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

[vsnet-grb-info 40826] GRB 251116D: SVOM/GRM observation of a long GRB
by GCN Circulars 19 Nov '25

19 Nov '25

TITLE: GCN CIRCULAR NUMBER: 42759 SUBJECT: GRB 251116D: SVOM/GRM observation of a long GRB DATE: 25/11/19 11:43:21 GMT FROM: Xinghao Luo at SVOM/GRN <2952704891(a)qq.com> GRB 251116D: SVOM/GRM observation of a long GRB SVOM/GRM team: Xing-Hao Luo, Chen-Wei Wang, Zheng-Hang Yu, Yue Huang, Shi-Jie Zheng, Shao-Lin Xiong, Shuang-Nan Zhang (IHEP) SVOM/ECLAIRs team: Marius Brunet (IRAP) Report on behalf of the SVOM team: SVOM/GRM was triggered in-flight by GRB 251116D(SVOM trigger reference: sb25111606) at 2025-11-16T19:22:37.000 UTC(T0), which is also detected by AstroSat/CZTI (Harsha K. H. et.al., GCN #42715) , Konus-Wind and Glowbug (C.C. Cheung et.al., GCN #42718). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of multi-pulses and a possible bump with a T90 of 45 +3/-21 s in the 15-5000 keV band. The SVOM/GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb251116D.png In addition, the position of this burst, as determined by Glowbug (RA=148.0 , DEC=-37.6, with a raidus of 3.7 der (95% confidence), C.C. Cheung et.al., GCN #42718), is located at about 131 degrees form the SVOM optical axis, which is outside the ECLAIRs field of view. However this burst is seen by ECLAIRs by reflection on the atmosphere. With this localization, the time-averaged spectrum from T0-2 to T0+20 s is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -1.52 +0.21/-0.17 and the cutoff energy, parameterized as Epeak, is 498 +294/-139 keV. The event fluence (10-1000keV) in this time interval is (3.31 +0.18/-0.21)E-05 erg/cm^2. The localization of GRB 251116D in the 'Amati' relation diagram is shown at: https://www.bursthub.cn//admin/static/svgrb251116D_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: Xing-Hao Luo (2952704891(a)qq.com) View this GCN Circular online at https://gcn.nasa.gov/circulars/42759. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40825] EP251118a: GOTO optical afterglow detection
by GCN Circulars 19 Nov '25

19 Nov '25

TITLE: GCN CIRCULAR NUMBER: 42758 SUBJECT: EP251118a: GOTO optical afterglow detection DATE: 25/11/19 11:15:29 GMT FROM: Sergey Belkin at Monash University <sergey.belkin(a)monash.edu> S. Belkin, M. E. Wortley, D. O'Neill, B. P. Gompertz, G. Ramsay, R. L. C. Starling, K. Ackley, M. Dyer, J. Lyman, K. Ulaczyk, D. Steeghs, D. Galloway, V. Dhillon, P. O'Brien, K. Noysena, R. Kotak, R. Breton, J. Casares, L. Nuttall, B. Godson, T. Killestein, A. Kumar, M. Pursiainen report on behalf of GOTO collaboration: We report on optical observations with the Gravitational-wave Optical Transient Observer (GOTO; Steeghs et al. 2022, Dyer et al 2024) in response to the EP/WXT alert WXT11900480769 (Jiang et al., GCN 42749). Observations covering the position began on 2025-11-19 at 02:58:22 UT (+10.26 hr post trigger) and continued through to 2025-11-19 at 04:30:49 UT (+11.81 hr post trigger). Three epochs were obtained: the first through serendipitous survey coverage (4x45 s) and the second and third through targeted response (4x90 s), all in the GOTO L-band (400-700 nm). Images were processed immediately after acquisition using the GOTO pipeline. Difference imaging was performed using deeper template observations. We detect the optical counterpart (Malesani et al., GCN 42751), consistent with the X-ray counterpart (Shi et al., GCN 42754), with L = 20.08 ± 0.21 (AB) on 2025-11-19 at 02:58:22 UT (+10.26 hr). Follow-up L-band images at 03:22:37 UT (+10.67 hr) and 04:30:49 (+11.81 hr) yield L = 20.24 ± 0.17 and 20.17 ± 0.16 (AB), respectively. Magnitudes were calibrated using ATLAS-REFCAT2 (Tonry et al. 2018) and are not corrected for Galactic extinction. GOTO (https://goto-observatory.org) is a network of telescopes that is principally funded by the STFC and operated at the Roque de los Muchachos Observatory on La Palma, Spain, and Siding Spring Observatory in NSW, Australia, on behalf of a consortium including the University of Warwick, Monash University, Armagh Observatory & Planetarium, the University of Leicester, the University of Sheffield, the National Astronomical Research Institute of Thailand (NARIT), the University of Turku, the University of Portsmouth, the University of Manchester, the University of Birmingham, and the Instituto de Astrofisica de Canarias (IAC). View this GCN Circular online at https://gcn.nasa.gov/circulars/42758. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40824] GRB 251119A: SVOM detection of a possible burst
by GCN Circulars 19 Nov '25

19 Nov '25

TITLE: GCN CIRCULAR NUMBER: 42757 SUBJECT: GRB 251119A: SVOM detection of a possible burst DATE: 25/11/19 09:26:05 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> C. Wu (NAOC), K.X. Gong (CHO), D. Turpin, S. Schanne, D. Gotz (CEA), U. Jacob (LUPM) report on behalf of the SVOM mission team: At 2025-11-19T08:47:44 UTC (T0), SVOM/ECLAIRs triggered and located the gamma-ray burst GRB 251119A (SVOM burst-id sb25111901). The following trigger information was received on the ground with low latency by the SVOM VHF Alert Network. The burst was only detected by the Count-Rate Trigger (CRT), which produced a sequence of 3 alerts. CRT provided the alert with the best signal-to-noise-ratio in the image (SNR) of 7.89 in the [5-8] keV energy band over a time window of 20.40 seconds starting at 2025-11-19T08:47:23 (Tb). The localization of the best alert is R.A., Dec. 84.4289, 12.2431 degrees: R.A. (J2000) = 5h37m42.93s Dec. (J2000) = 12d14m35.17s with a 90% confidence level (C.L.) radius of 9.96 arcmin (including systematic error of 2 arcmin added in quadrature). We notice that the Crab is located near the border of the field of view and about 9.8 degrees away from the burst’s position with a SNR of 9.0 (similar to the burst’s SNR) in the sky image. SVOM slewed to the burst position. SVOM/MXT began observing the field at 08:51:08 UTC, 206 seconds after T0. Using onboard processed data, no source was detected in 225 seconds. The SVOM/MXT team is waiting for the full dataset to detect and localise the possible SVOM/MXT counterpart. VT began observing the field after the slew. The analysis of the data will be published in a future circular. 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 Chao Wu: cwu(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/42757. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40823] EP251118a: NOT spectroscopic redshift of z = 1.216
by GCN Circulars 19 Nov '25

19 Nov '25

TITLE: GCN CIRCULAR NUMBER: 42756 SUBJECT: EP251118a: NOT spectroscopic redshift of z = 1.216 DATE: 25/11/19 09:17:33 GMT FROM: J. An <jiean0813(a)foxmail.com> J. An (NAOC), D. B. Malesani (DAWN/NBI and Radboud), L.B. He, D. Xu, X.Liu (NAOC), G. Corcoran (UCD), L. Cotter (UCD), A. J. Levan (Radboud and Warwick), P. G. Jonker (Radboud), L. Fuglsang (NOT), report on behalf of a large collaboration: We observed the optical afterglow (Malesani et al., GCN 42751) of EP251118a (Jiang et al., GCN 42749) with the Nordic Optical Telescope (NOT) equipped with the ALFOSC camera. A spectrum using grism #4 was secured starting on 2025 Nov 19.19 UT (11.9 h after the GRB). A total of 4 spectra of 1200 s each were obtained, covering the wavelength range 3500-9600 AA. Preliminary reduction of the stacked spectrum shows a clear continuum down to at least 3700 AA. The lack of a Ly-alpha feature in the spectrum sets a redshift limit z < 2. A few narrow absorption features are detected, which we attribute to the Mg II doublet and several Fe II lines (2600, 2586, 2344), all at a common redshift of z = 1.216. We suggest this is the redshift of EP251118a. View this GCN Circular online at https://gcn.nasa.gov/circulars/42756. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40822] EP251118a: Global MASTER-Net observations report
by GCN Circulars 19 Nov '25

19 Nov '25

TITLE: GCN CIRCULAR NUMBER: 42755 SUBJECT: EP251118a: Global MASTER-Net observations report DATE: 25/11/19 08:27:23 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-OAFA robotic telescope [1] located in Argentina (OAFA observatory of San Juan National University) was pointed to the EP251118a ( EP Team et al., GCN 42749) errorbox 12817 sec after notice time and 54875 sec after trigger time at 2025-11-19 07:57:04 UT, with upper limit up to 20.2 mag. The observations began at zenith distance = 44 deg. The sun altitude is -17.5 deg. The galactic latitude b = 23 deg., longitude l = 213 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3046754 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 54905 | 2025-11-19 07:57:04 | MASTER-OAFA | (08h 12m 31.85s , +10d 55m 21.3s) | C | 60 | 20.2 | 54982 | 2025-11-19 07:58:20 | MASTER-OAFA | (08h 12m 38.49s , +10d 54m 18.7s) | C | 60 | 20.0 | 55059 | 2025-11-19 07:59:38 | MASTER-OAFA | (08h 12m 32.20s , +10d 53m 14.4s) | C | 60 | 20.0 | 55137 | 2025-11-19 08:00:55 | MASTER-OAFA | (08h 12m 37.33s , +10d 53m 29.6s) | C | 60 | 20.1 | 55223 | 2025-11-19 08:02:21 | MASTER-OAFA | (08h 12m 33.38s , +10d 54m 50.5s) | C | 60 | 20.2 | 55301 | 2025-11-19 08:03:39 | MASTER-OAFA | (08h 12m 32.94s , +10d 53m 07.3s) | C | 60 | 20.1 | 55408 | 2025-11-19 08:04:56 | MASTER-OAFA | (08h 12m 34.44s , +10d 54m 29.2s) | C | 120 | 20.0 | 55544 | 2025-11-19 08:07:13 | MASTER-OAFA | (08h 12m 28.30s , +10d 53m 45.7s) | C | 120 | 20.1 | 55681 | 2025-11-19 08:09:30 | MASTER-OAFA | (08h 12m 28.13s , +10d 54m 37.0s) | C | 120 | 20.0 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. [1] - V.M. Lipunov, V.G. Kornilov, E.S. Gorbovskoy, N.A. Tiurina & A.S.Kuznetsov, 2023, Astronomical Robotic Networks and Operative Multichanel Astrophysics, Lomonosov MSU PRESS, 591pp. http : // www.pereplet.ru/lipunov/625.html View this GCN Circular online at https://gcn.nasa.gov/circulars/42755. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40821] EP251118a: preliminary result of EP-FXT follow-up observation
by GCN Circulars 19 Nov '25

19 Nov '25

TITLE: GCN CIRCULAR NUMBER: 42754 SUBJECT: EP251118a: preliminary result of EP-FXT follow-up observation DATE: 25/11/19 07:36:46 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> R. Shi, Q. J. Huang, D. F. Hu (PMO, CAS), F. F. Song (YNAO, CAS), S. Q. Jiang (NAO, CAS), Q. C. Liu (THU), C. C. Jin (NAO, CAS) report on behalf of the Einstein Probe team: The Follow-up X-ray Telescope (FXT) on board the Einstein Probe (EP) performed one ToO observation for EP251118a, starting at 2025-11-19T04:02:14 (UTC). Within the WXT error circle, an uncatalogued X-ray source was detected at R.A. = 123.1677 deg, DEC = 10.9364 deg (J2000) with an uncertainty of 20 arcsec in radius (90% C.L. statistical and systematic). The position is consistent with the optical counterpart reported before (Malesani et al. GCN [42751](https://gcn.nasa.gov/circulars/42751)) with a seperation of 14.75 arcsec. Further information will be updated when the telemetry data is received. Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with X-ray follow-up capability (Yuan et al. 2022, Handbook of X-ray and Gamma-ray Astrophysics). View this GCN Circular online at https://gcn.nasa.gov/circulars/42754. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40820] LAT GRB251118.86: Global MASTER-Net observations report
by GCN Circulars 19 Nov '25

19 Nov '25

TITLE: GCN CIRCULAR NUMBER: 42753 SUBJECT: LAT GRB251118.86: Global MASTER-Net observations report DATE: 25/11/19 06:11:24 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-OAFA robotic telescope [1] located in Argentina (OAFA observatory of San Juan National University) was pointed to the LAT GRB251118.86 (trigger No 785190695,10h 40m 19.92s , -34d 34m 33.6s, R=0.173833) errorbox 972 sec after notice time and 28422 sec after trigger time at 2025-11-19 04:25:12 UT, with upper limit up to 19.1 mag. The observations began at zenith distance = 83 deg. The sun altitude is -39.6 deg. The galactic latitude b = 21 deg., longitude l = 275 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3046739 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 28452 | 2025-11-19 04:25:12 | MASTER-OAFA | (10h 40m 39.45s , -34d 39m 40.3s) | C | 60 | 13.8 | 28518 | 2025-11-19 04:26:18 | MASTER-OAFA | (10h 40m 39.40s , -34d 39m 38.3s) | C | 60 | 14.7 | 28584 | 2025-11-19 04:27:23 | MASTER-OAFA | (10h 40m 39.38s , -34d 39m 35.5s) | C | 60 | 15.0 | 28649 | 2025-11-19 04:28:29 | MASTER-OAFA | (10h 40m 39.39s , -34d 39m 32.7s) | C | 60 | 15.4 | 28715 | 2025-11-19 04:29:35 | MASTER-OAFA | (10h 40m 39.27s , -34d 39m 30.8s) | C | 60 | 15.7 | 28780 | 2025-11-19 04:30:40 | MASTER-OAFA | (10h 40m 39.19s , -34d 39m 28.4s) | C | 60 | 16.1 | 28846 | 2025-11-19 04:31:46 | MASTER-OAFA | (10h 40m 39.06s , -34d 39m 25.8s) | C | 60 | 16.2 | 28913 | 2025-11-19 04:32:52 | MASTER-OAFA | (10h 40m 38.91s , -34d 39m 23.6s) | C | 60 | 16.5 | 28978 | 2025-11-19 04:33:58 | MASTER-OAFA | (10h 40m 38.80s , -34d 39m 21.9s) | C | 60 | 16.5 | 29044 | 2025-11-19 04:35:03 | MASTER-OAFA | (10h 40m 38.68s , -34d 39m 19.9s) | C | 60 | 16.7 | 29110 | 2025-11-19 04:36:10 | MASTER-OAFA | (10h 40m 38.57s , -34d 39m 17.8s) | C | 60 | 17.0 | 29175 | 2025-11-19 04:37:15 | MASTER-OAFA | (10h 40m 38.40s , -34d 39m 16.0s) | C | 60 | 17.1 | 29241 | 2025-11-19 04:38:20 | MASTER-OAFA | (10h 40m 38.33s , -34d 39m 13.9s) | C | 60 | 17.3 | 29307 | 2025-11-19 04:39:26 | MASTER-OAFA | (10h 40m 38.21s , -34d 39m 12.1s) | C | 60 | 17.3 | 29372 | 2025-11-19 04:40:32 | MASTER-OAFA | (10h 40m 38.07s , -34d 39m 10.1s) | C | 60 | 17.3 | 29438 | 2025-11-19 04:41:38 | MASTER-OAFA | (10h 40m 37.93s , -34d 39m 08.0s) | C | 60 | 17.3 | 29504 | 2025-11-19 04:42:44 | MASTER-OAFA | (10h 40m 37.75s , -34d 39m 06.1s) | C | 60 | 17.6 | 29570 | 2025-11-19 04:43:49 | MASTER-OAFA | (10h 40m 37.59s , -34d 39m 04.2s) | C | 60 | 17.6 | 29635 | 2025-11-19 04:44:55 | MASTER-OAFA | (10h 40m 37.45s , -34d 39m 02.1s) | C | 60 | 17.6 | 29701 | 2025-11-19 04:46:01 | MASTER-OAFA | (10h 40m 37.31s , -34d 39m 00.4s) | C | 60 | 17.9 | 29767 | 2025-11-19 04:47:06 | MASTER-OAFA | (10h 40m 37.14s , -34d 38m 58.3s) | C | 60 | 17.9 | 29832 | 2025-11-19 04:48:12 | MASTER-OAFA | (10h 40m 36.96s , -34d 38m 56.4s) | C | 60 | 17.9 | 29899 | 2025-11-19 04:49:18 | MASTER-OAFA | (10h 40m 36.87s , -34d 38m 54.3s) | C | 60 | 17.9 | 29965 | 2025-11-19 04:50:24 | MASTER-OAFA | (10h 40m 36.75s , -34d 38m 52.3s) | C | 60 | 18.0 | 30030 | 2025-11-19 04:51:30 | MASTER-OAFA | (10h 40m 36.61s , -34d 38m 50.3s) | C | 60 | 18.0 | 30096 | 2025-11-19 04:52:36 | MASTER-OAFA | (10h 40m 36.50s , -34d 38m 48.1s) | C | 60 | 18.1 | 30162 | 2025-11-19 04:53:41 | MASTER-OAFA | (10h 40m 36.37s , -34d 38m 46.0s) | C | 60 | 18.2 | 30227 | 2025-11-19 04:54:47 | MASTER-OAFA | (10h 40m 36.23s , -34d 38m 44.6s) | C | 60 | 18.2 | 30293 | 2025-11-19 04:55:53 | MASTER-OAFA | (10h 40m 36.14s , -34d 38m 42.1s) | C | 60 | 18.3 | 30359 | 2025-11-19 04:56:58 | MASTER-OAFA | (10h 40m 36.02s , -34d 38m 40.1s) | C | 60 | 18.3 | 30424 | 2025-11-19 04:58:04 | MASTER-OAFA | (10h 40m 35.89s , -34d 38m 38.1s) | C | 60 | 18.4 | 30491 | 2025-11-19 04:59:10 | MASTER-OAFA | (10h 40m 35.75s , -34d 38m 36.2s) | C | 60 | 18.5 | 30556 | 2025-11-19 05:00:16 | MASTER-OAFA | (10h 40m 35.66s , -34d 38m 33.8s) | C | 60 | 18.5 | 30621 | 2025-11-19 05:01:21 | MASTER-OAFA | (10h 40m 35.53s , -34d 38m 31.4s) | C | 60 | 18.5 | 30687 | 2025-11-19 05:02:27 | MASTER-OAFA | (10h 40m 35.40s , -34d 38m 29.6s) | C | 60 | 18.6 | 30753 | 2025-11-19 05:03:32 | MASTER-OAFA | (10h 40m 35.26s , -34d 38m 27.7s) | C | 60 | 18.6 | 30818 | 2025-11-19 05:04:38 | MASTER-OAFA | (10h 40m 35.17s , -34d 38m 25.6s) | C | 60 | 18.6 | 30885 | 2025-11-19 05:05:44 | MASTER-OAFA | (10h 40m 35.05s , -34d 38m 23.5s) | C | 60 | 18.7 | 30950 | 2025-11-19 05:06:50 | MASTER-OAFA | (10h 40m 34.89s , -34d 38m 21.4s) | C | 60 | 18.7 | 31016 | 2025-11-19 05:07:55 | MASTER-OAFA | (10h 40m 34.75s , -34d 38m 19.4s) | C | 60 | 18.7 | 31082 | 2025-11-19 05:09:02 | MASTER-OAFA | (10h 40m 34.60s , -34d 38m 17.2s) | C | 60 | 18.7 | 31147 | 2025-11-19 05:10:07 | MASTER-OAFA | (10h 40m 34.49s , -34d 38m 15.4s) | C | 60 | 18.8 | 31213 | 2025-11-19 05:11:13 | MASTER-OAFA | (10h 40m 34.36s , -34d 38m 13.2s) | C | 60 | 18.8 | 31279 | 2025-11-19 05:12:19 | MASTER-OAFA | (10h 40m 34.23s , -34d 38m 11.3s) | C | 60 | 18.8 | 31345 | 2025-11-19 05:13:24 | MASTER-OAFA | (10h 40m 34.10s , -34d 38m 09.0s) | C | 60 | 18.8 | 31410 | 2025-11-19 05:14:30 | MASTER-OAFA | (10h 40m 33.98s , -34d 38m 07.1s) | C | 60 | 18.9 | 31476 | 2025-11-19 05:15:36 | MASTER-OAFA | (10h 40m 33.86s , -34d 38m 04.6s) | C | 60 | 18.9 | 31542 | 2025-11-19 05:16:41 | MASTER-OAFA | (10h 40m 33.76s , -34d 38m 02.4s) | C | 60 | 18.9 | 31607 | 2025-11-19 05:17:47 | MASTER-OAFA | (10h 40m 33.66s , -34d 38m 00.3s) | C | 60 | 18.9 | 31673 | 2025-11-19 05:18:52 | MASTER-OAFA | (10h 40m 33.53s , -34d 37m 58.3s) | C | 60 | 18.9 | 31738 | 2025-11-19 05:19:58 | MASTER-OAFA | (10h 40m 33.38s , -34d 37m 56.0s) | C | 60 | 18.9 | 31804 | 2025-11-19 05:21:03 | MASTER-OAFA | (10h 40m 33.26s , -34d 37m 53.7s) | C | 60 | 18.9 | 31870 | 2025-11-19 05:22:10 | MASTER-OAFA | (10h 40m 33.13s , -34d 37m 51.8s) | C | 60 | 18.9 | 31936 | 2025-11-19 05:23:16 | MASTER-OAFA | (10h 40m 33.01s , -34d 37m 49.6s) | C | 60 | 18.9 | 32002 | 2025-11-19 05:24:21 | MASTER-OAFA | (10h 40m 32.90s , -34d 37m 47.5s) | C | 60 | 18.9 | 32068 | 2025-11-19 05:25:27 | MASTER-OAFA | (10h 40m 32.77s , -34d 37m 45.1s) | C | 60 | 19.0 | 32133 | 2025-11-19 05:26:33 | MASTER-OAFA | (10h 40m 32.64s , -34d 37m 42.8s) | C | 60 | 18.9 | 32198 | 2025-11-19 05:27:38 | MASTER-OAFA | (10h 40m 32.50s , -34d 37m 40.9s) | C | 60 | 18.9 | 32265 | 2025-11-19 05:28:44 | MASTER-OAFA | (10h 40m 32.41s , -34d 37m 38.8s) | C | 60 | 18.9 | 32330 | 2025-11-19 05:29:50 | MASTER-OAFA | (10h 40m 32.29s , -34d 37m 36.8s) | C | 60 | 19.0 | 32396 | 2025-11-19 05:30:55 | MASTER-OAFA | (10h 40m 32.17s , -34d 37m 34.7s) | C | 60 | 19.0 | 32462 | 2025-11-19 05:32:01 | MASTER-OAFA | (10h 40m 32.05s , -34d 37m 32.6s) | C | 60 | 19.0 | 32527 | 2025-11-19 05:33:07 | MASTER-OAFA | (10h 40m 31.94s , -34d 37m 30.3s) | C | 60 | 19.0 | 32592 | 2025-11-19 05:34:12 | MASTER-OAFA | (10h 40m 31.81s , -34d 37m 28.3s) | C | 60 | 19.0 | 32659 | 2025-11-19 05:35:18 | MASTER-OAFA | (10h 40m 31.72s , -34d 37m 26.0s) | C | 60 | 19.0 | 32724 | 2025-11-19 05:36:24 | MASTER-OAFA | (10h 40m 31.62s , -34d 37m 24.0s) | C | 60 | 19.0 | 32790 | 2025-11-19 05:37:29 | MASTER-OAFA | (10h 40m 31.49s , -34d 37m 22.0s) | C | 60 | 19.0 | 32856 | 2025-11-19 05:38:36 | MASTER-OAFA | (10h 40m 31.39s , -34d 37m 19.8s) | C | 60 | 19.0 | 32922 | 2025-11-19 05:39:41 | MASTER-OAFA | (10h 40m 31.28s , -34d 37m 17.6s) | C | 60 | 19.0 | 32987 | 2025-11-19 05:40:47 | MASTER-OAFA | (10h 40m 31.23s , -34d 37m 15.6s) | C | 60 | 19.0 | 33053 | 2025-11-19 05:41:53 | MASTER-OAFA | (10h 40m 31.08s , -34d 37m 13.4s) | C | 60 | 19.1 | 33118 | 2025-11-19 05:42:58 | MASTER-OAFA | (10h 40m 31.04s , -34d 37m 11.1s) | C | 60 | 19.0 | 33184 | 2025-11-19 05:44:03 | MASTER-OAFA | (10h 40m 30.92s , -34d 37m 09.5s) | C | 60 | 19.0 | 33250 | 2025-11-19 05:45:10 | MASTER-OAFA | (10h 40m 30.85s , -34d 37m 07.0s) | C | 60 | 19.0 | 33316 | 2025-11-19 05:46:15 | MASTER-OAFA | (10h 40m 30.75s , -34d 37m 05.0s) | C | 60 | 19.0 | 33381 | 2025-11-19 05:47:21 | MASTER-OAFA | (10h 40m 30.69s , -34d 37m 03.0s) | C | 60 | 19.0 | 33448 | 2025-11-19 05:48:28 | MASTER-OAFA | (10h 40m 30.59s , -34d 37m 00.4s) | C | 60 | 19.1 | 33513 | 2025-11-19 05:49:33 | MASTER-OAFA | (10h 40m 30.50s , -34d 36m 58.5s) | C | 60 | 19.0 | 33579 | 2025-11-19 05:50:38 | MASTER-OAFA | (10h 40m 30.45s , -34d 36m 56.3s) | C | 60 | 19.1 | 33645 | 2025-11-19 05:51:44 | MASTER-OAFA | (10h 40m 30.39s , -34d 36m 54.0s) | C | 60 | 19.0 | 33710 | 2025-11-19 05:52:50 | MASTER-OAFA | (10h 40m 30.29s , -34d 36m 51.8s) | C | 60 | 19.0 | 33776 | 2025-11-19 05:53:56 | MASTER-OAFA | (10h 40m 30.20s , -34d 36m 50.0s) | C | 60 | 19.0 | 33842 | 2025-11-19 05:55:02 | MASTER-OAFA | (10h 40m 30.14s , -34d 36m 47.5s) | C | 60 | 19.0 | 33908 | 2025-11-19 05:56:08 | MASTER-OAFA | (10h 40m 30.05s , -34d 36m 45.1s) | C | 60 | 19.1 | 33973 | 2025-11-19 05:57:13 | MASTER-OAFA | (10h 40m 29.97s , -34d 36m 43.0s) | C | 60 | 19.0 | 34039 | 2025-11-19 05:58:19 | MASTER-OAFA | (10h 40m 29.87s , -34d 36m 40.9s) | C | 60 | 19.0 | 34104 | 2025-11-19 05:59:24 | MASTER-OAFA | (10h 40m 29.79s , -34d 36m 38.4s) | C | 60 | 19.0 | 34169 | 2025-11-19 06:00:29 | MASTER-OAFA | (10h 40m 29.72s , -34d 36m 36.7s) | C | 60 | 19.0 | 34236 | 2025-11-19 06:01:35 | MASTER-OAFA | (10h 40m 29.62s , -34d 36m 34.4s) | C | 60 | 19.0 | 34302 | 2025-11-19 06:02:41 | MASTER-OAFA | (10h 40m 29.57s , -34d 36m 32.4s) | C | 60 | 19.0 | 34367 | 2025-11-19 06:03:47 | MASTER-OAFA | (10h 40m 29.51s , -34d 36m 29.9s) | C | 60 | 19.0 | 34433 | 2025-11-19 06:04:53 | MASTER-OAFA | (10h 40m 29.42s , -34d 36m 27.6s) | C | 60 | 19.0 | 34499 | 2025-11-19 06:05:58 | MASTER-OAFA | (10h 40m 29.36s , -34d 36m 25.3s) | C | 60 | 19.0 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. [1] - V.M. Lipunov, V.G. Kornilov, E.S. Gorbovskoy, N.A. Tiurina & A.S.Kuznetsov, 2023, Astronomical Robotic Networks and Operative Multichanel Astrophysics, Lomonosov MSU PRESS, 591pp. http : // www.pereplet.ru/lipunov/625.html View this GCN Circular online at https://gcn.nasa.gov/circulars/42753. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40819] GRB 251118A: Fermi-LAT detection
by GCN Circulars 19 Nov '25

19 Nov '25

TITLE: GCN CIRCULAR NUMBER: 42752 SUBJECT: GRB 251118A: Fermi-LAT detection DATE: 25/11/19 05:39:12 GMT FROM: Rahul Gupta at NASA GSFC <rahul.gupta(a)nasa.gov> R. Gupta (NASA GSFC) and T. Khalil (Univ. of Johannesburg) report on behalf of the Fermi-LAT Collaboration: On November 18 2025, Fermi-LAT detected high-energy emission from GRB 251118A, which was also detected by Fermi-GBM (trigger 785190695 / 251118855, GCN 42743). The best LAT on-ground location is found to be: RA, Dec = 160.08, -34.58 (J2000) with an error radius of 0.17 deg (90 % containment, statistical error only). This was 69 deg from the LAT boresight at the time of the GBM trigger (T0 = 20:31:30.09 UT). The data from the Fermi-LAT shows a significant increase in the event rate that is spatially and temporally correlated with the GBM emission with high significance. The photon flux above 100 MeV in the time interval 0 - 1.5 ks after the GBM trigger is (1.8 ± 0.7) E-6 ph/cm2/s. The estimated photon index above 100 MeV is -1.8 ± 0.3. The highest-energy photon is a 6.8 GeV event which is observed ~1400 seconds after the GBM trigger. A Swift ToO has been approved for this burst. The Fermi-LAT point of contact for this burst is Aldana Holzmann Airasca (a.holzmannairasca(a)unitn.it) The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden. View this GCN Circular online at https://gcn.nasa.gov/circulars/42752. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40818] EP251118a: NOT candidate optical counterpart
by GCN Circulars 19 Nov '25

19 Nov '25

TITLE: GCN CIRCULAR NUMBER: 42751 SUBJECT: EP251118a: NOT candidate optical counterpart DATE: 25/11/19 05:20:57 GMT FROM: Daniele Bjørn Malesani at Cosmic Dawn Center, Niels Bohr Institute <daniele.malesani(a)nbi.ku.dk> D. B. Malesani (DAWN/NBI and Radboud), G. Corcoran (UCD), L. Cotter (UCD), J. An, Z.P. Zhu, D. Xu (NAOC), P. G. Jonker (Radboud), L. Fuglsang (NOT), report on behalf of a larger collaboration: We observed the field of the transient event EP251118a (Jiang et al., GCN 42749) detected by the Einstein Probe Wide-field X-ray Telescope (EP WXT), using the Nordic Optical Telescope (NOT) equipped with the ALFOSC camera. Observations were obtained in the r (3x300 s) and z (5x200 s) bands, starting on 2025-11-19 at 03:55:38 UT (11.22 hr after the EP/WXT trigger). In our first r-band exposure, within the WXT uncertainty region, we detect a source significantly brighter than in the archival images from the Legacy Survey. This object has coordinates: RA(J2000): 08:12:39.4 Dec(J2000): +10:56:18.88 with an uncertainty of 0.5" in both RA and Dec. In the NOT image, we measure an AB magnitude of r = 20.52+/-0.04, calibrated against the Pan-STARRS catalog and not corrected for Galactic extinction. At this location, a source can be marginally seen in the deeper Legacy Source images, with an AB magnitude of r = 24.18 +/- 0.26. The source seen in the NOT images is a candidate optical afterglow of EP251118a, and the archival counterpart in the Legacy Survey is its candidate host galaxy. Further multi-wavelength observations are encouraged to confirm the nature of this object. View this GCN Circular online at https://gcn.nasa.gov/circulars/42751. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 40817] EP251118a: NOT candidate optical counterpart
by GCN Circulars 19 Nov '25

19 Nov '25

TITLE: GCN CIRCULAR NUMBER: 42751 SUBJECT: EP251118a: NOT candidate optical counterpart DATE: 25/11/19 05:20:57 GMT FROM: Daniele Bjørn Malesani at Cosmic Dawn Center, Niels Bohr Institute <daniele.malesani(a)nbi.ku.dk> D. B. Malesani (DAWN/NBI and Radboud), G. Corcoran (UCD), L. Cotter (UCD), J. An, Z.P. Zhu, D. Xu (NAOC), P. G. Jonker (Radboud), L. Fuglsang (NOT), report on behalf of a larger collaboration: We observed the field of the transient event EP251118a (Jiang et al., GCN 42749) detected by the Einstein Probe Wide-field X-ray Telescope (EP WXT), using the Nordic Optical Telescope (NOT) equipped with the ALFOSC camera. Observations were obtained in the r (3x300 s) and z (5x200 s) bands, starting on 2025-11-19 at 03:55:38 UT (11.22 hr after the EP/WXT trigger). In our first r-band exposure, within the WXT uncertainty region, we detect a source significantly brighter than in the archival images from the Legacy Survey. This object has coordinates: RA(J2000): 08:12:39.4 Dec(J2000): +10:56:18.88 with an uncertainty of 0.5" in both RA and Dec. In the NOT image, we measure an AB magnitude of r = 20.52+/-0.04, calibrated against the Pan-STARRS catalog and not corrected for Galactic extinction. At this location, a source can be marginally seen in the deeper Legacy Source images, with an AB magnitude of r = 24.18 +/- 0.26. The source seen in the NOT images is a candidate optical afterglow of EP251118a, and the archival counterpart in the Legacy Survey is its candidate host galaxy. Further multi-wavelength observations are encouraged to confirm the nature of this object. View this GCN Circular online at https://gcn.nasa.gov/circulars/42751. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

1 0