GRB231106A

This page lists all entries on GRB231106A in GRBweb

Summary Fermi GBM IPN GCN 34956 GCN 34959 GCN 34965 GCN 34966 GCN 35013 GCN 35047

Summary table
Variable Value Source
GRB_name_Fermi GRB231106759
T0 18:13:23 UTC GCN_circulars,Fermi GBM final loc
ra 113.4500° IPN
decl 29.2167° IPN
pos_error 1.67e-03° IPN
T90 23.552 s Fermi_GBM
T90_error 1.049 s Fermi_GBM
T90_start 18:13:23.170 UTC Fermi_GBM
fluence 7.62e-06 erg/cm² Fermi_GBM
fluence_error 5.11e-08 erg/cm² Fermi_GBM
T100 23.722 s
GBM_located False
mjd 60254.75929398148 GCN_circulars,Fermi GBM final loc
Fermi GBM table
GRB_name_Fermi GRB231106759
trigger_name bn231106759
ra 113.8100°
decl 25.5700°
pos_error 2.65e+00°
datum 2023-11-06
t_trigger 18:13:23.394 UTC
T90 23.552 s
T90_error 1.049 s
T90_start 18:13:23.170 UTC
fluence 7.62e-06 erg/cm²
fluence_error 5.11e-08 erg/cm²
flux_1024 5.41e+00 erg/cm²/s
flux_1024_error 3.61e-01 erg/cm²/s
flux_1024_time 4.77e+00 erg/cm²/s
flux_64 7.54e+00 erg/cm²/s
flux_64_error 1.52e+00 erg/cm²/s
IPN table
GRB_name GRB231106A
ra 113.4500°
decl 29.2167°
pos_error 1.67e-03°
GCN 34956 table
GRB_name GRB231106A
GCN_number 34956
Detection_method Fermi GBM final loc
t_trigger 18:13:23 UTC
ra 113.8000°
decl 25.6000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 34956 SUBJECT: GRB 231106A: Fermi GBM Final Real-time Localization DATE: 23/11/06 18:24:51 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 18:13:23 UT on 6 Nov 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 231106A (trigger 720987208.394416 / 231106759). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 113.8, Dec = 25.6 (J2000 degrees, equivalent to J2000 07h 35m, 25d 36'), with a statistical uncertainty of 3.4 degrees. The angle from the Fermi LAT boresight is 120.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231106759/quicklook/glg_skymap_all_bn231106759.png The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231106759/quicklook/glg_healpix_all_bn231106759.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231106759/quicklook/glg_lc_medres34_bn231106759.gif
GCN 34959 table
GRB_name GRB231106A
GCN_number 34959
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 34959 SUBJECT: Fermi GRB 231106A: Global MASTER-Net observations report DATE: 23/11/06 22:01:20 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko, G.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij (Lomonosov Moscow State University, SAI, Physics Department), R. Podesta, C.Lopez, F. Podesta, C.Francile (Observatorio Astronomico Felix Aguilar OAFA), R. Rebolo, M. Serra (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), O.A. Gress, N.M. Budnev, O.Ershova (Irkutsk State University, API), L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), V. Yurkov, A. Gabovich (Blagoveschensk Educational State University) MASTER-Tavrida robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 231106A ( Fermi GBM team, GCN 34956) errorbox 7435 sec after notice time and 7476 sec after trigger time at 2023-11-06 20:18:00 UT, with upper limit up to 19.0 mag. The observations began at zenith distance = 68 deg. The sun altitude is -58.5 deg. The galactic latitude b = 21 deg., longitude l = 194 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2296397 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 7507 | 2023-11-06 20:18:00 | MASTER-Tavrida | (07h 18m 58.76s , +28d 01m 31.6s) | C | 60 | 16.6 | 7579 | 2023-11-06 20:19:12 | MASTER-Tavrida | (07h 11m 43.66s , +26d 07m 24.0s) | C | 60 | 16.1 | 8169 | 2023-11-06 20:29:02 | MASTER-Tavrida | (07h 27m 01.04s , +29d 55m 54.0s) | C | 60 | 17.4 | 8317 | 2023-11-06 20:31:30 | MASTER-Tavrida | (07h 36m 13.30s , +28d 00m 34.7s) | C | 60 | 15.6 | 8390 | 2023-11-06 20:32:43 | MASTER-Tavrida | (07h 45m 13.60s , +28d 02m 01.0s) | C | 60 | 13.5 | 8610 | 2023-11-06 20:36:22 | MASTER-Tavrida | (07h 18m 54.71s , +28d 00m 53.6s) | C | 60 | 17.7 | 9277 | 2023-11-06 20:47:30 | MASTER-Tavrida | (07h 28m 03.37s , +28d 00m 48.0s) | C | 60 | 17.8 | 9351 | 2023-11-06 20:48:43 | MASTER-Tavrida | (07h 11m 38.63s , +26d 07m 42.0s) | C | 60 | 18.0 | 9423 | 2023-11-06 20:49:56 | MASTER-Tavrida | (07h 20m 32.94s , +26d 06m 27.4s) | C | 60 | 17.8 | 9642 | 2023-11-06 20:53:35 | MASTER-Tavrida | (07h 28m 30.97s , +26d 08m 26.4s) | C | 60 | 17.5 | 9714 | 2023-11-06 20:54:47 | MASTER-Tavrida | (07h 37m 30.51s , +26d 07m 36.6s) | C | 60 | 17.3 | 9788 | 2023-11-06 20:56:01 | MASTER-Tavrida | (07h 21m 38.45s , +24d 12m 21.0s) | C | 60 | 17.4 | 9861 | 2023-11-06 20:57:14 | MASTER-Tavrida | (07h 30m 29.86s , +24d 12m 54.8s) | C | 60 | 17.0 | 9935 | 2023-11-06 20:58:28 | MASTER-Tavrida | (07h 27m 01.91s , +29d 55m 58.0s) | C | 60 | 18.5 | 10007 | 2023-11-06 20:59:40 | MASTER-Tavrida | (07h 36m 15.07s , +29d 54m 58.4s) | C | 60 | 18.2 | 10159 | 2023-11-06 21:02:12 | MASTER-Tavrida | (07h 24m 04.95s , +22d 19m 29.7s) | C | 60 | 17.1 | 10234 | 2023-11-06 21:03:27 | MASTER-Tavrida | (07h 36m 06.69s , +28d 02m 41.0s) | C | 60 | 18.2 | 10306 | 2023-11-06 21:04:39 | MASTER-Tavrida | (07h 45m 14.82s , +28d 01m 51.3s) | C | 60 | 17.7 | 10379 | 2023-11-06 21:05:52 | MASTER-Tavrida | (07h 38m 17.32s , +24d 12m 47.6s) | C | 60 | 17.3 | 10452 | 2023-11-06 21:07:05 | MASTER-Tavrida | (07h 47m 07.78s , +24d 13m 19.4s) | C | 60 | 16.2 | 10526 | 2023-11-06 21:08:19 | MASTER-Tavrida | (07h 18m 57.19s , +28d 02m 21.1s) | C | 60 | 18.3 | 11903 | 2023-11-06 21:31:16 | MASTER-Tavrida | (07h 27m 56.23s , +28d 02m 55.0s) | C | 60 | 18.3 | 11975 | 2023-11-06 21:32:28 | MASTER-Tavrida | (07h 11m 40.50s , +26d 07m 34.7s) | C | 60 | 18.6 | 12048 | 2023-11-06 21:33:41 | MASTER-Tavrida | (07h 20m 28.35s , +26d 06m 44.0s) | C | 60 | 18.5 | 12121 | 2023-11-06 21:34:54 | MASTER-Tavrida | (07h 31m 55.79s , +22d 19m 23.2s) | C | 60 | 18.1 | 12193 | 2023-11-06 21:36:06 | MASTER-Tavrida | (07h 40m 32.06s , +22d 21m 04.8s) | C | 60 | 18.2 | 12266 | 2023-11-06 21:37:19 | MASTER-Tavrida | (07h 37m 26.81s , +26d 07m 27.4s) | C | 60 | 18.7 | 12338 | 2023-11-06 21:38:31 | MASTER-Tavrida | (07h 30m 29.80s , +24d 14m 40.3s) | C | 60 | 18.5 | 12411 | 2023-11-06 21:39:44 | MASTER-Tavrida | (07h 26m 57.61s , +29d 55m 51.6s) | C | 60 | 18.9 | 12483 | 2023-11-06 21:40:56 | MASTER-Tavrida | (07h 36m 10.40s , +29d 57m 03.1s) | C | 60 | 18.7 | 12628 | 2023-11-06 21:43:21 | MASTER-Tavrida | (07h 24m 02.93s , +22d 18m 52.3s) | C | 60 | 18.3 | 12702 | 2023-11-06 21:44:35 | MASTER-Tavrida | (07h 45m 14.98s , +28d 01m 29.2s) | C | 60 | 18.8 | 12774 | 2023-11-06 21:45:47 | MASTER-Tavrida | (07h 47m 05.00s , +24d 15m 07.1s) | C | 60 | 18.5 | 12848 | 2023-11-06 21:47:00 | MASTER-Tavrida | (07h 27m 58.96s , +28d 01m 19.4s) | C | 60 | 18.9 | 13142 | 2023-11-06 21:51:54 | MASTER-Tavrida | (07h 20m 26.86s , +26d 08m 02.8s) | C | 60 | 19.0 | 13215 | 2023-11-06 21:53:08 | MASTER-Tavrida | (07h 40m 28.08s , +22d 21m 25.6s) | C | 60 | 18.7 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 34965 table
GRB_name GRB231106A
GCN_number 34965
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 34965 SUBJECT: GRB 231106A: CALET Gamma-Ray Burst Monitor detection DATE: 23/11/08 07:00:36 GMT FROM: Yuta Kawakubo at Louisiana State University T. Sakamoto, A. Yoshida, S. Sugita (AGU), Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA), Y. Asaoka (ICRR), S. Torii, Y. Akaike, K. Kobayashi (Waseda U), Y. Shimizu, 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 long GRB 231106A (Fermi GBM Final Real-time Localization: Fermi GBM team, GCN Circ. 34956) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 18:12:50.43 UTC on 6 November 2023 (http://cgbm.calet.jp/cgbm_trigger/flight/1383329517). The burst signal was seen by all CGBM detectors. The burst light curve shows a multi-peaked structure that starts at T-8.5 sec, peaks at T+38.1 sec, and ends at T+80.9 sec. The T90 duration measured by the SGM data are 61.6 +/- 6.3 sec (40-1000 keV). The ground-processed light curve is available at http://cgbm.calet.jp/cgbm_trigger/ground/1383329517/index.html The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at Waseda University.
GCN 34966 table
GRB_name GRB231106A
GCN_number 34966
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 34966 SUBJECT: GRB 231106A: AstroSat CZTI detection DATE: 23/11/08 09:10:39 GMT FROM: Gaurav Waratkar at IIT Bombay P. K. Navaneeth (IUCAA), G. Waratkar (IITB), A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka University/IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al., 2021, JApA, 42, 73) showed the detection of a GRB 231106A which was also detected by Fermi - GBM (Fermi GBM Team, GCN Circ. 34956) and CALET (Sakamoto et al., GCN Circ. 34965). The source was clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2023-11-06 18:13:23.15 UTC. The measured peak count rate associated with the burst is 213 (+67, -26) counts/s above the background in the combined data of all quadrants, with a total of 3452 (+1277, -1014) counts. The local mean background count rate was 1235 (+4, -5) counts/s. We measure a T90 of 54 (+22, -11) s from the cumulative Veto light curve. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, URSC, IUCAA, SAC, and PRL. The Indian Space Research Organisation funded, managed, and facilitated the project. CZTI GRB detections are reported regularly on the payload site at: http://astrosat.iucaa.in/czti/?q=grb
GCN 35013 table
GRB_name GRB231106A
GCN_number 35013
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 35013 SUBJECT: GRB 231106A: Glowbug gamma-ray detection DATE: 23/11/13 15:39:22 GMT FROM: C.C. Cheung at Naval Research Lab C.C. Cheung, M. Kerr, J. E. Grove, R. Woolf (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge (MSFC), and M.S. Briggs (UAH) report: The Glowbug gamma-ray telescope [1,2], operating on the International Space Station, reports the detection of GRB 231106A, which was also detected by Fermi/GBM, CALET, and AstroSat/CZTI (GCN 34956, 34965, 34966). Using an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2023-11-06 18:12:49.696. The light curve comprises an initial peak followed by a multi-peaked structure as observed by CALET (GCN 34965). In the Glowbug data, the initial peak has a duration of 6.1 s and a total significance of about 24.1 sigma. Using a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a photon index dN/dE~E^x of x=0.4 and a cutoff energy ("Epeak") of 356 keV. The modeled 10-10000 keV fluence is 1.9e-06 erg/cm^2. The onset of the later multi-peaked structure observed by Glowbug is determined to be 2023-11-06 18:13:18.368 with a duration of 26.6 s and a total significance of about 46.1 sigma. Using a standard power-law function with an exponential high-energy cutoff to model the emission over this duration results in a photon index of x=2.0 and an Epeak of 204 keV. The modeled 10-10000 keV fluence is 4.2e-06 erg/cm^2. The analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS. Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Program’s STP-H9 to the ISS. The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2/3 sky) over a wide energy band of 50 keV to >2 MeV. [1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959 [2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O [3] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006 Distribution Statement A: Approved for public release. Distribution is unlimited.
GCN 35047 table
GRB_name GRB231106A
GCN_number 35047
Detection_method Optical
ra 113.4482°
decl 29.2245°
Circular_text TITLE: GCN CIRCULAR NUMBER: 35047 SUBJECT: GRB 231106A: TESS identification of candidate optical counterpart DATE: 23/11/15 22:20:46 GMT FROM: Rahul Jayaraman at MIT R. Jayaraman (MIT/MKI), R. Vanderspek (MIT/MKI), M.M. Fausnaugh (TTU), G. Mo (MIT/LIGO), and G.R. Ricker (MIT/MKI) report: The Transiting Exoplanet Survey Satellite (TESS; Ricker et al. JATIS 1 2015) was observing 91% of the Fermi-GBM localization region for the gamma-ray burst GRB 231106A (GCN 34956). TESS observed this region at a 200 second cadence continuously from 1.5 days before the trigger to 6.4 days after the trigger. The GRB occurred during TESS observational Sector 71, and most of the GBM localization fell within Camera 4, CCD 1. We inspected the full-frame image (FFI) from the publicly available TICA data archived at MAST (https://archive.stsci.edu/hlsp/tica) at the time of the Fermi trigger and identified a bright point source not present in previous TESS images. This point source is located at RA = 113.4482, Dec = 29.2245 (uncertainty 1-2"), which is 3.6° from the center of the Fermi-GBM error region, and is located within the 39.7% credible region of the Fermi sky map. We extracted a light curve for this source from the calibrated TESS FFIs produced by TICA (Fausnaugh et al. RNAAS 2020) using difference imaging and forced photometry. Our analysis procedure is described in Fausnaugh et al. 2023 (ApJ 956(2):108). TESS observations show that this optical transient rises rapidly (in less than 200 seconds), peaks at a magnitude of 13.8 in the TESS band (600 nm–1000 nm), and then decays to the detection limit within 2000 seconds, with a power-law index of -0.95 ± 0.28. The 3-sigma detection limit around the time of the trigger was 17.5. This circular includes data collected with the TESS mission, obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the TESS mission is provided by the NASA Explorer Program. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555.