January 2026 - vsnet-grb-info - ooruri.kusastro.kyoto-u.ac.jp

[vsnet-grb-info 41679] GRB 260127B: AstroSat CZTI detection
by GCN Circulars 31 Jan '26

31 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43576 SUBJECT: GRB 260127B: AstroSat CZTI detection DATE: 26/01/31 05:11:40 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 short GRB 260127B which was also detected by Fermi GBM (Fermi GBM Team, GCN Circ. 43533), Swift BAT (Evans et al., GCN Circ. 43542), and Konus IPN (Ridnaia et al., GCN Circ. 43559). The source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve peaks at 2026-01-27 20:02:32.605 UTC. The measured peak count rate associated with the burst is 2558 (+901, -550) counts/s above the background in the combined data of all quadrants, with a total of 233 (+42, -31) counts. The local mean background count rate was 261 (+9, -32) counts/s. Using cumulative rates, we measure a T90 of 0.17 (+0.11, -0.03) s. The source was also detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve peaks at 2026-01-27 20:02:32.292 UTC. The measured peak count rate associated with the burst is 602 (+68, -74) counts/s above the background in the combined data of all quadrants, with a total of 604 (+160, -170) counts. The local mean background count rate was 1239 (+7, -8) 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/43576. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41678] GRB 260130A: Fermi GBM Detection
by GCN Circulars 31 Jan '26

31 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43575 SUBJECT: GRB 260130A: Fermi GBM Detection DATE: 26/01/31 05:10:32 GMT FROM: Peter Veres at University of Alabama in Huntsville <veresp(a)gmail.com> A. Jameson (UAH), C. Meegan (UAH), and M. Dafčíková (MUNI) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 13:29:20.82 UT on 30 January 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260130A (trigger 791472565/260130562). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 48.70, Dec = 64.17 (J2000 degrees, equivalent to J2000 3h 14m, +64d 10'), with a statistical uncertainty of 1.60 degrees. (radius, 1-sigma containment, statistical only; there is additionally a systematic error which we have characterized as a mixture of two Gaussians, one with a radius of 1.8 degrees (52% contribution) and one with a radius of 4.1 degrees (47% contribution) [A. Goldstein et al. 2020, ApJ, 895, 1]). The angle from the Fermi LAT boresight is 16 degrees. The GBM light curve consists of a single emission episode with a duration (T90) of about 0.5 s (50-300 keV). The time-averaged spectrum from T0-0.07 to T0+0.20 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.41 +/- 0.02 and the cutoff energy, parameterized as Epeak, is 730 +/- 30 keV. The event fluence (10-1000 keV) in this time interval is (8.8 +/- 0.4)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 27 +/- 1 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 570 +/- 20 keV, alpha = -0.33 +/- 0.02 and beta = -2 +/- 0.1. 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/43575. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41677] EP260131a: Einstein Probe detection of an X-ray transient
by GCN Circulars 31 Jan '26

31 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43574 SUBJECT: EP260131a: Einstein Probe detection of an X-ray transient DATE: 26/01/31 04:36:37 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> H. C. Ding, T. Wu (AHNU), Q. Y. Wu, H. Sun (NAO, CAS) on behalf of the Einstein Probe (EP) team: We report on the detection of an X-ray transient by the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) mission, designated EP260131a. The transient triggered EP-WXT (ID: 01709254172) at 2026-01-31T03:31:25 (UTC). The WXT position of the source is R.A. = 149.921 deg, DEC = -3.291 deg (J2000) with an uncertainty of 3 arcmin in radius (90% C.L. statistical and systematic). A follow-up observation with the Follow-up X-ray Telescope (FXT) was performed automatically. Within the WXT error circle, an uncatalogued X-ray source was detected at R.A. = 149.9027 deg, DEC = -3.3094 deg (J2000) with an uncertainty of 20 arcsec in radius (90% C.L. statistical and systematic). 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/43574. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41676] GRB 260127B: Fermi GBM Detection
by GCN Circulars 30 Jan '26

30 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43573 SUBJECT: GRB 260127B: Fermi GBM Detection DATE: 26/01/30 21:27:55 GMT FROM: atrigg2(a)lsu.edu A. C. Trigg (NPP ORAU, NASA MSFC) reports on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 20:02:32.57 UT on 27 January 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260127B (trigger 791236957/260127835). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 190.42, Dec = 56.88 (J2000 degrees, equivalent to J2000 12h 41m, +56d 52'), with a statistical uncertainty of 5.21 degrees. (radius, 1-sigma containment, statistical only; there is additionally a systematic error which we have characterized as a mixture of two Gaussians, one with a radius of 1.8 degrees (52% contribution) and one with a radius of 4.1 degrees (47% contribution) [A. Goldstein et al. 2020, ApJ, 895, 1]). The angle from the Fermi LAT boresight is 109 degrees. The GBM light curve displays a single short peak with a duration (T90) of about 1 s (50-300 keV). The time-averaged spectrum from T0-0.1 to T0+0.3 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.11 +/- 0.01 and the cutoff energy, parameterized as Epeak, is 710 +/- 30 keV. The event fluence (10-1000 keV) in this time interval is (1.29 +/- 0.09)E-06 erg/cm^2. The 64-ms peak photon flux measured starting from T0+0.064 s in the 10-1000 keV band is 22 +/- 2 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 570 +/- 20 keV, alpha = -0.040 +/- 0.002 and beta = -2 +/- 0.1. 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/43573. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41675] EP260128a / GRB 260128A: COLIBRÍ optical upper limit
by GCN Circulars 30 Jan '26

30 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43572 SUBJECT: EP260128a / GRB 260128A: COLIBRÍ optical upper limit DATE: 26/01/30 15:46:49 GMT FROM: Jean-Luc Atteia at IRAP <jean-luc.atteia(a)irap.omp.eu> Jean-Luc Atteia (IRAP), Enrique Moreno Méndez (UNAM), Alan M. Watson (UNAM), Stéphane Basa (UAR Pytheas), William H. Lee (UNAM), Edilberto Aguilar-Ruiz (UNAM), Camila Angulo (UNAM), Dalya Akl (NYUAD), Sarah Antier (IJCLAB), Rosa L. Becerra (UNAM), Nathaniel R. Butler (ASU), Damien Dornic (CPPM), Jean-Grégoire Ducoin (CPPM), Francis Fortin (IRAP), Leonardo García García (UNAM), Ramandeep Gill (UNAM), Noémie Globus (UNAM), Asuka Kuwata (UNAM), Nikos Mandarakas (LAM), Diego López-Cámara (UNAM), Francesco Magnani (CPPM), Margarita Pereyra (UNAM), Ny Avo Rakotondrainibe (LAM), Fredd Sánchez Álvarez (UNAM), Benjamin Schneider (LAM) and Antonio de Ugarte Postigo (LAM) report: We imaged the field of the X-ray transient EP260128a / GRB 260128a (Zhou et al., GCN Circ. 43549, Ravasio et al., GCN Circ. 43556) using the DDRAGO two-channel wide-field imager on the COLIBRÍ telescope. We observed from 2026-01-30 04:48 to 10:12 UTC (from 29.14 to 35.53 hours after the trigger) and obtained 238 minutes of simultaneous exposure in the i 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. In the stacked images, we do not detect any new source at the Liverpool Telescope proposed candidate position (Eyles-Ferris et al., GCN Circ. 43553) nor at the NOT proposed candidate position (He et al., GCN Circ. 43555), down to the following 3-sigma limits: i > 23.6 z > 23.1 These upper limits are consistent with the one reported by Malesani et al. (GCN Circ. 43570). 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/43572. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41674] Fermi GRB 260130A: Global MASTER-Net observations report
by GCN Circulars 30 Jan '26

30 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43571 SUBJECT: Fermi GRB 260130A: Global MASTER-Net observations report DATE: 26/01/30 15:30:22 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-Kislovodsk robotic telescope [1] located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 260130A ( Fermi GBM team, GCN 43569) errorbox 6593 sec after notice time and 6628 sec after trigger time at 2026-01-30 15:19:49 UT, with upper limit up to 15.6 mag. Observations started at twilight. The observations began at zenith distance = 23 deg. The sun altitude is -11.2 deg. The galactic latitude b = 6 deg., longitude l = 138 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3118825 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 6659 | 2026-01-30 15:19:49 | MASTER-Kislovodsk | (03h 14m 10.80s , +65d 46m 26.8s) | C | 60 | 15.4 | 6760 | 2026-01-30 15:21:30 | MASTER-Kislovodsk | (03h 33m 51.07s , +65d 44m 38.9s) | C | 60 | 15.3 | 6860 | 2026-01-30 15:23:10 | MASTER-Kislovodsk | (03h 28m 09.77s , +63d 51m 38.5s) | C | 60 | 15.6 | 6964 | 2026-01-30 15:24:54 | MASTER-Kislovodsk | (03h 46m 28.40s , +63d 52m 21.7s) | C | 60 | 15.4 | 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/43571. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41673] EP260128a / GRB 260128A: NOT and TNG optical and NIR upper limits
by GCN Circulars 30 Jan '26

30 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43570 SUBJECT: EP260128a / GRB 260128A: NOT and TNG optical and NIR upper limits DATE: 26/01/30 14:23:44 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), J. An (NAOC), G. Corcoran (UCD), P. D’Avanzo (INAF/OAB), M. De Pasquale (U. Messina), L.B. He (NAOC), A. Martin-Carrillo (UCD), A. Melandri (INAF/OAR), D. Xu (NAOC), W. Boschin (TNG), V. Lorenzi (TNG), H. Lucio Medeiros (TNG), T. Pursimo (NOT), report on behalf of a larger collaboration: We observed the optical counterpart (He et al., GCN 43555) of the high-energy transient EP260128a / GRB 260128A (Zhou et al., GCN 43549; Ravasio et al., GCN 43556) in both the optical and infrared. Optical observations were carried out at the Nordic Optical Telescope (NOT) equipped with the ALFOSC camera, for a total of 14x200 s in the SDSS z filter. NIR observations were carried out at the Telescopio Nazionale Galileo (TNG) equipped with the NICS camera, for a total of 40x60 s in the J filter. The afterglow (He et al., GCN 43555) is not detected in any of our stacked images. We report 3-sigma limiting magnitudes: z > 23.2, mean epoch 2026 Jan 29.961 UT (23.39 hr after the EP trigger); J > 22.0, mean epoch 2026 Jan 29.939 UT (22.88 hr after the EP trigger). The above magnitudes are in the AB system, are calibrated against nearby objects from the Pan-STARRS (z) and VHS (J) catalogs, and are not corrected for Galactic extinction. View this GCN Circular online at https://gcn.nasa.gov/circulars/43570. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41672] GRB 260130A: Fermi GBM Final Real-time Localization
by GCN Circulars 30 Jan '26

30 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43569 SUBJECT: GRB 260130A: Fermi GBM Final Real-time Localization DATE: 26/01/30 13:39:52 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply(a)GIOC.nsstc.nasa.gov> The Fermi GBM team reports the detection of a likely SHORT GRB At 13:29:20 UT on 30 Jan 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260130A (trigger 791472565.82111 / 260130562). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 48.7, Dec = 64.2 (J2000 degrees, equivalent to J2000 03h 14m, 64d 12'), with a statistical uncertainty of 1.6 degrees. The angle from the Fermi LAT boresight is 16.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260130562/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260130562/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260130562/… View this GCN Circular online at https://gcn.nasa.gov/circulars/43569. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41671] Fermi GRB 260129A: Global MASTER-Net observations report
by GCN Circulars 30 Jan '26

30 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43568 SUBJECT: Fermi GRB 260129A: Global MASTER-Net observations report DATE: 26/01/30 09:45:35 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) started inspect of the Fermi GRB 260129A ( "The Fermi GBM team, GCN 43560) errorbox 11097 sec after trigger time at 2026-01-29 07:38:10 UT, with upper limit up to 20.3 mag. The observations began at zenith distance = 14 deg. The sun altitude is -26.1 deg. MASTER-SAAO robotic telescope located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 260129A errorbox 11436 sec after notice time and 62790 sec after trigger time at 2026-01-29 21:59:43 UT, with upper limit up to 18.7 mag. The observations began at zenith distance = 29 deg. The sun altitude is -38.6 deg. The galactic latitude b = 10 deg., longitude l = 281 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3118323 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 11158 | 2026-01-29 07:38:10 | MASTER-OAFA | (11h 27m 13.34s , -44d 41m 02.7s) | C | 120 | 20.3 | 11292 | 2026-01-29 07:40:24 | MASTER-OAFA | (11h 27m 07.54s , -44d 41m 59.8s) | C | 120 | 20.3 | 11428 | 2026-01-29 07:42:41 | MASTER-OAFA | (11h 27m 15.05s , -44d 41m 35.1s) | C | 120 | 20.3 | 62821 | 2026-01-29 21:59:43 | MASTER-SAAO | (10h 11m 50.86s , -45d 52m 29.4s) | C | 60 | 18.4 | 62821 | 2026-01-29 21:59:43 | MASTER-SAAO | (10h 14m 26.54s , -46d 07m 36.2s) | C | 60 | 18.5 | 63446 | 2026-01-29 22:10:08 | MASTER-SAAO | (10h 11m 53.44s , -45d 51m 31.8s) | C | 60 | 18.5 | 63446 | 2026-01-29 22:10:08 | MASTER-SAAO | (10h 14m 29.91s , -46d 06m 40.7s) | C | 60 | 18.5 | 63538 | 2026-01-29 22:11:41 | MASTER-SAAO | (10h 23m 16.96s , -45d 52m 29.2s) | C | 60 | 18.5 | 63538 | 2026-01-29 22:11:41 | MASTER-SAAO | (10h 25m 53.45s , -46d 07m 38.5s) | C | 60 | 18.7 | 69831 | 2026-01-29 23:56:34 | MASTER-SAAO | (10h 11m 31.47s , -45d 50m 19.4s) | C | 60 | 18.5 | 69831 | 2026-01-29 23:56:34 | MASTER-SAAO | (10h 14m 12.48s , -46d 05m 44.3s) | C | 60 | 18.6 | 69924 | 2026-01-29 23:58:06 | MASTER-SAAO | (10h 23m 08.92s , -45d 50m 23.0s) | C | 60 | 18.5 | 69924 | 2026-01-29 23:58:06 | MASTER-SAAO | (10h 25m 49.94s , -46d 05m 48.7s) | C | 60 | 18.7 | 71379 | 2026-01-30 00:22:22 | MASTER-SAAO | (11h 35m 50.59s , -53d 50m 24.1s) | C | 60 | 18.4 | 72378 | 2026-01-30 00:39:01 | MASTER-SAAO | (11h 35m 50.52s , -53d 49m 57.6s) | C | 60 | 18.4 | 97583 | 2026-01-30 07:39:05 | MASTER- | (11h 14m 18.98s , -40d 12m 46.3s) | C | 60 | 12.5 | 98173 | 2026-01-30 07:48:55 | MASTER- | (10h 28m 29.18s , -38d 41m 20.6s) | C | 60 | 17.5 | 98173 | 2026-01-30 07:48:55 | MASTER- | (10h 29m 56.16s , -39d 15m 37.1s) | C | 60 | 17.8 | 98242 | 2026-01-30 07:50:04 | MASTER- | (10h 39m 15.98s , -39d 16m 29.4s) | C | 60 | 17.7 | 98242 | 2026-01-30 07:50:04 | MASTER- | (10h 37m 49.29s , -38d 42m 11.6s) | C | 60 | 17.4 | 98312 | 2026-01-30 07:51:14 | MASTER- | (10h 49m 27.34s , -39d 17m 20.5s) | C | 60 | 16.0 | 98312 | 2026-01-30 07:51:14 | MASTER- | (10h 48m 02.65s , -38d 43m 01.0s) | C | 60 | 16.9 | 98384 | 2026-01-30 07:52:26 | MASTER- | (10h 13m 19.68s , -40d 15m 49.2s) | C | 60 | 14.8 | 98384 | 2026-01-30 07:52:26 | MASTER- | (10h 14m 48.12s , -40d 50m 02.2s) | C | 60 | 14.8 | 98453 | 2026-01-30 07:53:36 | MASTER- | (10h 16m 32.79s , -40d 50m 27.7s) | C | 60 | 13.0 | 98453 | 2026-01-30 07:53:36 | MASTER- | (10h 14m 46.66s , -40d 16m 18.6s) | C | 60 | 12.3 | 98524 | 2026-01-30 07:54:47 | MASTER- | (10h 41m 57.54s , -37d 23m 14.9s) | C | 60 | 18.1 | 98524 | 2026-01-30 07:54:47 | MASTER- | (10h 40m 33.59s , -36d 49m 02.8s) | C | 60 | 17.6 | 98594 | 2026-01-30 07:55:56 | MASTER- | (10h 51m 59.28s , -37d 21m 24.5s) | C | 60 | 18.0 | 98594 | 2026-01-30 07:55:56 | MASTER- | (10h 50m 35.55s , -36d 47m 11.0s) | C | 60 | 17.7 | 98666 | 2026-01-30 07:57:08 | MASTER- | (10h 15m 39.98s , -40d 15m 20.6s) | C | 60 | 12.3 | 98806 | 2026-01-30 07:59:28 | MASTER- | (10h 27m 25.44s , -40d 50m 52.5s) | C | 60 | 15.6 | 98806 | 2026-01-30 07:59:28 | MASTER- | (10h 25m 56.82s , -40d 16m 28.3s) | C | 60 | 15.6 | 98950 | 2026-01-30 08:01:52 | MASTER- | (10h 28m 26.76s , -38d 43m 31.6s) | C | 60 | 17.8 | 98950 | 2026-01-30 08:01:52 | MASTER- | (10h 29m 53.21s , -39d 17m 54.3s) | C | 60 | 17.9 | 99020 | 2026-01-30 08:03:02 | MASTER- | (10h 39m 13.65s , -39d 17m 26.4s) | C | 60 | 17.9 | 99020 | 2026-01-30 08:03:02 | MASTER- | (10h 37m 47.28s , -38d 43m 02.2s) | C | 60 | 17.7 | 99090 | 2026-01-30 08:04:12 | MASTER- | (10h 47m 58.95s , -38d 41m 25.0s) | C | 60 | 17.5 | 99090 | 2026-01-30 08:04:12 | MASTER- | (10h 49m 25.13s , -39d 15m 51.5s) | C | 60 | 17.8 | 99162 | 2026-01-30 08:05:24 | MASTER- | (10h 13m 13.05s , -40d 17m 55.1s) | C | 60 | 14.9 | 99162 | 2026-01-30 08:05:24 | MASTER- | (10h 14m 41.45s , -40d 52m 16.3s) | C | 60 | 14.8 | 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/43568. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41670] GRB 260128B: LCO optical upper limits
by GCN Circulars 30 Jan '26

30 Jan '26

TITLE: GCN CIRCULAR NUMBER: 43567 SUBJECT: GRB 260128B: LCO optical upper limits DATE: 26/01/30 09:25:29 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> C. Wu (NAOC), J. X. Cao (GXU), A. Saccardi (CEA/Irfu), D. Turpin (CEA/Irfu), report on behalf of the SVOM mission team: We observed the field of the SVOM GRB 260128B (Brunet et al., GCN 43561) with the LCO 1m telescope at Cerro Tololo Interamerican Observatory equipped with the Sinistro instrument. Our observation started on 2026-01-30 at 00:48:11 UT (about 1.75 days after the trigger) and we obtained 6x300 s exposures in the SDSS r and 5x300 s exposures in the Pan-STARRS z filters. In the stacked image, we do not detect any new source within the SVOM/ECLAIRs error box, in agreement with Méndez et al. (GCN 43566). We measure the following upper limit calibrated against the PanSTARSS DR1 catalog, and not corrected for Galactic extinction: r > 22.4 AB (3-sigma, mid-time 42.5 hr after the trigger) z > 21.3 AB (3-sigma, mid-time 42.2 hr after the trigger). This project is funded by the SVOM collaboration. View this GCN Circular online at https://gcn.nasa.gov/circulars/43567. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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