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[vsnet-grb-info 41549] EP260119a: Global MASTER-Net observations report
by GCN Circulars 19 Jan '26

19 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43454 SUBJECT: EP260119a: Global MASTER-Net observations report DATE: 26/01/19 17:36:27 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-Tunka robotic telescope [1] located in Russia (Applied Physics Institute, Irkutsk State University) was pointed to the EP260119a ( EP Team et al., GCN 43447) errorbox 32012 sec after notice time and 60248 sec after trigger time at 2026-01-19 16:57:56 UT, with upper limit up to 20.4 mag. The observations began at zenith distance = 26 deg. The sun altitude is -59.1 deg. The galactic latitude b = 46 deg., longitude l = 143 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3107348 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 60279 | 2026-01-19 16:57:56 | MASTER-Tunka | (10h 31m 16.45s , +66d 08m 29.3s) | C | 60 | 20.3 | 60279 | 2026-01-19 16:57:56 | MASTER-Tunka | (10h 29m 47.72s , +66d 16m 01.1s) | C | 60 | 20.0 | 60352 | 2026-01-19 16:59:09 | MASTER-Tunka | (10h 31m 09.89s , +66d 07m 36.5s) | C | 60 | 20.4 | 60352 | 2026-01-19 16:59:09 | MASTER-Tunka | (10h 29m 41.26s , +66d 15m 08.6s) | C | 60 | 20.0 | 60427 | 2026-01-19 17:00:24 | MASTER-Tunka | (10h 31m 09.54s , +66d 08m 35.2s) | C | 60 | 20.3 | 60427 | 2026-01-19 17:00:24 | MASTER-Tunka | (10h 29m 40.79s , +66d 16m 07.0s) | C | 60 | 20.0 | 60507 | 2026-01-19 17:01:44 | MASTER-Tunka | (10h 31m 15.00s , +66d 07m 33.2s) | C | 60 | 20.4 | 60507 | 2026-01-19 17:01:44 | MASTER-Tunka | (10h 29m 46.20s , +66d 15m 05.6s) | C | 60 | 19.9 | 60580 | 2026-01-19 17:02:57 | MASTER-Tunka | (10h 31m 07.97s , +66d 06m 32.0s) | C | 60 | 20.4 | 60580 | 2026-01-19 17:02:57 | MASTER-Tunka | (10h 29m 39.21s , +66d 14m 03.9s) | C | 60 | 19.9 | 60653 | 2026-01-19 17:04:11 | MASTER-Tunka | (10h 31m 13.12s , +66d 06m 55.4s) | C | 60 | 20.4 | 60653 | 2026-01-19 17:04:11 | MASTER-Tunka | (10h 29m 44.32s , +66d 14m 27.1s) | C | 60 | 20.0 | 60729 | 2026-01-19 17:05:27 | MASTER-Tunka | (10h 31m 10.06s , +66d 08m 03.1s) | C | 60 | 20.4 | 60729 | 2026-01-19 17:05:27 | MASTER-Tunka | (10h 29m 41.17s , +66d 15m 34.4s) | C | 60 | 20.0 | 60815 | 2026-01-19 17:06:52 | MASTER-Tunka | (10h 31m 09.77s , +66d 06m 47.2s) | C | 60 | 20.3 | 60815 | 2026-01-19 17:06:52 | MASTER-Tunka | (10h 29m 40.81s , +66d 14m 18.8s) | C | 60 | 19.9 | 60887 | 2026-01-19 17:08:05 | MASTER-Tunka | (10h 31m 13.15s , +66d 08m 15.5s) | C | 60 | 20.4 | 60887 | 2026-01-19 17:08:05 | MASTER-Tunka | (10h 29m 44.02s , +66d 15m 47.0s) | C | 60 | 20.0 | 60961 | 2026-01-19 17:09:18 | MASTER-Tunka | (10h 31m 05.28s , +66d 07m 24.6s) | C | 60 | 20.4 | 60961 | 2026-01-19 17:09:18 | MASTER-Tunka | (10h 29m 36.21s , +66d 14m 55.7s) | C | 60 | 20.0 | 61036 | 2026-01-19 17:10:34 | MASTER-Tunka | (10h 31m 05.02s , +66d 08m 23.0s) | C | 60 | 20.4 | 61036 | 2026-01-19 17:10:34 | MASTER-Tunka | (10h 29m 35.82s , +66d 15m 54.2s) | C | 60 | 20.0 | 61111 | 2026-01-19 17:11:48 | MASTER-Tunka | (10h 31m 11.19s , +66d 07m 21.5s) | C | 60 | 20.4 | 61111 | 2026-01-19 17:11:49 | MASTER-Tunka | (10h 29m 41.99s , +66d 14m 52.8s) | C | 60 | 19.9 | 61186 | 2026-01-19 17:13:04 | MASTER-Tunka | (10h 31m 05.60s , +66d 06m 19.1s) | C | 60 | 20.4 | 61186 | 2026-01-19 17:13:04 | MASTER-Tunka | (10h 29m 36.47s , +66d 13m 50.5s) | C | 60 | 20.0 | 61262 | 2026-01-19 17:14:19 | MASTER-Tunka | (10h 31m 09.69s , +66d 06m 22.9s) | C | 60 | 20.4 | 61262 | 2026-01-19 17:14:19 | MASTER-Tunka | (10h 29m 40.43s , +66d 13m 54.9s) | C | 60 | 20.0 | 61335 | 2026-01-19 17:15:33 | MASTER-Tunka | (10h 31m 06.90s , +66d 07m 57.6s) | C | 60 | 20.4 | 61335 | 2026-01-19 17:15:33 | MASTER-Tunka | (10h 29m 37.54s , +66d 15m 48.4s) | C | 60 | 19.7 | 61409 | 2026-01-19 17:16:47 | MASTER-Tunka | (10h 31m 06.53s , +66d 06m 43.7s) | C | 60 | 20.3 | 61409 | 2026-01-19 17:16:47 | MASTER-Tunka | (10h 29m 37.16s , +66d 14m 35.6s) | C | 60 | 19.9 | 61483 | 2026-01-19 17:18:00 | MASTER-Tunka | (10h 31m 08.49s , +66d 07m 46.8s) | C | 60 | 20.3 | 61483 | 2026-01-19 17:18:00 | MASTER-Tunka | (10h 29m 38.92s , +66d 15m 38.1s) | C | 60 | 20.0 | 61558 | 2026-01-19 17:19:15 | MASTER-Tunka | (10h 31m 03.24s , +66d 07m 11.2s) | C | 60 | 20.4 | 61558 | 2026-01-19 17:19:16 | MASTER-Tunka | (10h 29m 33.66s , +66d 15m 02.3s) | C | 60 | 20.0 | 61631 | 2026-01-19 17:20:28 | MASTER-Tunka | (10h 31m 03.39s , +66d 08m 09.2s) | C | 60 | 20.4 | 61631 | 2026-01-19 17:20:28 | MASTER-Tunka | (10h 29m 33.60s , +66d 16m 00.6s) | C | 60 | 19.9 | 61703 | 2026-01-19 17:21:41 | MASTER-Tunka | (10h 29m 38.69s , +66d 14m 59.2s) | C | 60 | 20.0 | 61703 | 2026-01-19 17:21:41 | MASTER-Tunka | (10h 31m 08.49s , +66d 07m 07.4s) | C | 60 | 20.4 | 61777 | 2026-01-19 17:22:55 | MASTER-Tunka | (10h 31m 01.86s , +66d 06m 05.4s) | C | 60 | 20.4 | 61777 | 2026-01-19 17:22:55 | MASTER-Tunka | (10h 29m 32.07s , +66d 13m 57.0s) | C | 60 | 19.9 | 61852 | 2026-01-19 17:24:09 | MASTER-Tunka | (10h 31m 08.12s , +66d 06m 25.5s) | C | 60 | 20.3 | 61852 | 2026-01-19 17:24:09 | MASTER-Tunka | (10h 29m 38.21s , +66d 14m 17.5s) | C | 60 | 19.9 | 61925 | 2026-01-19 17:25:23 | MASTER-Tunka | (10h 31m 04.08s , +66d 07m 59.9s) | C | 60 | 20.4 | 61926 | 2026-01-19 17:25:23 | MASTER-Tunka | (10h 29m 34.06s , +66d 15m 51.6s) | C | 60 | 19.9 | 61999 | 2026-01-19 17:26:36 | MASTER-Tunka | (10h 31m 03.79s , +66d 06m 09.1s) | C | 60 | 20.4 | 61999 | 2026-01-19 17:26:36 | MASTER-Tunka | (10h 29m 33.75s , +66d 14m 01.0s) | C | 60 | 19.9 | 62072 | 2026-01-19 17:27:49 | MASTER-Tunka | (10h 31m 06.81s , +66d 07m 44.6s) | C | 60 | 20.4 | 62072 | 2026-01-19 17:27:49 | MASTER-Tunka | (10h 29m 36.65s , +66d 15m 36.3s) | C | 60 | 20.0 | 62145 | 2026-01-19 17:29:03 | MASTER-Tunka | (10h 30m 59.37s , +66d 06m 57.6s) | C | 60 | 20.4 | 62145 | 2026-01-19 17:29:03 | MASTER-Tunka | (10h 29m 29.23s , +66d 14m 49.2s) | C | 60 | 20.0 | 62225 | 2026-01-19 17:30:23 | MASTER-Tunka | (10h 31m 00.13s , +66d 07m 55.9s) | C | 60 | 20.4 | 62225 | 2026-01-19 17:30:23 | MASTER-Tunka | (10h 29m 29.89s , +66d 15m 47.5s) | C | 60 | 19.9 | 62299 | 2026-01-19 17:31:37 | MASTER-Tunka | (10h 31m 06.28s , +66d 06m 54.1s) | C | 60 | 20.4 | 62299 | 2026-01-19 17:31:37 | MASTER-Tunka | (10h 29m 36.01s , +66d 14m 45.6s) | C | 60 | 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/43454. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41548] GRB 260115A: AstroSat CZTI detection
by GCN Circulars 19 Jan '26

19 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43453 SUBJECT: GRB 260115A: AstroSat CZTI detection DATE: 26/01/19 16:33:28 GMT FROM: Anuraag Arya at IIT Bombay <aryaanuraag910(a)gmail.com> A. Arya (IITB), A. Goyal (IITB), M. Tembhurnikar (IUCAA), S. Salunke (IUCAA), Harsha K. H. (IUCAA), G. Waratkar (Caltech/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 260115A which was also detected by Fermi GBM (Fermi GBM Team, GCN Circ. 43417), and GECAM-B (Zhang et. al., GCN Circ. 43434). The source was faintly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve peaks at 2026-01-15 17:46:47.72 UTC. The measured peak count rate associated with the burst is 252 (+64, -69) counts/s above the background in the combined data of all quadrants, with a total of 270 (+117, -120) counts. The local mean background count rate was 1327 (+9, -12) counts/s. Due to the intrinsic 1 s binning of veto data, we cannot reliably estimate a T90 for our detection. 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 View this GCN Circular online at https://gcn.nasa.gov/circulars/43453. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41547] EP260119a: LCO optical observations
by GCN Circulars 19 Jan '26

19 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43452 SUBJECT: EP260119a: LCO optical observations DATE: 26/01/19 13:02:37 GMT FROM: Daniele Bjørn Malesani at Cosmic Dawn Center, Niels Bohr Institute <daniele.malesani(a)nbi.ku.dk> R. A. J. Eyles-Ferris (Leicester), J. A. Quirola-Vasquez (Radboud), G. Corcoran (UCD), D. B. Malesani (DAWN-NBI and Radboud), A. van Hoof (Radboud), A. Martin-Carrillo (UCD), P. G. Jonker (Radboud), A. J. Levan (Radboud and Warwick) report on behalf of a larger group: We observed the field of the fast X-ray transient EP260119a (Jiang et al., GCN 43447; Cheng et al., GCN 43449) using an LCO 1m telescope located at the McDonald Observatory (Texas, USA) equipped with the SINISTRO instrument. A series of 3x300 s exposures was taken in each of the SDSS-r and SDSS-z filters, starting on 2026-01-19 at 09:40:45 UT (9.45 hr after the trigger). The optical counterpart discovered by COLIBRÍ (Fortin et al., GCN 43450) is detected in our images, with magnitudes: r = 22.83 +- 0.33 (9.54 hr after trigger) z = 20.26 +- 0.13 (9.81 hr after trigger) These values are in the AB system, are calibrated against the Pan-STARRS survey, and are not corrected for Galactic extinction. Our measurements confirm the red r-z color of the afterglow (Fortin et al., GCN 43450). No host galaxy is detected in the r band in a stack of archival CFHT images, down to a limiting magnitude r > 24.5. View this GCN Circular online at https://gcn.nasa.gov/circulars/43452. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41546] GRB 260117A: ZTSh optical upper limit
by GCN Circulars 19 Jan '26

19 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43451 SUBJECT: GRB 260117A: ZTSh optical upper limit DATE: 26/01/19 11:53:13 GMT FROM: Alina Volnova at IKI RAS <alinusss(a)gmail.com> A. A. Volnova (IKI), V. Rumyantsev (CrAO), N. Pankov (HSE, IKI), A. S. Pozanenko (IKI) report on behalf of IKI-GRB-FuN: We observed the field of the SVOM GRB 260117A (Palmerio et al., GCN Circ. 43437) with the ZTSH telescope of CrAO starting on 2026-01-18 at 20:50:34 UT and taking several 120s exposures in R-band. At the position of the source detected by Swift/XRT (Salvaggio et al., GCN 43439; Evans et al., GCN 43438) we do not detect the optical source reported previously by SVOM/VT (Li et al., GCN Circ. 43441) and SVOM/COLIBRÍ (FM-GFT; Fortin et al., GCN 43445). Preliminary photometry is the following: Date UT start t-T0 Exp. Filter Obj. Err. UL Site/Telescope (mid,days) (n*s) (3sigma) 2026-01-18 20:50:34 1.07354 37*120 R n/d n/d 23.2 CrAO/ZTSh The photometry is based on nearby stars from the USNO-B1 catalogue (R2 magnitudes) and is not corrected for the Galactic extinction. View this GCN Circular online at https://gcn.nasa.gov/circulars/43451. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41545] EP260119a: COLIBRÍ optical counterpart candidate
by GCN Circulars 19 Jan '26

19 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43450 SUBJECT: EP260119a: COLIBRÍ optical counterpart candidate DATE: 26/01/19 11:36:14 GMT FROM: F. Fortin at IRAP <ffortin.sci.edu(a)gmail.com> Francis Fortin (IRAP), Leonardo García García (UNAM), Jean-Grégoire Ducoin (CPPM), Stéphane Basa (UAR Pytheas), William H. Lee (UNAM), Alan M. Watson (UNAM), Jean-Luc Atteia (IRAP), Camila Angulo (UNAM), Dalya Akl (NYUAD), Sarah Antier (IJCLAB), Rosa L. Becerra (UNAM), Nathaniel R. Butler (ASU), Damien Dornic (CPPM), Ramandeep Gill (UNAM), Noémie Globus (UNAM), Kin Ocelotl López (UNAM), Diego López-Cámara (UNAM), Francesco Magnani (CPPM), Enrique Moreno Méndez (UNAM), Margarita Pereyra (UNAM), Ny Avo Rakotondrainibe (LAM), Benjamin Schneider (LAM), Fredd Sánchez Álvarez (UNAM), and Antonio de Ugarte Postigo (LAM): We imaged the field of EP260119a (Jiang et al., GCN Circ. 43447) using the DDRAGO two-channel wide-field imager on the COLIBRÍ telescope. We observed from 2026-01-19T09:00:10 to 09:43:40 UTC (from 8.7 to 9.5 hours after the trigger) and obtained 32 minutes of simultaneous exposure in the r and z filters. The data were reduced and coadded with the COLIBRÍ pipelines and analysed with STDWeb/STDPipe (Karpov 2025). The photometry was calibrated using nearby stars from the PanSTARRS DR1 catalog, is in the AB system, and is not corrected for Galactic extinction. We detect an uncatalogued source (revealed by image subtraction using PanSTARRS as template) and consistent with the WXT 2.3 arcmin error circle and located 8 arcsec away from the FXT position (20 arcsec error circle, Cheng et al., GCN Circ 43449) at: RA(J2000) = 10:32:24.4 = 158.1018 degrees Dec(J2000) = +65:29:44.2 = +65.4956 degrees with an uncertainty of 0.5 arcsec. The preliminary magnitudes for this source are: r = 23.02 +/- 0.14 z = 20.08 +/- 0.03 This source is a good candidate for being the optical counterpart of EP260119a, and we encourage further observations to confirm its nature. We also note that the candidate is very red, which could indicate a source located at high redshift. Further observations with COLIBRÍ are ongoing. We thank the staff of the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir and the COLIBRÍ and DDRAGO engineering teams. COLIBRÍ is an astronomical observatory developed and operated jointly by France (AMU, CNES and CNRS) and Mexico (UNAM and SECIHTI). It is located at the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir, Baja California, Mexico. View this GCN Circular online at https://gcn.nasa.gov/circulars/43450. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41544] EP260119a: preliminary result from the EP-FXT observation
by GCN Circulars 19 Jan '26

19 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43449 SUBJECT: EP260119a: preliminary result from the EP-FXT observation DATE: 26/01/19 09:24:28 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> Y.H. Cheng (SWIFAR,YNU), Y. H. Jiang (NJU), D. Zhu, K.J. Zhang (SWIFAR,YNU), R. X. Hu (WHU)，H. Sun (NAO, CAS) report on behalf of the Einstein Probe team We performed a follow-up observation of EP260119a (detected by EP-WXT Jiang et al ., GCN #43447 ), with the Follow-up X-ray Telescope (FXT) on board the Einstein Probe (EP) mission. The observation began at 2026-01-19T07:21:31 UTC, about 7 hours after the detection. The FXT onboard alert shows that one uncatalogued source was detected by both FXT-A and FXT-B. The position of the source is R.A. = 158.1047 deg, DEC = 65.4975 deg, (J2000) with an uncertainty of 20 arcsec in radius (90% C.L. statistical and systematic). The estimated flux in the 0.5-10 keV band inferred from the alert information is around 5.0 x 10^-13 erg/cm^2/s. More 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). EP is a mission of the Chinese Academy of Sciences in collaboration with ESA, MPE and CNES. View this GCN Circular online at https://gcn.nasa.gov/circulars/43449. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41543] GRB 260110A: SVOM detection of a burst through offline search
by GCN Circulars 19 Jan '26

19 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43448 SUBJECT: GRB 260110A: SVOM detection of a burst through offline search DATE: 26/01/19 08:24:17 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> M. Brunet, O. Godet (IRAP), N. Dagoneau (CEA) report on behalf of the SVOM team: The SVOM/ECLAIRs telescope detected a transient source, labelled GRB 260110A, starting at 2026-01-10T03:28:54.35 UTC (T0), through an offline search with the event-by-event data downloaded through the X-band ground station. The burst was detected within several energy ranges and timescales. The best detection is obtained by the onground Image Trigger (IMT) with a signal-to-noise ratio of 7.1 within 4-20 keV over a time window of 20.48 seconds starting at T0-20.48s. The event is also seen by the onboard trigger but below the alert threshold. The lightcurve shows a single peaked structure lasting around 20 s. The localization of the source is RA, Dec = 333.649, 34.236 degrees: RA (J2000) = 22h14m35.76s Dec (J2000) = 34d14m09.60s with a 90% C.L. radius of 12.4 arcmin (including systematic error of 6 arcmin added in quadrature). We note that no bright catalogued X-ray sources are found in the error box. The time-averaged spectrum from T0-18.5 s to T0+1.5 s in the energy range 5-50 keV is best fitted by a power law. The powerlaw index is -1.77 -0.29/+0.33. With this model, the total fluence in 4-120 keV is (2.95 +0.32/-1.63)e-7 erg/cm^2. All quoted errors are at the 68% confidence level. The Space 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 APC, CEA, CNES, and IRAP. The SVOM point of contact for this event is : Marius Brunet : marius.brunet at irap.omp.eu Please contact him by email if you require additional information regarding the SVOM follow-up of this burst. View this GCN Circular online at https://gcn.nasa.gov/circulars/43448. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41542] EP260119a: EP-WXT detection of a fast X-ray transient
by GCN Circulars 19 Jan '26

19 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43447 SUBJECT: EP260119a: EP-WXT detection of a fast X-ray transient DATE: 26/01/19 08:03:26 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> Y. H. Jiang (NJU), D. Zhu, K.J. Zhang ,Y.H. Cheng (SWIFAR,YNU), R. X. Hu (WHU)，H. Sun (NAO, CAS) on behalf of the Einstein Probe (EP) team: We report on the detection of a fast X-ray transient by the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) mission, designated EP260119a. The source has a signal-to-noise ratio of 7.5. But the total number of counts is insufficient to trigger the WXT on-board trigger unit. The event started at 2026-01-19T00:13:48 (UTC) and lasted for almost 300 seconds. The WXT position of the source is R.A. = 158.082 deg, DEC = 65.505 deg (J2000) with an uncertainty of 2.3 arcmin in radius (90% C.L. statistical and systematic). The average WXT 0.5-4 keV spectrum can be fitted with an absorbed power law with a photon index of 1.8(-/+0.6) and with a fixed galactic hydrogen column density of 1.2 x 10^20 cm^-2. The derived average unabsorbed 0.5-4 keV flux is 4.4 (-1.3/+1.8) x 10^-11 erg/s/cm^2. The peak flux in the 0.5-4 keV band reaches 4.8 x 10^-10 erg/s/cm^2. The uncertainties are at the 90% confidence level for the above parameters. The stellar flare origin can not be fully ruled out. A follow-up observation with EP-FXT has been scheduled. 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/43447. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41541] Swift GRB260118.48: Global MASTER-Net observations report
by GCN Circulars 18 Jan '26

18 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43446 SUBJECT: Swift GRB260118.48: Global MASTER-Net observations report DATE: 26/01/18 20:38:22 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-SAAO robotic telescope [1] located in South Africa (South African Astronomical Observatory) was pointed to the Swift GRB260118.48 (trigger No 1442056,11h 20m 55.22s , -61d 54m 33.5s, R=0.05) errorbox 32275 sec after notice time and 32359 sec after trigger time at 2026-01-18 20:27:14 UT, with upper limit up to 18.2 mag. The observations began at zenith distance = 59 deg. The sun altitude is -27.5 deg. The galactic latitude b = -1 deg., longitude l = 293 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3106346 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 32450 | MASTER-SAAO | C | 180 | 18.0 | 32450 | MASTER-SAAO | C | 180 | 18.3 | 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/43446. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41540] GRB 260117A: SVOM/COLIBRÍ (FM-GFT) optical observations
by GCN Circulars 18 Jan '26

18 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43445 SUBJECT: GRB 260117A: SVOM/COLIBRÍ (FM-GFT) optical observations DATE: 26/01/18 19:35:14 GMT FROM: Alan Watson at UNAM <alan(a)astro.unam.mx> Francis Fortin (IRAP), William H. Lee (UNAM), Benjamin Schneider (LAM), Noémie Globus (UNAM), Stéphane Basa (UAR Pytheas), Alan M. Watson (UNAM), Edilberto Aguilar-Ruiz (UNAM), Jean-Luc Atteia (IRAP), Camila Angulo (UNAM), Dalya Akl (NYUAD), Sarah Antier (IJCLAB), Rosa L. Becerra (UNAM), Nathaniel R. Butler (ASU), Damien Dornic (CPPM), Jean-Grégoire Ducoin (CPPM), Leonardo García García (UNAM), Ramandeep Gill (UNAM), Asuka Kuwata (UNAM), Nikos Mandarakas (LAM), Diego López-Cámara (UNAM), Francesco Magnani (CPPM), Enrique Moreno Méndez (UNAM), Margarita Pereyra (UNAM), Ny Avo Rakotondrainibe (LAM), Fredd Sánchez Álvarez (UNAM), Antonio de Ugarte Postigo (LAM), J. T. Palmerio (CEA/Irfu) report: We imaged the field of the SVOM GRB 260117A (Palmerio et al., GCN Circ. 43437) using the DDRAGO wide-field imager on the SVOM/COLIBRÍ (FM-GFT) telescope. We observed from 2026-01-18 07:56 to 13:25 UTC (from 12.22 to 17.70 hours after the trigger) and obtained 240 minutes of simultaneous exposure in the r and z filters. The data were reduced, coadded, calibrated, and analyzed with the COLIBRÍ ASU pipeline. The photometry was calibrated using nearby stars from the PanSTARRS DR1 catalog, is in the AB system, and is not corrected for Galactic extinction. At the position of the source detected with Swift/XRT (Salvaggio et al., GCN 43439; Evans et al., GCN 43438) and SVOM/VT (Li et al., GCN Circ. 43441), we detect a source with preliminary magnitudes of r = 24.27 +/- 0.12, z > 23.7 (3 sigma). It is not trivial to compare our results with SVOM/VT as our filters are different. Our r filter lies within VT_B and our z filter lies within VT_R. Nevertheless, our z upper limit does suggest that the source seen by Li et al. has faded and therefore is the afterglow. We also note that in deep CFHT images from previous epochs, there is a source at this position with r = 24.41 ± 0.17. The source is also faintly visible in the PS1 r image. Therefore, we suggest that this source might be the host galaxy. We thank the staff of the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir and the COLIBRÍ and DDRAGO engineering teams. COLIBRÍ is an astronomical observatory developed and operated jointly by France (AMU, CNES and CNRS) and Mexico (UNAM and SECIHTI). It is located at the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir, Baja California, Mexico. View this GCN Circular online at https://gcn.nasa.gov/circulars/43445. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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