signal). The burst light curve shows a multi-peak structure which starts at T-0.168 sec, peaks at 0.008 sec and ends at T+0.192 sec. The T90 and T50 durations measured by the SGM data are 0.240 +- 0.079 sec and 0.104 +- 0.008 sec (40-1000 keV), respectively. The ground processed light curve is available at http://cgbm.calet.jp/cgbm_trigger/ground/1256592147/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at the Waseda University.
GCN 26841 table
GRB_name GRB191031D
GCN_number 26841
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 26841 SUBJECT: GRB 191031D: XMM-Newton upper limit DATE: 20/01/21 16:38:21 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo, S. Campana, M. G. Bernardini (INAF-OAB), M. Branchesi (GSSI), E. Chassande-Mottin (APC, CNRS/IN2P3), S. Covino (INAF-OAB), V. D'Elia (ASI-SSDC), G. Ghirlanda, G. Ghisellini, A. Melandri, L. Nava, O. S. Salafia (INAF-OAB), R. Salvaterra (INAF-IASFMi), G. Tagliaferri (INAF-OAB), S. D. Vergani (GEPI/Obs. Paris) report: XMM-Newton started observing the field of the short GRB 191031D (Fermi-GBM et al., GCN Circ. 26111; D'Elia et al., GCN Circ. 26112; Mailyan et al., GCN Circ. 26118; Ursi et al., GCN Circ. 26123; Frederiks et al., GCN Circ. 26126; Gaikwad et al., GCN Circ. 26129; Frederiks et al., GCN Circ. 26149; Shimizu et al., GCN Circular. 26240) on 14 November 2019 at 09:58:00 UT, ~ 13.5 d after the burst. The last ~18 ks of the observation were affected by an enhanced background and were filtered out. The resulting EPIC/pn exposure time is 27.2 ks. No X-ray source is detected within the enhanced XRT position (Osborne et al., GCN Circ. 26117) down to a 3sigma limit of ~ 1.6e-3 cts/s in the 0.3-10 keV energy range. Assuming the spectral parameters derived by Swift/XRT, the above value translates into an unabsorbed flux limit of ~ 4.8e-15 erg/cm^2/s in the 0.3-10 keV energy range. We acknowledge the XMM-Newton staff for their support in scheduling and executing these observations.