October 2025 - vsnet-grb-info - ooruri.kusastro.kyoto-u.ac.jp

[vsnet-grb-info 40254] GRB 251007A: SVOM/GRM observation
by GCN Circulars 10 Oct '25

10 Oct '25

TITLE: GCN CIRCULAR NUMBER: 42184 SUBJECT: GRB 251007A: SVOM/GRM observation DATE: 25/10/10 12:47:58 GMT FROM: yzh807926(a)163.com SVOM/GRM team: Zheng-Hang Yu, Chen-Wei Wang, Yue Huang, Shi-Jie Zheng, Shao-Lin Xiong, Shuang-Nan Zhang (IHEP) SVOM/ECLAIRs team: Feliu Lacreu (IAP), Sebastien Guillot (IRAP), Olivier GODET (IRAP), Marius Brunet (IRAP), Frédéric Piron (LUPM), Jean-Luc Atteia (IRAP) Report on behalf of the SVOM team: SVOM/GRM was triggered in-flight by a burst GRB 251007A (SVOM trigger reference: sb25100703) at 2025-10-07T19:37:53.000 UTC (T0), which is also detected by Swift/BAT (Ambrosi et al. 2025, GCN #42146), Glowbug (Cheung et al. 2025, GCN #42151) and CALET/GBM (A. Yoshida et al. 2025, GCN #42156). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of a precursor followed by a main episode with multiple peaks a T90 of 58.0 +1.5/-5.5 s in the 15-5000 keV band. The SVOM/GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb251007A.png In addition, the position of this burst, as determined by Swift/BAT (RA= 128.1775, DEC= 21.8138, GCN#42146), is located at about 49 degrees from the SVOM optical axis, which is outside the ECLAIRs field of view. Nevertheless, ECLAIRs detected the burst above 50 keV through its shield. With this localization, the time-averaged spectrum from T0-50 to T0+30 s is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -1.27 +0.04/-0.04 and the cutoff energy, parameterized as Epeak, is 761 +219/-152 keV. The event fluence (10-1000 keV) in this time interval is (3.97 +0.14/-0.15)E-05 erg/cm^2. The localization of GRB 251007A in the 'Amati' relation diagram is shown at: https://www.bursthub.cn//admin/static/svgrb251007A_amati.png The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. GRM is developed by the Institute of High Energy Physics (IHEP) of CAS. The SVOM point of contact for this burst is: Zheng-Hang Yu(IHEP)(zhyu(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/42184. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40253] GRB 251007A: Insight-HXMT detection
by GCN Circulars 10 Oct '25

10 Oct '25

TITLE: GCN CIRCULAR NUMBER: 42183 SUBJECT: GRB 251007A: Insight-HXMT detection DATE: 25/10/10 12:33:04 GMT FROM: Chenwei Wang at IHEP <cwwang(a)ihep.ac.cn> Chen-Wei Wang, Zheng-Hang Yu, Cheng-Kui Li, Shao-Lin Xiong, and Chao Zheng report on behalf of the Insight-HXMT team: At 2025-10-07T19:37:51.750 (T0), Insight-HXMT/HE detected the burst GRB 251007A, which is also detected by Swift/BAT (E. Ambrosi et al, GCN#42146), Glowbug (C.C. Cheun et al., GCN#42151), CALET/GBM (A. Yoshida et al., GCN#42156) and AstroSat (S. Salunke et al., GCN#42167). The Insight-HXMT/HE light curve mainly consists of multi-pulses with a T90 of 57.4 +1.8/-16.2 s. The 1s peak rate, measured from T0+0.7 s, is 7246 cnts/sec. The total counts from this burst is 52938 counts. The HXMT/HE light curve can be found here: https://www.bursthub.cn//admin/static/hxmtgrb251007A.png All measurements above are made with the CsI detectors operating in the regular mode with the energy range of about 60-900 keV (deposited 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. 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. View this GCN Circular online at https://gcn.nasa.gov/circulars/42183. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40252] GRB 251006A: CALET Gamma-Ray Burst Monitor detection
by GCN Circulars 10 Oct '25

10 Oct '25

TITLE: GCN CIRCULAR NUMBER: 42182 SUBJECT: GRB 251006A: CALET Gamma-Ray Burst Monitor detection DATE: 25/10/10 10:17:47 GMT FROM: Yuta Kawakubo at Aoyama Gakuin University <kawakubo(a)phys.aoyama.ac.jp> T. Sakamoto, A. Yoshida, S. Sugita, Y. Kawakubo (AGU), 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 short GRB 251006A (Fermi GBM Final Real-time Localization: Fermi GBM team, GCN Circ. 42124; Glowbug gamma-ray detection: Cheung et al., GCN Circ. 42130; Swift/BAT-GUANO subthreshold detection: DeLaunay et al., GCN Circ. 42144; Fermi GBM Observation: Palafox et al., GCN Circ. 42175) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 13:27:35.21 UTC on 6 October 2025 (https://cgbm.calet.jp/cgbm_trigger/flight/1443792004/index.html) The burst signal was seen by only the SGM detector. 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 single pulse that starts at T-0.22 sec and ends at T+0.04 sec. The T90 and T50 durations measured by the SGM data are 0.21 +/- 0.05 sec and 0.11 +/- 0.05 sec (40-1000 keV), respectively. The ground-processed light curve is available at https://cgbm.calet.jp/cgbm_trigger/ground/1443792004/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at Waseda University. View this GCN Circular online at https://gcn.nasa.gov/circulars/42182. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40251] GRB 251007B - SVOM/ECLAIRs refined analysis
by GCN Circulars 10 Oct '25

10 Oct '25

TITLE: GCN CIRCULAR NUMBER: 42181 SUBJECT: GRB 251007B - SVOM/ECLAIRs refined analysis DATE: 25/10/10 08:31:06 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> Authors: O. Godet, S. Guillot (IRAP), F. Lacreu (IAP), M. Brunet, N. A. Webb (IRAP) Using the event-by-event data downloaded through the X-band ground stations, we report further analysis of ECLAIRs observations of GRB 251007B (SVOM burst-id sb25100703). The burst that triggered ECLAIRs onboard (Webb et al., GCN Circ. #42148) consists of a simple peak structure with a duration of T90 = 33.16 -6.76 / +3.58 s in the 4-120 keV energy band. The time-averaged spectrum from T0-18 s to T0+22 s (T0 = 2025-10-07T19:43:23) in the energy range 5-70 keV is best fitted by a powerlaw model with a photon index of 1.58 +0.15/-0.14. With this model, the total 4-120 keV fluence is (9.0 +0.4/-0.2)e-7 erg/cm^2. All the quoted errors are at the 68% confidence level. The Space-based multi-band astronomical Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA), French Space Agency (CNES), and the Chinese Academy of Sciences (CAS), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. ECLAIRs was developed jointly by CNES, CEA-IRFU, CNRS-IRAP, CNRS-APC. The SVOM/ECLAIRs point of contact for this burst is: O. Godet (IRAP) (ogodet at irap.omp.eu) View this GCN Circular online at https://gcn.nasa.gov/circulars/42181. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40250] SVOM/sb25101004: SVOM detection of a stellar flare
by GCN Circulars 10 Oct '25

10 Oct '25

TITLE: GCN CIRCULAR NUMBER: 42180 SUBJECT: SVOM/sb25101004: SVOM detection of a stellar flare DATE: 25/10/10 07:23:03 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> Donghua ZHAO, Chao Wu, Wenjin Xie (NAOC), Hatsunegoto Goto(Kanazawa Univ./CEA)，Florent Robinet (IJCLab), Nicolas Dagoneau, J. T. Palmerio (CEA) report on behalf of the SVOM mission team At 2025-10-10T03:51:58 UTC (T0), SVOM/ECLAIRs triggered and located the source (SVOM burst-id sb25101004). The following trigger information was received on the ground with low latency by the SVOM VHF Alert Network. The source was only detected by the Image Trigger (IMT), which produced a sequence of 5 alerts. IMT provided the alert with the best signal-to-noise-ratio in the image (SNR) of 9.82 in the [5-20] keV energy band over a time window of 327.68 seconds starting at 2025-10-10T03:47:53. The localization of the best alert is R.A., Dec.: 311.3214, -31.4119 degrees (J2000) with a 90% confidence level (C.L.) radius of 8.10 arcmin (including systematic error of 2 arcmin added in quadrature). SVOM slewed to the source. SVOM/MXT began observing the field at 2025-10-10T04:00:23 UTC, 505 seconds after T0. Using X band data we found a source located at R.A., Dec.: 311.2972, -31.3445 degrees: R.A. (J2000) = 20h45m11.338s Dec. (J2000) = -31d20m40.213s with a 90% C.L. radius of 25.8 arcseconds (including a systematic error of 25 arcsec added in quadrature). This location is 4.23 arcminutes from the ECLAIRs onboard position. No uncatalogued fading X-ray counterpart was detected. There is a known source HD 197481 (Au Mic: a young red dwarf star ) which is 4.23 arcmin away from ECLAIRs position and is 26 arcsec away from MXT position. These results show that this trigger is probably caused by the stellar flare of HD 197481 (Au Mic). The Space-based multi-band astronomical Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA), French Space Agency (CNES), and the Chinese Academy of Sciences (CAS), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. SVOM/ECLAIRs was developed jointly by CNES, CEA-IRFU, CNRS-IRAP, CNRS-APC. SVOM/GRM was developed by the Institute of High Energy Physics (IHEP) of CAS. SVOM/MXT was developed jointly by CNES, CEA-IRFU, CNRS-IJCLab, University of Leicester, MPE. The Burst Advocate (BA) on shift for this alert is Donghua Zhao: zhaodh(a)bao.ac.cn. Please contact the BA by email if you require additional information. View this GCN Circular online at https://gcn.nasa.gov/circulars/42180. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40249] GRB 251009A: Fermi GBM Final Localization
by GCN Circulars 10 Oct '25

10 Oct '25

TITLE: GCN CIRCULAR NUMBER: 42179 SUBJECT: GRB 251009A: Fermi GBM Final Localization DATE: 25/10/10 00:04:26 GMT FROM: Matt Godwin <msg0028(a)uah.edu> The Fermi GBM team reports the detection of a likely SHORT GRB "At 15:58:56.61 UT on 09 October 2025, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 251009A (trigger 781718341/251009666). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 72.05, Dec = -25.84 (J2000 degrees, equivalent to J2000 4h 48m, -25d 50'), with a statistical uncertainty of 25.22 degrees. The angle from the Fermi LAT boresight is 86 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2025/bn251009666/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2025/bn251009666/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2025/bn251009666/…" View this GCN Circular online at https://gcn.nasa.gov/circulars/42179. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40248] GRB 250916A: TERI Gamma-ray detection
by GCN Circulars 09 Oct '25

09 Oct '25

TITLE: GCN CIRCULAR NUMBER: 42178 SUBJECT: GRB 250916A: TERI Gamma-ray detection DATE: 25/10/09 21:13:22 GMT FROM: Daniel Shy <danielshy(a)danielshy.com> Daniel Shy (a), C.C. Cheung (a), Bernard Phlips (a), Michael Streicher (b), James Mason (b), Douglas M. Groves (b), Feng Zhang (b), Willy Kaye (b) (a) U.S. Naval Research Laboratory, 4555 Overlook Ave SW, Washington, DC 20375 (b) H3D, Inc., 812 Avis Dr., Ann Arbor, MI 48108, USA The cadmium zinc TElluride Radiation Imager (TERI) gamma-ray telescope [1], operating on the International Space Station, reports the detection of GRB 250916A, which was also detected by Fermi/GBM (Fermi GBM Team, GCN Circ., 41839), Astrosat/CZTI (Arya et al., GCN Circ. 41843), Glowbug (Cheung et al., GCN Circ. 41855), CALET/GBM (Trig ID. 1442064382), and NuSTAR (41871). Using 1 Hz binning, the peak count rate is roughly 23 excess counts per second (cps) at ~T0+259s (adopting T0 = 2025-09-16 13:29:21.1) over a baseline rate of 41-cps observed in nearby off-source intervals. We do not detect the initial faint burst at T0 detected by Fermi/GBM. The analysis results presented here are preliminary and currently lack a detailed response function. TERI is an Office of Naval Research funded technology demonstrator for large-volume pixelated CdZnTe detectors developed, built, and operated by the U.S. Naval Research Laboratory (NRL) in conjunction with H3D, Inc. The pixelated CdZnTe detectors have an energy of 40 keV to 3 MeV per pixel. It was launched on 2025 April 21 aboard the Department of Defense Space Test Program’s STP-H10 to the ISS. On the ISS, it is located on the SOX external payload facility on the Columbus module. [1] Shy, Daniel, et al. "Development of the cadmium zinc TElluride Radiation Imager." Journal of Astronomical Telescopes, Instruments, and Systems 10.4 (2024): 044009-044009 (arXiv:2408.04559). Distribution Statement A: Approved for public release. Distribution is unlimited. View this GCN Circular online at https://gcn.nasa.gov/circulars/42178. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40247] GRB 250919A: TERI gamma-ray detection
by GCN Circulars 09 Oct '25

09 Oct '25

TITLE: GCN CIRCULAR NUMBER: 42177 SUBJECT: GRB 250919A: TERI gamma-ray detection DATE: 25/10/09 21:09:21 GMT FROM: Daniel Shy <danielshy(a)danielshy.com> Daniel Shy (a), C.C. Cheung (a), Bernard Phlips (a), Michael Streicher (b), James Mason (b), Douglas M. Groves (b), Feng Zhang (b), Willy Kaye (b) (a) U.S. Naval Research Laboratory, 4555 Overlook Ave SW, Washington, DC 20375 (b) H3D, Inc., 812 Avis Dr., Ann Arbor, MI 48108, USA The cadmium zinc TElluride Radiation Imager (TERI) gamma-ray telescope [1], operating on the International Space Station, reports the detection of GRB 250919A, which was also detected by Fermi/GBM, SVOM/GRM, EP/WXT, NuSTAR, Glowbug, Insight-HXMT, and Konus-Wind (Fermi GBM team, GCN 41874; Wang et al., GCN 41882; Liang et al., GCN 41879; Waratkar & Grefenstette, GCN 41888; Cheung et al., GCN 41891, Wang et al., GCN 41900; Frederiks et al., GCN 41905) Using 1 Hz binning, and adopting T0 = 2025-09-19 00:28:52.28, we observe the three dominant peaks seen in the Fermi/GBM lightcurve (GCN 41874) at ~T0+24s, ~T0+26s, and ~T0+29s with respective peak excess count rates of roughly 57, 171, and 104 counts per second (cps) above the 27-cps baseline rate observed in nearby off-source intervals. We do not observe the fainter, leading feature at ~T0, as seen in the Fermi/GBM lightcurve. The analysis results presented here are preliminary and currently lack a detailed response function. TERI is an Office of Naval Research funded technology demonstrator for large-volume pixelated CdZnTe detectors developed, built, and operated by the U.S. Naval Research Laboratory (NRL) in conjunction with H3D, Inc. The pixelated CdZnTe detectors have an energy of 40 keV to 3 MeV per pixel. It was launched on 2025 April 21 aboard the Department of Defense Space Test Program’s STP-H10 to the ISS. On the ISS, it is located on the SOX external payload facility on the Columbus module. [1] Shy, Daniel, et al. "Development of the cadmium zinc TElluride Radiation Imager." Journal of Astronomical Telescopes, Instruments, and Systems 10.4 (2024): 044009-044009 (arXiv:2408.04559). Distribution Statement A: Approved for public release. Distribution is unlimited. View this GCN Circular online at https://gcn.nasa.gov/circulars/42177. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40246] EP251006a: Global MASTER-Net observations report
by GCN Circulars 09 Oct '25

09 Oct '25

TITLE: GCN CIRCULAR NUMBER: 42176 SUBJECT: EP251006a: Global MASTER-Net observations report DATE: 25/10/09 20:18:28 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, A.Kuznetsov, K.Zhirkov, I.Panchenko, N.Tiurina, P.Balanutsa, V.Topolev, D.Vlasenko, G.Antipov, A.Sankovich, Yu.Tselik, Ya.Kechin, V.Senik, A.Chasovnikov, K.Labsina, I. Gorbunov (Lomonosov MSU), O.Gress, N.Budnev (ISU), C.Francile, F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), A.Sosnovskij (CrAO), A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity), D.Buckley (SAAO), R.Rebolo (The Instituto de Astrofisica de Canarias), L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory) MASTER-Kislovodsk robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) was pointed to the EP251006a ( EP Team et al., GCN 42137) errorbox 196 sec after trigger time at 2025-10-07 18:11:57 UT, with upper limit up to 16.6 mag. The observations began at zenith distance = 79 deg. The sun altitude is -37.7 deg. MASTER-SAAO robotic telescope located in South Africa (South African Astronomical Observatory) was pointed to the EP251006a errorbox 3541 sec after trigger time at 2025-10-07 19:07:42 UT, with upper limit up to 18.5 mag. The observations began at zenith distance = 75 deg. The sun altitude is -29.6 deg. MASTER-OAFA robotic telescope located in Argentina (OAFA observatory of San Juan National University) was pointed to the EP251006a errorbox 40526 sec after trigger time at 2025-10-08 05:24:07 UT, with upper limit up to 18.7 mag. The observations began at zenith distance = 27 deg. The sun altitude is -50.3 deg. The galactic latitude b = -56 deg., longitude l = 180 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3010044 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 226 | 2025-10-07 18:11:57 | MASTER-Kislovodsk | (02h 39m 56.00s , -06d 09m 59.8s) | C | 60 | 14.6 | 226 | 2025-10-07 18:11:57 | MASTER-Kislovodsk | (02h 39m 54.59s , -05d 47m 17.6s) | C | 60 | 15.4 | 508 | 2025-10-07 18:16:38 | MASTER-Kislovodsk | (02h 39m 49.79s , -05d 48m 02.3s) | C | 60 | 15.5 | 508 | 2025-10-07 18:16:38 | MASTER-Kislovodsk | (02h 39m 51.52s , -06d 10m 40.5s) | C | 60 | 14.6 | 823 | 2025-10-07 18:21:54 | MASTER-Kislovodsk | (02h 39m 48.84s , -05d 45m 43.0s) | C | 60 | 15.5 | 883 | 2025-10-07 18:21:54 | MASTER-Kislovodsk | (02h 39m 48.82s , -05d 45m 42.9s) | C | 180 | 16.2 | Coadd 823 | 2025-10-07 18:21:54 | MASTER-Kislovodsk | (02h 39m 51.15s , -06d 08m 22.6s) | C | 60 | 14.9 | 903 | 2025-10-07 18:23:14 | MASTER-Kislovodsk | (02h 39m 51.14s , -06d 10m 23.8s) | C | 60 | 14.9 | 903 | 2025-10-07 18:23:14 | MASTER-Kislovodsk | (02h 39m 48.76s , -05d 47m 43.3s) | C | 60 | 15.5 | 1250 | 2025-10-07 18:29:00 | MASTER-Kislovodsk | (02h 39m 55.32s , -05d 47m 15.7s) | C | 60 | 15.6 | 1250 | 2025-10-07 18:29:00 | MASTER-Kislovodsk | (02h 39m 57.09s , -06d 10m 09.1s) | C | 60 | 14.6 | 3572 | 2025-10-07 19:07:42 | MASTER-SAAO | (02h 38m 20.93s , -06d 05m 34.6s) | C | 60 | 17.0 | 3572 | 2025-10-07 19:07:42 | MASTER-SAAO | (02h 40m 07.46s , -06d 21m 24.6s) | C | 60 | 13.5 | 40556 | 2025-10-08 05:24:07 | MASTER-OAFA | (02h 38m 04.24s , -06d 11m 37.8s) | C | 60 | 18.6 | 40631 | 2025-10-08 05:25:22 | MASTER-OAFA | (02h 38m 03.16s , -06d 10m 39.1s) | C | 60 | 18.6 | 40868 | 2025-10-08 05:29:18 | MASTER-OAFA | (02h 38m 02.78s , -06d 12m 42.4s) | C | 60 | 18.7 | 40945 | 2025-10-08 05:30:36 | MASTER-OAFA | (02h 46m 13.59s , -06d 12m 15.1s) | C | 60 | 18.7 | 41021 | 2025-10-08 05:31:52 | MASTER-OAFA | (02h 46m 09.43s , -06d 10m 39.7s) | C | 60 | 18.6 | 41099 | 2025-10-08 05:33:10 | MASTER-OAFA | (02h 46m 09.23s , -06d 12m 05.1s) | C | 60 | 18.6 | 43486 | 2025-10-08 06:12:57 | MASTER-OAFA | (02h 46m 25.97s , -05d 55m 21.1s) | C | 60 | 18.7 | 43564 | 2025-10-08 06:14:15 | MASTER-OAFA | (02h 46m 30.99s , -05d 55m 10.3s) | C | 60 | 18.7 | 43638 | 2025-10-08 06:15:29 | MASTER-OAFA | (02h 46m 28.25s , -05d 53m 31.6s) | C | 60 | 18.7 | 86664 | 2025-10-08 18:12:34 | MASTER-Kislovodsk | (02h 39m 48.87s , -05d 45m 56.5s) | C | 60 | 15.5 | 86724 | 2025-10-08 18:12:34 | MASTER-Kislovodsk | (02h 39m 48.87s , -05d 45m 56.4s) | C | 180 | 16.0 | Coadd 86664 | 2025-10-08 18:12:34 | MASTER-Kislovodsk | (02h 39m 49.14s , -06d 09m 00.5s) | C | 60 | 14.8 | 86744 | 2025-10-08 18:13:54 | MASTER-Kislovodsk | (02h 39m 58.79s , -05d 49m 41.8s) | C | 60 | 15.4 | 86744 | 2025-10-08 18:13:54 | MASTER-Kislovodsk | (02h 39m 59.30s , -06d 12m 47.1s) | C | 60 | 14.1 | 87245 | 2025-10-08 18:22:15 | MASTER-Kislovodsk | (02h 39m 49.23s , -05d 46m 24.8s) | C | 60 | 15.4 | 87245 | 2025-10-08 18:22:15 | MASTER-Kislovodsk | (02h 39m 52.54s , -06d 09m 03.4s) | C | 60 | 15.4 | 88594 | 2025-10-08 18:44:45 | MASTER-Kislovodsk | (02h 39m 53.25s , -05d 46m 54.7s) | C | 60 | 15.8 | 88654 | 2025-10-08 18:44:45 | MASTER-Kislovodsk | (02h 39m 53.24s , -05d 46m 54.5s) | C | 180 | 16.6 | Coadd 88594 | 2025-10-08 18:44:45 | MASTER-Kislovodsk | (02h 39m 57.09s , -06d 10m 00.7s) | C | 60 | 16.3 | 88935 | 2025-10-08 18:50:26 | MASTER-Kislovodsk | (02h 39m 52.51s , -05d 45m 44.1s) | C | 60 | 16.0 | 88935 | 2025-10-08 18:50:26 | MASTER-Kislovodsk | (02h 39m 58.82s , -06d 08m 32.2s) | C | 60 | 16.4 | 89015 | 2025-10-08 18:51:46 | MASTER-Kislovodsk | (02h 39m 58.46s , -05d 46m 41.6s) | C | 60 | 16.0 | 89015 | 2025-10-08 18:51:46 | MASTER-Kislovodsk | (02h 40m 04.85s , -06d 09m 31.8s) | C | 60 | 16.3 | 89095 | 2025-10-08 18:53:06 | MASTER-Kislovodsk | (02h 39m 48.54s , -05d 44m 54.1s) | C | 60 | 15.9 | 89155 | 2025-10-08 18:53:06 | MASTER-Kislovodsk | (02h 39m 48.54s , -05d 44m 54.2s) | C | 180 | 16.6 | Coadd 89095 | 2025-10-08 18:53:06 | MASTER-Kislovodsk | (02h 39m 55.02s , -06d 07m 45.0s) | C | 60 | 16.4 | 89175 | 2025-10-08 18:54:25 | MASTER-Kislovodsk | (02h 39m 54.56s , -05d 46m 36.7s) | C | 60 | 16.0 | 89175 | 2025-10-08 18:54:25 | MASTER-Kislovodsk | (02h 40m 01.09s , -06d 09m 28.4s) | C | 60 | 16.2 | 89255 | 2025-10-08 18:55:46 | MASTER-Kislovodsk | (02h 39m 54.62s , -05d 44m 51.0s) | C | 60 | 16.1 | 89255 | 2025-10-08 18:55:46 | MASTER-Kislovodsk | (02h 40m 01.20s , -06d 07m 42.8s) | C | 60 | 16.4 | 89335 | 2025-10-08 18:57:06 | MASTER-Kislovodsk | (02h 40m 00.54s , -05d 48m 27.7s) | C | 60 | 15.9 | 89335 | 2025-10-08 18:57:06 | MASTER-Kislovodsk | (02h 40m 07.15s , -06d 11m 19.7s) | C | 60 | 16.3 | 89937 | 2025-10-08 19:07:07 | MASTER-Kislovodsk | (02h 39m 50.59s , -05d 42m 57.7s) | C | 60 | 16.1 | 89937 | 2025-10-08 19:07:07 | MASTER-Kislovodsk | (02h 39m 56.71s , -06d 06m 09.4s) | C | 60 | 16.4 | 90017 | 2025-10-08 19:08:27 | MASTER-Kislovodsk | (02h 39m 53.56s , -05d 47m 41.3s) | C | 60 | 16.0 | 90017 | 2025-10-08 19:08:27 | MASTER-Kislovodsk | (02h 39m 59.66s , -06d 10m 54.2s) | C | 60 | 16.4 | 111807 | 2025-10-09 01:11:38 | MASTER-SAAO | (02h 41m 40.45s , -06d 20m 51.9s) | C | 60 | 18.2 | 111807 | 2025-10-09 01:11:38 | MASTER-SAAO | (02h 39m 51.83s , -06d 05m 32.4s) | C | 60 | 18.5 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. View this GCN Circular online at https://gcn.nasa.gov/circulars/42176. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40245] GRB 251006A: Fermi GBM Observation
by GCN Circulars 09 Oct '25

09 Oct '25

TITLE: GCN CIRCULAR NUMBER: 42175 SUBJECT: GRB 251006A: Fermi GBM Observation DATE: 25/10/09 15:08:56 GMT FROM: Eva MP <eva.palafox(a)gmail.com> E. Palafox (INAOE), M. Godwin (UAH) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 13:27:35.03 UT on 06 October 2025, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 251006A (trigger 781450060/251006561), which was also detected by Swift/BAT-GUANO (J. DeLaunay et al. 2025, GCN 42144) and Glowbug (C. C. Cheung et al. 2025, GCN 42130). The Fermi GBM on-ground location is consistent with the Swift/BAT-GUANO position. The angle from the Fermi LAT boresight is 30 degrees. The GBM light curve consists of one short emission with total duration (T90) of about 1.4 s (50-300 keV). The time-averaged spectrum from T0-0.3 to T0+0.3 s is best fit by a Comptonized function with Epeak of 490 +/- 170 and alpha of -0.9 +/- 0.2. The event fluence (10-1000 keV) in this time interval is (4.8 +/- 0.6)E-07 erg/cm^2. The 64-ms peak photon flux measured starting from T0+0.0 s in the 10-1000 keV band is 7 +/- 1 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/" View this GCN Circular online at https://gcn.nasa.gov/circulars/42175. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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