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[vsnet-grb-info 41821] Fermi GBM Sub-Threshold Detection of GRB 260211A
by GCN Circulars 12 Feb '26

12 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43713 SUBJECT: Fermi GBM Sub-Threshold Detection of GRB 260211A DATE: 26/02/12 14:47:00 GMT FROM: rhamburg(a)usra.edu R. Hamburg (USRA) reports on behalf of the Fermi-GBM Team: SVOM/ECLAIRs detected GRB 260211A on 2026-02-11 at 19:24:33 UTC (GCN 43705). There was no Fermi-GBM onboard trigger around this time. An automated, blind search for gamma-ray bursts below the onboard triggering threshold in Fermi-GBM identified no candidates. The GBM Targeted Search [1], the most sensitive coherent search for GRB-like signals in GBM, identified a transient starting 0.8 seconds after the ECLAIRs trigger time, most significantly on the 16 s timescale and with a false alarm rate of 4.3e-05 Hz. The Fermi-MET of this transient is 792530678.844 s. The Targeted Search localization is consistent with the ECLAIRs location. Additionally, the GBM Targeted Search transient was found with highest significance using a soft spectral template (i.e., Band function with Epeak = 70 keV, alpha = -1.9, beta = -3.7). [1] Goldstein et al. 2019 arXiv:1903.1259 View this GCN Circular online at https://gcn.nasa.gov/circulars/43713. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41820] Konus-Wind detection of GRB 260207B
by GCN Circulars 12 Feb '26

12 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43712 SUBJECT: Konus-Wind detection of GRB 260207B DATE: 26/02/12 14:06:38 GMT FROM: Dmitry Svinkin at Ioffe Institute <svinkin(a)mail.ioffe.ru> D. Svinkin, D. Frederiks, A. Lysenko, A. Ridnaia, A. Tsvetkova, M. Ulanov, and T. Cline on behalf of the Konus-Wind team, report: The short-duration GRB with extended emission (EE) GRB 260207B (Fermi-GBM detection: Fermi GBM team, GCN 43629; Sonawane & Bala, GCN 43634; GECAM-B detection: Zao et al., GCN 43644; AstroSat-CZTI detection: Goyal et al., GCN 43680; IPN triangulation: Kozyrev et al., GCN 43691; GRID detection: Zeng et al., GCN 43710) triggered Konus-Wind at T0=47529.467 s UT (13:12:09.467). The burst light curve shows a short initial pulse, which starts at ~T0-40 ms and has a duration of ~220 ms. The initial pulse is followed by a weaker extended emission (EE), starting at ~T0+9 s, peaking at ~T0+43 s, and lasting up to ~T0+95 s. The emission in the initial pulse is seen up to ~2 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB260207_T47529/ As observed by Konus-Wind, the initial pulse had the fluence of 2.66(-0.19,+0.20)x10^-6 erg/cm2, and the 16-ms peak flux, measured from T0+0.104 s, of 4.41(-0.54,+0.58)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum of the initial pulse (measured from T0 to T0+0.192 s) is best fit in the 20 keV - 10 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -0.99(-0.08,+0.08) and Ep = 495(-60,+72) keV (chi2 = 44/43 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -3.1 (chi2 = 44/42 dof). The time-averaged spectrum of the EE (measured from T0+8.448 s to T0+73.984 s) is best fit in the 20 keV - 10 MeV range by a power law with exponential cutoff model: with alpha = -1.67(-0.21,+0.24) and Ep = 44 (-19,+11) keV (chi2 = 93/98 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -3.0 (chi2 = 93/97 dof). From this spectrum, the total EE fluence is 5.02(-0.4,+0.4)x10^-6 erg/cm2, a factor of ~2 higher than that of the initial pulse. All the quoted errors are at the 68% confidence level. All the quoted values are preliminary. View this GCN Circular online at https://gcn.nasa.gov/circulars/43712. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41819] GRB 260208A: Swift UVOT detection
by GCN Circulars 12 Feb '26

12 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43702 SUBJECT: GRB 260208A: Swift UVOT detection DATE: 26/02/11 17:42:26 GMT FROM: Paul Kuin at MSSL <npkuin(a)gmail.com> Paul Kuin (MSSL/UCL) and Brad Cenko (NSA/GSFC) reports on behalf of the Swift/UVOT team: The Swift/UVOT began observations of the Fermi-detected GRB 260208A 35.4 ks after the Fermi Trigger (Fermi GBM team, GCN Circ. 43635; Longo et al., GCN Circ. 43645). We detect the afterglow at the position given by Podesta et al., GCN Circ. 43640. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white 35662.9 41566.1 1208 20.84 +/-0.10 white 46325.8 47072.6 735 21.45 +/-0.21 u 35131.3 40857.7 1208 20.34 +/-0.14 u 45572.3 46319.1 735 20.12 +/-0.15 v 36195.1 47089.2 938 20.01 +/-0.32 View this GCN Circular online at https://gcn.nasa.gov/circulars/43702. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41818] GRB 260128B: SVOM/ECLAIRs refined analysis
by GCN Circulars 12 Feb '26

12 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43711 SUBJECT: GRB 260128B: SVOM/ECLAIRs refined analysis DATE: 26/02/12 09:13:11 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> M. Brunet, O. Godet (IRAP), S. Le Stum, A. Coleiro (APC) on behalf of the ECLAIRs team Using the event-by-event data downloaded through the X-band ground station, we report further analysis of ECLAIRs observations of GRB 260128B (GCN 43561). The burst that triggered ECLAIRs consists of a single peak lasting around 10 s in the 4-50 keV energy band. The time-averaged spectrum from T0-9.24 s to T0-0.24 s (T0 = 2026-01-28T06:48:34.72 UT) in the energy range 4-50 keV is not well fitted by a simple powerlaw model. This indicates some spectral curvature. Using a blackbody with a temperature kT = (2.29 +0.22/-0.20) keV provides a good fit. With this model, the fluence in the energy range 4-120 keV is (1.04 +0.05/-0.30) e-7 erg/cm². Using either a broken power law or a power law with an exponential cutoff provides acceptable fits. However, given the faintness of the event, the model parameters remain poorly constrained. All the quoted errors are at the 68% confidence level. The Space-based multi-band astronomical Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA), French Space Agency (CNES), and the Chinese Academy of Sciences (CAS), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. ECLAIRs was developed jointly by CNES, CEA-IRFU, CNRS-IRAP, CNRS-APC. The SVOM/ECLAIRs point of contact for this burst is: Marius Brunet (IRAP) (marius.brunet at irap.omp.eu) View this GCN Circular online at https://gcn.nasa.gov/circulars/43711. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41817] GRID detection of GRB 250207B
by GCN Circulars 12 Feb '26

12 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43710 SUBJECT: GRID detection of GRB 250207B DATE: 26/02/12 08:33:36 GMT FROM: GRID Student Team at Tsinghua University <grid(a)tsinghua.edu.cn> Ming Zeng, Chenyu Wang, Longhao Li, Zirui Yang report on behalf of the GRID Collaboration: GRID reports the detection of GRB 250207B, which was also observed by Fermi-GBM (Fermi GBM team, GCN 43629; Sonawane & Bala, GCN 43634), GECAM-B (Zao et al., GCN 43644), and AstroSat CZTI (Goyal et al., GCN 43680). The event triggered GRID-09B, GRID-10B, and GRID-11B at T0 = 2026-02-07 13:12:10 UTC. This burst was simultaneously detected by three GRID nanosatellites, marking the first event jointly observed by three GRID satellites. Temporal analysis of the main emission yields a duration of T90 = 0.42 ± 0.08 s in the 30–2000 keV energy range. Although extended emission appears to be present, the limited sensitivity of GRID does not allow for a detailed characterization of this component. At the trigger time, GRID-10B was operating in 1 s bin mode, which prevents a refined localization. Nevertheless, the reconstructed direction is consistent with the position reported by Fermi-GBM. At present, only the GRID light curve is available. Spectral analysis is not yet reported. The GRID light curve of this event can be found at https://mirrors.tuna.tsinghua.edu.cn/GRID/data/GRID-GCN/GRB260207B/GRID_GRB… GRID is a student-led project to monitor the transient gamma-ray sky with multiple detectors onboard different nanosatellites in the era of multi-messenger astronomy. For more information about GRID, please refer to: https://doi.org/10.1007/s10686-019-09636-w, https://doi.org/10.1007/s10686-021-09819-4. View this GCN Circular online at https://gcn.nasa.gov/circulars/43710. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41816] GRB 260211A: LCO optical upper limits
by GCN Circulars 12 Feb '26

12 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43709 SUBJECT: GRB 260211A: LCO optical upper limits DATE: 26/02/12 08:30:28 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> C. Wu (NAOC), A. Saccardi (CEA/Irfu), D. Turpin (CEA/Irfu), D. Gotz (CEA/Irfu), D. Adrien (CEA/Irfu), report on behalf of the SVOM mission team: We observed the field of GRB 260211A (Gotz et al., GCN 43705) with the LCO 1-m telescope at Cerro Tololo Interamerican Observatory equipped with the Sinistro instrument. Our observation started on 2026-02-12 at 02:37:50 UT (about 7.22 hr after the trigger) and we obtained 3x200 s exposures in the SDSS r filter. In the stacked image, we do not detect any new source within the SVOM/ECLAIRs error box, in agreement with Globus et al. (GCN 43707). We measure the following upper limit calibrated against the UCAC4 catalog, and not corrected for Galactic extinction: r > 22.2 AB (5-sigma, mid-time 7.28 hr after the trigger). This project is funded by the SVOM collaboration. View this GCN Circular online at https://gcn.nasa.gov/circulars/43709. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41815] GRB260131A/B: 3.6m DOT Optical Observations
by GCN Circulars 12 Feb '26

12 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43708 SUBJECT: GRB260131A/B: 3.6m DOT Optical Observations DATE: 26/02/12 07:33:33 GMT FROM: ANSHIKA GUPTA at ARIES <anshika05180(a)gmail.com> Anshika Gupta, Kuntal Misra, Debalina Kar, Pankaj Pawar, and Dhruv Jain (ARIES) report: We observed the field of GRB 260131A/B detected by (Fermi GBM team; GCN 43579) with the 3.6m Devasthal Optical Telescope (DOT), located at the Devasthal Observatory of the Aryabhatta Research Institute of Observational Sciences (ARIES), India. The observations were started on 2026-02-08 at 14:20:45 UT, i.e., ~8.32 days after the Fermi trigger. We have taken multiple frames with an exposure time of 300s in the R filter. We stacked the images after the alignment. We detect an optical counterpart in our stacked image at the location reported by (Gompertz et al. 2026; GCN 43586). We obtain the following preliminary magnitude in the stacked image: Date Start_UT T_start-T0(days) Filter Exp time(s) Magnitude ================================================================== 2026-02-08 14:20:45 ~8.32 R 300s*16 21.76 +/-0.03 Our detection is consistent with Gompertz et al. 2026 (GCN 43586); Lee et al. 2026 (GCN 43587); Saccardi et al. 2026 (GCN 43595); García García et al. 2026 (GCN 43599); Shi et al. 2026 (GCN 43601); Jayaraman et al. 2026 (GCN 43606); Zhu et al. 2026 (GCN 43607); Zheng et al. 2026 (GCN 43609); Adami et al. 2026 (GCN 43610); Volnova et al. 2026 (GCN 43632, 43670). The magnitude is not corrected for the Galactic extinction in the direction of the burst. Photometric calibration is performed using the standard stars from the USNO-B1.0 catalogue. View this GCN Circular online at https://gcn.nasa.gov/circulars/43708. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41814] GRB 260211A: SVOM/COLIBRÍ (FM-GFT) optical upper limits
by GCN Circulars 12 Feb '26

12 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43707 SUBJECT: GRB 260211A: SVOM/COLIBRÍ (FM-GFT) optical upper limits DATE: 26/02/12 05:39:25 GMT FROM: globus(a)astro.unam.mx Noémie Globus (UNAM), Damien Dornic (CPPM), Alan M. Watson (UNAM), Stéphane Basa (UAR Pytheas), William H. Lee (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), Jean-Grégoire Ducoin (CPPM), Francis Fortin (IRAP), 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), N. A. Rakotondrainibe (LAM), Fredd Sánchez Álvarez (UNAM), Benjamin Schneider (LAM), Antonio de Ugarte Postigo (LAM), and Diego Gotz (CEA/Irfu) report: We imaged the field of GRB 260211A (Gotz et al., GCN Circ. 43705) using the DDRAGO wide-field imager on the SVOM/COLIBRÍ (FM-GFT) telescope. We observed from 2026-02-12 04:19 UTC to 05:20 UTC (from 8.9 to 9.9 hours after the trigger) and obtained 30 minutes of simultaneous exposure in the r and z filters. The data were reduced 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. WIthin the 5.7 arcmin error circle (Gotz et al., GCN Circ. 43705), and comparing to the PS1 catalog and images, we do not detect any new sources to preliminary 5-sigma limiting magnitudes of: r > 23.0, z > 21.6. Further observations 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/43707. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41813] Fermi trigger No 792537871: Global MASTER-Net observations report
by GCN Circulars 12 Feb '26

12 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43706 SUBJECT: Fermi trigger No 792537871: Global MASTER-Net observations report DATE: 26/02/12 03:45:23 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-Kislovodsk robotic telescope [1] located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB260211.89 (trigger No 792537871,23h 48m 28.80s , +30d 46m 12.0s, R=34.27) errorbox 18265 sec after notice time and 18297 sec after trigger time at 2026-02-12 02:29:23 UT, with upper limit up to 17.2 mag. The observations began at zenith distance = 78 deg. The sun altitude is -19.5 deg. The galactic latitude b = -30 deg., longitude l = 108 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3130746 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 18327 | 2026-02-12 02:29:23 | MASTER-Kislovodsk | (21h 58m 56.93s , +35d 01m 22.9s) | C | 60 | 16.3 | 18530 | 2026-02-12 02:32:46 | MASTER-Kislovodsk | (21h 44m 21.28s , +31d 13m 22.2s) | C | 60 | 16.7 | 18633 | 2026-02-12 02:34:29 | MASTER-Kislovodsk | (21h 44m 08.70s , +35d 03m 08.1s) | C | 60 | 17.2 | 18737 | 2026-02-12 02:36:13 | MASTER-Kislovodsk | (22h 16m 28.22s , +36d 53m 34.1s) | C | 60 | 16.8 | 18843 | 2026-02-12 02:37:59 | MASTER-Kislovodsk | (22h 01m 25.76s , +36d 55m 41.2s) | C | 60 | 16.9 | 18950 | 2026-02-12 02:39:46 | MASTER-Kislovodsk | (21h 46m 16.13s , +36d 55m 11.8s) | C | 60 | 17.1 | 19053 | 2026-02-12 02:41:29 | MASTER-Kislovodsk | (21h 58m 25.10s , +31d 13m 00.7s) | C | 60 | 17.0 | 19157 | 2026-02-12 02:43:13 | MASTER-Kislovodsk | (21h 57m 53.44s , +33d 06m 38.0s) | C | 60 | 16.8 | 19268 | 2026-02-12 02:45:04 | MASTER-Kislovodsk | (21h 32m 38.88s , +29d 21m 20.9s) | C | 60 | 17.1 | 19375 | 2026-02-12 02:46:51 | MASTER-Kislovodsk | (21h 29m 10.76s , +33d 10m 27.5s) | C | 60 | 17.1 | 19483 | 2026-02-12 02:48:38 | MASTER-Kislovodsk | (22h 12m 19.53s , +33d 07m 06.1s) | C | 60 | 16.8 | 19614 | 2026-02-12 02:50:50 | MASTER-Kislovodsk | (21h 49m 55.83s , +27d 26m 35.5s) | C | 60 | 16.7 | 19846 | 2026-02-12 02:54:42 | MASTER-Kislovodsk | (21h 41m 32.63s , +25d 32m 40.8s) | C | 60 | 16.6 | 19963 | 2026-02-12 02:56:39 | MASTER-Kislovodsk | (22h 05m 28.01s , +38d 49m 01.7s) | C | 60 | 17.0 | 20093 | 2026-02-12 02:58:49 | MASTER-Kislovodsk | (22h 12m 30.29s , +31d 13m 05.4s) | C | 60 | 16.3 | 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/43706. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41812] GRB 260211A: SVOM detection of a burst
by GCN Circulars 11 Feb '26

11 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43705 SUBJECT: GRB 260211A: SVOM detection of a burst DATE: 26/02/11 19:49:48 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> D. Gotz, D. ADRIEN, D. Turpin , S. Schanne (CEA), T. Maiolino (LUPM), report on behalf of the SVOM mission team: At 2026-02-11T19:24:33 UTC (T0), SVOM/ECLAIRs triggered and located the gamma-ray burst GRB 260211A (SVOM burst-id sb26021102). The following trigger information was received on the ground with low latency by the SVOM VHF Alert Network. The burst was detected both by the Count-Rate Trigger (CRT) and the Image Trigger (IMT), which produced a sequence of 22 alerts. CRT provided the alert with the best signal-to-noise-ratio in the image (SNR) of 14.48 in the [5-20] keV energy band over a time window of 20.40 seconds starting at 2026-02-11T19:24:28. The localization of the best alert is R.A., Dec. 86.9994, -0.4306 degrees: R.A. (J2000) = 5h47m59.85s Dec. (J2000) = -0d25m50.14s with a 90% confidence level (C.L.) radius of 5.68 arcmin (including systematic error of 2 arcmin added in quadrature). The SVOM/ECLAIRs light curve showed a single/multiple broad/narrow peak structure with a T90 duration of about 15.15 (-1.54/+1.27) (5-120 keV). This burst was also detected by SVOM/GRM with a significance of 12.50. The SVOM/GRM light curve showed a single/multiple broad/narrow peak structure with a T90 duration of about 27.45(-8.13/+6.72) (4-550 keV). Due to satellite constraints, no immediate slew was performed on this burst. No X-ray observation could be performed by SVOM/MXT for the time being.No optical observation could be performed by SVOM/VT for the time being. 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 Diego Gotz: diego.gotz(a)cea.fr. Please contact the BA by email if you require additional information. View this GCN Circular online at https://gcn.nasa.gov/circulars/43705. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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