Gamma-ray Burst 231106A

(All information courtesy of the instrument teams.)

Previous IAU Circulars

none

Results of Observations

GCN Circular #34956
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 Circular #34959
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 Circular #34965
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 Circular #34966
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 Circular #35013
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 det= ermined 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 s= ignificance of about 24.1 sigma. Using a standard power-law function with = an exponential high-energy cutoff [3] to model the emission over this durat= ion results in a photon index dN/dE~E^x of x=3D0.4 and a cutoff energy ("Ep= eak") 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 determ= ined to be 2023-11-06 18:13:18.368 with a duration of 26.6 s and a total si= gnificance of about 46.1 sigma. Using a standard power-law function with an= exponential high-energy cutoff to model the emission over this duration re= sults in a photon index of x=3D2.0 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 func= tion that lacks a detailed characterization of the surrounding passive stru= cture of the ISS.
Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost ga= mma-ray transient telescopes developed, built, and operated by the U.S. Nav= al 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=E2=80=99s 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 unl= imited.
GCN Circular #35047
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 =3D 113.4482, Dec =3D 29.2245 (uncertainty 1-2"), which is 3.6=C2=B0 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 =C2=B1 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=E2=80=9326555.

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Jochen Greiner, last update: 15-Nov-2023 [Disclaimer]