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[vsnet-grb-info 42127] GRB 260310A / AT2026fgk: SAO RAS optical observations
by GCN Circulars 14 Mar '26

14 Mar '26

TITLE: GCN CIRCULAR NUMBER: 44006 SUBJECT: GRB 260310A / AT2026fgk: SAO RAS optical observations DATE: 26/03/14 15:46:52 GMT FROM: Alexander Moskvitin at SAO RAS <mosk(a)sao.ru> A. Moskvitin (SAO RAS), O. Spiridonova (SAO RAS), A. Pozanenko (IKI), N. Pankov (IKI), A. Volnova (IKI), report on behalf of GRB follow-up team and IKI-GRB-FuN. We observed the field of the AT2026fgk, potential counterpart of the GRB 260310A (Fermi GBM team, GCN 43951; Hamburg and Meegan, GCN 43975; Salunke et al., GCN 43958) with the Zeiss-1000 1m telescope of the SAO RAS equipped with the CCD photometer. We obtained series of 300 sec images in B, V, Rc, Ic filters on March 12/13 and 13/14. The observations carried out under a good weather conditions and typical seeing of 1".5--2".5. The candidate discovered by GOTO (O'Neill et al. 2026, TNS Discovery Report 294132) and observed by numerous observatories (Konno et al., GCN 43974; Hinds et al., GCN 43977; Lipunov et al., GCN 43978; Martin-Carrillo et al., GCN 43979; Moren Méndez et al., GCN 43980; de Ugarte Postigo et al., GCN 43984; Hsu et al., GCN 43986; Pursiainen et al., GCN 43990; Becerra et al., GCN 43991; Li et al., GCN 43993; Jayaraman et al., GCN 43994; Stein et al., GCN 43996; Martin-Carrillo et al., GCN 44000; Watson et al., GCN 44001; Lai et al., GCN 44002; Izzo, GCN 44003; Brivio et al., GCN 44004; Rhodes et al., GCN 44005) is clearly detected in our images with the following brightness. Date UT_start t_mid - T0, filter exp, mag +/- err days s 2026.03.12T23:27:00 2.80565 B 5*300 18.77 +/- 0.01 2026.03.12T23:09:50 2.79577 Rc 6*300 18.00 +/- 0.01 2026.03.13T23:56:42 3.82450 B 5*300 18.92 +/- 0.01 2026.03.13T23:45:30 3.81664 Rc 4*300 18.14 +/- 0.01 This preliminary photometry is based on the nearby stars from PanSTARRS catalogue. Magnitudes of standards converted to B, Rc with the Lupton 2005 equations. The magnitudes of the AT2026fgk are not corrected for Galactic and host extinction and may be contaminated by the host galaxy. We can not trace any colour evolution between the two epochs (2.8 and 3.8 days after GRB trigger). View this GCN Circular online at https://gcn.nasa.gov/circulars/44006. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42126] GRB 260310A/AT 2026fgk: radio detection at 15GHz
by GCN Circulars 14 Mar '26

14 Mar '26

TITLE: GCN CIRCULAR NUMBER: 44005 SUBJECT: GRB 260310A/AT 2026fgk: radio detection at 15GHz DATE: 26/03/14 15:23:56 GMT FROM: Lauren Rhodes at McGill <lauren.rhodes(a)mcgill.ca> Lauren Rhodes (McGill), Andrew Hughes, Rob Fender (Oxford), Joe Bright (Oxford/Breakthrough Listen), Dave Green, Dave Titterington (Cambridge) report: We observed the position of GRB 260310A/AT 2026fgk (Fermi GBM Team, GCN 43951; Konno et al., GCN 43974; Hinds et al., AstroNote 2026-65; O’Neill et al. 2026, TNS Discovery Report 294132) with the Arcminute Microkelvin Imager Large-Array (AMI-LA) at 15.2 GHz beginning at 2026 March 13 23:20:06 for a total of 8 hours. The flux standard 3c286 was used to calibrate the bandpass response and flux scale of the AMI-LA and J1435+7605 was used as an interleaved complex gain calibrator. We detect an unresolved source with coordinates consistent with those of GRB 260310A/AT 2026fgk. We measure a peak flux density of 9.8 +/- 0.5 mJy/beam. Given the high flux density of the source, we cross checked with the VLASS survey and find no preexisting radio emission at the afterglow coordinates down to a 3sigma upper limit of around 0.5mJy/beam. We thank the staff at the Mullard Radio Astronomy Observatory for carrying out these observations and operating the AMI-LA. View this GCN Circular online at https://gcn.nasa.gov/circulars/44005. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42125] GRB 260310A / AT2026fgk: TNG NIR detection
by GCN Circulars 14 Mar '26

14 Mar '26

TITLE: GCN CIRCULAR NUMBER: 44004 SUBJECT: GRB 260310A / AT2026fgk: TNG NIR detection DATE: 26/03/14 14:48:10 GMT FROM: Riccardo Brivio at INAF-OAB <riccardo.brivio(a)inaf.it> R. Brivio (INAF-OAB), D. Malesani (DAWN/NBI and Radboud), L. Izzo (INAF-OACn and DARK/NBI), P. D’Avanzo (INAF-OAB), V. D’Elia (ASI-SSDC), A. Melandri (INAF-OAR), A. Rossi (INAF-OAS), M. de Pasquale (Univ. Messina), Aldo Fiorenzano (INAF-TNG), Carmen Padilla (INAF-TNG) report on behalf of the CIBO collaboration: We observed the likely counterpart of GRB 260310A, detected by Fermi/GBM (Fermi GBM team, GCN 43951; Hamburg & Meagan, GCNC 43975) and AstroSat CZTI (Salunke et al., GCN 43958) with the Italian 3.6m TNG telescope equipped with the near-infrared camera NICS. A series of images was obtained with the J and H filters starting on 2026 March 14 at 05:11:46 UT (i.e. 96.2 hours after the burst), and lasted 40 minutes for each filter. The optical/NIR counterpart, also reported as AT2026fgk (Konno et al., GCN 43974; Hinds et al., GCN 43977; Lipunov et al., GCN 43978; Martin-Carrillo et al., GCN 43979; Moreno Méndez et al., GCN 43980; de Ugarte Postigo et al., GCN 43984; Hsu et al., GCN 43986; Pursiainen et al., GCN 43990; Becerra et al., GCN 43991; Li et al., GCN 43993; Stein et al, GCN 43996; Martin-Carrillo et al., GCN 44000; Watson et al., GCN 44001; Lai et al., GCN 44002; L. Izzo, GCN 44003) is detected in the co-added images with the following magnitudes: J = 17.0 +/- 0.1 (Vega, calibrated against the 2MASS catalogue), at a mid-time of 96.5 hr after the trigger; H = 15.9 +/- 0.1 (Vega, calibrated against the 2MASS catalogue), at a mid-time of 97.1 hr after the trigger. View this GCN Circular online at https://gcn.nasa.gov/circulars/44004. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42124] GRB 260310A / AT2026fgk: OASDG optical observations
by GCN Circulars 14 Mar '26

14 Mar '26

TITLE: GCN CIRCULAR NUMBER: 44003 SUBJECT: GRB 260310A / AT2026fgk: OASDG optical observations DATE: 26/03/14 09:12:46 GMT FROM: luca.izzo(a)inaf.it L. Izzo (INAF-OACn and DARK/NBI) reports: We observed the likely counterpart of GRB 261013A (Fermi GBM team, GCN #43951; Hamburg et al., GCN #43975) using the 0.5-m T1 telescope of the Osservatorio Astronomico S. Di Giacomo, located in Agerola, Italy. Our observations started on 2026 March 14 at 00:04 UT, 3.797 days after the GRB trigger. We acquired a series of 8 × 300 s images in the Rc and Ic filters. The optical counterpart, also reported as AT2026fgk (Konno et al., GCN #43974; Hinds et al., GCN #43977; Lipunov et al., GCN #43978; Martin-Carrillo et al., GCN #43979; Moreno Méndez et al., GCN #43980; de Ugarte Postigo et al., GCN #43984; Hsu et al., GCN #43986; Pursiainen et al., GCN #43990; Becerra et al., GCN #43991; Martin-Carrillo et al., GCN #44000; Watson et al., GCN #44001; Lai et al., GCN #44002) is clearly detected in the individual frames. In the Rc-band stacked image, we measure a preliminary magnitude of Rc = 18.21 +/- 0.07 mag (AB), calibrated against nearby stars from the Pan-STARRS catalog and appropriately transformed to Rc magnitudes. The measured magnitude may still be affected by contamination from the bright host galaxy, but further analysis is ongoing. View this GCN Circular online at https://gcn.nasa.gov/circulars/44003. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42123] GRB 260310A / AT2026fgk: Multiband optical follow-up with Kinder observations
by GCN Circulars 14 Mar '26

14 Mar '26

TITLE: GCN CIRCULAR NUMBER: 44002 SUBJECT: GRB 260310A / AT2026fgk: Multiband optical follow-up with Kinder observations DATE: 26/03/14 08:19:29 GMT FROM: Amar Aryan at National Central University, Institute of Astronomy (NCUIA) <amararyan941(a)gmail.com> C.-H. Lai, A. Aryan, Y.-H. Lee, C.-S. Lin, T.-W. Chen (all NCU), A. K. H. Kong (NTHU), J. H. Gillanders, S. J. Smartt (both Oxford), Y. J. Yang (NYUAD), A. Sankar.K, M.-H. Lee, Y.-C. Pan, C.-C. Ngeow, W.-J. Hou, H.-Y. Hsiao, H.-C. Lin, J.-K. Guo (all NCU), S. Yang, Z. N. Wang, L. L. Fan, G. H. Sun (all HNAS), H.-W. Lin (UMich), H. F. Stevance, S. Srivastav, L. Rhodes (all Oxford), M. Nicholl, M. Fulton, T. Moore, K. W. Smith, C. Angus, A. Aamer (all QUB), A. Schultz, and M. Huber (both IfA, Hawaii) report: We performed multiband optical observations of the field of the GRB 260310A (Fermi GBM team, GCN 43951, Hamburg et al., GCN 43975) using the 1m LOT at the Lulin observatory, as part of the Kinder collaboration (Chen et al. 2025, ApJ, 983, 86, doi:10.3847/1538-4357/adb428). The first LOT epoch of observations in g-band started at 13:45 UTC on 13th of March 2026 (MJD 61092.577), 3.37 days after the Fermi GBM detection. The reported optical counterpart, AT 2026fgk (Konno et al., GCN 43974; Hinds et al., GCN 43977; Lipunov et al., GCN 43978; Martin-Carrillo et al., GCN 43979; Moreno Méndez et al., GCN 43980; Ugarte Postigo et al., GCN 43984; Hsu et al., GCN 43986; Pursiainen et al., GCN 43990; Becerra et al., GCN 43991; Martin-Carrillo et al., GCN 44000; Watson et al., GCN 44001), is clearly visible in each individual frame. The GRB also had X-ray (Salunke et al., GCN 43958; Jayaraman et al., GCN 43994) and NIR (Li et al., GCN 43993; Stein et al., GCN 43996) detections. We utilized the Python-based package AutoPhOT (Brennan & Fraser, 2022, A&A, 667, A62) to perform template subtractions with the Pan-STARRS1 3Pi archive images (Chambers et al. 2016 arXiv:1612.05560) using the 'SFFT' (Hu et al. 2022, ApJ, 936, 157) algorithm. Moreover, we further used AutoPhOT to perform PSF photometry. The details of the observations and the measured photometry (in the AB system) are as follows: Telescope | Filter | MJD (start) | t-t0 (d) | Exposure (s) | Magnitude | avg.Seeing | Airmass LOT | g | 61112.573 | 3.367 | 300 * 1 | 18.72 +/- 0.02 | 1".94 | 2.35 LOT | r | 61112.576 | 3.371 | 300 * 1 | 18.42 +/- 0.02 | 1".70 | 2.32 LOT | i | 61112.581 | 3.374 | 300 * 1 | 18.26 +/- 0.02 | 1".77 | 2.28 LOT | z | 61112.584 | 3.378 | 300 * 1 | 17.96 +/- 0.05 | 1".90 | 2.25 In multiband photometry, the optical counterpart appears red. The presented magnitudes are calibrated using the field stars from the ATLAS-refcat2 catalog from MAST (Tonry J. L. et al. 2018, ApJ, 867, 105). In the direction of the transient, these magnitudes are not corrected for the expected Galactic foreground extinctions of 0.09, 0.06, 0.04, and 0.03 mags (Schlafly & Finkbeiner 2011) for the g, r, i, and z bands, respectively. The details on the Lulin observatory telescopes and the follow-up methodology for such transients are presented in Aryan et al. (2025, ApJS, 281, 20, doi:10.3847/1538-4365/adfc69). View this GCN Circular online at https://gcn.nasa.gov/circulars/44002. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42122] GRB 260310A / AT 2026fgk: COLIBRÍ continuing optical observations
by GCN Circulars 14 Mar '26

14 Mar '26

TITLE: GCN CIRCULAR NUMBER: 44001 SUBJECT: GRB 260310A / AT 2026fgk: COLIBRÍ continuing optical observations DATE: 26/03/14 06:20:02 GMT FROM: Alan Watson at UNAM <alan(a)astro.unam.mx> Alan M. Watson (UNAM), Damien Dornic (CPPM), Rosa L. Becerra (UNAM), Antonio de Ugarte Postigo (LAM), Stéphane Basa (UAR Pytheas), William H. Lee (UNAM), Edilberto Aguilar-Ruiz (UNAM), Jean-Luc Atteia (IRAP), Dalya Akl (NYUAD), Camila Angulo (UNAM), Sarah Antier (IJCLAB), Nathaniel R. Butler (ASU), Jean-Grégoire Ducoin (CPPM), Francis Fortin (IRAP), Leonardo García García (UNAM), Ramandeep Gill (UNAM), Noémie Globus (UNAM), Marion Guelfand (CPPM), Asuka Kuwata (UNAM), Massimiliano Lincetto (CPPM), 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), and Benjamin Schneider (LAM) report: We again imaged the field of AT 2026fgk (Lipunov et al., GCN Circ. 43954; Konno et al., GCN Circ. 43975; Hinds et al., GCN Circ. 43977; Lipunov et al., GCN Circ. 43978, Martin-Carrillo et al., GCN Circ. 43079; Moren Méndez et al., GCN Circ 43980; de Ugarte Postiga et al., GCN Circ. 43984; Hsu et al., GCN Circ. 43986; Pursiainen et al., GCN Circ. 43990; Becerra et al., GCN Circ 43991; Li et al., GCn Circ. 43993; Stein et al., GCN Circ 43996; Martin-Carrillo et al., GCn Circ. 44000), a possible counterpart of the Fermi GBM GRB 260310A (Fermi GBM Team, GCN Circ. 43951; Humburg & Meegan, GCN Circ. 43975) and also detected by AstroSat CZTI (Salunke et al., GCN Circ. 43958), using the DDRAGO two-channel wide-field imager on the COLIBRÍ telescope. We observed from 2026-03-14 02:46 to 05:07 UTC (from 93.82 to 96.17 hours after the GRB trigger) and obtained 15, 14, and 28 minutes, respectively, of exposure in the g, r, and z filters. The data were reduced, coadded, calibrated, and analysed with the 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 continue to detect AT 2026fgk with a preliminary PSF magnitude of: r = 18.47 +/- 0.01 Compared to the magnitudes in our first epoch reported in Moreno Méndez et al. (GCN Circ. 43980), we estimate a temporal decay index of about -1.2, consistent with the normal decay observed in GRBs. Moreover, from the optical/IR magnitudes from our first epoch and the photometry reported with WINTER (Stein et al., GCN Circ. 43996) between T+71.5 and T+72.5 hours, we estimate a spectral index beta of about -1.1 also supporting a synchrotron spectrum and a likely origin in a GRB afterglow. We thank the staff of the Observatorio Astronómico Nacional at Sierra de San Pedro Mártir, as well as the technical and engineering teams at CEA, CPPM, IRAP, LAM, OHP, OSU Pytheas, and UNAM. 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/44001. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42121] GRB 260310A / AT2026fgk: further CAHA 1.23m telescope optical observations suggest shallow decay
by GCN Circulars 14 Mar '26

14 Mar '26

TITLE: GCN CIRCULAR NUMBER: 44000 SUBJECT: GRB 260310A / AT2026fgk: further CAHA 1.23m telescope optical observations suggest shallow decay DATE: 26/03/14 04:43:17 GMT FROM: Antonio Martin-Carrillo at UCD,Space Science Group <antonio.martin-carrillo(a)ucd.ie> A. Martin-Carrillo, E. Aasen, L. Brown, D. Colfer, M. Collins, J. Costello, C. Harris, R. Odunuga, H. O'Leary Jeffers, C. O'Malley, J. Parimkayala, J. Roca Garcia-Valino, R. Roddy, D. Scott, A. Valdivia y Alvarado Carvajal (UCD), A. Fernandez-Martin (CAHA), J. F. Agui Fernandez (CAHA), report on behalf of a larger collaboration: We observed the position of AT2026fgk, the likely counterpart to GRB 260310A (Fermi GBM team, GCN 43951; Salunke et al., GCN 43958; Konno et al., GCN 43974; Hinds et al., GCN 43977; Lipunov et al., GCN 43978; Martin-Carrillo et al., GCN 43979; Méndez et al., GCN 43980; de Ugarte Postigo et al., GCN 43984; Hsu et al., GCN 43986; Malesani et al., GCN 43990; Becerra et al., GCN 43991, Li et al., GCN 43993; Stein et al., GCN 43996; discovered by GOTO; O'Neill et al. 2026, TNS Discovery Report 294132) using the CAHA 1.23m telescope equipped with the DLR-MkIII CCD camera. A series of 3 x 150s exposures were taken in the BVRI bands starting at 2026-03-13T23:59:00 (~3.793 days after the Fermi trigger). The candidate is still well detected in the individual images with a preliminary AB magnitude of R = 18.3 +/- 0.1. Our photometry was calibrated using nearby stars from the Pan-STARRS catalogue and is neither corrected for Galactic extinction nor the host galaxy contribution. Comparing this new epoch with our previously reported R-band magnitude (Martin-Carrillo et al., GCN 43979) we infer a shallow decay with a power-law index of ~0.3, significantly shallower than the decay observed (~0.7) since the initial report by Konno et al., GCN 43974. These observations were made during the UCD Academy observing run at Calar Alto Observatory (Almeria, Spain) as part of the final year undergraduate projects of the University College Dublin BSc (Hons) in Physics with Astronomy and Space Science. View this GCN Circular online at https://gcn.nasa.gov/circulars/44000. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42120] Fermi GRB 260314A: Global MASTER-Net observations report
by GCN Circulars 14 Mar '26

14 Mar '26

TITLE: GCN CIRCULAR NUMBER: 43999 SUBJECT: Fermi GRB 260314A: Global MASTER-Net observations report DATE: 26/03/14 01:18:37 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 260314A ( Fermi GBM team, GCN 43997) errorbox 83 sec after trigger time at 2026-03-14 01:00:13 UT, with upper limit up to 18.8 mag. The observations began at zenith distance = 28 deg. The sun altitude is -26.8 deg. The galactic latitude b = 34 deg., longitude l = 92 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3185241 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 93 | 2026-03-14 01:00:13 | MASTER-Kislovodsk | (17h 29m 20.27s , +62d 52m 60.0s) | C | 20 | 17.8 | 134 | 2026-03-14 01:00:54 | MASTER-Kislovodsk | (17h 29m 20.09s , +62d 53m 03.0s) | C | 20 | 17.8 | 179 | 2026-03-14 01:01:34 | MASTER-Kislovodsk | (17h 29m 19.85s , +62d 53m 05.9s) | C | 30 | 18.1 | 234 | 2026-03-14 01:02:24 | MASTER-Kislovodsk | (17h 29m 19.53s , +62d 53m 09.3s) | C | 40 | 18.4 | 300 | 2026-03-14 01:03:25 | MASTER-Kislovodsk | (17h 29m 19.14s , +62d 53m 12.2s) | C | 50 | 18.5 | 380 | 2026-03-14 01:04:35 | MASTER-Kislovodsk | (17h 29m 18.64s , +62d 53m 15.1s) | C | 70 | 18.8 | 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/43999. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42119] Fermi GRB 260313A: Global MASTER-Net observations report
by GCN Circulars 14 Mar '26

14 Mar '26

TITLE: GCN CIRCULAR NUMBER: 43998 SUBJECT: Fermi GRB 260313A: Global MASTER-Net observations report DATE: 26/03/14 01:16:55 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 260313A ( Fermi GBM team, GCN 43987) errorbox 31381 sec after notice time and 31405 sec after trigger time at 2026-03-13 20:43:54 UT, with upper limit up to 18.7 mag. The observations began at zenith distance = 76 deg. The sun altitude is -49.0 deg. The galactic latitude b = 39 deg., longitude l = 17 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3184597 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 91 | 2026-03-13 12:01:49 | MASTER- | (16h 26m 25.94s , +10d 37m 52.9s) | C | 20 | 19.1 | 91 | 2026-03-13 12:01:49 | MASTER- | (16h 27m 45.04s , +10d 04m 45.6s) | C | 20 | 19.3 | 121 | 2026-03-13 12:02:19 | MASTER- | (16h 26m 25.91s , +10d 36m 25.9s) | C | 20 | 19.0 | 121 | 2026-03-13 12:02:19 | MASTER- | (16h 27m 45.05s , +10d 03m 19.4s) | C | 20 | 19.2 | 156 | 2026-03-13 12:02:49 | MASTER- | (16h 26m 28.86s , +10d 38m 02.1s) | C | 30 | 19.3 | 156 | 2026-03-13 12:02:49 | MASTER- | (16h 27m 48.04s , +10d 04m 55.7s) | C | 30 | 19.6 | 201 | 2026-03-13 12:03:29 | MASTER- | (16h 26m 23.44s , +10d 37m 13.5s) | C | 40 | 19.6 | 201 | 2026-03-13 12:03:29 | MASTER- | (16h 27m 42.65s , +10d 04m 07.8s) | C | 40 | 19.7 | 256 | 2026-03-13 12:04:19 | MASTER- | (16h 26m 22.44s , +10d 38m 13.7s) | C | 50 | 19.7 | 256 | 2026-03-13 12:04:19 | MASTER- | (16h 27m 41.66s , +10d 05m 08.4s) | C | 50 | 19.8 | 321 | 2026-03-13 12:05:19 | MASTER- | (16h 26m 30.02s , +10d 37m 13.3s) | C | 60 | 19.8 | 321 | 2026-03-13 12:05:19 | MASTER- | (16h 27m 49.26s , +10d 04m 08.7s) | C | 60 | 19.9 | 397 | 2026-03-13 12:06:30 | MASTER- | (16h 26m 22.89s , +10d 36m 13.8s) | C | 70 | 19.9 | 397 | 2026-03-13 12:06:30 | MASTER- | (16h 27m 42.12s , +10d 03m 09.8s) | C | 70 | 19.9 | 914 | 2026-03-13 12:15:13 | MASTER- | (16h 27m 20.26s , +10d 02m 33.4s) | C | 60 | 19.9 | 914 | 2026-03-13 12:15:13 | MASTER- | (16h 26m 01.06s , +10d 35m 40.9s) | C | 60 | 19.7 | 1058 | 2026-03-13 12:17:36 | MASTER- | (16h 21m 46.15s , +08d 09m 04.5s) | C | 60 | 19.8 | 1058 | 2026-03-13 12:17:36 | MASTER- | (16h 20m 27.41s , +08d 42m 10.1s) | C | 60 | 19.7 | 1131 | 2026-03-13 12:18:49 | MASTER- | (16h 29m 54.57s , +08d 10m 15.0s) | C | 60 | 19.9 | 1131 | 2026-03-13 12:18:49 | MASTER- | (16h 28m 35.81s , +08d 43m 20.6s) | C | 60 | 19.7 | 1644 | 2026-03-13 12:27:23 | MASTER- | (16h 27m 24.44s , +10d 02m 47.0s) | C | 60 | 19.9 | 1644 | 2026-03-13 12:27:23 | MASTER- | (16h 26m 05.20s , +10d 35m 52.9s) | C | 60 | 19.7 | 1787 | 2026-03-13 12:29:45 | MASTER- | (16h 21m 44.33s , +08d 09m 55.3s) | C | 60 | 19.8 | 1787 | 2026-03-13 12:29:45 | MASTER- | (16h 20m 25.58s , +08d 42m 59.8s) | C | 60 | 19.7 | 1859 | 2026-03-13 12:30:57 | MASTER- | (16h 29m 49.96s , +08d 10m 36.5s) | C | 60 | 19.8 | 1859 | 2026-03-13 12:30:57 | MASTER- | (16h 28m 31.19s , +08d 43m 41.1s) | C | 60 | 19.7 | 2387 | 2026-03-13 12:39:45 | MASTER- | (16h 26m 07.46s , +10d 36m 46.3s) | C | 60 | 19.4 | 2387 | 2026-03-13 12:39:45 | MASTER- | (16h 24m 53.49s , +11d 09m 55.3s) | C | 60 | 19.5 | 2530 | 2026-03-13 12:42:08 | MASTER- | (16h 19m 23.33s , +09d 16m 12.3s) | C | 60 | 19.2 | 2530 | 2026-03-13 12:42:08 | MASTER- | (16h 20m 36.37s , +08d 43m 04.5s) | C | 60 | 19.1 | 2601 | 2026-03-13 12:43:19 | MASTER- | (16h 27m 22.55s , +09d 14m 45.8s) | C | 60 | 19.3 | 2601 | 2026-03-13 12:43:19 | MASTER- | (16h 28m 35.59s , +08d 41m 38.2s) | C | 60 | 19.0 | 3152 | 2026-03-13 12:52:30 | MASTER- | (16h 26m 13.15s , +10d 36m 57.7s) | C | 60 | 18.0 | 3152 | 2026-03-13 12:52:30 | MASTER- | (16h 24m 59.66s , +11d 10m 07.2s) | C | 60 | 18.2 | 3298 | 2026-03-13 12:54:56 | MASTER- | (16h 20m 35.88s , +08d 42m 46.2s) | C | 60 | 17.7 | 3298 | 2026-03-13 12:54:56 | MASTER- | (16h 19m 23.36s , +09d 15m 54.5s) | C | 60 | 17.8 | 3370 | 2026-03-13 12:56:08 | MASTER- | (16h 27m 25.46s , +09d 16m 34.4s) | C | 60 | 17.7 | 3370 | 2026-03-13 12:56:08 | MASTER- | (16h 28m 38.01s , +08d 43m 26.8s) | C | 60 | 17.4 | 31435 | 2026-03-13 20:43:54 | MASTER-Kislovodsk | (15h 57m 41.97s , +04d 46m 40.9s) | C | 60 | 18.1 | 31540 | 2026-03-13 20:45:38 | MASTER-Kislovodsk | (16h 01m 07.45s , +06d 40m 48.5s) | C | 60 | 18.1 | 31645 | 2026-03-13 20:47:24 | MASTER-Kislovodsk | (15h 48m 59.18s , +06d 43m 14.5s) | C | 60 | 18.1 | 31753 | 2026-03-13 20:49:11 | MASTER-Kislovodsk | (15h 55m 31.20s , +02d 53m 04.3s) | C | 60 | 18.2 | 31853 | 2026-03-13 20:50:52 | MASTER-Kislovodsk | (15h 53m 31.18s , +08d 36m 59.4s) | C | 60 | 18.3 | 31960 | 2026-03-13 20:52:39 | MASTER-Kislovodsk | (15h 54m 36.75s , +08d 36m 58.4s) | C | 60 | 12.5 | 41297 | 2026-03-13 23:28:15 | MASTER-Kislovodsk | (16h 09m 55.10s , +04d 56m 04.0s) | C | 60 | 17.9 | 41401 | 2026-03-13 23:29:59 | MASTER-Kislovodsk | (16h 05m 46.45s , +08d 42m 26.9s) | C | 60 | 18.5 | 41506 | 2026-03-13 23:31:44 | MASTER-Kislovodsk | (16h 07m 41.96s , +03d 01m 52.5s) | C | 60 | 18.3 | 41604 | 2026-03-13 23:33:22 | MASTER-Kislovodsk | (16h 13m 25.35s , +06d 48m 48.5s) | C | 60 | 18.4 | 41707 | 2026-03-13 23:35:05 | MASTER-Kislovodsk | (15h 59m 05.81s , +10d 38m 10.3s) | C | 60 | 18.7 | 41820 | 2026-03-13 23:36:58 | MASTER-Kislovodsk | (15h 43m 40.10s , +03d 02m 39.4s) | C | 60 | 18.1 | 42252 | 2026-03-13 23:44:10 | MASTER-Kislovodsk | (15h 54m 29.49s , +01d 08m 26.1s) | C | 60 | 18.5 | 42360 | 2026-03-13 23:45:58 | MASTER-Kislovodsk | (15h 41m 30.91s , +08d 43m 08.7s) | C | 60 | 18.6 | 42478 | 2026-03-13 23:47:56 | MASTER-Kislovodsk | (15h 37m 05.30s , +06d 50m 16.8s) | C | 60 | 18.6 | 42581 | 2026-03-13 23:49:39 | MASTER-Kislovodsk | (15h 46m 50.58s , +10d 36m 59.0s) | C | 60 | 18.6 | 42681 | 2026-03-13 23:51:19 | MASTER-Kislovodsk | (16h 06m 25.20s , +01d 06m 49.4s) | C | 60 | 18.4 | 42802 | 2026-03-13 23:53:20 | MASTER-Kislovodsk | (16h 11m 16.05s , +10d 36m 20.0s) | C | 60 | 18.4 | 42914 | 2026-03-13 23:55:12 | MASTER-Kislovodsk | (16h 12m 12.42s , +10d 36m 20.3s) | C | 60 | 13.0 | 43021 | 2026-03-13 23:56:59 | MASTER-Kislovodsk | (16h 13m 46.32s , +10d 36m 17.0s) | C | 60 | 12.9 | 43195 | 2026-03-13 23:59:53 | MASTER-Kislovodsk | (16h 19m 39.08s , +03d 02m 31.4s) | C | 60 | 18.3 | 43305 | 2026-03-14 00:01:43 | MASTER-Kislovodsk | (15h 33m 51.88s , +04d 55m 55.3s) | C | 60 | 18.1 | 43425 | 2026-03-14 00:03:43 | MASTER-Kislovodsk | (15h 42m 27.14s , +01d 09m 22.2s) | C | 60 | 18.2 | 43540 | 2026-03-14 00:05:39 | MASTER-Kislovodsk | (15h 53m 26.55s , +12d 31m 34.8s) | C | 60 | 18.3 | 43643 | 2026-03-14 00:07:21 | MASTER-Kislovodsk | (16h 25m 31.18s , +06d 50m 11.1s) | C | 60 | 17.6 | 43748 | 2026-03-14 00:09:06 | MASTER-Kislovodsk | (16h 05m 42.64s , +12d 31m 14.8s) | C | 60 | 18.1 | 43962 | 2026-03-14 00:12:40 | MASTER-Kislovodsk | (15h 54m 17.96s , -00d 44m 27.8s) | C | 60 | 12.1 | 46601 | 2026-03-14 00:56:39 | MASTER-Kislovodsk | (16h 06m 19.90s , -00d 45m 06.5s) | C | 60 | 17.9 | 46699 | 2026-03-14 00:58:17 | MASTER-Kislovodsk | (16h 18m 28.04s , +01d 10m 17.3s) | C | 60 | 18.1 | 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/43998. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42118] GRB 260314A: Fermi GBM Final Real-time Localization
by GCN Circulars 14 Mar '26

14 Mar '26

TITLE: GCN CIRCULAR NUMBER: 43997 SUBJECT: GRB 260314A: Fermi GBM Final Real-time Localization DATE: 26/03/14 01:09:31 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 LONG GRB At 00:58:50 UT on 14 Mar 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260314A (trigger 795142735.353478 / 260314041). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 260.2, Dec = 62.9 (J2000 degrees, equivalent to J2000 17h 20m, 62d 53'), with a statistical uncertainty of 8.2 degrees. The angle from the Fermi LAT boresight is 59.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260314041/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260314041/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260314041/… View this GCN Circular online at https://gcn.nasa.gov/circulars/43997. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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