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[vsnet-grb-info 41840] EP260213a: SVOM/C-GFT upper limit
by GCN Circulars 14 Feb '26

14 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43731 SUBJECT: EP260213a: SVOM/C-GFT upper limit DATE: 26/02/14 09:22:49 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> C. Wu (NAOC), Z. Kang (CHO), L.P. Xin, X.H. Han, P.P. Zhang, X.M. Lu (NAOC), Z.W. Li, Y. Lv (CHO), R.S. Zhang, Y.J. Xiao, Y.L. Qiu, J. Wang, J.S. Deng, L. Huang, J.Y. Wei (NAOC) report on behalf of the SVOM/C-GFT team: We observed the field of EP260213a (ID:01709258378) detected by EP/WXT (Yang et al., GCN 43729) with LATIOS on SVOM/C-GFT. Observations started at 2026-02-13T19:58:40 UTC, ~6.78 min after the trigger. We obtained g, r, and i-band follow-up imaging. After preliminary analysis，no credible candidate was detected within the error box provided by EP/FXT (Li et al., GCN 43730) in our images. The 3-sigma upper limits are: | Mid_t - T0 (min) | Exposure Time (s) | Band | Upper Limit (AB) | |----------------|-------------------|------|------------------| | 10.76 | 6×30 | g | 19.9 | | 13.75 | 11×30 | i | 19.8 | | 15.28 | 6×30 | r | 19.9 | The photometry was calibrated against Pan-STARRS1 stars and no correction for Galactic dust extinction was applied. Our result is consistent with GCN 43728 (Cotter et al.) We thank the observation assistants Hong-Xu Xue and Bo-Wen Li at Jilin observatory for their excellent support. The Chinese Ground Follow-up Telescope (C-GFT) for the SVOM mission is located at Jilin Station, Changchun Observatory, National Astronomical Observatories, CAS. It features two instruments: (1) CATCH at the Cassegrain focus with a 21 arcsec x 21 arcsec FOV for simultaneous g/r/i-band imaging, and (2) LATIOS, a 4k x 4k CMOS camera at the prime focus with a 1.28 deg x 1.28 deg FOV that images in g, r, and i bands via filter switching. View this GCN Circular online at https://gcn.nasa.gov/circulars/43731. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41839] EP260213a: refined analysis of the EP-FXT observation
by GCN Circulars 14 Feb '26

14 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43730 SUBJECT: EP260213a: refined analysis of the EP-FXT observation DATE: 26/02/14 06:39:43 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> R.-Z. Li (YNAO, CAS), J. Yang (ZZU), X. Tian (GXU), W. D. Zhang (NAOC) on behalf of the Einstein Probe (EP) team: The fast X-ray transient EP260213a triggered the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) mission (Yang et al., GCN 43729), and was followed by NOT (Cotter et al., GCN 43728). The autonomous observation by the Follow-up X-ray Telescope (FXT) was performed at 2026-02-13T20:03:06 (UTC), about 5 minutes after T0. The effective exposure time of this observation is around 4.7 ks. The on-ground analysis shows that an uncatalogued source was detected at R.A. = 167.0070, DEC = 3.9470 (J2000) with an uncertainty of 10 arcsec in radius (90% C.L. statistical and systematic). The average 0.5-10 keV spectrum can be fitted with an absorbed power law with a fixed Galactic hydrogen column density of 5.60 × 10^20 cm^-2 and a photon index of 2.18 (-0.15/+0.16). The derived average unabsorbed 0.5-10 keV flux is 1.77 (-0.17/+0.19) × 10^(-12) erg/cm^2/s. The uncertainties are at the 90% confidence level for the above parameters. Further FXT follow-up observations have been arranged. 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/43730. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41838] EP260213a: Einstein Probe detection of a fast X-ray transient
by GCN Circulars 14 Feb '26

14 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43729 SUBJECT: EP260213a: Einstein Probe detection of a fast X-ray transient DATE: 26/02/14 02:42:27 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> J. Yang (ZZU), R.-Z. Li (YNAO, CAS), X. Tian (GXU), W. D. Zhang (NAOC) 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 EP260213a. The transient triggered EP-WXT (ID: 01709258378) at 2026-02-13T19:58:40 (UTC). The WXT position of the source is R.A. = 167.008 deg, DEC = 3.965 deg (J2000) with an uncertainty of 3 arcmin in radius (90% C.L. statistical and systematic). The preliminary analysis of the WXT data shows that the event started at T0=2026-02-13T19:58:00 (UTC), and lasted for approximately 40 seconds. The average WXT 0.5-4 keV spectrum can be fitted with an absorbed power law with a fixed Galactic hydrogen column density of 5.60 × 10^20 cm^-2 and a photon index of 0.6 (+/-0.6). The derived average unabsorbed 0.5-4 keV flux is 1.4 (-0.4/+0.5) × 10^(-9) erg/s/cm^2. 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. = 167.0083 deg, DEC = 3.9451 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/43729. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41837] EP/WXT 01709258378: NOT optical upper limits
by GCN Circulars 14 Feb '26

14 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43728 SUBJECT: EP/WXT 01709258378: NOT optical upper limits DATE: 26/02/14 01:29:01 GMT FROM: Laura Cotter at University College Dublin <laura.cotter(a)ucdconnect.ie> L. Cotter (UCD), G. Corcoran (UCD), A. Martin-Carrillo (UCD), D. B. Malesani (DAWN/NBI and Radboud), F. E. Bauer (SSI and UTA) and P. G. Jonker (Radboud) report on behalf of a larger collaboration: We observed the field of the fast X-ray transient WXT 01709258378 using the Nordic Optical Telescope (NOT) equipped with the ALFOSC camera. Observations were obtained in the SDSS r (3x300 s) and z (5x200 s) bands, starting on 2026-02-13 at 23:08:39 UT (3.17 hours after the WXT trigger). We do not find any new, uncatalogued sources within the EP/WXT uncertainty region. From the stacked images we obtain the following 3-sigma upper limits: r>24.0 z>22.3 These limits are in the AB system, were calibrated using nearby stars from the Pan-STARRS catalog and are not corrected for Galactic extinction. View this GCN Circular online at https://gcn.nasa.gov/circulars/43728. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41836] GRB 260212A: SVOM/GRM observation of a long burst
by GCN Circulars 14 Feb '26

14 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43727 SUBJECT: GRB 260212A: SVOM/GRM observation of a long burst DATE: 26/02/14 01:04:56 GMT FROM: zhangjinpeng(a)ihep.ac.cn SVOM/GRM team: Jin-Peng Zhang, Chen-Wei Wang, Shi-Jie Zheng, Yue Huang, Shao-Lin Xiong, Shuang-Nan Zhang (IHEP) SVOM/ECLAIRs team: Frédéric Daigne (IAP), Olivier GODET (IRAP) Report on behalf of the SVOM team: SVOM/GRM was triggered in-flight by GRB 260212A at 2026-02-12T17:49:08.000 (T0), which is also detected by Fermi/GBM (Fermi GBM Team, GCN #43716) and Glowbug (C.C. Cheung et al., GCN #43719). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of multiple pulses with a T90 of 23.6 +1.4/-1.4 s in the 15-5000 keV band. The SVOM/GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb260212A.png In addition, the position of this burst, according to Fermi/GBM localization (RA = 228.9, Dec = 74.1, Fermi GBM Team, GCN #43716), is located at about 53 degrees from the SVOM optical axis, which is outside the ECLAIRs field of view. ECLAIRs was not collecting data at the time of this burst. With this localization, the time-averaged spectrum from T0-1.0 to T0+11.0 s is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -0.87 +0.07/-0.07 and the cutoff energy, parameterized as Epeak, is 116 +6/-5 keV. The event fluence (10-1000 keV) in this time interval is (7.24 +0.20/-0.19)E-06 erg/cm^2. The 1s peak spectrum, measured from T0+8.8 to T0+9.8 s, is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -1.03 +0.09/-0.08 and the cutoff energy, parameterized as Epeak, is 157 +16/-13 keV. The flux (10-1000 keV) in this time interval is (1.88 +0.09/-0.08)E-06 erg/cm^2/s. The localization of GRB 260212A in the 'Amati' relation diagram is shown at: https://www.bursthub.cn//admin/static/svgrb260212A_amati.png And the localization in the 'Yonetoku' relation diagram is shown at: https://www.bursthub.cn//admin/static/svgrb260212A_yonetoku.png The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. GRM is developed by the Institute of High Energy Physics (IHEP) of CAS. The SVOM/GRM point of contact for this burst is: Jin-Peng Zhang (IHEP) (zhangjinpeng(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/43727. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41835] GRB 260213B: Fermi GBM Final Localization
by GCN Circulars 13 Feb '26

13 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43726 SUBJECT: GRB 260213B: Fermi GBM Final Localization DATE: 26/02/13 18:38:56 GMT FROM: oindabimukherjee(a)gmail.com The Fermi GBM team reports the detection of a likely LONG GRB "At 17:40:09.97 UT on 13 February 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260213B (trigger 792697214/260213736). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 145.98, Dec = -40.63 (J2000 degrees, equivalent to J2000 9h 43m, -40d 37'), with a statistical uncertainty of 3.63 degrees. The angle from the Fermi LAT boresight is 95 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260213736/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260213736/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260213736/…" View this GCN Circular online at https://gcn.nasa.gov/circulars/43726. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41834] GRB 260213B: Fermi GBM Final Localization
by GCN Circulars 13 Feb '26

13 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43726 SUBJECT: GRB 260213B: Fermi GBM Final Localization DATE: 26/02/13 18:38:56 GMT FROM: oindabimukherjee(a)gmail.com The Fermi GBM team reports the detection of a likely LONG GRB "At 17:40:09.97 UT on 13 February 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260213B (trigger 792697214/260213736). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 145.98, Dec = -40.63 (J2000 degrees, equivalent to J2000 9h 43m, -40d 37'), with a statistical uncertainty of 3.63 degrees. The angle from the Fermi LAT boresight is 95 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260213736/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260213736/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260213736/…" View this GCN Circular online at https://gcn.nasa.gov/circulars/43726. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41833] GRB 260213A: BALROG localization (Fermi Trigger 792697214 / GRB 260213736)
by GCN Circulars 13 Feb '26

13 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43725 SUBJECT: GRB 260213A: BALROG localization (Fermi Trigger 792697214 / GRB 260213736) DATE: 26/02/13 18:16:48 GMT FROM: Jochen Greiner at MPE <jcgrog(a)mpe.mpg.de> T. Preis (University of Innsbruck) & J. Greiner (MPE Garching) report: The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger 792697214 at 17:40:09 on 13 Feb. 2026 were automatically fitted for spectrum and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427; Berlato et al. 2019, ApJ 873, 60). The best-fit position is: RA(2000.0) = 155.7 deg Decl.(2000.0) = -45.6 deg The 1 sigma statistical error radius is 1.6 deg. We estimate an additional systematic error of 1 deg. Further details are available at: https://grb.mpe.mpg.de/grb/GRB260213736/ The Healpix map can be downloaded from: https://grb.mpe.mpg.de/grb/GRB260213736/healpix The location parameters are available as JSON at: https://grb.mpe.mpg.de/grb/GRB260213736/json View this GCN Circular online at https://gcn.nasa.gov/circulars/43725. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41832] GRB 260211A - SVOM/ECLAIRs refined analysis
by GCN Circulars 13 Feb '26

13 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43724 SUBJECT: GRB 260211A - SVOM/ECLAIRs refined analysis DATE: 26/02/13 15:39:21 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> T. Maiolino (LUPM), D. Götz, D. Adrien (CEA/Irfu), M. Brunet (IRAP), F. Piron (LUPM) 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 260211A (SVOM burst-id 26021102), which was also detected by Fermi/GBM sub-threshold event (GCN #43713). The burst that triggered ECLAIRs onboard (GCN #43705) consists of a double-peaked pulse with a duration of T90 = 21.6 +9.2/-2.8 s in the 4-120 keV energy band. The time-averaged spectrum from T0-7.54 s to T0+13.12 s (T0 = 2026-02-11T19:24:33 UTC) in the energy range 5-120 keV is best fitted by a powerlaw model with a photon index of -1.71 +0.06/-0.07. With this model, the total 4-120 keV fluence is (1.08 ± 0.06)*E-6 erg/cm^2. 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: Tais Maiolino (LUPM) (tais.maiolino at lupm.in2p3.fr) View this GCN Circular online at https://gcn.nasa.gov/circulars/43724. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41831] GRB 260204A: SVOM/ECLAIRs refined analysis
by GCN Circulars 13 Feb '26

13 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43723 SUBJECT: GRB 260204A: SVOM/ECLAIRs refined analysis DATE: 26/02/13 14:24:15 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> M. Brunet, O. Godet (IRAP), M. Pillas, M. Dennefeld (IAP) 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 260204A (SVOM burst-id sb26020403, GCN 43613), which was also detected by Fermi/GBM as a sub-threshold event (GCN 43618). ECLAIRs started collecting data at T0-8.91 s (T0 = 2026-02-04T14:48:49 UT), the Fermi sub-threshold detection starting at T0-47 s shows that part of the burst emission has been missed by ECLAIRs. The burst as seen by ECLAIRs is featureless in the 4-120 keV lightcurve. The burst emission is detected up to T0+220 s. The time-averaged spectrum before the slew from T0-8.91 s to T0+36.03 s in the 4-120 keV energy range is best fitted by a power-law model with a photon index of 1.76 +0.12/-0.11. With this model, the fluence in the 4-120 keV energy band is (7.55 +0.55/-1.02)e-7 erg/cm². After the slew, the GRB emission is still detectable below 10 keV for around 80 s, but it is rather faint. So, it is not possible to derive meaningful spectral information. 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/43723. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41830] GRB 260213A: Fermi GBM Final Localization
by GCN Circulars 13 Feb '26

13 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43722 SUBJECT: GRB 260213A: Fermi GBM Final Localization DATE: 26/02/13 14:20:26 GMT FROM: Elisabetta Bissaldi at Politecnico and INFN Bari <elisabetta.bissaldi(a)ba.infn.it> The Fermi GBM team reports the detection of a likely SHORT GRB "At 08:23:49.89 UT on 13 February 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260213A (trigger 792663834/260213350). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 244.99, Dec = -18.22 (J2000 degrees, equivalent to J2000 16h 19m, -18d 13'), with a statistical uncertainty of 11.02 degrees. The angle from the Fermi LAT boresight is 67 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260213350/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260213350/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260213350/…" View this GCN Circular online at https://gcn.nasa.gov/circulars/43722. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41829] GRB 260211A: EP-FXT follow-up observation
by GCN Circulars 13 Feb '26

13 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43721 SUBJECT: GRB 260211A: EP-FXT follow-up observation DATE: 26/02/13 14:06:23 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> R.D. Liang, M. J. Liu (NAOC), H. Z. Wu (HUST), H. Sun (NAOC) on behalf of the Einstein Probe (EP) team: EP-FXT performed a follow-up observation of the SVOM/ECLAIRs-detected burst GRB 260211A (SVOM/sb26021102, Gotz et al., GCN 43705) at 2026-02-11 21:16:34 (UTC), about 52 minutes after the SVOM/ECLAIRs trigger, with an exposure time of 4569 s. Two uncataloged sources are detected within the ECLAIRs error circle. Preliminary analysis on these sources is automatically conducted, and the details are listed as follows. EPF_J054755.7-002705 RA (J2000): 86.9816 Dec (J2000): -0.4505 Flux: 1.2432 x 10^-12 erg/s/cm2 (observed, 0.5-10 keV) Flux_err: 2.2401 x 10^-13 erg/s/cm2 (1 sigma) EPF_J054802.6-002834 RA (J2000): 87.0127 Dec (J2000): -0.4750 Flux: 3.1645 x 10^-13 erg/s/cm2 (observed, 0.5-10 keV) Flux_err: 4.0267x 10^-14 erg/s/cm2 (1 sigma) Note that the position of the second candidate is consistent with a known X-ray source 1eRASS J054803.1-002833. 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/43721. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41828] GRB 260211A: SVOM/VT optical observation
by GCN Circulars 13 Feb '26

13 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43720 SUBJECT: GRB 260211A: SVOM/VT optical observation DATE: 26/02/13 09:02:26 GMT FROM: Huali Li at at NAOC, SVOM <lhl(a)nao.cas.cn> H. L. Li, Y. N. Ma, C. Wu, Z. H. Yao, Y. L. Qiu, L. P. Xin, X. H. Han, J. Wang, Y. Xu, P. P. Zhang, W. J. Xie, Y. J. Xiao, H. B. Cai, L. Lan, J. R. Xu, J. S. Deng, J. Y. Wei (NAOC), J. Palmerio (CEA/Irfu), R. C. Chen (NJU), A. Li (BNU), W. K. Zheng (UCB) report on behalf of the SVOM/VT team. SVOM/VT performed ToO observation to GRB260211A detected by SVOM/Eclairs (sb26021102, Gotz et al., GCN 43705) and Fermi GBM (Hamburg et al., GCN 43713). The observation started at 2026-02-11T20:48:38 UTC, i.e., 1.41 hours post trigger in the VT_B (400nm-650nm) and VT_R (650nm-1000nm) channels simultaneously. SVOM/VT performed ToO observation to GRB260211A detected by SVOM/Eclairs (sb26021102, Gotz et al., GCN 43705) and Fermi GBM (Hamburg et al., GCN 43713). The observation started at 2026-02-11T20:48:38 UTC, i.e., 1.41 hours post trigger in the VT_B (400nm-650nm) and VT_R (650nm-1000nm) channels simultaneously. Following EP-FXT's detections, two optical candidates were detected only in VT_R images compared to the PanSTARRS catalogue: Source1 : R.A., Dec. (2000)= 86.978758, -0.450528 4.7 arcsecs from the center of FXT src-1 Source2 : R.A., Dec. (2000)= 86.977490, -0.453334 17.9 arcsecs from the center of FXT src-1 The positions are given with an uncertainty of 0.5 arcsec. The measurements in AB magnitudes are given below: ID. Mid time. Band Exposure Time Magnitude (AB) Source1. 2.35 hour VT_R 16*70 sec 22.5+/-0.3 mag 5.63 hour VT_R 12*70 sec >22.6 mag 1.52 hour VT_B 16*70 sec >23.0 mag 5.95 hour VT_B 6*70 sec >22.5 mag Source2. 2.35 hour VT_R 16*70 sec 21.9+/-0.2 mag 5.63 hour VT_R 12*70 sec 21.9+/-0.2 mag 1.52 hour VT_B 16*70 sec >23.0 mag 5.95 hour. VT_B 6*70 sec >22.5 mag Our photometry was not corrected for Galactic extinction. For source2, we notice that there is a faint source in the PanSTARRS image. More followup observation is encouraged to confirm the nature of the sources. The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. VT was jointly developed by Xi'an Institute of Optics and Precision Mechanics (XIOPM), CAS and National astronomical observatories (NAOC), CAS. View this GCN Circular online at https://gcn.nasa.gov/circulars/43720. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41827] GRB 260212A: Glowbug gamma-ray detection
by GCN Circulars 13 Feb '26

13 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43719 SUBJECT: GRB 260212A: Glowbug gamma-ray detection DATE: 26/02/13 03:41:12 GMT FROM: C.C. Cheung at Naval Research Lab <Teddy.Cheung(a)nrl.navy.mil> C.C. Cheung, R. Woolf, M. Kerr, J.E. Grove (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report: The Glowbug gamma-ray telescope [1,2,3], operating on the International Space Station, reports the detection of GRB 260212A, which was also detected by Fermi/GBM (GCN 43716). Using an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2026-02-12 17:49:06.400 with a duration of 10.5 s and a total significance of about 69 sigma. The light curve comprises two primary peaks at ~T0+1s and +10s. The analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS. Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Program’s STP-H9 to the ISS and operated until 2024 April when it was put in safe storage on orbit. Glowbug was removed from storage and resumed operation on 2025 September 12. [1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959 [2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O [3] Woolf, R.S. et al. 2024, Proc. SPIE, 13151, id. 1315108 Distribution Statement A: Approved for public release. Distribution is unlimited. View this GCN Circular online at https://gcn.nasa.gov/circulars/43719. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41826] GRB 260211A: GOTO optical upper limit
by GCN Circulars 12 Feb '26

12 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43718 SUBJECT: GRB 260211A: GOTO optical upper limit DATE: 26/02/12 19:44:39 GMT FROM: I. Worssam at University of Birmingham <ixw352(a)student.bham.ac.uk> S. Belkin, I. Worssam, A. Kumar, D. O’Neill, G. Ramsay, B. P. Gompertz, R. Starling, M. Wortley, M. Kennedy, K. Ackley, M. Dyer, J. Lyman, K. Ulaczyk, D. Steeghs, D. Galloway, V. Dhillon, P. O'Brien, K. Noysena, R. Kotak, R. Breton, J. Casares, L. Nuttall, B. Godson, T. Killestein, M. Pursiainen, on behalf of GOTO collaboration: We report on optical observations with the Gravitational-wave Optical Transient Observer (GOTO; Steeghs et al. 2022, Dyer et al. 2024) in response to the SVOM detected GRB 260211A (Gotz et al., GCN 43705). Two epochs of observations covering the localisation area were taken at 2026-02-11 20:08:30 UT (+44min post trigger) and 2026-02-11 21:16:33 UT (+1.87h post trigger) utilising GOTO-North. Each observation consisted of 4x90 s exposures in the GOTO L-band (400-700 nm). Images were processed immediately after acquisition using the GOTO pipeline. Difference imaging was performed using deeper template observations. No new transients that could be credibly associated with GRB 260211A were detected down to an average 5-sigma depth of 20.6 mag (AB), see also Globus et al., GCN 43707; Wu et al., GCN 43709; Konno et al., GCN 43715. GOTO (https://goto-observatory.org) is a network of telescopes that is principally funded by the STFC and operated at the Roque de los Muchachos Observatory on La Palma, Spain, and Siding Spring Observatory in NSW, Australia, on behalf of a consortium including the University of Warwick, Monash University, Armagh Observatory & Planetarium, the University of Leicester, the University of Sheffield, the National Astronomical Research Institute of Thailand (NARIT), the University of Turku, the University of Portsmouth, the University of Manchester, the University of Birmingham and the Instituto de Astrofisica de Canarias (IAC). View this GCN Circular online at https://gcn.nasa.gov/circulars/43718. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41825] Fermi GRB 260212A: Global MASTER-Net observations report
by GCN Circulars 12 Feb '26

12 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43717 SUBJECT: Fermi GRB 260212A: Global MASTER-Net observations report DATE: 26/02/12 19:15:22 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 260212A ( Fermi GBM team, GCN 43716) errorbox 552 sec after notice time and 585 sec after trigger time at 2026-02-12 17:58:53 UT, with upper limit up to 18.0 mag. The observations began at zenith distance = 59 deg. The sun altitude is -37.1 deg. The galactic latitude b = 40 deg., longitude l = 111 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3132416 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 645 | 2026-02-12 17:58:53 | MASTER-Kislovodsk | (15h 16m 06.75s , +73d 36m 46.3s) | C | 120 | 18.0 | 786 | 2026-02-12 18:01:14 | MASTER-Kislovodsk | (15h 16m 08.64s , +73d 36m 52.0s) | C | 120 | 17.5 | 926 | 2026-02-12 18:03:34 | MASTER-Kislovodsk | (15h 16m 10.47s , +73d 36m 57.7s) | C | 120 | 17.6 | 1068 | 2026-02-12 18:05:56 | MASTER-Kislovodsk | (15h 16m 12.12s , +73d 37m 03.6s) | C | 120 | 17.7 | 1209 | 2026-02-12 18:08:16 | MASTER-Kislovodsk | (15h 16m 13.41s , +73d 37m 09.3s) | C | 120 | 17.4 | 1652 | 2026-02-12 18:16:09 | MASTER-Kislovodsk | (15h 10m 30.28s , +72d 55m 28.4s) | C | 60 | 17.0 | 1860 | 2026-02-12 18:19:38 | MASTER-Kislovodsk | (15h 30m 36.29s , +74d 48m 40.5s) | C | 60 | 17.3 | 2274 | 2026-02-12 18:26:31 | MASTER-Kislovodsk | (15h 03m 57.80s , +76d 45m 03.8s) | C | 60 | 17.0 | 2516 | 2026-02-12 18:30:34 | MASTER-Kislovodsk | (15h 52m 21.24s , +72d 54m 23.0s) | C | 60 | 17.3 | 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/43717. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41824] GRB 260212A: Fermi GBM Final Real-time Localization
by GCN Circulars 12 Feb '26

12 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43716 SUBJECT: GRB 260212A: Fermi GBM Final Real-time Localization DATE: 26/02/12 17:59:41 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 17:49:08 UT on 12 Feb 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260212A (trigger 792611353.21224 / 260212742). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 228.9, Dec = 74.1 (J2000 degrees, equivalent to J2000 15h 15m, 74d 05'), with a statistical uncertainty of 1.1 degrees. The angle from the Fermi LAT boresight is 127.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260212742/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260212742/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260212742/… View this GCN Circular online at https://gcn.nasa.gov/circulars/43716. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41823] GRB 260211A: LAST optical upper limit
by GCN Circulars 12 Feb '26

12 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43715 SUBJECT: GRB 260211A: LAST optical upper limit DATE: 26/02/12 17:46:24 GMT FROM: Ruslan Konno at Weizmann Institute of Science <ruslankonno(a)gmail.com> R. Konno (WIS), S. Garrappa (WIS), E. A. Zimmerman (WIS), A. Horowicz (WIS), E. O. Ofek (WIS), S. Ben-Ami (WIS), D. Polishook (WIS), O. Yaron (WIS), S. Fainer (WIS), A. Krassilchtchikov (WIS), Y. M. Shani (WIS), E. Segre (WIS), A. Gal-Yam (WIS), and S. Spitzer (WIS) report on behalf of the LAST Collaboration. We report observations of GRB 260211A, detected by SVOM (Gotz et al., GCN 43705). Observations were conducted with the Large Array Survey Telescope (LAST; Ofek et al. 2023, PASP 135, 5001; Ben-Ami et al. 2023, PASP 135, 5002). We observed the field of GRB 260211A using 4 divergent telescopes (each with a 7.4 deg^2 FoV) in clear band (similar to the Gaia Bp band) over 18 sequential epochs. Each epoch consists of 20x20s exposures. We began observations at 2026-02-11 19:27:31 UTC (T-T0 = 178 s). We coadd a total of 220x20s exposure images and perform image subtraction using a reference image of the field. We do not detect any new optical source up to a limiting magnitude of 20.12 (AB) within the error region reported in Gotz et al., GCN 43705. LAST is a survey telescope array of the Weizmann Astrophysical Observatory (https://www.weizmann.ac.il/wao/) View this GCN Circular online at https://gcn.nasa.gov/circulars/43715. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41822] GRB 260210A: SVOM/GRM observation
by GCN Circulars 12 Feb '26

12 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43714 SUBJECT: GRB 260210A: SVOM/GRM observation DATE: 26/02/12 16:38:55 GMT FROM: guohx(a)ihep.ac.cn SVOM/GRM team: Hao-Xuan Guo, Chen-Wei Wang, Shi-Jie Zheng, Yue Huang, Shao-Lin Xiong, Shuang-Nan Zhang (IHEP) SVOM/ECLAIRs team: Feliu Lacreu (IAP), Olivier GODET (IRAP) Report on behalf of the SVOM team: SVOM/GRM was triggered in-flight by GRB 260210A at 2026-02-10T11:27:37.300 (T0), which is also detected by KONUS-Wind, AstroSat CZTI (Arya et al., GCN #43686) and Glowbug (Cheung et al., GCN #43689). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of multiple pulses with a T90 of 34.4 +8.8/-5.2 s in the 15-5000 keV band. The SVOM/GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb260210A.png In addition, the position of this burst, as determined by on-ground trigger (RA = 254, Dec = 19, Error = 57), is located at about 72 degrees from the SVOM optical axis, which is outside the ECLAIRs field of view. But this burst is still detected by ECLAIRs through the shield. With this localization, the time-averaged spectrum from T0-30 to T0+62 s is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -1.33 +0.15/-0.14 and the cutoff energy, parameterized as Epeak, is 182 +65/-36 keV. The event fluence (10-1000 keV) in this time interval is (1.67 +0.17/-0.15)E-05 erg/cm^2. The 1s peak spectrum, measured from T0+0.7 to T0+1.7 s, is also best fitted by a power law function with an exponential high-energy cutoff. The power law index is -0.74 +0.17/-0.16 and the cutoff energy, parameterized as Epeak, is 207 +33/-24 keV. The flux (10-1000 keV) in this time interval is (1.34 +0.11/-0.10)E-06 erg/cm^2/s. The localization of GRB 260210A in the 'Amati' relation diagram is shown at: https://www.bursthub.cn//admin/static/svgrb260210A_amati.png And the localization in the 'Yonetoku' relation diagram is shown at: https://www.bursthub.cn//admin/static/svgrb260210A_yonetoku.png The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. GRM is developed by the Institute of High Energy Physics (IHEP) of CAS. The SVOM/GRM point of contact for this burst is: Hao-Xuan Guo (IHEP) (guohx(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/43714. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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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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[vsnet-grb-info 41811] Swift Operations Update + Community Forum (Friday, February 13 @ 10:00 AM EST)
by GCN Circulars 11 Feb '26

11 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43704 SUBJECT: Swift Operations Update + Community Forum (Friday, February 13 @ 10:00 AM EST) DATE: 26/02/11 19:39:43 GMT FROM: Brad Cenko at NASA/GSFC <brad.cenko(a)nasa.gov> Brad Cenko (NASA/GSFC) on behalf of the Swift team: I’m writing to provide an update about Swift and the associated efforts to boost its orbit prior to atmospheric re-entry. For the last several months we have attempted to reduce the rate of altitude decay by orienting the Swift spacecraft in a manner to minimize drag over the part of each orbit where the atmospheric density is at a maximum. While this has had a positive impact on orbital altitude (and had only a modest impact on science), increased solar activity and refined altitude predictions in recent weeks both indicate an increasing risk of Swift not maintaining sufficient altitude for the Katalyst capture attempt. After careful consideration, we are opting to transition Swift full-time to an operations mode where the top priority is to prolong its orbital lifetime to maximize the chances of reboost success. As a result, few (if any) pointed observations with the XRT and UVOT will be feasible. Once it has been brought back fully online from the safe hold on 1/28, BAT will continue to collect science data as per usual (though prompt slews to newly detected GRBs will be disabled). While this is a significant reduction in science capability, we believe the prospect of extended operations at much higher altitude post-reboost justify the risk. We will re-evaluate Swift’s orbital status regularly throughout the coming weeks and months, and should this posture change for any reason we will notify the community (e.g, on our new blog: https://science.nasa.gov/blogs/swift) In the mean time, we will hold a community forum on Friday, February 13 at 10:00 AM EST to answer any questions you may have about this change (Teams connection information is below). — Microsoft Teams meeting Join: https://teams.microsoft.com/meet/21954448887326?p=Dxe4X1ehWXNNh1Dsni Meeting ID: 219 544 488 873 26 Passcode: qu6kf3q5 Need help? | System reference Dial in by phone +1 256-715-9946,,137633183# United States, Huntsville Find a local number Phone conference ID: 137 633 183# View this GCN Circular online at https://gcn.nasa.gov/circulars/43704. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41810] Swift Operations Update + Community Forum (Friday, February 13 @ 10:00 AM EST)
by GCN Circulars 11 Feb '26

11 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43704 SUBJECT: Swift Operations Update + Community Forum (Friday, February 13 @ 10:00 AM EST) DATE: 26/02/11 19:39:43 GMT FROM: Brad Cenko at NASA/GSFC <brad.cenko(a)nasa.gov> Brad Cenko (NASA/GSFC) on behalf of the Swift team: I’m writing to provide an update about Swift and the associated efforts to boost its orbit prior to atmospheric re-entry. For the last several months we have attempted to reduce the rate of altitude decay by orienting the Swift spacecraft in a manner to minimize drag over the part of each orbit where the atmospheric density is at a maximum. While this has had a positive impact on orbital altitude (and had only a modest impact on science), increased solar activity and refined altitude predictions in recent weeks both indicate an increasing risk of Swift not maintaining sufficient altitude for the Katalyst capture attempt. After careful consideration, we are opting to transition Swift full-time to an operations mode where the top priority is to prolong its orbital lifetime to maximize the chances of reboost success. As a result, few (if any) pointed observations with the XRT and UVOT will be feasible. Once it has been brought back fully online from the safe hold on 1/28, BAT will continue to collect science data as per usual (though prompt slews to newly detected GRBs will be disabled). While this is a significant reduction in science capability, we believe the prospect of extended operations at much higher altitude post-reboost justify the risk. We will re-evaluate Swift’s orbital status regularly throughout the coming weeks and months, and should this posture change for any reason we will notify the community (e.g, on our new blog: https://science.nasa.gov/blogs/swift) In the mean time, we will hold a community forum on Friday, February 13 at 10:00 AM EST to answer any questions you may have about this change (Teams connection information is below). — Microsoft Teams meeting Join: https://teams.microsoft.com/meet/21954448887326?p=Dxe4X1ehWXNNh1Dsni Meeting ID: 219 544 488 873 26 Passcode: qu6kf3q5 Need help? | System reference Dial in by phone +1 256-715-9946,,137633183# United States, Huntsville Find a local number Phone conference ID: 137 633 183# View this GCN Circular online at https://gcn.nasa.gov/circulars/43704. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41809] Konus-Wind detection of GRB 260209B
by GCN Circulars 11 Feb '26

11 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43703 SUBJECT: Konus-Wind detection of GRB 260209B DATE: 26/02/11 19:06:19 GMT FROM: Dmitry Frederiks at Ioffe Institute <fred(a)mail.ioffe.ru> D. Frederiks, A.Lysenko, A. Ridnaia, D. Svinkin, A. Tsvetkova, M. Ulanov, and T. Cline, on behalf of the Konus-Wind team, report: The long-duration, hard-spectrum GRB 260209B triggered Konus-Wind (KW) at T0=66273.996 s UT (18:24:33.996). The burst consists of two bright, multi-peaked emission pulses and has a total duration of ~26 s. The emission is seen up to ~7 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB260209_T66273/ As observed by Konus-Wind, the burst had the fluence of (3.44 ± 0.35)x10^-5 erg/cm^2 and the 64-ms peak energy flux, measured from T0 + 2.880 s, of (3.70 ± 0.28)x10^-5 erg/cm^2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum of the burst (measured from T0 to T0+24.832 s) is best fitted in the 20 keV - 15 MeV range by a power law with exponential cutoff (CPL) model dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -1.34 (-0.04, + 0.05) and Ep = 1340(-257,+343) keV, chi^2 = 112/98 dof. Fitting this spectrum by a Band GRB function yields the same values of alpha and Ep, and only an upper limit on the high energy photon index beta of -2.7 The spectrum near the peak count rate (measured from T0 to T0+8.448 s) is best fitted in the 20 keV - 15 MeV range by a CPL model with alpha = -1.25 (-0.3, + 0.04)and Ep = 1704(-233,+277) keV, chi^2 = 97/85 dof. Fitting this spectrum by a Band function yields the same values of alpha and Ep, and only an upper limit on the high energy photon index beta of -2.8 All the quoted errors are estimated at the 68% confidence level. All the presented results are preliminary View this GCN Circular online at https://gcn.nasa.gov/circulars/43703. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41808] GRB 260228A: Swift UVOT detection
by GCN Circulars 11 Feb '26

11 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43702 SUBJECT: GRB 260228A: 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 y. 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 41807] Konus-Wind detection of GRB 260127B
by GCN Circulars 11 Feb '26

11 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43701 SUBJECT: Konus-Wind detection of GRB 260127B DATE: 26/02/11 17:39:39 GMT FROM: Anna Ridnaia at Ioffe Institute <ridnaia(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 260127B (Fermi-GBM detection: The Fermi GBM team, GCN 43533; Trigg, GCN 43573; IPN triangulation: Ridnaia et al., GCN 43559; AstroSat-CZTI detection: ,GCN 43576; GECAM-B observation: Ren et al., GCN 43597; Insight-HXMT/HE detection: Ren et al., GCN 43598) triggered Konus-Wind at T0=72154.163 s UT (20:02:34.163). The burst light curve shows a multipeaked structure, which starts at ~T0-0.1 s and has a total duration of ~0.3 s. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB260127_T72154/ As observed by Konus-Wind, the burst had a fluence of 2.09(-0.27,+0.38)x10^-6 erg/cm2, and a 16-ms peak flux, measured from T0+0.062 s, of 1.80(-0.40,+0.51)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum of the burst (measured from T0 to T0+0.128 s) is best fit in the 20 keV - 1.3 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -0.21(-0.27,+0.31) and Ep = 796(-151,+261) keV (chi2 = 24/25 dof). 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/43701. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41806] EP260209a: COLIBRÍ optical upper limit
by GCN Circulars 11 Feb '26

11 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43700 SUBJECT: EP260209a: COLIBRÍ optical upper limit DATE: 26/02/11 16:49:52 GMT FROM: Jean-Luc Atteia at IRAP <jean-luc.atteia(a)irap.omp.eu> Jean-Luc Atteia (IRAP), Fredd Sánchez Álvarez (UNAM), Stéphane Basa (UAR Pytheas), William H. Lee (UNAM), Alan M. Watson (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), Enrique Moreno Méndez (UNAM), Margarita Pereyra (UNAM), Ny Avo Rakotondrainibe (LAM), Benjamin Schneider (LAM) and Antonio de Ugarte Postigo (LAM) report: We imaged the field of the EP transient EP260209a (Zhang et al., GCN Circ. 43693) using the DDRAGO two-channel wide-field imager on the COLIBRÍ telescope. We observed from 2026-02-11 12:43 to 13:02 UTC ( 47.0 to 47.4 hours after the trigger) and obtained 960 seconds 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. In the stacked image, we do not detect any new source at the FXT source position (Zhang et al., GCN Circ. 43693) down to the following 5-sigma limit: r > 20.4, z > 18.8. These limits are compatible with those of LCO (Corcoran et al. GCN Circ. 43698) 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/43700. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41805] Fermi GRB 260210C: Global MASTER-Net observations report
by GCN Circulars 11 Feb '26

11 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43699 SUBJECT: Fermi GRB 260210C: Global MASTER-Net observations report DATE: 26/02/11 16:45:47 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 260210C ( Fermi GBM team, GCN 43690) errorbox 71030 sec after notice time and 71220 sec after trigger time at 2026-02-11 15:36:42 UT, with upper limit up to 17.7 mag. Observations started at twilight. The observations began at zenith distance = 67 deg. The sun altitude is -11.6 deg. The galactic latitude b = -30 deg., longitude l = 87 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3128802 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 71250 | 2026-02-11 15:36:42 | MASTER-Kislovodsk | (22h 34m 34.78s , +22d 28m 07.7s) | C | 60 | 15.8 | 71357 | 2026-02-11 15:38:29 | MASTER-Kislovodsk | (22h 21m 37.65s , +22d 26m 29.0s) | C | 60 | 15.9 | 71964 | 2026-02-11 15:48:36 | MASTER-Kislovodsk | (22h 27m 29.52s , +24d 20m 43.1s) | C | 60 | 16.7 | 72653 | 2026-02-11 16:00:05 | MASTER-Kislovodsk | (22h 30m 03.09s , +20d 30m 18.0s) | C | 60 | 17.4 | 72765 | 2026-02-11 16:01:57 | MASTER-Kislovodsk | (22h 14m 25.78s , +24d 18m 57.0s) | C | 60 | 17.5 | 72867 | 2026-02-11 16:03:39 | MASTER-Kislovodsk | (22h 21m 40.66s , +26d 11m 29.9s) | C | 60 | 17.7 | 72975 | 2026-02-11 16:05:27 | MASTER-Kislovodsk | (22h 47m 29.43s , +22d 24m 59.2s) | C | 60 | 17.3 | 73080 | 2026-02-11 16:07:12 | MASTER-Kislovodsk | (22h 17m 16.21s , +20d 30m 58.2s) | C | 60 | 16.7 | 73648 | 2026-02-11 16:16:40 | MASTER-Kislovodsk | (22h 42m 55.62s , +20d 31m 49.9s) | C | 60 | 17.3 | 74157 | 2026-02-11 16:25:09 | MASTER-Kislovodsk | (22h 53m 48.41s , +24d 19m 15.5s) | C | 60 | 16.9 | 74286 | 2026-02-11 16:27:18 | MASTER-Kislovodsk | (22h 44m 21.71s , +28d 05m 30.3s) | C | 60 | 16.8 | 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/43699. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41804] EP260209a: LCO optical upper limits
by GCN Circulars 11 Feb '26

11 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43698 SUBJECT: EP260209a: LCO optical upper limits DATE: 26/02/11 16:41:01 GMT FROM: Gregory Corcoran at University College Dublin <gregory.corcoran(a)ucdconnect.ie> G. Corcoran (UCD) and J. A. Quirola-Vasquez (Radboud) report on behalf of a larger collaboration: We observed the field of the fast X-ray transient EP260209a (Zhang et al., GCN 43693) using the LCO 1m telescope located at the McDonald Observatory (Texas, USA) equipped with the SINISTRO instrument. Our observations consisted of a sequence of 4x300 s exposures in the SDSS r-band starting on 2026-02-11 at 12:22:56 UT (~1.44 days after the WXT trigger). We do not detect any sources within the EP/FXT uncertainty region (Zhang et al., GCN 43693). From the stacked image, we obtain the following 3-sigma upper limiting magnitude:  r > 22.5 This limit is in the AB system, calibrated using nearby stars from the Pan-STARRS catalog, and not corrected for Galactic extinction. View this GCN Circular online at https://gcn.nasa.gov/circulars/43698. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41803] EP260210a: Global MASTER-Net observations report
by GCN Circulars 11 Feb '26

11 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43697 SUBJECT: EP260210a: Global MASTER-Net observations report DATE: 26/02/11 15:54:23 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-Tunka robotic telescope [1] located in Russia (Applied Physics Institute, Irkutsk State University) was pointed to the EP260210a ( EP Team et al., GCN 43681) errorbox 1 days 8970 sec after notice time and 1 days 16089 sec after trigger time at 2026-02-11 14:49:07 UT, with upper limit up to 20.9 mag. The observations began at zenith distance = 41 deg. The sun altitude is -42.1 deg. The galactic latitude b = 65 deg., longitude l = 162 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3130129 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 7568 | 2026-02-10 12:25:35 | MASTER- | (11h 18m 01.50s , +46d 01m 48.3s) | C | 180 | 20.1 | 7568 | 2026-02-10 12:25:35 | MASTER- | (11h 19m 42.26s , +45d 29m 04.1s) | C | 180 | 19.9 | 7757 | 2026-02-10 12:28:45 | MASTER- | (11h 18m 02.83s , +46d 02m 53.1s) | C | 180 | 20.0 | 7757 | 2026-02-10 12:28:45 | MASTER- | (11h 19m 43.41s , +45d 30m 08.6s) | C | 180 | 19.8 | 7947 | 2026-02-10 12:31:54 | MASTER- | (11h 18m 09.32s , +46d 01m 59.2s) | C | 180 | 19.9 | 7947 | 2026-02-10 12:31:54 | MASTER- | (11h 19m 49.66s , +45d 29m 14.2s) | C | 180 | 19.7 | 8137 | 2026-02-10 12:35:04 | MASTER- | (11h 18m 03.97s , +46d 01m 06.6s) | C | 180 | 19.7 | 8137 | 2026-02-10 12:35:04 | MASTER- | (11h 19m 44.15s , +45d 28m 20.7s) | C | 180 | 19.5 | 8327 | 2026-02-10 12:38:14 | MASTER- | (11h 19m 50.14s , +45d 28m 55.2s) | C | 180 | 18.1 | 9693 | 2026-02-10 13:01:01 | MASTER- | (11h 18m 06.50s , +46d 04m 07.7s) | C | 180 | 19.5 | 9693 | 2026-02-10 13:01:01 | MASTER- | (11h 19m 42.80s , +45d 31m 23.3s) | C | 180 | 19.3 | 102519 | 2026-02-11 14:49:07 | MASTER-Tunka | (11h 17m 51.29s , +45d 05m 25.7s) | C | 60 | 20.1 | 102519 | 2026-02-11 14:49:07 | MASTER-Tunka | (11h 17m 17.48s , +45d 11m 57.6s) | C | 60 | 20.1 | 102579 | 2026-02-11 14:49:07 | MASTER-Tunka | (11h 17m 17.48s , +45d 11m 57.6s) | C | 180 | 20.8 | Coadd 102593 | 2026-02-11 14:50:21 | MASTER-Tunka | (11h 17m 48.72s , +45d 07m 01.6s) | C | 60 | 20.1 | 102593 | 2026-02-11 14:50:21 | MASTER-Tunka | (11h 17m 14.82s , +45d 13m 33.5s) | C | 60 | 20.1 | 102675 | 2026-02-11 14:51:42 | MASTER-Tunka | (11h 17m 14.77s , +45d 11m 48.3s) | C | 60 | 20.2 | 102675 | 2026-02-11 14:51:42 | MASTER-Tunka | (11h 17m 48.77s , +45d 05m 16.6s) | C | 60 | 20.1 | 102777 | 2026-02-11 14:52:55 | MASTER-Tunka | (11h 17m 18.23s , +45d 13m 40.4s) | C | 120 | 20.3 | 102897 | 2026-02-11 14:52:55 | MASTER-Tunka | (11h 17m 18.23s , +45d 13m 40.3s) | C | 360 | 20.9 | Coadd 102777 | 2026-02-11 14:52:55 | MASTER-Tunka | (11h 17m 52.48s , +45d 07m 09.3s) | C | 120 | 20.3 | 102911 | 2026-02-11 14:55:08 | MASTER-Tunka | (11h 17m 11.60s , +45d 12m 39.5s) | C | 120 | 20.4 | 102911 | 2026-02-11 14:55:08 | MASTER-Tunka | (11h 17m 46.09s , +45d 06m 09.1s) | C | 120 | 20.4 | 103052 | 2026-02-11 14:57:30 | MASTER-Tunka | (11h 17m 46.28s , +45d 07m 08.1s) | C | 120 | 20.4 | 103052 | 2026-02-11 14:57:30 | MASTER-Tunka | (11h 17m 11.47s , +45d 13m 37.9s) | C | 120 | 20.4 | 103185 | 2026-02-11 14:59:43 | MASTER-Tunka | (11h 17m 52.89s , +45d 06m 06.4s) | C | 120 | 20.3 | 103185 | 2026-02-11 14:59:43 | MASTER-Tunka | (11h 17m 17.88s , +45d 12m 35.6s) | C | 120 | 20.4 | 103349 | 2026-02-11 15:02:26 | MASTER-Tunka | (11h 16m 48.88s , +46d 09m 10.4s) | C | 120 | 20.4 | 103349 | 2026-02-11 15:02:26 | MASTER-Tunka | (11h 17m 28.36s , +46d 01m 15.6s) | C | 120 | 20.3 | 103469 | 2026-02-11 15:02:26 | MASTER-Tunka | (11h 17m 28.35s , +46d 01m 15.6s) | C | 360 | 20.8 | Coadd 103485 | 2026-02-11 15:04:42 | MASTER-Tunka | (11h 16m 55.90s , +46d 09m 20.0s) | C | 120 | 20.4 | 103485 | 2026-02-11 15:04:42 | MASTER-Tunka | (11h 17m 35.59s , +46d 01m 25.7s) | C | 120 | 20.4 | 103618 | 2026-02-11 15:06:56 | MASTER-Tunka | (11h 16m 51.63s , +46d 10m 48.7s) | C | 120 | 20.4 | 103618 | 2026-02-11 15:06:56 | MASTER-Tunka | (11h 17m 31.57s , +46d 02m 54.6s) | C | 120 | 20.3 | 103751 | 2026-02-11 15:09:09 | MASTER-Tunka | (11h 16m 51.33s , +46d 09m 05.5s) | C | 120 | 20.3 | 103751 | 2026-02-11 15:09:09 | MASTER-Tunka | (11h 17m 31.48s , +46d 01m 11.8s) | C | 120 | 20.3 | 103871 | 2026-02-11 15:09:09 | MASTER-Tunka | (11h 17m 31.47s , +46d 01m 11.8s) | C | 360 | 20.7 | Coadd 103885 | 2026-02-11 15:11:23 | MASTER-Tunka | (11h 17m 34.65s , +46d 02m 45.1s) | C | 120 | 20.3 | 103885 | 2026-02-11 15:11:23 | MASTER-Tunka | (11h 16m 54.22s , +46d 10m 39.3s) | C | 120 | 20.3 | 104023 | 2026-02-11 15:13:41 | MASTER-Tunka | (11h 17m 29.15s , +46d 02m 05.1s) | C | 120 | 20.3 | 104023 | 2026-02-11 15:13:41 | MASTER-Tunka | (11h 16m 48.47s , +46d 09m 59.3s) | C | 120 | 20.3 | 104159 | 2026-02-11 15:15:56 | MASTER-Tunka | (11h 17m 27.69s , +46d 03m 03.6s) | C | 120 | 20.3 | 104279 | 2026-02-11 15:15:56 | MASTER-Tunka | (11h 17m 27.68s , +46d 03m 03.7s) | C | 360 | 20.7 | Coadd 104159 | 2026-02-11 15:15:56 | MASTER-Tunka | (11h 16m 46.62s , +46d 10m 57.7s) | C | 120 | 20.3 | 104292 | 2026-02-11 15:18:10 | MASTER-Tunka | (11h 16m 53.54s , +46d 09m 55.8s) | C | 120 | 20.3 | 104292 | 2026-02-11 15:18:10 | MASTER-Tunka | (11h 17m 34.89s , +46d 02m 02.3s) | C | 120 | 20.2 | 104425 | 2026-02-11 15:20:23 | MASTER-Tunka | (11h 16m 46.28s , +46d 08m 53.8s) | C | 120 | 20.3 | 104425 | 2026-02-11 15:20:23 | MASTER-Tunka | (11h 17m 27.96s , +46d 01m 00.0s) | C | 120 | 20.3 | 104559 | 2026-02-11 15:22:36 | MASTER-Tunka | (11h 16m 53.19s , +46d 09m 18.6s) | C | 120 | 20.3 | 104559 | 2026-02-11 15:22:36 | MASTER-Tunka | (11h 17m 35.15s , +46d 01m 24.7s) | C | 120 | 20.3 | 104679 | 2026-02-11 15:22:36 | MASTER-Tunka | (11h 17m 35.15s , +46d 01m 24.6s) | C | 360 | 20.7 | Coadd 104693 | 2026-02-11 15:24:50 | MASTER-Tunka | (11h 16m 48.89s , +46d 10m 36.4s) | C | 120 | 20.2 | 104693 | 2026-02-11 15:24:50 | MASTER-Tunka | (11h 17m 31.14s , +46d 02m 42.6s) | C | 120 | 20.2 | 104826 | 2026-02-11 15:27:04 | MASTER-Tunka | (11h 16m 48.61s , +46d 08m 57.8s) | C | 120 | 20.2 | 104826 | 2026-02-11 15:27:04 | MASTER-Tunka | (11h 17m 31.07s , +46d 01m 04.0s) | C | 120 | 20.0 | 104964 | 2026-02-11 15:29:21 | MASTER-Tunka | (11h 16m 51.20s , +46d 10m 29.3s) | C | 120 | 20.2 | 104964 | 2026-02-11 15:29:21 | MASTER-Tunka | (11h 17m 33.89s , +46d 02m 34.8s) | C | 120 | 20.0 | 105084 | 2026-02-11 15:29:21 | MASTER-Tunka | (11h 17m 33.89s , +46d 02m 34.8s) | C | 360 | 20.6 | Coadd 105098 | 2026-02-11 15:31:35 | MASTER-Tunka | (11h 16m 44.36s , +46d 09m 44.7s) | C | 120 | 20.2 | 105098 | 2026-02-11 15:31:35 | MASTER-Tunka | (11h 17m 27.28s , +46d 01m 49.9s) | C | 120 | 20.2 | 105231 | 2026-02-11 15:33:48 | MASTER-Tunka | (11h 16m 43.65s , +46d 10m 43.2s) | C | 120 | 20.2 | 105231 | 2026-02-11 15:33:48 | MASTER-Tunka | (11h 17m 26.90s , +46d 02m 48.1s) | C | 120 | 20.2 | 105363 | 2026-02-11 15:36:01 | MASTER-Tunka | (11h 16m 49.86s , +46d 09m 40.6s) | C | 120 | 20.2 | 105363 | 2026-02-11 15:36:01 | MASTER-Tunka | (11h 17m 33.35s , +46d 01m 46.0s) | C | 120 | 20.2 | 105513 | 2026-02-11 15:36:01 | MASTER-Tunka | (11h 17m 33.35s , +46d 01m 46.1s) | C | 420 | 20.6 | Coadd 105496 | 2026-02-11 15:38:13 | MASTER-Tunka | (11h 16m 44.46s , +46d 08m 38.1s) | C | 120 | 19.8 | 105496 | 2026-02-11 15:38:13 | MASTER-Tunka | (11h 17m 28.25s , +46d 00m 43.9s) | C | 120 | 19.9 | 105659 | 2026-02-11 15:40:27 | MASTER-Tunka | (11h 16m 48.73s , +46d 08m 57.2s) | C | 180 | 20.1 | 105659 | 2026-02-11 15:40:27 | MASTER-Tunka | (11h 17m 32.92s , +46d 01m 02.1s) | C | 180 | 20.1 | 105853 | 2026-02-11 15:43:40 | MASTER-Tunka | (11h 16m 46.04s , +46d 10m 05.2s) | C | 180 | 20.1 | 105853 | 2026-02-11 15:43:40 | MASTER-Tunka | (11h 17m 30.80s , +46d 02m 10.3s) | C | 180 | 20.1 | 106045 | 2026-02-11 15:46:53 | MASTER-Tunka | (11h 17m 30.87s , +46d 00m 58.4s) | C | 180 | 20.0 | 106045 | 2026-02-11 15:46:53 | MASTER-Tunka | (11h 16m 45.59s , +46d 08m 52.7s) | C | 180 | 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/43697. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41802] EP260210a: refined analysis of the EP-FXT observation
by GCN Circulars 11 Feb '26

11 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43696 SUBJECT: EP260210a: refined analysis of the EP-FXT observation DATE: 26/02/11 14:20:01 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> Z. H. Yang, R. Shi (PMO), Q. C. Zhao (IHEP), G. Y. Zhao (SYSU), Y. J. Zhang (THU) and Z. X. Ling (NAOC) on behalf of the Einstein Probe (EP) team: The fast X-ray transient EP260210a was detected by the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) mission (Shi et al., GCN 43681). The refined analysis of the WXT data shows that the event started at T0=2026-02-10T10:20:58.53 (UTC), and lasted for approximately 220 seconds. The average WXT 0.5-4 keV spectrum can be fitted with an absorbed power law with a fixed Galactic hydrogen column density of 1.6×10^20 cm^-2, and a photon index of 1.57 (-0.4/+0.4). The derived average unabsorbed 0.5-4 keV flux is 1.5 (-0.3/+0.4) × 10^(-10) erg/s/cm^2. The Follow-up X-ray Telescope (FXT) on board EP autonomously observed this source a few minutes after the on board trigger. The FXT observation started at 2026-02-10T10:24:57 (UTC, T0+238 s). The effective exposure time of the observation is around 5 ks. On-ground analysis of the FXT data found an uncatalogued source at R.A. = 169.8314, DEC = 45.3949 (J2000) with an uncertainty of 10 arcsec in radius (90% C.L. statistical and systematic). The average 0.5-10 keV spectrum can be fitted with an absorbed power law with a fixed Galactic hydrogen column density of 1.6 × 10^20 cm^-2, and a photon index of 2.7 (-0.1/+0.1). The derived average unabsorbed 0.5-10 keV flux is 6.4 (-1.0/+1.0) ×10^(-12) erg/s/cm^2. The uncertainties are at the 90% confidence level for the above parameters. Further FXT follow-up observations have been arranged. 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/43696. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41801] EP260209a: Global MASTER-Net observations report
by GCN Circulars 11 Feb '26

11 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43695 SUBJECT: EP260209a: Global MASTER-Net observations report DATE: 26/02/11 12:45:25 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 EP260209a ( EP Team et al., GCN 43693) errorbox 105 sec after notice time and 1 days 79337 sec after trigger time at 2026-02-11 11:46:23 UT, with upper limit up to 19.1 mag. Observations started at twilight. The observations began at zenith distance = 73 deg. The sun altitude is -14.9 deg. The galactic latitude b = 61 deg., longitude l = 203 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3129906 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 165768 | 2026-02-11 11:46:23 | MASTER-Tunka | (10h 36m 50.32s , +28d 07m 55.2s) | C | 60 | 18.9 | 165768 | 2026-02-11 11:46:23 | MASTER-Tunka | (10h 37m 06.41s , +28d 01m 58.3s) | C | 60 | 19.1 | 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/43695. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41800] GRB 260208A: LCO detection of the optical counterpart
by GCN Circulars 11 Feb '26

11 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43694 SUBJECT: GRB 260208A: LCO detection of the optical counterpart DATE: 26/02/11 12:33:24 GMT FROM: Ismael Perez-Fournon at Instituto de Astrofisica de Canarias <ipf(a)iac.es> I. Pérez-Fournon (IAC and ULL), F. Poidevin (IAC and ULL), D. Cano-Morales, A.E. Hernández-Díaz, I. Correa-Plasencia, E. Lekaroz-Urriza, M. Quintana-Ansaldo (all ULL), and A. López-Oramas (IAC and ULL) Following the detection of the bright and long GRB 260208A detected by Fermi GMB (Fermi GBM Team, GCN #43635; Mukherjee and Meegan, GCN #43673), Fermi LAT (Longo et al., GCN #43645), Swift-XRT (Dichiara et al., GCN #43652; Longo et al., GCN #43643), GECAM-B (Luo et al., GCN #43658), NuSTAR (Waratkar et al., GCN #43674), and Glowbug (Cheung et al., GCN #43675), we observed the field with one of the three Las Cumbres Observatory (LCO) 1-m telescopes located at the LCO node at Cerro Tololo Inter-American Observatory (CTIO), Chile. The observation, a single exposure of 300 sec in the SDSS r' filter, started on 2026-02-09 at 07:48:36 UT, about 26.69 hours after the Fermi trigger. The optical counterpart AT 2026ciw (MASTER OT J133855.62+334806.9, GOTO26aob, ZTF26aafswob) first detected by Podesta et al. (MASTER, GCN #43640) and Wortley et al. (GOTO, GCN #43641) is detected in our image with an AB magnitude of r' = 20.92 +/- 0.17, calibrated against PanSTARRS-1 DR2 stars and not corrected for Galactic extinction. This result is consistent with the late evolution of the optical afterglow of this redshfit z = 2.36 GRB (Dimple et al., GCN #43662). Optical detections have been reported by Podesta et al. (GCN #43640), Wortley et al. (GCN #43641), Ma et al. (GCN #43655), Ahumada et al. (GCN #43657), Dimple et al. (GCN #43661), Dimple et al. (GCN #43662), Magnani et al. (GCN #43664), Gupta et al. (GCN #43665), Volnova et al. (GCN #43666), and Bochenek et al. (GCN #43676). This work makes use of observations from the Las Cumbres Observatory global telescope network (LCO program IAC2026A-011, SGLF and Superluminous Supernovae surveys). This work made use of the Astro-COLIBRI platform (P. Reichherzer et al. 2021, ApJS, 256, 5). View this GCN Circular online at https://gcn.nasa.gov/circulars/43694. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41799] EP260209a: Einstein Probe detection of a fast X-ray transient
by GCN Circulars 11 Feb '26

11 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43693 SUBJECT: EP260209a: Einstein Probe detection of a fast X-ray transient DATE: 26/02/11 11:43:58 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> Y.J. Zhang (THU), R. Shi (PMO), Z. H. Yang, Q. C. Zhao (IHEP), G. Y. Zhao (SYSU) and Z. X. Ling (NAOC) 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 EP260209a. The EP-WXT observation started at 2026-02-09T13:44:06 (UTC). The WXT position of the source is R.A. = 159.683 deg, DEC = 28.312 deg (J2000) with an uncertainty of 3 arcmin in radius (90% C.L. statistical and systematic). The light curve exhibits a flare in the first 50 seconds of the WXT observation, with a 0.5--4 keV flux of approximately 7.4 × 10^-10 erg s^-1 cm^-2. The delayed report of the transient is due to its relatively low detection significance. We performed a follow-up observation with the Follow-up X-ray Telescope (FXT), starting at 2026-02-10T07:02:41 (UTC), about 17 hours after the detection. Within the WXT error circle, an uncatalogued X-ray source was detected at R.A. = 159.6834 deg, DEC = 28.3078 deg (J2000) with an uncertainty of 10 arcsec in radius (90% C.L. statistical and systematic). The uncatalogued X-ray source has a 0.5--10 keV flux of 1.1 x 10^-13 erg s^-1 cm^-2, with a powerlaw index of 1.3 and a fixed galactic NH value (1.6 x 10^20 cm^-2). 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/43693. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41798] EP260210a: Optical upper limits with Kinder observations
by GCN Circulars 11 Feb '26

11 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43692 SUBJECT: EP260210a: Optical upper limits with Kinder observations DATE: 26/02/11 08:35:06 GMT FROM: Amar Aryan at National Central University, Institute of Astronomy (NCUIA) <amararyan941(a)gmail.com> A. Aryan, 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), Y.-H. Lee, A. Sankar.K, M.-H. Lee, C.-H. Lai, 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 observed the field of the fast X-ray transient EP260210a (Shi et al. GCN 43681) using the 40cm SLT and 1m LOT at the Lulin Observatory in Taiwan as part of the Kinder collaboration (Chen & Yang et al. 2025, ApJ, 983, 86, doi:10.3847/1538-4357/adb428). The first SLT epoch of observations in r-band started at 13:57 UTC on 10th of February 2026 (MJD 61081.582), 3.57 hr after the EP-WXT trigger. We utilized the astroalign (Beroiz et al. 2020, A&C, 32, 100384) and astropy (Astropy Collaboration et al. 2022, ApJ, 935, 167) packages to align and stack the individual frames. We utilized the Python-based package AutoPhOT (Brennan & Fraser 2022, A&A, 667, A62) to perform template subtraction with the DESI Legacy Survey (Dey et al. 2019, AJ 157, 168) DR10 image (for r-band) and Pan-STARRS1 3Pi (Chambers et al. 2016, arXiv:1612.05560) archive image (for i-band) using the 'SFFT' (Hu et al. 2022, ApJ, 936, 157) algorithm. Moreover, we used AutoPhOT to perform PSF photometry. We do not detect any new or uncataloged sources within the 20" EP-FXT localization circle. The details of the observations and the measured 3-sigma upper limits (in the AB system) are as follows: Telescope | Filter | MJD (start)| t-t0 (hr) | Exposure (s) | Magnitude | avg. Seeing | med. Airmass SLT | r | 61081.582 | 3.57 | 300 * 12 | >22.0 | 1".5 | 1.47 LOT | r | 61081.584 | 3.62 | 300 * 6 | >22.9 | 1".3 | 1.54 SLT | i | 61081.628 | 4.69 | 300 * 20 | >21.6 | 1".4 | 1.18 The non-detections in our observations are consistent with those reported by Kang et al. (GCN 43683), Fortin et al. (GCN 43684), and Li et al. (GCN 43687). The presented magnitude is calibrated using the field stars from the ATLAS-RefCat2 catalog from MAST (Tonry J. L. et al. 2018, ApJ, 867, 105) and is not corrected for the expected Galactic foreground extinction of A_r = 0.034 mag and A_i = 0.026 mag in the direction of the transient (Schlafly & Finkbeiner 2011). The methodology, details on the Lulin observatory telescopes, and a compilation of our optical follow-up campaign for FXTs discovered within the first year of operation of the Einstein-Probe mission 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/43692. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41797] IPN triangulation of GRB 260207B (short/hard with EE)
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43691 SUBJECT: IPN triangulation of GRB 260207B (short/hard with EE) DATE: 26/02/10 20:33:53 GMT FROM: Anna Ridnaia at Ioffe Institute <ridnaia(a)mail.ioffe.ru> A.S. Kozyrev, D.V. Golovin, M.L. Litvak, I.G. Mitrofanov, and A.B. Sanin on behalf of the HEND/Mars Odyssey team, A. Ridnaia, D. Frederiks, A. Lysenko, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, A. Goldstein, M. S. Briggs, C. Wilson-Hodge, and E. Burns on behalf of the Fermi GBM team, and W. Boynton, C. Fellows, K. Harshman, H. Enos, R. Starr, and A.S. Gardner on on behalf of the GRS-Odyssey GRB team, report: The short-duration GRB with extended emission GRB 260207B (Fermi-GBM detection: Fermi GBM team, GCN 43629; Sonawane & Bala, GCN 43634; GECAM-B observation: Zao et al., GCN 43644; AstroSat CZTI detection: Goyal et al., GCN 43680) was detected by Fermi (GBM trigger 792162735), Konus-Wind, GECAM-B, AstroSat (CZTI), and Mars-Odyssey (HEND) at about 47531 s UT (13:12:11). We have triangulated it to a preliminary, 3 sigma error box whose coordinates are: --------------------------------------------- RA(2000), deg Dec(2000), deg --------------------------------------------- Center: 283.695 (18h 54m 47s) +51.643 (+51d 38' 34") Corners: 284.134 (18h 56m 32s) +51.778 (+51d 46' 39") 283.959 (18h 55m 50s) +51.758 (+51d 45' 29") 283.258 (18h 53m 02s) +51.506 (+51d 30' 22") 283.432 (18h 53m 44s) +51.527 (+51d 31' 36") --------------------------------------------- The error box area is 67 sq. arcmin, and its maximum dimension is 36 arcmin (the minimum one is 2 arcmin). The Sun distance was 74 deg. A triangulation map and HEALPix FITS file are posted at http://www.ioffe.ru/LEA/GRBs/GRB260207_T47529/IPN The HEALPix triangulation map is the multi-order HEALPix in units of probability density. The Konus-Wind time history and spectrum will be given in a forthcoming GCN Circular. View this GCN Circular online at https://gcn.nasa.gov/circulars/43691. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41796] GRB 260210C: Fermi GBM Final Real-time Localization
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43690 SUBJECT: GRB 260210C: Fermi GBM Final Real-time Localization DATE: 26/02/10 20:00:13 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 19:49:42 UT on 10 Feb 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260210C (trigger 792445787.668744 / 260210826). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 338.7, Dec = 22.6 (J2000 degrees, equivalent to J2000 22h 34m, 22d 36'), with a statistical uncertainty of 7.5 degrees. The angle from the Fermi LAT boresight is 26.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260210826/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260210826/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260210826/… View this GCN Circular online at https://gcn.nasa.gov/circulars/43690. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41795] GRB 260210A: Glowbug gamma-ray detection
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43689 SUBJECT: GRB 260210A: Glowbug gamma-ray detection DATE: 26/02/10 19:04:18 GMT FROM: C.C. Cheung at Naval Research Lab <Teddy.Cheung(a)nrl.navy.mil> C.C. Cheung, R. Woolf, M. Kerr, J.E. Grove (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report: The Glowbug gamma-ray telescope [1,2,3], operating on the International Space Station, reports the detection of GRB 260210A, which was also detected by AstroSat/CZTI, SVOM/GRM, and Konus-Wind (GCN 43686). Using an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2026-02-10 11:27:33.624 with a duration of 27.6 s and a total significance of about 49 sigma. The Glowbug light curve comprises three main peaks at ~T0+4s, +16s, and +26s. The analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS. Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Program’s STP-H9 to the ISS and operated until 2024 April when it was put in safe storage on orbit. Glowbug was removed from storage and resumed operation on 2025 September 12. [1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959 [2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O [3] Woolf, R.S. et al. 2024, Proc. SPIE, 13151, id. 1315108 Distribution Statement A: Approved for public release. Distribution is unlimited. View this GCN Circular online at https://gcn.nasa.gov/circulars/43689. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41794] GRB 260210B: Fermi GBM Final Real-time Localization
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43688 SUBJECT: GRB 260210B: Fermi GBM Final Real-time Localization DATE: 26/02/10 18:24:59 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 18:14:06 UT on 10 Feb 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260210B (trigger 792440051.126154 / 260210760). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 6.0, Dec = -48.3 (J2000 degrees, equivalent to J2000 00h 24m, -48d 17'), with a statistical uncertainty of 10.3 degrees. The angle from the Fermi LAT boresight is 22.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260210760/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260210760/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260210760/… View this GCN Circular online at https://gcn.nasa.gov/circulars/43688. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41793] EP260210a: SVOM/VT optical upper limit
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43687 SUBJECT: EP260210a: SVOM/VT optical upper limit DATE: 26/02/10 17:33:25 GMT FROM: Huali Li at at NAOC, SVOM <lhl(a)nao.cas.cn> H. L. Li, Y. N. Ma, L. P. Xin, Y. L. Qiu, C. Wu, Z. H. Yao, X. H. Han, Y. Xu, J. Wang, P. P. Zhang, W. J. Xie, Y. J. Xiao, H. B. Cai, L. Lan, J. R. Xu, J. S. Deng, J. Y. Wei (NAOC), J. Palmerio (CEA) report on behalf of the SVOM/VT team. SVOM/VT performed a Target of Opportunity observation of EP260210a detected by Einstein Probe (Shi et al., GCN 43681). The observation started at 2026-02-10T10:56:57 UTC, 34.52 minutes after the trigger, in the VT_B (400nm-650nm) and VT_R (650nm-1000nm) channels simultaneously. No uncatalogued sources are detected in single or stacked images within the error box of EP-FXT (Shi et al., GCN 43681), which is compatible with the earlier upper limits from SVOM/C-GFT (Kang et al., GCN 43683) and COLIBRÍ (Fortin et al, GCN 43684). The 3 sigma limit magnitudes are derived as below: Mid time | Band | Exposure Time | 3 sigma limit magnitude 2.316 hour VT_B 42*50 sec > 23.2 mag 1.535 hour VT_R 39*50 sec > 22.9 mag Our photometry was not corrected for Galactic extinction. The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. VT was jointly developed by Xi'an Institute of Optics and Precision Mechanics (XIOPM), CAS and National astronomical observatories (NAOC), CAS. View this GCN Circular online at https://gcn.nasa.gov/circulars/43687. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41792] GRB 260210A: AstroSat CZTI detection
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43686 SUBJECT: GRB 260210A: AstroSat CZTI detection DATE: 26/02/10 17:17:11 GMT FROM: Gaurav Waratkar at Caltech <gauravwaratkar(a)iitb.ac.in> 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 long GRB 260210A which was also detected by SVOM/GRM (via GCN notices), and KONUS-Wind (via IPN notices). The source was clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2026-02-10 11:27:38.52 UTC. The measured peak count rate associated with the burst is 292 (+76, -33) counts/s above the background in the combined data of all quadrants, with a total of 3215 (+487, -705) counts. The local mean background count rate was 1390 (+5, -5) counts/s. We measure a T90 of 34 (+2, -9) s from the cumulative Veto light curve. 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/43686. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41791] GRB 260208C: AstroSat CZTI detection
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43685 SUBJECT: GRB 260208C: AstroSat CZTI detection DATE: 26/02/10 17:14:45 GMT FROM: Gaurav Waratkar at Caltech <gauravwaratkar(a)iitb.ac.in> M. Tembhurnikar (IUCAA), Harsha K. H. (IUCAA), S. Salunke (IUCAA), A. Arya (IITB), A. Goyal (IITB), 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 long GRB 260208C which was also detected by Fermi/GBM (Fermi GBM Team, GCN Circ. 43646) and SVOM/GRM (Yue Wang, GCN Circ. 43679). The source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2026-02-08 15:12:17.5 UTC. The measured peak count rate associated with the burst is 99 (+40, -11) counts/s above the background in the combined data of all quadrants, with a total of 577 (+174, -169) counts. The local mean background count rate was 283 (+3, -4) counts/s. Using cumulative rates, we measure a T90 of 13 (+1, -8) s. 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/43685. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41790] EP260210a: COLIBRÍ optical upper limit
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43684 SUBJECT: EP260210a: COLIBRÍ optical upper limit DATE: 26/02/10 14:47:40 GMT FROM: F. Fortin at IRAP <ffortin.sci.edu(a)gmail.com> Francis Fortin (IRAP), Edilberto Aguilar-Ruiz (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), Leonardo García García (UNAM), Ramandeep Gill (UNAM), Noémie Globus (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), Benjamin Schneider (LAM) and Antonio de Ugarte Postigo (LAM) report: We imaged the field of the EP260210a (Shi et al., GCN Circ. 43681) using the DDRAGO two-channel wide-field imager on the COLIBRÍ telescope. We observed from 2026-02-10 11:13:20 to 13:11:12 UTC (from 0.83 to 2.80 hours after the trigger) and obtained 85 minutes of simultaneous exposure in the r and z filters. The data were reduced and coadded with the COLIBRÍ pipeline 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. In the stacked image, we do not detect any new source at the FXT source position (Shi et al., GCN Circ. 43681) down to the following 5-sigma limit: r > 23.59 z > 22.15 Our upper limits are compatible with the earlier upper limits of Kang et al. (GCN Circ. 43683). 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/43684. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41789] EP260210a: SVOM/C-GFT upper limit
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43683 SUBJECT: EP260210a: SVOM/C-GFT upper limit DATE: 26/02/10 13:35:22 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> Z. Kang (CHO), C. Wu, L.P. Xin, X.H. Han, P.P. Zhang, X.M. Lu (NAOC), Z.W. Li, Y. Lv (CHO), R.S. Zhang, Y.J. Xiao, Y.L. Qiu, J. Wang, J.S. Deng, L. Huang, J.Y. Wei (NAOC) report on behalf of the SVOM/C-GFT team: We observed the field of EP260210a detected by EP/WXT (Shi et al., GCN 43681) with LATIOS on SVOM/C-GFT. Observations started at 2026-02-10T10:32:54 UTC, ~ 9.88 min after the trigger. We obtained g, r, and i-band follow-up imaging. After preliminary analysis，no credible candidate was detected within the error box provided by EP/FXT (Shi et al., GCN 43681) in our images. The 3-sigma upper limits are: | Mid_T - T0 (min) | Exposure Time (s) | Band | Upper Limit (AB) | |------------------|---------------------|------|------------------| | 36.13 | 10×60 | i | 20.02 | | 47.01 | 10×60 | g | 20.15 | | 59.39 | 10×60 | r | 20.23 | The photometry was calibrated against UCAC4 catalogue and no correction for Galactic dust extinction was applied. We thank the observation assistants Chun-Lei Guo and Yin-Huai Hao at Jilin observatory for their excellent support. The Chinese Ground Follow-up Telescope (C-GFT) for the SVOM mission is located at Jilin Station, Changchun Observatory, National Astronomical Observatories, CAS. It features two instruments: (1) CATCH at the Cassegrain focus with a 21 arcsec x 21 arcsec FOV for simultaneous g/r/i-band imaging, and (2) LATIOS, a 4k x 4k CMOS camera at the prime focus with a 1.28 deg x 1.28 deg FOV that images in g, r, and i bands via filter switching. View this GCN Circular online at https://gcn.nasa.gov/circulars/43683. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41788] GRB 260208B: refined analysis of the EP-FXT observation
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43682 SUBJECT: GRB 260208B: refined analysis of the EP-FXT observation DATE: 26/02/10 12:51:13 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> S. Q. Jiang, H. N. Yang, Y. L. Wang, Y. Liu (NAO, CAS), Z. H. Yang, Q. C. Zhao (IHEP, CAS) on behalf of the Einstein Probe (EP) team: EP-FXT performed a follow-up observation on GRB 260208B (The Fermi GBM team, GCN 43638; Preis & Greiner, GCN 43639; Longo et al., GCN 43647; Sonawane et al., GCN 43649; Luo et al., GCN 43650; Harsha et al., GCN 43677) at 2026-02-09T06:37:35 (UTC), about 20.748 hours after the Fermi/GBM trigger. With a 4.6 ks exposure, the afterglow (Li et al., GCN 43659; Magnani et al., GCN 43668; Beardmore et al., GCN 43671) is clearly detected by EP-FXT. The average 0.5-10 keV spectrum can be fitted with an absorbed power law with a fixed Galactic hydrogen column density of 4.3 × 10^21 cm^-2, and a photon index of 2.01 (-0.21/+0.21). The derived average unabsorbed 0.5-10 keV flux is 7.28 (-0.81/+0.97) × 10^(-13) erg/s/cm^2. The uncertainties are at the 90% confidence level for the above parameters. Compared to the flux reported by Swift/XRT (Beardmore et al., GCN 43671), the temporal decay index is approximately -1.4. 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/43682. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41787] EP260210a: Einstein Probe detection of an X-ray transient
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43681 SUBJECT: EP260210a: Einstein Probe detection of an X-ray transient DATE: 26/02/10 12:13:39 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> R. Shi (PMO), Z. H. Yang, Q. C. Zhao (IHEP), G. Y. Zhao (SYSU), Y. J. Zhang (THU) and Z. X. Ling (NAOC) 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 EP260210a. The transient triggered EP-WXT (ID: 01709257873) at 2026-02-10T10:23:01 (UTC). The WXT position of the source is R.A. = 169.840 deg, DEC = 45.408 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. = 169.8314 deg, DEC = 45.3949 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/43681. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41786] GRB 260207B: AstroSat CZTI detection
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43680 SUBJECT: GRB 260207B: AstroSat CZTI detection DATE: 26/02/10 11:47:42 GMT FROM: Anuraag Arya at IIT Bombay <aryaanuraag910(a)gmail.com> A. Goyal (IITB), A. Arya (IITB), S. Salunke (IUCAA), Harsha K. H. (IUCAA), M. Tembhurnikar (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 260207B which was also detected by Fermi GBM (Fermi GBM Team, GCN Circ. 43629) and GECAM (Zao et. al., GCN Circ. 43644). The source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve peaks at 2026-02-07 13:12:07 UTC. The measured peak count rate associated with the burst is 1402 (+767, -219) counts/s above the background in the combined data of all four quadrants, with a total of 82 (+26, -21) counts. The local mean background count rate was 269 (+12, -45) counts/s. Using cumulative rates, we measure a T90 of 0.09 (+0.06, -0.03) s. We only observed the main emission (ME) part of the burst. The source was also detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve peaks at 2026-02-07 13:12:07 UTC. The measured peak count rate associated with the burst is 446 (+68, -75) counts/s above the background in the combined data of all quadrants, with a total of 630 (+143, -162) counts. The local mean background count rate was 1340 (+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/43680. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41785] GRB 260208C: SVOM/GRM observation
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43679 SUBJECT: GRB 260208C: SVOM/GRM observation DATE: 26/02/10 11:05:49 GMT FROM: Yue Wang <m18509381757(a)163.com> SVOM/GRM team: Yue Wang, Chen-Wei Wang, Xing-Hao Luo, Shi-Jie Zheng, Yue Huang, Shao-Lin Xiong, Shuang-Nan Zhang (IHEP) SVOM/ECLAIRs team: Marius Brunet (IRAP) Report on behalf of the SVOM team: SVOM/GRM was triggered in-flight by GRB 260208C at 2026-02-08T15:12:21.000 (T0), which is also detected by Fermi/GBM (Fermi GBM team, GCN #43653). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of multiple pulses with a T90 of 10 +4/-4 s in the 15-5000 keV band. The SVOM/GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb260208C.png In addition, the position of this burst, as determined by Fermi/GBM (RA = 281.3, Dec = -49.2, Error = 2.3, GCN #43653), is located at about 107 degrees from the SVOM optical axis, which is outside the ECLAIRs field of view. With this localization, the time-averaged spectrum from T0-1 to T0+5 s is best fitted by a power law function. The power law index is -2.22 +0.13/-0.13. The event fluence (10-1000 keV) in this time interval is (4.21 +0.79/-0.72)E-06 erg/cm^2. The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. GRM is developed by the Institute of High Energy Physics (IHEP) of CAS. The SVOM/GRM point of contact for this burst is: Yue Wang (IHEP) (yuewang(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/43679. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41784] GRB 260204A: Swift-XRT afterglow detection
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43678 SUBJECT: GRB 260204A: Swift-XRT afterglow detection DATE: 26/02/10 08:34:30 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> J.P. Osborne (U. Leicester), M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) , M. Capalbi (INAF-OAR), D.N. Burrows (PSU), S. Lanava (PSU), S. Dichiara (PSU), K.L. Page (U. Leicester) and P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Swift-XRT has performed a second epoch of follow-up observations of GRB 260204A (Pillas et al., GCN Circ. 43613), collecting a further 2.6 ks between T0+363 ks and T0+458 ks. "Source 1" (Evans et al., GCN Circ. 43622), which corresponds to the fading optical counterpart (Li et al., GCN Circs 43620, 43623), is no longer detected and has faded with >3-sigma significance. The upper limit is 6.97e-3 ct/sec, compared to the previous detection level of 2.36 +/- 0.46 ct/sec, giving a power-law decay index of alpha >0.4. Using 1659 s of PC mode data and 1 UVOT image, we find an enhanced XRT position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 205.10623, +1.93075 which is equivalent to: RA (J2000): 13h 40m 25.49s Dec(J2000): +01d 55' 50.7" with an uncertainty of 4.4 arcsec (radius, 90% confidence). The results of the XRT-team automatic analysis are available at https://www.swift.ac.uk/xrt_products/03000405. The results of the full analysis of the XRT observations are available at https://www.swift.ac.uk/SVOM/SVOM_FIELD00057. This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/43678. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41783] GRB 260208B: AstroSat CZTI detection of a bright long burst
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43677 SUBJECT: GRB 260208B: AstroSat CZTI detection of a bright long burst DATE: 26/02/10 02:01:04 GMT FROM: Anuraag Arya at IIT Bombay <aryaanuraag910(a)gmail.com> Harsha K. H. (IUCAA), M. Tembhurnikar (IUCAA), S. Salunke (IUCAA), U. Pathak (IITB), A. Arya (IITB), A. Goyal (IITB), 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 ML pipeline (Abraham et al., 2021, MNRAS, 504, 3084) and the CIFT framework (Sharma et al., 2021, JApA, 42, 73) showed the detection of a long, bright GRB 260208B which was also detected by Fermi/GBM (Fermi GBM Team, GCN Circ. 43638), Fermi/LAT (F. Longo et al., GCN Circ. 43647), and SVOM/GRM (SVOM GRM Team, GCN Circ. 43650). We also see a relatively faint burst episode about 100 s after the initial bright burst in both CZT & CsI detectors. The source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2026-02-08 09:52:59.50 UTC. The measured peak count rate associated with the burst is 1334 (+64, -68) counts/s above the background in the combined data of all quadrants, with a total of 14112 (+381, -416) counts. The local mean background count rate was 272 (+2, -3) counts/s. Using cumulative rates, we measure a T90 of 24 (+6, -2) s. In the preliminary analysis, we find 2125 Compton events associated with this event. The source was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2026-02-08 09:52:58.95 UTC. The measured peak count rate associated with the burst is 3595 (+111, -118) counts/s above the background in the combined data of all quadrants, with a total of 32443 (+740, -736) counts. The local mean background count rate was 1199 (+4, -5) counts/s. We measure a T90 of 22 (+1, -1) s from the cumulative Veto light curve. 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/43677. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41782] GRB260208A: Liverpool Telescope optical follow-up observations
by GCN Circulars 10 Feb '26

10 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43676 SUBJECT: GRB260208A: Liverpool Telescope optical follow-up observations DATE: 26/02/10 00:51:14 GMT FROM: A. Bochenek at Liverpool John Moores University <a.m.bochenek(a)2023.ljmu.ac.uk> A. Bochenek, J. Wise, D. A. Perley (LJMU), report: We observed the field of GRB260208a (Fermi GBM team, GCN 43635; Sonawane et al., GCN 43642; Longo et al., GCN 43645; Luo et al., GCN 43658; Mukherjee et al. GCN 43673; Waratkar et al., GCN 43674, Cheung et al., GCN 43675) using the IO:O optical camera on the 2m robotic Liverpool Telescope. We obtained two epochs of 3x100s exposures in the SDSS r, i, z filters and 4x100s in SDSS g, starting at 2026-02-09 02:49:11 UT, approximately 21.7 hours after trigger, and the second epoch at 24.4 hours after the trigger. We report detections in stacked images in all filters at the position first reported by Lipunov et al., GCN 43640 and Wortley et al., GCN 43641, although we note some exposures were discarded due to poor seeing or telescope movement. MJD (mid) T_mid-T_0 Filter Mag. (AB) 61080.11951 21.74 h z 20.03 ± 0.16 61080.12395 21.85 h i 20.24 ± 0.25 61080.12842 21.95 h r 20.75 ± 0.10 61080.13428 22.09 h g 21.34 ± 0.24 61080.22567 24.29 h z 20.35 ± 0.11 61080.23080 24.41 h i 20.49 ± 0.09 61060.04432 24.54 h r 20.97 ± 0.15 61080.23595 24.64 h g 21.39 ± 0.14 The photometry is consistent with measurements taken at similar time by Dimple et al., GCN 43661 and Magnani et al., GCN 43664. The photometry was obtained using nearby PanSTARRS secondary standards and was not corrected for extinction. View this GCN Circular online at https://gcn.nasa.gov/circulars/43676. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41781] GRB 260208A: Glowbug gamma-ray detection
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43675 SUBJECT: GRB 260208A: Glowbug gamma-ray detection DATE: 26/02/09 23:42:07 GMT FROM: C.C. Cheung at Naval Research Lab <Teddy.Cheung(a)nrl.navy.mil> C.C. Cheung, R. Woolf, M. Kerr, J.E. Grove (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report: The Glowbug gamma-ray telescope [1,2,3], operating on the International Space Station, reports the detection of GRB 260208A, which was also detected by Fermi/GBM (GCN 43635, 43673), Fermi/LAT (GCN 43645), GECAM-B (GCN 43658), and NuSTAR (GCN 43674). Using an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2026-02-08 05:07:25.856 with a duration of 53.2 s and a total significance of about 369 sigma. The Glowbug light curve comprises a triple-peaked structure as seen in the Fermi/GBM light curve (GCN 43635). The analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS. Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Program’s STP-H9 to the ISS and operated until 2024 April when it was put in safe storage on orbit. Glowbug was removed from storage and resumed operation on 2025 September 12. [1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959 [2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O [3] Woolf, R.S. et al. 2024, Proc. SPIE, 13151, id. 1315108 Distribution Statement A: Approved for public release. Distribution is unlimited. View this GCN Circular online at https://gcn.nasa.gov/circulars/43675. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41780] GRB 260208A: NuSTAR detection of prompt emission
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43674 SUBJECT: GRB 260208A: NuSTAR detection of prompt emission DATE: 26/02/09 21:01:46 GMT FROM: Gaurav Waratkar at Caltech <gauravwaratkar(a)iitb.ac.in> G. Waratkar (Caltech) and B. Grefenstette (Caltech) report on behalf of the NuSTAR Search for INteresting Gamma-ray Signals (SINGS) working group: The NuSTAR SINGS working group reports the detection of prompt emission from the long-duration GRB 260208A in both the NuSTAR CsI anti-coincidence shields. This GRB was identified through a blind search using the CsI shield rates. Details of the search algorithm will be described in a future paper. The NuSTAR SINGS algorithm triggered at 2026-02-08 05:07:29.00 (with a resolution ~5-seconds). This is consistent with the detections of GRB 260208A by Fermi/GBM (Fermi GBM Team, GCN Circ. 43635) and GECAM-B (Luo et al., GCN Circ. 43658). The NuSTAR CsI shield data are recorded at 1 Hz. We detect one peak lasting for ~40-s, consistent with the detections of Fermi/GBM & GECAM-B. The peak count rate is ~4500-cps with a baseline rate of ~1000-cps during this time period. We also see marginal evidence in the signal above 100 keV in the CdZnTe detectors. The optical counterpart (Podesta et al., GCN Circ. 43640) at RA = 204.731, Dec = 33.801 implies an offset from the NuSTAR boresight of 99-deg (i.e. from the side of the instrument) and an offset from the geocenter of 111-deg. Lightcurves and analysis for this GRB can be found here: https://nustarsoc.caltech.edu/NuSTAR_Public/grbs/reports/2026/260208A/ Information on NuSTAR SINGS can be found here: https://nustarsoc.caltech.edu/NuSTAR_Public/grbs/ NuSTAR is a NASA Small Explorer mission led by Caltech and managed by JPL for NASA's Science Mission Directorate in Washington. View this GCN Circular online at https://gcn.nasa.gov/circulars/43674. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41779] GRB 260208A: Fermi GBM Observation
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43673 SUBJECT: GRB 260208A: Fermi GBM Observation DATE: 26/02/09 20:09:35 GMT FROM: oindabimukherjee(a)gmail.com O. Mukherjee (USRA) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 05:07:28.24 UT on 08 February 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260208A (trigger 792220053/260208214), which was also detected by Fermi-LAT (F. Longo et al. 2026, GCN 43645), Swift XRT (S. Dichiara et al. 2026, GCN 43652), and NOT (Dimple et al. 2026, GCN 43662) with a spectroscopic redshift of z = 2.36. The Fermi GBM on-ground location is consistent with the Fermi-LAT position. The angle from the Fermi LAT boresight is 78 degrees. The GBM light curve consists of a single emission episode with a duration (T90) of about 35.3 s (50-300 keV). The time-averaged spectrum from T0-3.6 to T0+66.0 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.87 +/- 0.01 and the cutoff energy, parameterized as Epeak, is 460 +/- 0.1 keV. The event fluence (10-1000 keV) in this time interval is (1.50 +/- 0.06)E-04 erg/cm^2. The 1-sec peak photon flux measured starting from T0+17 s in the 10-1000 keV band is 29.7 +/- 0.4 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 328 +/- 1 keV, alpha = -0.76 +/- 0.01 and beta = -2 +/- 0.01. 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/43673. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41778] Fermi GRB 260209A: Global MASTER-Net observations report
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43672 SUBJECT: Fermi GRB 260209A: Global MASTER-Net observations report DATE: 26/02/09 19:30:26 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) started inspect of the Fermi GRB 260209A ( Fermi GBM team, GCN 43656) errorbox 49515 sec after notice time and 49546 sec after trigger time at 2026-02-09 16:31:43 UT, with upper limit up to 20.1 mag. The observations began at zenith distance = 43 deg. The sun altitude is -52.3 deg. The galactic latitude b = -5 deg., longitude l = 172 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3126944 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 270 | 2026-02-09 02:49:57 | MASTER- | (04h 52m 45.79s , +29d 28m 36.0s) | C | 60 | 19.7 | 270 | 2026-02-09 02:49:57 | MASTER- | (04h 51m 19.70s , +30d 01m 22.9s) | C | 60 | 19.5 | 341 | 2026-02-09 02:51:07 | MASTER- | (05h 00m 34.67s , +30d 03m 14.8s) | C | 60 | 19.5 | 341 | 2026-02-09 02:51:07 | MASTER- | (05h 02m 00.76s , +29d 30m 27.9s) | C | 60 | 19.8 | 412 | 2026-02-09 02:52:18 | MASTER- | (04h 39m 10.77s , +31d 56m 54.0s) | C | 60 | 19.6 | 412 | 2026-02-09 02:52:18 | MASTER- | (04h 40m 38.89s , +31d 24m 06.5s) | C | 60 | 19.8 | 481 | 2026-02-09 02:53:28 | MASTER- | (04h 50m 08.80s , +31d 23m 21.8s) | C | 60 | 19.6 | 481 | 2026-02-09 02:53:28 | MASTER- | (04h 48m 40.63s , +31d 56m 09.5s) | C | 60 | 19.5 | 552 | 2026-02-09 02:54:39 | MASTER- | (04h 47m 33.22s , +27d 34m 39.4s) | C | 60 | 19.7 | 552 | 2026-02-09 02:54:39 | MASTER- | (04h 46m 09.05s , +28d 07m 26.2s) | C | 60 | 19.5 | 622 | 2026-02-09 02:55:49 | MASTER- | (04h 56m 33.05s , +27d 36m 28.2s) | C | 60 | 19.8 | 622 | 2026-02-09 02:55:49 | MASTER- | (04h 55m 08.77s , +28d 09m 14.6s) | C | 60 | 19.5 | 693 | 2026-02-09 02:57:00 | MASTER- | (04h 35m 19.05s , +29d 29m 37.1s) | C | 60 | 19.7 | 694 | 2026-02-09 02:57:00 | MASTER- | (04h 33m 53.12s , +30d 02m 23.9s) | C | 60 | 19.7 | 763 | 2026-02-09 02:58:10 | MASTER- | (04h 42m 58.81s , +30d 02m 04.1s) | C | 60 | 19.6 | 763 | 2026-02-09 02:58:10 | MASTER- | (04h 44m 24.81s , +29d 29m 17.3s) | C | 60 | 19.8 | 834 | 2026-02-09 02:59:21 | MASTER- | (04h 28m 32.61s , +33d 16m 56.5s) | C | 60 | 19.5 | 834 | 2026-02-09 02:59:21 | MASTER- | (04h 27m 02.16s , +33d 49m 45.5s) | C | 60 | 19.4 | 904 | 2026-02-09 03:00:30 | MASTER- | (04h 38m 00.38s , +33d 16m 09.1s) | C | 60 | 19.5 | 904 | 2026-02-09 03:00:30 | MASTER- | (04h 36m 29.75s , +33d 48m 58.6s) | C | 60 | 19.5 | 980 | 2026-02-09 03:01:47 | MASTER- | (04h 52m 48.14s , +29d 28m 53.8s) | C | 60 | 19.7 | 980 | 2026-02-09 03:01:47 | MASTER- | (04h 51m 21.87s , +30d 01m 41.0s) | C | 60 | 19.5 | 1049 | 2026-02-09 03:02:56 | MASTER- | (05h 01m 58.44s , +29d 30m 17.6s) | C | 60 | 19.6 | 1049 | 2026-02-09 03:02:56 | MASTER- | (05h 00m 32.04s , +30d 03m 04.7s) | C | 60 | 19.3 | 1120 | 2026-02-09 03:04:07 | MASTER- | (04h 40m 43.00s , +31d 22m 37.0s) | C | 60 | 19.7 | 1120 | 2026-02-09 03:04:07 | MASTER- | (04h 39m 14.70s , +31d 55m 24.6s) | C | 60 | 19.5 | 1189 | 2026-02-09 03:05:16 | MASTER- | (04h 48m 40.92s , +31d 57m 06.9s) | C | 60 | 19.5 | 1189 | 2026-02-09 03:05:16 | MASTER- | (04h 50m 09.33s , +31d 24m 19.5s) | C | 60 | 19.6 | 1260 | 2026-02-09 03:06:27 | MASTER- | (04h 46m 03.02s , +28d 08m 18.2s) | C | 60 | 19.6 | 1260 | 2026-02-09 03:06:27 | MASTER- | (04h 47m 27.37s , +27d 35m 31.3s) | C | 60 | 19.6 | 1331 | 2026-02-09 03:07:37 | MASTER- | (04h 55m 06.21s , +28d 09m 31.4s) | C | 60 | 19.7 | 1331 | 2026-02-09 03:07:37 | MASTER- | (04h 56m 30.66s , +27d 36m 44.6s) | C | 60 | 19.8 | 1401 | 2026-02-09 03:08:48 | MASTER- | (04h 35m 19.58s , +29d 29m 16.6s) | C | 60 | 19.8 | 1401 | 2026-02-09 03:08:48 | MASTER- | (04h 33m 53.60s , +30d 02m 03.6s) | C | 60 | 19.6 | 1470 | 2026-02-09 03:09:57 | MASTER- | (04h 44m 24.96s , +29d 28m 28.4s) | C | 60 | 19.8 | 1470 | 2026-02-09 03:09:57 | MASTER- | (04h 42m 58.87s , +30d 01m 15.4s) | C | 60 | 19.6 | 1541 | 2026-02-09 03:11:08 | MASTER- | (04h 28m 32.79s , +33d 16m 37.8s) | C | 60 | 19.5 | 1541 | 2026-02-09 03:11:08 | MASTER- | (04h 27m 02.37s , +33d 49m 26.9s) | C | 60 | 19.4 | 1612 | 2026-02-09 03:12:18 | MASTER- | (04h 38m 04.44s , +33d 18m 03.8s) | C | 60 | 19.5 | 1612 | 2026-02-09 03:12:18 | MASTER- | (04h 36m 33.72s , +33d 50m 53.2s) | C | 60 | 19.4 | 1682 | 2026-02-09 03:13:29 | MASTER- | (04h 52m 45.82s , +29d 28m 45.0s) | C | 60 | 19.5 | 1682 | 2026-02-09 03:13:29 | MASTER- | (04h 51m 19.58s , +30d 01m 32.2s) | C | 60 | 19.4 | 1752 | 2026-02-09 03:14:39 | MASTER- | (05h 02m 01.23s , +29d 30m 39.1s) | C | 60 | 19.5 | 1752 | 2026-02-09 03:14:39 | MASTER- | (05h 00m 34.85s , +30d 03m 26.1s) | C | 60 | 19.3 | 1823 | 2026-02-09 03:15:50 | MASTER- | (04h 40m 40.64s , +31d 23m 29.7s) | C | 60 | 19.6 | 1823 | 2026-02-09 03:15:50 | MASTER- | (04h 39m 12.49s , +31d 56m 17.2s) | C | 60 | 19.5 | 1893 | 2026-02-09 03:16:59 | MASTER- | (04h 50m 02.79s , +31d 24m 41.9s) | C | 60 | 19.6 | 1893 | 2026-02-09 03:16:59 | MASTER- | (04h 48m 34.52s , +31d 57m 29.3s) | C | 60 | 19.5 | 1963 | 2026-02-09 03:18:10 | MASTER- | (04h 47m 32.22s , +27d 35m 44.0s) | C | 60 | 19.4 | 1963 | 2026-02-09 03:18:10 | MASTER- | (04h 46m 07.95s , +28d 08m 31.1s) | C | 60 | 19.3 | 2033 | 2026-02-09 03:19:19 | MASTER- | (04h 55m 05.96s , +28d 07m 42.2s) | C | 60 | 19.6 | 2033 | 2026-02-09 03:19:19 | MASTER- | (04h 56m 30.33s , +27d 34m 55.2s) | C | 60 | 19.6 | 2104 | 2026-02-09 03:20:30 | MASTER- | (04h 35m 20.57s , +29d 28m 51.9s) | C | 60 | 19.6 | 2104 | 2026-02-09 03:20:30 | MASTER- | (04h 33m 54.71s , +30d 01m 39.1s) | C | 60 | 19.6 | 2174 | 2026-02-09 03:21:40 | MASTER- | (04h 44m 28.83s , +29d 30m 41.7s) | C | 60 | 19.7 | 2174 | 2026-02-09 03:21:40 | MASTER- | (04h 43m 02.79s , +30d 03m 28.7s) | C | 60 | 19.6 | 2244 | 2026-02-09 03:22:51 | MASTER- | (04h 28m 29.69s , +33d 16m 36.9s) | C | 60 | 19.4 | 2244 | 2026-02-09 03:22:51 | MASTER- | (04h 26m 59.41s , +33d 49m 26.6s) | C | 60 | 19.2 | 2313 | 2026-02-09 03:24:00 | MASTER- | (04h 38m 07.96s , +33d 18m 10.8s) | C | 60 | 19.4 | 2313 | 2026-02-09 03:24:00 | MASTER- | (04h 36m 37.33s , +33d 51m 00.9s) | C | 60 | 19.5 | 2384 | 2026-02-09 03:25:11 | MASTER- | (04h 52m 43.58s , +29d 29m 55.7s) | C | 60 | 19.5 | 2384 | 2026-02-09 03:25:11 | MASTER- | (04h 51m 17.40s , +30d 02m 43.2s) | C | 60 | 19.6 | 2453 | 2026-02-09 03:26:20 | MASTER- | (05h 01m 54.17s , +29d 31m 07.3s) | C | 60 | 19.5 | 2453 | 2026-02-09 03:26:20 | MASTER- | (05h 00m 27.88s , +30d 03m 54.8s) | C | 60 | 19.5 | 2525 | 2026-02-09 03:27:31 | MASTER- | (04h 40m 45.25s , +31d 23m 44.6s) | C | 60 | 19.6 | 2525 | 2026-02-09 03:27:31 | MASTER- | (04h 39m 17.34s , +31d 56m 32.4s) | C | 60 | 19.7 | 2595 | 2026-02-09 03:28:41 | MASTER- | (04h 50m 03.28s , +31d 22m 54.6s) | C | 60 | 19.6 | 2595 | 2026-02-09 03:28:41 | MASTER- | (04h 48m 35.27s , +31d 55m 42.6s) | C | 60 | 19.6 | 2665 | 2026-02-09 03:29:52 | MASTER- | (04h 47m 34.09s , +27d 35m 22.0s) | C | 60 | 19.6 | 2665 | 2026-02-09 03:29:52 | MASTER- | (04h 46m 09.97s , +28d 08m 09.9s) | C | 60 | 19.5 | 2735 | 2026-02-09 03:31:01 | MASTER- | (04h 56m 32.52s , +27d 36m 51.2s) | C | 60 | 19.6 | 2735 | 2026-02-09 03:31:01 | MASTER- | (04h 55m 08.25s , +28d 09m 38.6s) | C | 60 | 19.7 | 2805 | 2026-02-09 03:32:12 | MASTER- | (04h 35m 16.70s , +29d 29m 00.2s) | C | 60 | 19.7 | 2805 | 2026-02-09 03:32:12 | MASTER- | (04h 33m 51.02s , +30d 01m 48.1s) | C | 60 | 19.8 | 2875 | 2026-02-09 03:33:22 | MASTER- | (04h 44m 32.58s , +29d 30m 38.7s) | C | 60 | 19.8 | 2875 | 2026-02-09 03:33:22 | MASTER- | (04h 43m 06.74s , +30d 03m 26.4s) | C | 60 | 19.7 | 2945 | 2026-02-09 03:34:32 | MASTER- | (04h 28m 27.57s , +33d 17m 44.5s) | C | 60 | 19.4 | 2945 | 2026-02-09 03:34:32 | MASTER- | (04h 26m 57.92s , +33d 50m 33.4s) | C | 60 | 19.4 | 3014 | 2026-02-09 03:35:41 | MASTER- | (04h 38m 02.25s , +33d 18m 52.7s) | C | 60 | 19.5 | 3014 | 2026-02-09 03:35:41 | MASTER- | (04h 36m 32.26s , +33d 51m 41.8s) | C | 60 | 19.5 | 3085 | 2026-02-09 03:36:52 | MASTER- | (04h 52m 48.39s , +29d 30m 09.9s) | C | 60 | 19.4 | 3085 | 2026-02-09 03:36:52 | MASTER- | (04h 51m 22.42s , +30d 02m 57.7s) | C | 60 | 19.5 | 3154 | 2026-02-09 03:38:01 | MASTER- | (05h 01m 55.13s , +29d 29m 19.8s) | C | 60 | 19.5 | 3154 | 2026-02-09 03:38:01 | MASTER- | (05h 00m 29.03s , +30d 02m 07.6s) | C | 60 | 19.4 | 3225 | 2026-02-09 03:39:12 | MASTER- | (04h 40m 47.07s , +31d 23m 13.4s) | C | 60 | 19.6 | 3225 | 2026-02-09 03:39:12 | MASTER- | (04h 39m 19.38s , +31d 56m 01.5s) | C | 60 | 19.5 | 3295 | 2026-02-09 03:40:22 | MASTER- | (04h 50m 06.41s , +31d 24m 54.8s) | C | 60 | 19.5 | 3295 | 2026-02-09 03:40:22 | MASTER- | (04h 48m 38.53s , +31d 57m 42.6s) | C | 60 | 19.5 | 3365 | 2026-02-09 03:41:32 | MASTER- | (04h 47m 30.12s , +27d 35m 16.0s) | C | 60 | 19.6 | 3365 | 2026-02-09 03:41:32 | MASTER- | (04h 46m 06.11s , +28d 08m 04.1s) | C | 60 | 19.6 | 3436 | 2026-02-09 03:42:42 | MASTER- | (04h 56m 35.72s , +27d 37m 03.3s) | C | 60 | 19.6 | 3436 | 2026-02-09 03:42:42 | MASTER- | (04h 55m 11.54s , +28d 09m 51.0s) | C | 60 | 19.6 | 3506 | 2026-02-09 03:43:53 | MASTER- | (04h 35m 13.49s , +29d 30m 06.0s) | C | 60 | 19.7 | 3506 | 2026-02-09 03:43:53 | MASTER- | (04h 33m 47.95s , +30d 02m 54.4s) | C | 60 | 19.5 | 3577 | 2026-02-09 03:45:04 | MASTER- | (04h 44m 24.95s , +29d 31m 13.9s) | C | 60 | 19.6 | 3577 | 2026-02-09 03:45:04 | MASTER- | (04h 42m 59.20s , +30d 04m 02.1s) | C | 60 | 19.6 | 3648 | 2026-02-09 03:46:15 | MASTER- | (04h 28m 33.50s , +33d 18m 04.0s) | C | 60 | 19.5 | 3648 | 2026-02-09 03:46:15 | MASTER- | (04h 27m 04.15s , +33d 50m 53.1s) | C | 60 | 19.3 | 3719 | 2026-02-09 03:47:25 | MASTER- | (04h 36m 33.00s , +33d 50m 00.2s) | C | 60 | 19.4 | 3719 | 2026-02-09 03:47:25 | MASTER- | (04h 38m 02.60s , +33d 17m 10.9s) | C | 60 | 19.5 | 3789 | 2026-02-09 03:48:36 | MASTER- | (04h 52m 49.31s , +29d 29m 43.0s) | C | 60 | 19.5 | 3789 | 2026-02-09 03:48:36 | MASTER- | (04h 51m 23.48s , +30d 02m 31.2s) | C | 60 | 19.3 | 3859 | 2026-02-09 03:49:45 | MASTER- | (05h 01m 58.05s , +29d 31m 31.8s) | C | 60 | 19.4 | 3859 | 2026-02-09 03:49:45 | MASTER- | (05h 00m 32.01s , +30d 04m 19.9s) | C | 60 | 19.4 | 3929 | 2026-02-09 03:50:56 | MASTER- | (04h 40m 43.73s , +31d 23m 25.4s) | C | 60 | 19.5 | 3929 | 2026-02-09 03:50:56 | MASTER- | (04h 39m 16.24s , +31d 56m 13.9s) | C | 60 | 19.5 | 4000 | 2026-02-09 03:52:07 | MASTER- | (04h 50m 09.29s , +31d 25m 06.3s) | C | 60 | 19.6 | 4000 | 2026-02-09 03:52:07 | MASTER- | (04h 48m 41.60s , +31d 57m 54.6s) | C | 60 | 19.5 | 4070 | 2026-02-09 03:53:16 | MASTER- | (04h 47m 27.37s , +27d 36m 32.2s) | C | 60 | 19.6 | 4070 | 2026-02-09 03:53:16 | MASTER- | (04h 46m 03.54s , +28d 09m 20.8s) | C | 60 | 19.5 | 4139 | 2026-02-09 03:54:26 | MASTER- | (04h 56m 29.27s , +27d 37m 39.1s) | C | 60 | 19.6 | 4139 | 2026-02-09 03:54:26 | MASTER- | (04h 55m 05.27s , +28d 10m 27.6s) | C | 60 | 19.6 | 4209 | 2026-02-09 03:55:36 | MASTER- | (04h 35m 19.42s , +29d 30m 25.0s) | C | 60 | 19.2 | 4210 | 2026-02-09 03:55:36 | MASTER- | (04h 33m 54.15s , +30d 03m 14.3s) | C | 60 | 19.0 | 4280 | 2026-02-09 03:56:46 | MASTER- | (04h 44m 27.09s , +29d 29m 32.4s) | C | 60 | 19.7 | 4280 | 2026-02-09 03:56:46 | MASTER- | (04h 43m 01.62s , +30d 02m 21.6s) | C | 60 | 19.5 | 4350 | 2026-02-09 03:57:57 | MASTER- | (04h 28m 34.30s , +33d 17m 43.8s) | C | 60 | 19.4 | 4350 | 2026-02-09 03:57:57 | MASTER- | (04h 27m 05.35s , +33d 50m 33.4s) | C | 60 | 19.2 | 4421 | 2026-02-09 03:59:07 | MASTER- | (04h 38m 05.72s , +33d 19m 27.8s) | C | 60 | 19.3 | 4421 | 2026-02-09 03:59:07 | MASTER- | (04h 36m 36.38s , +33d 52m 17.3s) | C | 60 | 19.2 | 4492 | 2026-02-09 04:00:19 | MASTER- | (04h 59m 39.40s , +25d 43m 51.4s) | C | 60 | 19.1 | 4492 | 2026-02-09 04:00:19 | MASTER- | (04h 58m 17.10s , +26d 16m 40.3s) | C | 60 | 19.3 | 4568 | 2026-02-09 04:01:34 | MASTER- | (05h 08m 26.80s , +25d 43m 00.7s) | C | 60 | 19.3 | 4568 | 2026-02-09 04:01:34 | MASTER- | (05h 07m 04.35s , +26d 15m 49.6s) | C | 60 | 19.2 | 4640 | 2026-02-09 04:02:46 | MASTER- | (04h 22m 58.33s , +31d 24m 33.2s) | C | 60 | 19.4 | 4640 | 2026-02-09 04:02:46 | MASTER- | (04h 21m 31.78s , +31d 57m 23.2s) | C | 60 | 19.1 | 4709 | 2026-02-09 04:03:56 | MASTER- | (04h 32m 14.01s , +31d 23m 38.1s) | C | 60 | 19.2 | 4709 | 2026-02-09 04:03:56 | MASTER- | (04h 30m 47.24s , +31d 56m 28.1s) | C | 60 | 19.0 | 4781 | 2026-02-09 04:05:07 | MASTER- | (04h 41m 22.01s , +26d 16m 26.6s) | C | 60 | 19.5 | 4781 | 2026-02-09 04:05:07 | MASTER- | (04h 42m 43.81s , +25d 43m 36.6s) | C | 60 | 19.5 | 4851 | 2026-02-09 04:06:18 | MASTER- | (04h 51m 37.00s , +25d 42m 03.6s) | C | 60 | 19.5 | 4851 | 2026-02-09 04:06:18 | MASTER- | (04h 50m 15.04s , +26d 14m 53.4s) | C | 60 | 19.5 | 4921 | 2026-02-09 04:07:28 | MASTER- | (04h 30m 17.54s , +27d 36m 46.8s) | C | 60 | 19.5 | 4921 | 2026-02-09 04:07:28 | MASTER- | (04h 28m 54.54s , +28d 09m 36.9s) | C | 60 | 19.4 | 4991 | 2026-02-09 04:08:37 | MASTER- | (04h 39m 19.22s , +27d 37m 51.8s) | C | 60 | 19.4 | 4991 | 2026-02-09 04:08:37 | MASTER- | (04h 37m 56.02s , +28d 10m 41.7s) | C | 60 | 19.2 | 5061 | 2026-02-09 04:09:48 | MASTER- | (04h 54m 59.20s , +23d 48m 05.8s) | C | 60 | 19.4 | 5061 | 2026-02-09 04:09:48 | MASTER- | (04h 53m 38.78s , +24d 20m 55.8s) | C | 60 | 19.3 | 5130 | 2026-02-09 04:10:57 | MASTER- | (05h 03m 51.59s , +23d 48m 38.6s) | C | 60 | 19.0 | 5130 | 2026-02-09 04:10:57 | MASTER- | (05h 02m 30.98s , +24d 21m 28.5s) | C | 60 | 19.0 | 5200 | 2026-02-09 04:12:06 | MASTER- | (04h 58m 14.89s , +26d 16m 36.5s) | C | 60 | 19.3 | 5200 | 2026-02-09 04:12:06 | MASTER- | (04h 59m 36.93s , +25d 43m 47.0s) | C | 60 | 19.1 | 5269 | 2026-02-09 04:13:16 | MASTER- | (05h 07m 08.04s , +26d 15m 25.8s) | C | 60 | 19.0 | 5269 | 2026-02-09 04:13:16 | MASTER- | (05h 08m 30.26s , +25d 42m 36.3s) | C | 60 | 19.0 | 5340 | 2026-02-09 04:14:27 | MASTER- | (04h 22m 57.61s , +31d 25m 26.4s) | C | 60 | 19.1 | 5340 | 2026-02-09 04:14:27 | MASTER- | (04h 21m 31.52s , +31d 58m 17.2s) | C | 60 | 18.9 | 5409 | 2026-02-09 04:15:36 | MASTER- | (04h 32m 14.67s , +31d 24m 59.2s) | C | 60 | 18.8 | 5409 | 2026-02-09 04:15:36 | MASTER- | (04h 30m 48.30s , +31d 57m 50.1s) | C | 60 | 18.7 | 5481 | 2026-02-09 04:16:47 | MASTER- | (04h 41m 19.94s , +26d 17m 01.9s) | C | 60 | 19.3 | 5481 | 2026-02-09 04:16:47 | MASTER- | (04h 42m 41.40s , +25d 44m 11.0s) | C | 60 | 19.5 | 5550 | 2026-02-09 04:17:57 | MASTER- | (04h 51m 41.01s , +25d 43m 16.1s) | C | 60 | 19.3 | 5550 | 2026-02-09 04:17:57 | MASTER- | (04h 50m 19.34s , +26d 16m 06.7s) | C | 60 | 19.2 | 5622 | 2026-02-09 04:19:08 | MASTER- | (04h 30m 16.85s , +27d 36m 09.1s) | C | 60 | 19.4 | 5622 | 2026-02-09 04:19:08 | MASTER- | (04h 28m 54.24s , +28d 09m 00.1s) | C | 60 | 19.2 | 5692 | 2026-02-09 04:20:18 | MASTER- | (04h 39m 25.98s , +27d 36m 30.1s) | C | 60 | 19.0 | 5692 | 2026-02-09 04:20:18 | MASTER- | (04h 38m 03.14s , +28d 09m 21.1s) | C | 60 | 18.7 | 5762 | 2026-02-09 04:21:29 | MASTER- | (04h 53m 42.44s , +24d 22m 49.5s) | C | 60 | 19.4 | 5762 | 2026-02-09 04:21:29 | MASTER- | (04h 55m 02.60s , +23d 49m 58.9s) | C | 60 | 19.4 | 5831 | 2026-02-09 04:22:38 | MASTER- | (05h 03m 47.67s , +23d 48m 38.0s) | C | 60 | 18.7 | 5831 | 2026-02-09 04:22:38 | MASTER- | (05h 02m 27.33s , +24d 21m 28.6s) | C | 60 | 18.6 | 5901 | 2026-02-09 04:23:48 | MASTER- | (04h 59m 41.01s , +25d 44m 17.1s) | C | 60 | 18.7 | 5901 | 2026-02-09 04:23:48 | MASTER- | (04h 58m 19.25s , +26d 17m 07.5s) | C | 60 | 18.9 | 5970 | 2026-02-09 04:24:57 | MASTER- | (05h 08m 28.02s , +25d 43m 35.0s) | C | 60 | 19.1 | 5970 | 2026-02-09 04:24:57 | MASTER- | (05h 07m 06.06s , +26d 16m 25.3s) | C | 60 | 19.1 | 6042 | 2026-02-09 04:26:09 | MASTER- | (04h 21m 27.64s , +31d 59m 10.6s) | C | 60 | 18.9 | 6042 | 2026-02-09 04:26:09 | MASTER- | (04h 22m 53.35s , +31d 26m 19.0s) | C | 60 | 19.2 | 6111 | 2026-02-09 04:27:18 | MASTER- | (04h 32m 20.83s , +31d 25m 22.8s) | C | 60 | 19.0 | 6111 | 2026-02-09 04:27:18 | MASTER- | (04h 30m 54.86s , +31d 58m 14.3s) | C | 60 | 18.9 | 6182 | 2026-02-09 04:28:29 | MASTER- | (04h 41m 19.54s , +26d 15m 24.6s) | C | 60 | 19.2 | 6182 | 2026-02-09 04:28:29 | MASTER- | (04h 42m 40.55s , +25d 42m 33.0s) | C | 60 | 19.5 | 6253 | 2026-02-09 04:29:39 | MASTER- | (04h 51m 39.40s , +25d 42m 40.4s) | C | 60 | 19.4 | 6253 | 2026-02-09 04:29:39 | MASTER- | (04h 50m 18.15s , +26d 15m 31.9s) | C | 60 | 19.2 | 6323 | 2026-02-09 04:30:50 | MASTER- | (04h 30m 21.22s , +27d 38m 12.2s) | C | 60 | 19.5 | 6323 | 2026-02-09 04:30:50 | MASTER- | (04h 28m 59.05s , +28d 11m 04.0s) | C | 60 | 19.2 | 6393 | 2026-02-09 04:32:00 | MASTER- | (04h 38m 00.75s , +28d 09m 37.8s) | C | 60 | 19.0 | 6393 | 2026-02-09 04:32:00 | MASTER- | (04h 39m 23.13s , +27d 36m 46.0s) | C | 60 | 19.4 | 6463 | 2026-02-09 04:33:10 | MASTER- | (04h 55m 05.41s , +23d 50m 41.4s) | C | 60 | 19.4 | 6463 | 2026-02-09 04:33:10 | MASTER- | (04h 53m 45.67s , +24d 23m 32.9s) | C | 60 | 19.1 | 6533 | 2026-02-09 04:34:19 | MASTER- | (05h 03m 44.63s , +23d 49m 52.0s) | C | 60 | 18.9 | 6533 | 2026-02-09 04:34:19 | MASTER- | (05h 02m 24.67s , +24d 22m 43.4s) | C | 60 | 18.7 | 6602 | 2026-02-09 04:35:29 | MASTER- | (04h 59m 34.92s , +25d 44m 49.4s) | C | 60 | 19.0 | 6602 | 2026-02-09 04:35:29 | MASTER- | (04h 58m 13.58s , +26d 17m 40.4s) | C | 60 | 19.2 | 6672 | 2026-02-09 04:36:38 | MASTER- | (05h 08m 33.81s , +25d 43m 55.3s) | C | 60 | 18.9 | 6672 | 2026-02-09 04:36:38 | MASTER- | (05h 07m 12.25s , +26d 16m 46.4s) | C | 60 | 19.0 | 6744 | 2026-02-09 04:37:50 | MASTER- | (04h 21m 27.44s , +31d 57m 36.2s) | C | 60 | 19.0 | 6744 | 2026-02-09 04:37:50 | MASTER- | (04h 22m 52.54s , +31d 24m 44.0s) | C | 60 | 19.3 | 6813 | 2026-02-09 04:39:00 | MASTER- | (04h 32m 22.15s , +31d 24m 48.5s) | C | 60 | 18.8 | 6813 | 2026-02-09 04:39:00 | MASTER- | (04h 30m 56.73s , +31d 57m 40.6s) | C | 60 | 18.7 | 6885 | 2026-02-09 04:40:11 | MASTER- | (04h 42m 44.63s , +25d 44m 50.9s) | C | 60 | 19.5 | 6885 | 2026-02-09 04:40:11 | MASTER- | (04h 41m 24.09s , +26d 17m 43.0s) | C | 60 | 19.4 | 6955 | 2026-02-09 04:41:21 | MASTER- | (04h 51m 37.63s , +25d 43m 19.6s) | C | 60 | 19.4 | 6955 | 2026-02-09 04:41:21 | MASTER- | (04h 50m 16.91s , +26d 16m 11.6s) | C | 60 | 19.3 | 7026 | 2026-02-09 04:42:32 | MASTER- | (04h 30m 24.49s , +27d 38m 55.9s) | C | 60 | 19.6 | 7026 | 2026-02-09 04:42:32 | MASTER- | (04h 29m 02.92s , +28d 11m 48.3s) | C | 60 | 19.3 | 7095 | 2026-02-09 04:43:42 | MASTER- | (04h 37m 57.88s , +28d 10m 53.0s) | C | 60 | 19.0 | 7095 | 2026-02-09 04:43:42 | MASTER- | (04h 39m 19.70s , +27d 38m 00.6s) | C | 60 | 19.3 | 7165 | 2026-02-09 04:44:52 | MASTER- | (04h 54m 59.66s , +23d 51m 10.3s) | C | 60 | 19.4 | 7165 | 2026-02-09 04:44:52 | MASTER- | (04h 53m 40.42s , +24d 24m 02.5s) | C | 60 | 19.3 | 7236 | 2026-02-09 04:46:02 | MASTER- | (05h 03m 50.98s , +23d 50m 14.2s) | C | 60 | 19.0 | 7236 | 2026-02-09 04:46:02 | MASTER- | (05h 02m 31.48s , +24d 23m 06.3s) | C | 60 | 19.0 | 7305 | 2026-02-09 04:47:12 | MASTER- | (04h 59m 35.06s , +25d 43m 12.4s) | C | 60 | 19.1 | 7305 | 2026-02-09 04:47:12 | MASTER- | (04h 58m 14.23s , +26d 16m 04.1s) | C | 60 | 19.4 | 7374 | 2026-02-09 04:48:21 | MASTER- | (05h 08m 33.53s , +25d 43m 24.8s) | C | 60 | 19.0 | 7374 | 2026-02-09 04:48:21 | MASTER- | (05h 07m 12.47s , +26d 16m 16.5s) | C | 60 | 19.1 | 7447 | 2026-02-09 04:49:34 | MASTER- | (04h 22m 57.08s , +31d 26m 58.6s) | C | 60 | 19.4 | 7447 | 2026-02-09 04:49:34 | MASTER- | (04h 21m 32.55s , +31d 59m 51.5s) | C | 60 | 19.2 | 7516 | 2026-02-09 04:50:43 | MASTER- | (04h 32m 19.62s , +31d 25m 36.7s) | C | 60 | 19.3 | 7516 | 2026-02-09 04:50:43 | MASTER- | (04h 30m 54.84s , +31d 58m 29.5s) | C | 60 | 19.2 | 7588 | 2026-02-09 04:51:54 | MASTER- | (04h 42m 47.81s , +25d 45m 21.3s) | C | 60 | 19.5 | 7588 | 2026-02-09 04:51:54 | MASTER- | (04h 41m 27.84s , +26d 18m 14.2s) | C | 60 | 19.5 | 7658 | 2026-02-09 04:53:04 | MASTER- | (04h 51m 34.36s , +25d 44m 23.9s) | C | 60 | 19.4 | 7658 | 2026-02-09 04:53:04 | MASTER- | (04h 50m 14.18s , +26d 17m 16.6s) | C | 60 | 19.3 | 7728 | 2026-02-09 04:54:15 | MASTER- | (04h 30m 19.17s , +27d 39m 23.1s) | C | 60 | 19.5 | 7728 | 2026-02-09 04:54:15 | MASTER- | (04h 28m 58.21s , +28d 12m 16.4s) | C | 60 | 19.4 | 7798 | 2026-02-09 04:55:24 | MASTER- | (04h 39m 27.61s , +27d 38m 24.6s) | C | 60 | 19.2 | 7798 | 2026-02-09 04:55:24 | MASTER- | (04h 38m 06.40s , +28d 11m 17.9s) | C | 60 | 19.1 | 7868 | 2026-02-09 04:56:35 | MASTER- | (04h 54m 59.82s , +23d 49m 33.6s) | C | 60 | 19.3 | 7868 | 2026-02-09 04:56:35 | MASTER- | (04h 53m 41.14s , +24d 22m 26.5s) | C | 60 | 19.4 | 7937 | 2026-02-09 04:57:44 | MASTER- | (05h 03m 51.05s , +23d 50m 03.0s) | C | 60 | 18.8 | 7937 | 2026-02-09 04:57:44 | MASTER- | (05h 02m 32.12s , +24d 22m 55.9s) | C | 60 | 18.9 | 8007 | 2026-02-09 04:58:54 | MASTER- | (04h 59m 37.90s , +25d 45m 11.3s) | C | 60 | 19.0 | 8007 | 2026-02-09 04:58:54 | MASTER- | (04h 58m 17.59s , +26d 18m 03.8s) | C | 60 | 19.3 | 8076 | 2026-02-09 05:00:03 | MASTER- | (05h 08m 30.98s , +25d 43m 51.9s) | C | 60 | 18.8 | 8076 | 2026-02-09 05:00:03 | MASTER- | (05h 07m 10.42s , +26d 16m 44.4s) | C | 60 | 18.8 | 8154 | 2026-02-09 05:01:21 | MASTER- | (04h 22m 59.94s , +31d 27m 18.1s) | C | 60 | 19.3 | 8154 | 2026-02-09 05:01:21 | MASTER- | (04h 21m 36.10s , +32d 00m 12.0s) | C | 60 | 19.0 | 8225 | 2026-02-09 05:02:31 | MASTER- | (04h 32m 17.73s , +31d 26m 38.4s) | C | 60 | 19.0 | 8225 | 2026-02-09 05:02:31 | MASTER- | (04h 30m 53.60s , +31d 59m 32.3s) | C | 60 | 19.0 | 8295 | 2026-02-09 05:03:42 | MASTER- | (04h 42m 42.46s , +25d 45m 46.9s) | C | 60 | 19.5 | 8295 | 2026-02-09 05:03:42 | MASTER- | (04h 41m 23.13s , +26d 18m 40.6s) | C | 60 | 19.5 | 8365 | 2026-02-09 05:04:52 | MASTER- | (04h 51m 40.89s , +25d 44m 48.2s) | C | 60 | 19.5 | 8365 | 2026-02-09 05:04:52 | MASTER- | (04h 50m 21.33s , +26d 17m 41.8s) | C | 60 | 19.5 | 8437 | 2026-02-09 05:06:03 | MASTER- | (04h 30m 20.11s , +27d 37m 49.8s) | C | 60 | 19.5 | 8437 | 2026-02-09 05:06:03 | MASTER- | (04h 28m 59.87s , +28d 10m 43.9s) | C | 60 | 19.2 | 8506 | 2026-02-09 05:07:13 | MASTER- | (04h 39m 27.58s , +27d 38m 16.5s) | C | 60 | 19.4 | 8506 | 2026-02-09 05:07:13 | MASTER- | (04h 38m 07.06s , +28d 11m 10.5s) | C | 60 | 19.3 | 8577 | 2026-02-09 05:08:24 | MASTER- | (04h 53m 45.57s , +24d 24m 50.9s) | C | 60 | 19.5 | 8577 | 2026-02-09 05:08:24 | MASTER- | (04h 55m 03.61s , +23d 51m 57.3s) | C | 60 | 19.4 | 8646 | 2026-02-09 05:09:33 | MASTER- | (05h 03m 48.43s , +23d 50m 11.9s) | C | 60 | 18.5 | 8646 | 2026-02-09 05:09:33 | MASTER- | (05h 02m 30.07s , +24d 23m 05.3s) | C | 60 | 18.6 | 8717 | 2026-02-09 05:10:44 | MASTER- | (05h 11m 38.42s , +23d 51m 05.1s) | C | 60 | 18.7 | 8717 | 2026-02-09 05:10:44 | MASTER- | (05h 10m 19.78s , +24d 23m 58.3s) | C | 60 | 18.8 | 8787 | 2026-02-09 05:11:54 | MASTER- | (05h 20m 22.79s , +23d 52m 08.6s) | C | 60 | 18.6 | 8787 | 2026-02-09 05:11:54 | MASTER- | (05h 19m 03.83s , +24d 25m 01.8s) | C | 60 | 18.7 | 8860 | 2026-02-09 05:13:07 | MASTER- | (04h 16m 05.42s , +35d 14m 02.4s) | C | 60 | 19.2 | 8860 | 2026-02-09 05:13:07 | MASTER- | (04h 14m 38.63s , +35d 46m 57.2s) | C | 60 | 19.1 | 8930 | 2026-02-09 05:14:16 | MASTER- | (04h 25m 58.74s , +35d 14m 12.9s) | C | 60 | 19.0 | 8930 | 2026-02-09 05:14:16 | MASTER- | (04h 24m 31.60s , +35d 47m 07.6s) | C | 60 | 18.9 | 9001 | 2026-02-09 05:15:27 | MASTER- | (04h 17m 52.04s , +29d 32m 22.8s) | C | 60 | 19.4 | 9001 | 2026-02-09 05:15:27 | MASTER- | (04h 16m 31.51s , +30d 05m 18.3s) | C | 60 | 19.2 | 9070 | 2026-02-09 05:16:37 | MASTER- | (04h 27m 06.08s , +29d 33m 59.7s) | C | 60 | 19.4 | 9070 | 2026-02-09 05:16:37 | MASTER- | (04h 25m 45.18s , +30d 06m 54.8s) | C | 60 | 19.1 | 9141 | 2026-02-09 05:17:48 | MASTER- | (04h 22m 24.63s , +37d 10m 11.3s) | C | 60 | 19.2 | 9141 | 2026-02-09 05:17:48 | MASTER- | (04h 20m 55.57s , +37d 43m 06.3s) | C | 60 | 19.3 | 9211 | 2026-02-09 05:18:58 | MASTER- | (04h 32m 32.35s , +37d 09m 11.5s) | C | 60 | 19.3 | 9211 | 2026-02-09 05:18:58 | MASTER- | (04h 31m 02.86s , +37d 42m 06.6s) | C | 60 | 19.1 | 9283 | 2026-02-09 05:20:10 | MASTER- | (04h 38m 30.20s , +23d 50m 39.1s) | C | 60 | 19.5 | 9283 | 2026-02-09 05:20:10 | MASTER- | (04h 37m 13.70s , +24d 23m 34.9s) | C | 60 | 19.4 | 9353 | 2026-02-09 05:21:20 | MASTER- | (04h 45m 54.66s , +24d 24m 54.0s) | C | 60 | 19.3 | 9353 | 2026-02-09 05:21:20 | MASTER- | (04h 47m 11.51s , +23d 51m 58.9s) | C | 60 | 19.4 | 9423 | 2026-02-09 05:22:30 | MASTER- | (05h 11m 41.13s , +23d 50m 30.7s) | C | 60 | 18.8 | 9423 | 2026-02-09 05:22:30 | MASTER- | (05h 10m 23.19s , +24d 23m 24.9s) | C | 60 | 18.7 | 9493 | 2026-02-09 05:23:39 | MASTER- | (05h 20m 28.56s , +23d 52m 18.1s) | C | 60 | 18.8 | 9493 | 2026-02-09 05:23:39 | MASTER- | (05h 19m 10.28s , +24d 25m 11.9s) | C | 60 | 19.0 | 9565 | 2026-02-09 05:24:52 | MASTER- | (04h 16m 06.15s , +35d 15m 30.8s) | C | 60 | 19.2 | 9565 | 2026-02-09 05:24:52 | MASTER- | (04h 14m 40.13s , +35d 48m 26.5s) | C | 60 | 19.0 | 9635 | 2026-02-09 05:26:02 | MASTER- | (04h 24m 26.97s , +35d 49m 26.6s) | C | 60 | 19.0 | 9635 | 2026-02-09 05:26:02 | MASTER- | (04h 25m 53.39s , +35d 16m 31.1s) | C | 60 | 19.3 | 9705 | 2026-02-09 05:27:12 | MASTER- | (04h 17m 54.78s , +29d 33m 42.8s) | C | 60 | 19.4 | 9705 | 2026-02-09 05:27:12 | MASTER- | (04h 16m 34.95s , +30d 06m 39.3s) | C | 60 | 19.0 | 9775 | 2026-02-09 05:28:22 | MASTER- | (04h 27m 00.43s , +29d 32m 42.4s) | C | 60 | 19.4 | 9775 | 2026-02-09 05:28:22 | MASTER- | (04h 25m 40.23s , +30d 05m 38.7s) | C | 60 | 19.0 | 9846 | 2026-02-09 05:29:33 | MASTER- | (04h 22m 31.37s , +37d 08m 55.6s) | C | 60 | 19.4 | 9846 | 2026-02-09 05:29:33 | MASTER- | (04h 21m 03.06s , +37d 41m 51.2s) | C | 60 | 19.5 | 9915 | 2026-02-09 05:30:42 | MASTER- | (04h 32m 30.03s , +37d 10m 38.4s) | C | 60 | 19.2 | 9915 | 2026-02-09 05:30:42 | MASTER- | (04h 31m 01.22s , +37d 43m 33.9s) | C | 60 | 19.0 | 9988 | 2026-02-09 05:31:54 | MASTER- | (04h 38m 27.32s , +23d 51m 02.9s) | C | 60 | 19.6 | 9988 | 2026-02-09 05:31:54 | MASTER- | (04h 37m 11.48s , +24d 23m 59.0s) | C | 60 | 19.5 | 10057 | 2026-02-09 05:33:04 | MASTER- | (04h 47m 14.95s , +23d 52m 45.6s) | C | 60 | 19.6 | 10057 | 2026-02-09 05:33:04 | MASTER- | (04h 45m 58.77s , +24d 25m 41.1s) | C | 60 | 19.6 | 10128 | 2026-02-09 05:34:15 | MASTER- | (05h 11m 38.61s , +23d 51m 55.0s) | C | 60 | 18.9 | 10128 | 2026-02-09 05:34:15 | MASTER- | (05h 10m 21.36s , +24d 24m 49.8s) | C | 60 | 19.0 | 10197 | 2026-02-09 05:35:24 | MASTER- | (05h 20m 23.63s , +23d 52m 57.6s) | C | 60 | 18.7 | 10197 | 2026-02-09 05:35:24 | MASTER- | (05h 19m 05.97s , +24d 25m 52.2s) | C | 60 | 19.0 | 10270 | 2026-02-09 05:36:37 | MASTER- | (04h 16m 12.36s , +35d 16m 00.3s) | C | 60 | 19.3 | 10270 | 2026-02-09 05:36:37 | MASTER- | (04h 14m 47.14s , +35d 48m 56.4s) | C | 60 | 19.1 | 10339 | 2026-02-09 05:37:46 | MASTER- | (04h 25m 55.12s , +35d 14m 59.8s) | C | 60 | 19.2 | 10339 | 2026-02-09 05:37:46 | MASTER- | (04h 24m 29.55s , +35d 47m 56.0s) | C | 60 | 19.0 | 10410 | 2026-02-09 05:38:57 | MASTER- | (04h 16m 36.85s , +30d 06m 37.3s) | C | 60 | 19.1 | 10410 | 2026-02-09 05:38:57 | MASTER- | (04h 17m 55.86s , +29d 33m 40.3s) | C | 60 | 19.4 | 10480 | 2026-02-09 05:40:07 | MASTER- | (04h 27m 04.72s , +29d 34m 58.3s) | C | 60 | 19.4 | 10480 | 2026-02-09 05:40:07 | MASTER- | (04h 25m 45.32s , +30d 07m 55.0s) | C | 60 | 19.3 | 10551 | 2026-02-09 05:41:17 | MASTER- | (04h 21m 01.21s , +37d 42m 25.8s) | C | 60 | 19.3 | 10551 | 2026-02-09 05:41:17 | MASTER- | (04h 22m 28.59s , +37d 09m 29.5s) | C | 60 | 19.2 | 10620 | 2026-02-09 05:42:27 | MASTER- | (04h 31m 05.00s , +37d 43m 47.4s) | C | 60 | 19.1 | 10620 | 2026-02-09 05:42:27 | MASTER- | (04h 32m 32.92s , +37d 10m 51.1s) | C | 60 | 19.1 | 10692 | 2026-02-09 05:43:39 | MASTER- | (04h 38m 25.58s , +23d 52m 22.3s) | C | 60 | 19.6 | 10692 | 2026-02-09 05:43:39 | MASTER- | (04h 37m 10.54s , +24d 25m 19.2s) | C | 60 | 21.0 | 10762 | 2026-02-09 05:44:49 | MASTER- | (04h 47m 08.65s , +23d 53m 23.0s) | C | 60 | 19.6 | 10762 | 2026-02-09 05:44:49 | MASTER- | (04h 45m 53.26s , +24d 26m 19.1s) | C | 60 | 19.5 | 10834 | 2026-02-09 05:46:00 | MASTER- | (05h 11m 45.31s , +23d 52m 21.2s) | C | 60 | 19.0 | 10834 | 2026-02-09 05:46:00 | MASTER- | (05h 10m 28.78s , +24d 25m 16.5s) | C | 60 | 19.1 | 10903 | 2026-02-09 05:47:10 | MASTER- | (05h 20m 23.31s , +23d 51m 23.6s) | C | 60 | 18.8 | 10903 | 2026-02-09 05:47:10 | MASTER- | (05h 19m 06.38s , +24d 24m 18.8s) | C | 60 | 18.9 | 10976 | 2026-02-09 05:48:22 | MASTER- | (04h 14m 48.38s , +35d 48m 50.6s) | C | 60 | 19.0 | 10976 | 2026-02-09 05:48:22 | MASTER- | (04h 16m 12.74s , +35d 15m 53.6s) | C | 60 | 19.2 | 11045 | 2026-02-09 05:49:32 | MASTER- | (04h 25m 57.95s , +35d 17m 11.4s) | C | 60 | 19.4 | 11045 | 2026-02-09 05:49:32 | MASTER- | (04h 24m 33.18s , +35d 50m 08.2s) | C | 60 | 19.2 | 11116 | 2026-02-09 05:50:43 | MASTER- | (04h 17m 53.62s , +29d 33m 45.1s) | C | 60 | 19.5 | 11116 | 2026-02-09 05:50:43 | MASTER- | (04h 16m 35.44s , +30d 06m 43.2s) | C | 60 | 19.0 | 11185 | 2026-02-09 05:51:52 | MASTER- | (04h 27m 07.50s , +29d 35m 21.1s) | C | 60 | 19.4 | 11185 | 2026-02-09 05:51:52 | MASTER- | (04h 25m 48.90s , +30d 08m 18.6s) | C | 60 | 19.3 | 11257 | 2026-02-09 05:53:03 | MASTER- | (04h 22m 26.02s , +37d 10m 37.6s) | C | 60 | 19.5 | 11257 | 2026-02-09 05:53:03 | MASTER- | (04h 20m 59.49s , +37d 43m 34.6s) | C | 60 | 19.5 | 11326 | 2026-02-09 05:54:13 | MASTER- | (04h 32m 28.78s , +37d 11m 36.6s) | C | 60 | 19.5 | 11326 | 2026-02-09 05:54:13 | MASTER- | (04h 31m 01.73s , +37d 44m 33.3s) | C | 60 | 19.3 | 11399 | 2026-02-09 05:55:25 | MASTER- | (04h 38m 30.85s , +23d 52m 51.2s) | C | 60 | 19.8 | 11399 | 2026-02-09 05:55:25 | MASTER- | (04h 37m 16.54s , +24d 25m 48.7s) | C | 60 | 19.5 | 11468 | 2026-02-09 05:56:35 | MASTER- | (04h 47m 09.05s , +23d 51m 50.9s) | C | 60 | 19.7 | 11468 | 2026-02-09 05:56:35 | MASTER- | (04h 45m 54.41s , +24d 24m 47.6s) | C | 60 | 19.5 | 11538 | 2026-02-09 05:57:45 | MASTER- | (05h 11m 45.28s , +23d 52m 17.5s) | C | 60 | 19.0 | 11538 | 2026-02-09 05:57:45 | MASTER- | (05h 10m 29.47s , +24d 25m 13.5s) | C | 60 | 18.9 | 11608 | 2026-02-09 05:58:55 | MASTER- | (05h 20m 27.26s , +23d 53m 35.0s) | C | 60 | 18.7 | 11608 | 2026-02-09 05:58:55 | MASTER- | (05h 19m 10.97s , +24d 26m 30.6s) | C | 60 | 18.8 | 11679 | 2026-02-09 06:00:06 | MASTER- | (04h 16m 10.81s , +35d 16m 18.5s) | C | 60 | 19.5 | 11679 | 2026-02-09 06:00:06 | MASTER- | (04h 14m 47.35s , +35d 49m 16.1s) | C | 60 | 19.1 | 11754 | 2026-02-09 06:01:21 | MASTER- | (04h 24m 38.46s , +35d 50m 38.0s) | C | 60 | 19.1 | 11754 | 2026-02-09 06:01:21 | MASTER- | (04h 26m 02.36s , +35d 17m 40.7s) | C | 60 | 19.6 | 11825 | 2026-02-09 06:02:32 | MASTER- | (04h 16m 34.71s , +30d 08m 10.1s) | C | 60 | 19.0 | 11825 | 2026-02-09 06:02:32 | MASTER- | (04h 17m 52.07s , +29d 35m 11.7s) | C | 60 | 19.6 | 11896 | 2026-02-09 06:03:42 | MASTER- | (04h 27m 02.53s , +29d 36m 10.1s) | C | 60 | 19.5 | 11896 | 2026-02-09 06:03:42 | MASTER- | (04h 25m 44.75s , +30d 09m 08.1s) | C | 60 | 19.0 | 11967 | 2026-02-09 06:04:53 | MASTER- | (04h 21m 07.44s , +37d 44m 05.4s) | C | 60 | 19.5 | 11967 | 2026-02-09 06:04:53 | MASTER- | (04h 22m 33.10s , +37d 11m 07.9s) | C | 60 | 19.6 | 12037 | 2026-02-09 06:06:03 | MASTER- | (04h 32m 29.77s , +37d 10m 06.2s) | C | 60 | 19.5 | 12037 | 2026-02-09 06:06:03 | MASTER- | (04h 31m 03.63s , +37d 43m 03.8s) | C | 60 | 19.0 | 12108 | 2026-02-09 06:07:15 | MASTER- | (04h 38m 31.77s , +23d 52m 35.3s) | C | 60 | 19.9 | 12108 | 2026-02-09 06:07:15 | MASTER- | (04h 37m 18.26s , +24d 25m 33.4s) | C | 60 | 21.0 | 12177 | 2026-02-09 06:08:24 | MASTER- | (04h 47m 13.39s , +23d 54m 03.9s) | C | 60 | 19.8 | 12177 | 2026-02-09 06:08:24 | MASTER- | (04h 45m 59.53s , +24d 27m 01.1s) | C | 60 | 19.5 | 12249 | 2026-02-09 06:09:35 | MASTER- | (05h 11m 42.83s , +23d 52m 33.5s) | C | 60 | 19.1 | 12249 | 2026-02-09 06:09:35 | MASTER- | (05h 10m 27.80s , +24d 25m 30.3s) | C | 60 | 18.9 | 12318 | 2026-02-09 06:10:45 | MASTER- | (05h 20m 31.37s , +23d 54m 17.1s) | C | 60 | 19.0 | 12318 | 2026-02-09 06:10:45 | MASTER- | (05h 19m 15.90s , +24d 27m 13.3s) | C | 60 | 19.0 | 12391 | 2026-02-09 06:11:58 | MASTER- | (04h 14m 45.02s , +35d 50m 28.8s) | C | 60 | 19.1 | 12391 | 2026-02-09 06:11:58 | MASTER- | (04h 16m 07.53s , +35d 17m 30.8s) | C | 60 | 18.7 | 12460 | 2026-02-09 06:13:07 | MASTER- | (04h 24m 32.28s , +35d 51m 27.3s) | C | 60 | 19.2 | 12460 | 2026-02-09 06:13:07 | MASTER- | (04h 25m 55.23s , +35d 18m 29.5s) | C | 60 | 19.7 | 12531 | 2026-02-09 06:14:17 | MASTER- | (04h 17m 57.82s , +29d 35m 42.9s) | C | 60 | 18.1 | 12531 | 2026-02-09 06:14:17 | MASTER- | (04h 16m 41.40s , +30d 08m 41.5s) | C | 60 | 19.3 | 12600 | 2026-02-09 06:15:27 | MASTER- | (04h 27m 04.16s , +29d 34m 40.6s) | C | 60 | 19.6 | 12601 | 2026-02-09 06:15:27 | MASTER- | (04h 25m 47.36s , +30d 07m 39.1s) | C | 60 | 19.3 | 12672 | 2026-02-09 06:16:39 | MASTER- | (04h 22m 34.25s , +37d 10m 59.1s) | C | 60 | 19.8 | 12672 | 2026-02-09 06:16:39 | MASTER- | (04h 21m 09.65s , +37d 43m 57.1s) | C | 60 | 19.6 | 12742 | 2026-02-09 06:17:48 | MASTER- | (04h 31m 07.48s , +37d 45m 10.3s) | C | 60 | 19.0 | 12742 | 2026-02-09 06:17:48 | MASTER- | (04h 32m 32.64s , +37d 12m 12.4s) | C | 60 | 19.5 | 12814 | 2026-02-09 06:19:00 | MASTER- | (04h 38m 29.08s , +23d 53m 04.7s) | C | 60 | 19.8 | 12814 | 2026-02-09 06:19:00 | MASTER- | (04h 37m 16.44s , +24d 26m 03.4s) | C | 60 | 21.0 | 12884 | 2026-02-09 06:20:10 | MASTER- | (04h 47m 17.03s , +23d 54m 41.3s) | C | 60 | 19.9 | 12884 | 2026-02-09 06:20:10 | MASTER- | (04h 46m 04.02s , +24d 27m 39.0s) | C | 60 | 19.6 | 13348 | 2026-02-09 06:27:55 | MASTER- | (04h 49m 44.25s , +22d 32m 01.4s) | C | 60 | 19.5 | 13417 | 2026-02-09 06:29:04 | MASTER- | (04h 59m 38.58s , +21d 59m 27.1s) | C | 60 | 19.9 | 13417 | 2026-02-09 06:29:04 | MASTER- | (04h 58m 27.05s , +22d 32m 29.7s) | C | 60 | 19.2 | 13487 | 2026-02-09 06:30:14 | MASTER- | (05h 07m 22.07s , +21d 59m 19.1s) | C | 60 | 19.6 | 13487 | 2026-02-09 06:30:14 | MASTER- | (05h 06m 10.20s , +22d 32m 21.4s) | C | 60 | 19.1 | 13556 | 2026-02-09 06:31:23 | MASTER- | (05h 14m 50.27s , +22d 33m 47.7s) | C | 60 | 19.0 | 13630 | 2026-02-09 06:32:37 | MASTER- | (05h 46m 12.26s , +39d 39m 43.8s) | C | 60 | 18.5 | 13630 | 2026-02-09 06:32:37 | MASTER- | (05h 47m 42.69s , +39d 06m 43.4s) | C | 60 | 18.6 | 14304 | 2026-02-09 06:43:51 | MASTER- | (04h 49m 47.24s , +22d 33m 41.3s) | C | 60 | 19.5 | 14373 | 2026-02-09 06:45:00 | MASTER- | (04h 59m 33.49s , +22d 01m 40.7s) | C | 60 | 19.9 | 14373 | 2026-02-09 06:45:00 | MASTER- | (04h 58m 23.03s , +22d 34m 41.5s) | C | 60 | 19.4 | 14443 | 2026-02-09 06:46:10 | MASTER- | (05h 06m 14.80s , +22d 33m 41.7s) | C | 60 | 19.0 | 14443 | 2026-02-09 06:46:10 | MASTER- | (05h 07m 25.56s , +22d 00m 41.1s) | C | 60 | 19.6 | 14514 | 2026-02-09 06:47:21 | MASTER- | (05h 14m 45.45s , +22d 32m 42.0s) | C | 60 | 19.0 | 14586 | 2026-02-09 06:48:33 | MASTER- | (05h 46m 21.53s , +39d 38m 38.5s) | C | 60 | 18.9 | 14586 | 2026-02-09 06:48:33 | MASTER- | (05h 47m 50.93s , +39d 05m 40.0s) | C | 60 | 19.0 | 15016 | 2026-02-09 06:55:43 | MASTER- | (04h 49m 47.78s , +22d 33m 18.1s) | C | 60 | 19.5 | 15085 | 2026-02-09 06:56:52 | MASTER- | (04h 59m 40.84s , +22d 00m 31.8s) | C | 60 | 18.1 | 15085 | 2026-02-09 06:56:52 | MASTER- | (04h 58m 30.99s , +22d 33m 27.0s) | C | 60 | 19.3 | 15155 | 2026-02-09 06:58:02 | MASTER- | (05h 07m 23.05s , +22d 01m 54.8s) | C | 60 | 17.8 | 15155 | 2026-02-09 06:58:02 | MASTER- | (05h 06m 12.88s , +22d 34m 49.3s) | C | 60 | 19.1 | 15225 | 2026-02-09 06:59:12 | MASTER- | (05h 14m 50.03s , +22d 33m 27.9s) | C | 60 | 19.0 | 15299 | 2026-02-09 07:00:25 | MASTER- | (05h 47m 52.29s , +39d 07m 46.9s) | C | 60 | 18.9 | 15299 | 2026-02-09 07:00:25 | MASTER- | (05h 46m 23.21s , +39d 40m 39.6s) | C | 60 | 18.9 | 15732 | 2026-02-09 07:07:39 | MASTER- | (04h 49m 51.39s , +22d 35m 29.2s) | C | 60 | 19.6 | 15802 | 2026-02-09 07:08:49 | MASTER- | (04h 59m 37.52s , +22d 00m 54.0s) | C | 60 | 18.1 | 15802 | 2026-02-09 07:08:49 | MASTER- | (04h 58m 28.62s , +22d 33m 48.0s) | C | 60 | 19.5 | 15873 | 2026-02-09 07:09:59 | MASTER- | (05h 07m 26.66s , +22d 02m 51.4s) | C | 60 | 17.9 | 15873 | 2026-02-09 07:09:59 | MASTER- | (05h 06m 17.41s , +22d 35m 44.8s) | C | 60 | 19.3 | 15942 | 2026-02-09 07:11:09 | MASTER- | (05h 14m 48.42s , +22d 34m 43.5s) | C | 60 | 19.2 | 16014 | 2026-02-09 07:12:21 | MASTER- | (05h 47m 46.87s , +39d 08m 25.1s) | C | 60 | 19.1 | 16014 | 2026-02-09 07:12:21 | MASTER- | (05h 46m 18.73s , +39d 41m 16.7s) | C | 60 | 19.0 | 16442 | 2026-02-09 07:19:29 | MASTER- | (04h 51m 02.76s , +22d 03m 28.4s) | C | 60 | 18.3 | 16442 | 2026-02-09 07:19:29 | MASTER- | (04h 49m 55.05s , +22d 36m 22.5s) | C | 60 | 19.6 | 16511 | 2026-02-09 07:20:38 | MASTER- | (04h 59m 34.18s , +22d 02m 25.9s) | C | 60 | 18.1 | 16511 | 2026-02-09 07:20:38 | MASTER- | (04h 58m 26.13s , +22d 35m 19.5s) | C | 60 | 19.4 | 16580 | 2026-02-09 07:21:47 | MASTER- | (05h 07m 19.73s , +22d 03m 24.0s) | C | 60 | 17.8 | 16580 | 2026-02-09 07:21:47 | MASTER- | (05h 06m 11.33s , +22d 36m 17.1s) | C | 60 | 19.3 | 16650 | 2026-02-09 07:22:57 | MASTER- | (05h 14m 56.36s , +22d 35m 14.8s) | C | 60 | 19.2 | 16722 | 2026-02-09 07:24:09 | MASTER- | (05h 47m 47.60s , +39d 06m 54.7s) | C | 60 | 19.3 | 16722 | 2026-02-09 07:24:09 | MASTER- | (05h 46m 20.34s , +39d 39m 45.9s) | C | 60 | 19.1 | 17151 | 2026-02-09 07:31:18 | MASTER- | (04h 50m 56.83s , +22d 04m 02.3s) | C | 60 | 18.5 | 17151 | 2026-02-09 07:31:18 | MASTER- | (04h 49m 50.07s , +22d 36m 56.0s) | C | 60 | 19.6 | 17220 | 2026-02-09 07:32:27 | MASTER- | (04h 59m 40.55s , +22d 02m 58.7s) | C | 60 | 18.0 | 17220 | 2026-02-09 07:32:27 | MASTER- | (04h 58m 33.46s , +22d 35m 51.9s) | C | 60 | 19.5 | 17290 | 2026-02-09 07:33:37 | MASTER- | (05h 07m 19.93s , +22d 01m 56.4s) | C | 60 | 17.8 | 17290 | 2026-02-09 07:33:37 | MASTER- | (05h 06m 12.52s , +22d 34m 49.1s) | C | 60 | 19.2 | 17360 | 2026-02-09 07:34:46 | MASTER- | (05h 14m 56.57s , +22d 34m 51.5s) | C | 60 | 19.2 | 17432 | 2026-02-09 07:35:59 | MASTER- | (05h 47m 50.53s , +39d 09m 00.3s) | C | 60 | 19.6 | 17433 | 2026-02-09 07:35:59 | MASTER- | (05h 46m 24.25s , +39d 41m 50.9s) | C | 60 | 19.2 | 49577 | 2026-02-09 16:31:43 | MASTER-Tunka | (05h 17m 48.83s , +30d 16m 05.7s) | C | 60 | 19.6 | 49637 | 2026-02-09 16:31:43 | MASTER-Tunka | (05h 17m 48.83s , +30d 16m 05.6s) | C | 180 | 20.1 | Coadd 49577 | 2026-02-09 16:31:43 | MASTER-Tunka | (05h 17m 13.75s , +30d 23m 29.6s) | C | 60 | 19.6 | 49649 | 2026-02-09 16:32:56 | MASTER-Tunka | (05h 17m 55.54s , +30d 15m 03.9s) | C | 60 | 19.6 | 49649 | 2026-02-09 16:32:56 | MASTER-Tunka | (05h 17m 20.49s , +30d 22m 26.9s) | C | 60 | 19.6 | 49725 | 2026-02-09 16:34:11 | MASTER-Tunka | (05h 17m 49.09s , +30d 14m 01.6s) | C | 60 | 19.6 | 49725 | 2026-02-09 16:34:11 | MASTER-Tunka | (05h 17m 14.05s , +30d 21m 23.7s) | C | 60 | 19.6 | 49830 | 2026-02-09 16:35:27 | MASTER-Tunka | (05h 17m 56.86s , +30d 14m 23.1s) | C | 120 | 19.7 | 49950 | 2026-02-09 16:35:27 | MASTER-Tunka | (05h 17m 56.86s , +30d 14m 23.1s) | C | 360 | 20.1 | Coadd 49830 | 2026-02-09 16:35:27 | MASTER-Tunka | (05h 17m 21.83s , +30d 21m 44.4s) | C | 120 | 19.7 | 49972 | 2026-02-09 16:37:49 | MASTER-Tunka | (05h 17m 53.08s , +30d 15m 49.3s) | C | 120 | 19.7 | 49972 | 2026-02-09 16:37:49 | MASTER-Tunka | (05h 17m 18.03s , +30d 23m 09.3s) | C | 120 | 19.6 | 50106 | 2026-02-09 16:40:03 | MASTER-Tunka | (05h 17m 53.30s , +30d 14m 15.9s) | C | 120 | 19.7 | 50106 | 2026-02-09 16:40:03 | MASTER-Tunka | (05h 17m 18.29s , +30d 21m 35.0s) | C | 120 | 19.8 | 50243 | 2026-02-09 16:42:19 | MASTER-Tunka | (05h 17m 53.18s , +33d 15m 35.2s) | C | 120 | 19.6 | 50363 | 2026-02-09 16:42:19 | MASTER-Tunka | (05h 17m 53.18s , +33d 15m 35.2s) | C | 360 | 20.0 | Coadd 50243 | 2026-02-09 16:42:19 | MASTER-Tunka | (05h 17m 16.14s , +33d 23m 02.4s) | C | 120 | 19.7 | 50375 | 2026-02-09 16:44:32 | MASTER-Tunka | (05h 17m 46.62s , +33d 14m 47.1s) | C | 120 | 19.7 | 50375 | 2026-02-09 16:44:32 | MASTER-Tunka | (05h 17m 09.60s , +33d 22m 13.5s) | C | 120 | 19.7 | 50509 | 2026-02-09 16:46:45 | MASTER-Tunka | (05h 17m 47.84s , +33d 15m 44.4s) | C | 120 | 19.6 | 50509 | 2026-02-09 16:46:45 | MASTER-Tunka | (05h 17m 10.90s , +33d 23m 10.2s) | C | 120 | 19.6 | 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/43672. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41777] GRB 260208B: Swift-XRT observations
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43671 SUBJECT: GRB 260208B: Swift-XRT observations DATE: 26/02/09 16:03:40 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> A.P. Beardmore (U. Leicester), J.P. Osborne (U. Leicester), P. D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA), J.A. Kennea (PSU), D.N. Burrows (PSU), S. Lanava (PSU) and P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the Fermi/LAT-detected burst GRB 260208B, collecting 1.6 ks of Photon Counting (PC) mode data between T0+33.1 ks and T0+44.4 ks. One uncatalogued X-ray source has been detected within the estimated 3-sigma Fermi/LAT error region (354 arcsec), it is below the RASS limit and shows no definitive signs of fading. Details of this source are given below: Source 1: RA (J2000.0): 99.6189 = 06h 38m 28.55s Dec (J2000.0): -13.7743 = -13d 46' 27.4" Error: 3.1 arcsec (radius, 90% conf. [Enhanced position]) Count-rate: 0.0338 +/- 0.0067 ct s^-1 Distance: 238 arcsec from Fermi/LAT position. Flux: (1.63 +/- 0.32)e-12 erg cm^-2 s^-1 (observed, 0.3-10 keV) The flux reported by EP-WXT for this source at 74.7 ks after the trigger (GCN Circ. 43663) is about a factor of 10 fainter than this XRT measurement, however, which suggests it is indeed the GRB afterglow. The results of the XRT-team automatic analysis of the XRT observations, including a position-specific upper limit calculator, are available at https://www.swift.ac.uk/ToO_GRBs/00021909. We note that the large number of spurious sources was due to unusually high background. This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/43671. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41776] GRB 260131A/B: continued Mondy optical observations
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43670 SUBJECT: GRB 260131A/B: continued Mondy optical observations DATE: 26/02/09 15:13:09 GMT FROM: Alina Volnova at IKI RAS <alinusss(a)gmail.com> A. Volnova (IKI), E. Klunko (ISTP), N. Pankov (IKI), A. Pozanenko (IKI) report on behalf of IKI-GRB-FuN: We continued observations of the field of GRB 260131A/B (Fermi GBM Team, GCN 43579; Sugai et al., GCN 43580; Roberts et al., GCN 43585; Frederiks et al., GCN 43590; Luo et al., GCN 43591; Jiang et al., GCN 43600; Li et al., GCN 43605) with the AZT-33IK 1.5m telescope of the Mondy observatory on Feb. 8 starting at 13:03:46 UT and taking several frames in R band. The optical counterpart reported by Gompertz et al., GCN 43586; Lee et al., GCN 43587; Saccardi et al., GCN 43595; García García et al., GCN 43599, Shi et al., GCN 43601; Sanchez-Ramirez et al., GCN 43604; Jayaraman et al., GCN 43606; Zhu et al., GCN 43607; Zheng et al., GCN 43609; Adami et al., GCN 43610; Volnova et al., GCN 43632 is detected in the stacked frame. Preliminary photometry and observational details are the following: Date UT start t-T0 Exp. Filter Obj. Err. UL Site/Telescope (mid,days) (n*s) (3sigma) 2026-02-08 13:03:46 8.30854 56*120 R 21.70 0.09 22.8 Mondy/AZT-33IK The photometry is based on several 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/43670. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41775] GRB 260204A: Swift/UVOT Upper Limits
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43669 SUBJECT: GRB 260204A: Swift/UVOT Upper Limits DATE: 26/02/09 13:22:25 GMT FROM: Alice Breeveld at MSSL-UCL <a.breeveld(a)ucl.ac.uk> A.A. Breeveld (UCL-MSSL) and S. Laha (GSFC/UMBC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of the SVOM/ECLAIRS-detected burst GRB 260204A (Pillas et al., GCN Circ. 43613) 2.3 ks after the trigger. The afterglow reported by Malesani et al. (in the r and z bands, GCN Circ. 43621) and Li et al. (GCN Circ. 43626) and consistent with XRT source 1 (Evans et al., GCN Circ. 43622) is not detected in the U-band exposures. Preliminary 3-sigma upper limit using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposure is: Filter T_start(s) T_stop(s) Exp(s) Mag u 23622 25281 1634 >20.8 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.023 in the direction of the burst (Schlegel et al. 1998). View this GCN Circular online at https://gcn.nasa.gov/circulars/43669. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41774] GRB 260208B: COLIBRÍ optical observations
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43668 SUBJECT: GRB 260208B: COLIBRÍ optical observations DATE: 26/02/09 13:16:57 GMT FROM: F. Magnani at Aix-Marseille Université, CPPM/CNRS <francesco.magnani.work(a)gmail.com> Francesco Magnani (CPPM), Leonardo García García (UNAM), Jean-Grégoire Ducoin (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), Damien Dornic (CPPM), Francis Fortin (IRAP), Ramandeep Gill (UNAM), Noémie Globus (UNAM), Asuka Kuwata (UNAM), Nikos Mandarakas (LAM), Diego López-Cámara (UNAM), Enrique Moreno Méndez (UNAM), 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 bright Fermi GRB 260208B (Fermi GBM Team, GCN Circ. 43638), also detected by SVOM/GRM (L. Xing-Hao, GCN Circ. 43650), using the DDRAGO two-channel wide-field imager on the COLIBRÍ telescope. We observed from 2026-02-09T05:10:25 to 2026-02-09T06:30:45 UTC (from 19.3 to 20.6 hours after the trigger) and obtained 30 minutes of simultaneous exposure in the r, z filters. The data were reduced and coadded with the COLIBRÍ pipeline 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 a source at the position of the SVOM/VT candidate (Li et al., GCN Circ. 43659), with the following preliminary magnitudes : r = 22.61 +/- 0.14 z = 21.99 +/- 0.25 Further analysis 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/43668. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41773] GRB 260208A: Mondy optical observations
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43667 SUBJECT: GRB 260208A: Mondy optical observations DATE: 26/02/09 12:00:08 GMT FROM: Alina Volnova at IKI RAS <alinusss(a)gmail.com> A. Volnova (IKI), E. Klunko (ISTP), N. Pankov (IKI), A. Pozanenko (IKI) report on behalf of IKI-GRB-FuN: We observed the field of GRB 260208A (Fermi GBM team, GCN 43635; Sonawane et al. 2026, GCN 43642; Longo et al. 2026, GCN 43645; Dichiara et al. 2026, GCN 43652; Luo et al. 2026, GCN 43658) at z = 2.36 (Dimple et al., GCN 43662) with the AZT-33IK 1.5m telescope of the Mondy observatory on Feb. 8 starting at 20:54:02 UT and taking several 120-seconds frames in the R band. The optical counterpart (Lipunov et al., GCN 43640; Wortley et al., GCN 43641; Dichiara et al., GCN 43652; Ma et al., GCN 43655; Ahumada et al., GCN 43657; Dimple et al.,GCN 43661; Magnani et al., GCN 43664; Gupta et al., GCN 43665) is detected in the single frame. Preliminary photometry and observational details are the following: Date UT start t-T0 Exp. Filter Obj. Err. UL Site/Telescope (mid,days) (n*s) (3sigma) 2026-02-08 20:54:02 0.66429 10*120 R 19.92 0.06 21.8 Mondy/AZT-33IK 2026-02-08 21:14:03 0.67819 10*120 R 20.14 0.07 21.8 Mondy/AZT-33IK 2026-02-08 21:34:04 0.69139 10*120 R 20.05 0.06 21.8 Mondy/AZT-33IK The photometry is based on nearby SDSS stars (R-magnitudes obtained using the 2005 Lupton transformation equations) and is not corrected for Galactic extinction. View this GCN Circular online at https://gcn.nasa.gov/circulars/43667. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41772] GRB 260208A: Mondy optical observations
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43666 SUBJECT: GRB 260208A: Mondy optical observations DATE: 26/02/09 11:57:27 GMT FROM: Alina Volnova at IKI RAS <alinusss(a)gmail.com> A. Volnova (IKI), E. Klunko (ISTP), N. Pankov (IKI), A. Pozanenko (IKI) report on behalf of IKI-GRB-FuN: We observed the field of GRB 260208A (Fermi GBM team, GCN 43635; Sonawane et al. 2026, GCN 43642; Longo et al. 2026, GCN 43645; Dichiara et al. 2026, GCN 43652; Luo et al. 2026, GCN 43658) at z = 2.36 (Dimple et al., GCN 43662) with the AZT-33IK 1.5m telescope of the Mondy observatory on Feb. 8 starting at 20:54:02 UT and taking several 120-seconds frames in the R band. The optical counterpart (Lipunov et al., GCN 43640; Wortley et al., GCN 43641; Dichiara et al., GCN 43652; Ma et al., GCN 43655; Ahumada et al., GCN 43657; Dimple et al.,GCN 43661; Magnani et al., GCN 43664; Gupta et al., GCN 43665) is detected in the single frame. Preliminary photometry and observational details are the following: Date UT start t-T0 Exp. Filter Obj. Err. UL Site/Telescope (mid,days) (n*s) (3sigma) 2026-02-08 20:54:02 0.66429 10*120 R 19.92 0.06 21.8 Mondy/AZT-33IK 2026-02-08 21:14:03 0.67819 10*120 R 20.14 0.07 21.8 Mondy/AZT-33IK 2026-02-08 21:34:04 0.69139 10*120 R 20.05 0.06 21.8 Mondy/AZT-33IK The photometry is based on nearby SDSS stars (R-magnitudes obtained using the 2005 Lupton transformation equations) and is not corrected for Galactic extinction. View this GCN Circular online at https://gcn.nasa.gov/circulars/43666. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41771] GRB 260208A: 1.3m DFOT optical detection
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43665 SUBJECT: GRB 260208A: 1.3m DFOT optical detection DATE: 26/02/09 11:24:07 GMT FROM: ANSHIKA GUPTA at ARIES <anshika05180(a)gmail.com> Anshika Gupta, Kuntal Misra, Dhruv Jain, Pankaj Pawar, and Debalina Kar (ARIES) report: We observed the field of GRB 260208A detected by (Fermi GBM team, GCN 43635; Sonawane et al. 2026, GCN 43642; Longo et al. 2026, GCN 43645; Dichiara et al. 2026, GCN 43652; Luo et al. 2026, GCN 43658) with the 1.3m Devasthal Fast Optical Telescope (DFOT), located at the Devasthal Observatory of the Aryabhatta Research Institute of Observational Sciences (ARIES), India. The observations were started on 2026-02-08 at 20:52:28 UT, i.e., ~ 15.75 hours after the Fermi/GBM trigger. We detect an optical afterglow in a single 300s R-band exposure at the position reported by (Podesta et al. 2026, GCN 43640). We obtain the following preliminary magnitude in the stacked image: Date Start_UT T_start-T0 (hour) Filter Exp time (s) Magnitude =============================================================== 2026-02-08 20:52:28 ~15.75 R 300s*1 19.89 +/-0.04 The optical detection of the burst is consistent with Lipunov et al. 2026 (GCN 43637); Podesta et al. 2026 (GCN 43640); Wortley et al. 2026 (GCN 43641); Ma et al. 2026 (GCN 43655); Ahumada et al. 2026 (GCN 43657); and Dimple et al. 2026 (GCN 43661, 43662). 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/43665. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41770] GRB 260208A: COLIBRÍ optical observations
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43664 SUBJECT: GRB 260208A: COLIBRÍ optical observations DATE: 26/02/09 11:14:54 GMT FROM: F. Magnani at Aix-Marseille Université, CPPM/CNRS <francesco.magnani.work(a)gmail.com> Francesco Magnani (CPPM), Leonardo García García (UNAM), Jean-Grégoire Ducoin (CPPM), Stéphane Basa (UAR Pytheas), William H. Lee (UNAM), 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), Francis Fortin (IRAP), Ramandeep Gill (UNAM), Noémie Globus (UNAM), Asuka Kuwata (UNAM), Nikos Mandarakas (LAM), Diego López-Cámara (UNAM), Enrique Moreno Méndez (UNAM), 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 Fermi GRB 260208A (43635, GCN Circ. 43642, Fermi LAT, GCN Circ. 43645, GECAM-B, GCN Circ. 43658) using the DDRAGO two-channel wide-field imager on the COLIBRÍ telescope. 2026-02-09T08:16:25.726 to 2026-02-09T09:37:56.715 UTC (from 27.15 to 28.51 hours after the trigger) and obtained 30 minutes of simultaneous exposure in the r, z filters. The data were reduced and coadded and analysed with the COLIBRÍ 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. We detected the optical counterpart Lipunov et al. (GCN Circ. 43640), Wortley et al. (GCN Circ. 43641), Dichiara et al. (GCN Circ. 43652), Ma et al. (GCN Circ. 43655), Ahumada et al. (GCN Circ. 43657), Dimple et al. (GCN Circ. 43661), with measured redshift z = 2.36 (Dimple et al. GCN Circ. 43662) at a preliminary magnitude of: r = 21.09 +/- 0.04 z = 20.64 +/- 0.06 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/43664. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41769] GRB 260208B: EP-FXT observation
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43663 SUBJECT: GRB 260208B: EP-FXT observation DATE: 26/02/09 11:06:20 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> S. Q. Jiang, H. N. Yang, Y. L. Wang, Y. Liu (NAO, CAS), Z. H. Yang, Q. C. Zhao (IHEP, CAS) on behalf of the Einstein Probe (EP) team: EP-FXT performed a follow-up observation on GRB 260208B detected by Fermi/GBM (The Fermi GBM team, GCN 43638; Preis & Greiner, GCN 43639; Sonawane et al., GCN 43649), Fermi/LAT (Longo et al., GCN 43647) and SVOM/GRM (Luo et al., GCN 43650) at 2026-02-09T06:37:35 (UTC), about 20.748 hours after the Fermi/GBM trigger. Two uncatalogued X-ray sources are detected around the Fermi/LAT error circle. Preliminary informations are listed as follows: Source 1: EPF_J063834.1-135348 RA (J2000): 99.6419 Dec (J2000): -13.8965 Flux: 1.12 x 10^-13 erg/cm^2/s (observed, 0.5-10 keV) Source 2: EPF_J063827.9-134635 RA (J2000): 99.6162 Dec (J2000): -13.7764 Flux: 0.96 x 10^-13 erg/cm^2/s (observed, 0.5-10 keV) The position is consistent with the source 1 detected by Swift-XRT (Evans et al., GCN 43651) and the optical candidate detected by SVOM/VT (Li et al., GCN 43659). The position uncertainties of the above sources are about 20 arcsec in radius (90% C.L. statistical and systematic). The current result is based on the FXT on-board alert and will be updated when the telemetry data are 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/43663. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41768] GRB 260208A: NOT spectroscopic redshift z = 2.36
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43662 SUBJECT: GRB 260208A: NOT spectroscopic redshift z = 2.36 DATE: 26/02/09 10:13:18 GMT FROM: Antonio de Ugarte Postigo at LAM, CNRS <adeugartepostigo(a)gmail.com> Dimple (U. Birmingham), D. B. Malesani (DAWN/NBI and Radboud), A. de Ugarte Postigo (LAM), A. Saccardi (CEA/Irfu), G. Corcoran (UCD), B. P. Gompertz (U. Birmingham), L. Izzo (INAF/OAC and DARK/NBI), A. Martin-Carrillo (UCD) and S. Bijavara Seshashayana (NOT and Malmo Univ.) report on behalf of a larger collaboration: We observed the optical counterpart AT2026ciw (Podesta et al., GCN 43640; Wortley et al., GCN 43641; Ma et al., GCN 43655; Ahumada et al., GCN 43657, Dimple et al., GCN 43661) of the GRB 260208A detected by Fermi (Fermi GBM Team, GCN 43635; Sonawane et al., GCN 43642; Longo et al., GCN 43645) and GECAM-B (Luo et al., GCN 43658), which was also detected in X-rays (Dichiara et al., GCN 43652). Observations started at 05:45:58 UT on 9 February 2026 (24.64 hr after the burst) and consisted of 4x1200 s exposures with grism 4, covering the wavelength range between 3200 and 9600 Å. From a preliminary reduction of the spectrum, a trough due to Lya absorption is visible at 4080 AA. From the detection of multiple absorption features, which we interpret as due to O I, C II, Si IV, Si II, C IV, Fe II, Al II, and Al III, we infer a redshift of z = 2.36. View this GCN Circular online at https://gcn.nasa.gov/circulars/43662. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41767] GRB 260208A: Liverpool Telescope optical detection
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43661 SUBJECT: GRB 260208A: Liverpool Telescope optical detection DATE: 26/02/09 10:00:09 GMT FROM: Dimple at University of Birmingham <dimplepanchal96(a)gmail.com> Dimple (U. Birmingham), B. P. Gompertz (U. Birmingham), D. O'Neill (U. Birmingham), and D. B. Malesani (DAWN/NBI and Radboud) report on behalf of a larger collaboration: We conducted follow-up observations of GRB 260208A (Fermi GBM team, GCN 43635; Sonawane et al., GCN 43642; Longo et al., GCN 43645; Luo et al., GCN 43658) with the IO:O camera on the 2m robotic Liverpool Telescope (LT). Observations began at 03:49:38 UT on 2026-02-09, ~22.8 hr after the Fermi trigger, and consisted of 5 x 180 s exposures in each of the SDSS r and i filters. We detect the optical counterpart (Podesta et al., GCN 43640; Wortley et al., GCN 43641; Ma et al., GCN 43655; Ahumada et al., GCN 43657; also detected in X-rays, Dichiara et al., GCN 43652) in both filters, and measure an AB magnitude of r = 20.63 ± 0.04. Magnitudes are calibrated against nearby Pan-STARRS stars and are not corrected for Galactic extinction. View this GCN Circular online at https://gcn.nasa.gov/circulars/43661. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41766] Fermi GRB 260208C: Global MASTER-Net observations report
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43660 SUBJECT: Fermi GRB 260208C: Global MASTER-Net observations report DATE: 26/02/09 09:30:23 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, A.Kuznetsov, K.Zhirkov, I.Panchenko, N.Tiurina, P.Balanutsa, V.Topolev, D.Vlasenko, G.Antipov, A.Sankovich, Yu.Tselik, Ya.Kechin, V.Senik, A.Chasovnikov, K.Labsina, I. Gorbunov (Lomonosov MSU), O.Gress, N.Budnev (ISU), C.Francile, F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), A.Sosnovskij (CrAO), A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity), D.Buckley (SAAO), R.Rebolo (The Instituto de Astrofisica de Canarias), L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez, A.R.Corella, L.H.Rodriguez (INAOE, Guillermo Haro Astrophysics Observatory) MASTER-OAFA robotic telescope [1] located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 260208C ( Fermi GBM team, GCN 43646) errorbox 63027 sec after notice time and 63048 sec after trigger time at 2026-02-09 08:43:07 UT, with upper limit up to 19.1 mag. The observations began at zenith distance = 61 deg. The sun altitude is -17.5 deg. The galactic latitude b = -20 deg., longitude l = 347 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3126450 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 63078 | 2026-02-09 08:43:07 | MASTER-OAFA | (18h 44m 17.79s , -49d 24m 20.8s) | C | 60 | 18.5 | 63138 | 2026-02-09 08:43:07 | MASTER-OAFA | (18h 44m 17.79s , -49d 24m 20.8s) | C | 180 | 19.0 | Coadd 63154 | 2026-02-09 08:44:22 | MASTER-OAFA | (18h 44m 23.14s , -49d 24m 13.2s) | C | 60 | 18.5 | 63231 | 2026-02-09 08:45:39 | MASTER-OAFA | (18h 44m 20.60s , -49d 22m 30.2s) | C | 60 | 18.5 | 63307 | 2026-02-09 08:46:55 | MASTER-OAFA | (18h 44m 25.93s , -47d 23m 58.0s) | C | 60 | 18.5 | 63367 | 2026-02-09 08:46:55 | MASTER-OAFA | (18h 44m 25.93s , -47d 23m 58.0s) | C | 180 | 18.9 | Coadd 63385 | 2026-02-09 08:48:13 | MASTER-OAFA | (18h 44m 28.06s , -47d 22m 15.4s) | C | 60 | 18.4 | 63458 | 2026-02-09 08:49:26 | MASTER-OAFA | (18h 44m 23.21s , -47d 22m 58.9s) | C | 60 | 18.4 | 63534 | 2026-02-09 08:50:42 | MASTER-OAFA | (18h 44m 11.06s , -51d 22m 15.4s) | C | 60 | 18.6 | 63594 | 2026-02-09 08:50:42 | MASTER-OAFA | (18h 44m 11.06s , -51d 22m 15.4s) | C | 180 | 19.1 | Coadd 63610 | 2026-02-09 08:51:59 | MASTER-OAFA | (18h 44m 17.39s , -51d 23m 13.9s) | C | 60 | 18.6 | 63684 | 2026-02-09 08:53:12 | MASTER-OAFA | (18h 44m 10.04s , -51d 24m 11.4s) | C | 60 | 18.6 | 64223 | 2026-02-09 09:02:11 | MASTER-OAFA | (18h 59m 29.75s , -47d 23m 37.4s) | C | 60 | 18.2 | 64299 | 2026-02-09 09:03:27 | MASTER-OAFA | (18h 59m 22.68s , -47d 24m 34.6s) | 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/43660. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41765] GRB 260208B: SVOM/VT optical candidate
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43659 SUBJECT: GRB 260208B: SVOM/VT optical candidate DATE: 26/02/09 09:10:45 GMT FROM: Huali Li at at NAOC, SVOM <lhl(a)nao.cas.cn> H. L. Li, C. W. Wang, Y. L. Qiu, Y. N. Ma, Z. H. Yao, C. Wu, L.P. Xin, X. H. Han, J. Wang, Y. Xu, P. P. Zhang, W. J. Xie, Y. J. Xiao, H. B. Cai, L. Lan, J. R. Xu, J. S. Deng, J. Y. Wei (NAOC), J. Palmerio (CEA/Irfu) report on behalf of the SVOM/VT team. SVOM/VT performed ToO observation to GRB 260208B detected by Fermi-GBM (The Fermi GBM team, GCN 43638; Preis & Greiner, GCN 43639; Sonawane et al., GCN 43649), Fermi-LAT (Longo et al., GCN 43647) and SVOM/GRM (Luo et al., GCN 43650). The observation started at 2026-02-08T18:13:53 UTC, i.e., 8.359 hours post trigger in the VT_B (400nm-650nm) and VT_R (650nm-1000nm) channels simultaneously. An uncatalogued source was detected within the error box of source 1 detected by Swift-XRT (Evans et al., GCN 43651). The position is at R.A., Dec. = 99.619042, -13.774177 degrees, equivalent to: R.A. (J2000) = +06:38:28.57 Dec. (J2000) = -13:46:27.04 with an uncertainty of 0.5 arcsec. The measurements in AB magnitudes are given below: Mid_time Band Exposure Time Magnitude (AB) 10.341 hour VT_R 53*50 sec 22.3+/-0.2 mag 10.341 hour VT_B 57*50 sec > 23.5 mag Our photometry was not corrected for Galactic extinction. Further SVOM/VT ToO observations are scheduled. The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. VT was jointly developed by Xi'an Institute of Optics and Precision Mechanics (XIOPM), CAS and National astronomical observatories (NAOC), CAS. View this GCN Circular online at https://gcn.nasa.gov/circulars/43659. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41764] GRB 260208A: GECAM-B observation of a bright burst
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43658 SUBJECT: GRB 260208A: GECAM-B observation of a bright burst DATE: 26/02/09 05:50:39 GMT FROM: Xinghao Luo at IHEP <2952704891(a)qq.com> Xing-Hao Luo, Zheng-Hang Yu, Chen-Wei Wang, Shao-Lin Xiong (IHEP) report on behalf of GECAM team: GECAM-B was triggered in-flight by GRB 260208A, at 2026-02-08T05:07:30.550 UTC (denoted as T0), which is also detected by Fermi/GBM (Fermi GBM team, GCN #43635) and Fermi/LAT (Fermi LAT team, GCN #43645). According to the GECAM-B light curves in about 70-6000 keV, this burst mainly consists of multiple pulses with a duration (T90) of 38 +2/-1 s. The GECAM-B light curve can be found here: https://www.bursthub.cn//admin/static/gecambgrb260208A.png GECAM-B localized this burst to the following position (J2000): Ra: 128.62 deg Dec: 6.25 deg Err: 0.34 deg (1-sigma, statistical only) The time-averaged spectrum from T0-11.5 s to T0+147.5 s is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -1.29 +0.10/-0.08 and the cutoff energy, parameterized as Epeak, is 651 +175/-134 keV. The event fluence (10-1000 keV) in this time interval is (1.62 +0..050/-0.066)E-04 erg/cm^2. Thus GRB 260208A is consistent with Type I GRBs in the 'Amati' relation diagram, as shown at: https://www.bursthub.cn//admin/static/grb250208A_amati.png Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM) mission originally consists of two micro-satellites (GECAM-A and GECAM-B) launched in Dec. 2020. As the third member of GECAM constellation, GECAM-C was launched onboard SATech-01 experimental satellite in July 2022. GECAM mission is funded by the Chinese Academy of Sciences (CAS). View this GCN Circular online at https://gcn.nasa.gov/circulars/43658. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41763] GRB 260208A: Zwicky Transient Facility Follow-Up of a Fermi GRB (Trigger 792220053)
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43657 SUBJECT: GRB 260208A: Zwicky Transient Facility Follow-Up of a Fermi GRB (Trigger 792220053) DATE: 26/02/09 03:44:52 GMT FROM: Tomas Ahumada <tomas.ahumada(a)noirlab.edu> Tomas Ahumada (NOIRLab), Robert Stein (UMD), Theophile du Laz (CIT), Igor Andreoni (UNC), Michael Coughlin (UMN), Mansi Kasliwal (CIT), Shreya Anand (Stanford), report on behalf of the ZTF collaboration: We observed the localization region of the long GRB 260208A (trigger 792220053.24286 / 260208214, Fermi GBM team, GCN 43635) detected by the Gamma-Ray Burst Monitor (GBM) on the Fermi satellite with the Palomar 48 inch telescope equipped with the 47 square degree Zwicky Transient Facility (ZTF) camera. We obtained a series of g- and r-band images covering 130 square degrees beginning at 2026-02-08T10:43:17 (5.6 hours after the burst trigger time). This corresponds to 93% of the probability enclosed in the Earth-occultation corrected GRB localization map. Each exposure was 300 seconds, reaching g-band and r-band median depths of 21.2 mag and 21.2 mag respectively. The images were processed in real-time through the ZTF reduction and image subtraction pipelines at IPAC (Masci et al. 2019). We queried the ZTF alert stream using Kowalski (Duev et al. 2019) through Fritz (Coughlin et al. 2023). We required at least 2 detections separated by at least 15 minutes to select against moving objects. Furthermore, we cross-match our candidates with the Minor Planet Center to flag known asteroids, reject stellar sources (Tachibana and Miller 2018), and apply machine learning algorithms (Mahabal et al. 2019). We require that no spatially coincident ZTF alerts were issued before the detection time of the GBM trigger. We detect the afterglow candidate AT 2026ciw (Podesta et al. GCN 43640, Wortley et al. GCN 43641) as ZTF26aafswob. This is the only source that passed our filtering scheme (Ahumada et al. 2022). The most recent ZTF visit to the field was 3 days prior to the detection. The ZTF detections are reported in the following table: Time (MJD) | Filter | Magnitude 61079.44815970 | g | 19.05 ± 0.05 61079.52940970 | r | 19.11 ± 0.05 This Circular is based on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Award #2407588 and a partnership including Caltech, USA; Caltech/IPAC, USA; University of Maryland, USA; University of California, Berkeley, USA; University of Wisconsin at Milwaukee, USA; Cornell University, USA; Drexel University, USA; University of North Carolina at Chapel Hill, USA; Institute of Science and Technology, Austria; National Central University, Taiwan; and OKC, University of Stockholm, Sweden. Operations are conducted by Caltech's Optical Observatory (COO), Caltech/IPAC, and the University of Washington at Seattle, USA. View this GCN Circular online at https://gcn.nasa.gov/circulars/43657. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41762] GRB 260209A: Fermi GBM Final Real-time Localization
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43656 SUBJECT: GRB 260209A: Fermi GBM Final Real-time Localization DATE: 26/02/09 02:56:37 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 02:45:57 UT on 9 Feb 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260209A (trigger 792297962.23625 / 260209115). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 75.8, Dec = 33.0 (J2000 degrees, equivalent to J2000 05h 03m, 33d 00'), with a statistical uncertainty of 9.2 degrees. The angle from the Fermi LAT boresight is 87.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260209115/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260209115/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260209115/… View this GCN Circular online at https://gcn.nasa.gov/circulars/43656. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41761] GRB 260208A: SVOM/VT optical observation
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43655 SUBJECT: GRB 260208A: SVOM/VT optical observation DATE: 26/02/09 02:31:49 GMT FROM: Yinuo Ma <mayn(a)bao.ac.cn> Y. N. Ma, L. P. Xin, Y. L. Qiu, C. Wu, H. L. Li, Z. H. Yao, X. H. Han, Y. Xu, J. Wang, P. P. Zhang, W. J. Xie, Y. J. Xiao, H. B. Cai, L. Lan, J. S. Deng, J. Y. Wei (NAOC), J. Palmerio (CEA) report on behalf of the SVOM/VT team. SVOM/VT performed a Target of Opportunity observation of GRB 260208A detected by Fermi/GBM and Fermi/LAT (Fermi GBM Team, GCN 43635; Sonawane et al., GCN 43642; Longo et al., GCN 43645). SVOM/VT began observing the field at 2026-02-08T13:57:59 UTC, 8.842 hours after the trigger, in the VT_B (400nm-650nm) and VT_R (650nm-1000nm) channels simultaneously. With X-band data available, the optical counterpart (Lipunov et al., GCN 43637; Podesta et al., GCN 43640; Wortley et al., GCN 43641) within Swift/XRT Source 1 errorbox (Dichiara et al., GCN 43652) was clearly detected in both VT_B and VT_R bands. The magnitudes are: mid time (h) | exposure time (s) | band | mag (AB) | mag err -------------|-------------------|------|----------|-------- 10.306 | 23*70 | VT_B | 21.15 | 0.06 10.170 | 19*70 | VT_R | 20.40 | 0.04 Our photometry was not corrected for Galactic extinction. Further SVOM/VT ToO observations are scheduled. The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. VT was jointly developed by Xi'an Institute of Optics and Precision Mechanics (XIOPM), CAS and National astronomical observatories (NAOC), CAS. View this GCN Circular online at https://gcn.nasa.gov/circulars/43655. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41760] Fermi GRB 260208D: Global MASTER-Net observations report
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43654 SUBJECT: Fermi GRB 260208D: Global MASTER-Net observations report DATE: 26/02/09 00:30:26 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 260208D ( Fermi GBM team, GCN 43653) errorbox 9638 sec after notice time and 9659 sec after trigger time at 2026-02-09 00:23:45 UT, with upper limit up to 13.1 mag. Observations started at twilight. The observations began at zenith distance = 83 deg. The sun altitude is -11.6 deg. The galactic latitude b = -51 deg., longitude l = 4 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3126729 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 9675 | 2026-02-09 00:23:45 | MASTER-OAFA | (21h 51m 37.44s , -38d 54m 31.8s) | C | 30 | 12.8 | 9722 | 2026-02-09 00:24:32 | MASTER-OAFA | (21h 51m 33.51s , -38d 53m 25.2s) | C | 30 | 13.1 | 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/43654. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41759] Fermi GRB 260208D: Global MASTER-Net observations report
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43654 SUBJECT: Fermi GRB 260208D: Global MASTER-Net observations report DATE: 26/02/09 00:30:26 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 260208D ( Fermi GBM team, GCN 43653) errorbox 9638 sec after notice time and 9659 sec after trigger time at 2026-02-09 00:23:45 UT, with upper limit up to 13.1 mag. Observations started at twilight. The observations began at zenith distance = 83 deg. The sun altitude is -11.6 deg. The galactic latitude b = -51 deg., longitude l = 4 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3126729 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 9675 | 2026-02-09 00:23:45 | MASTER-OAFA | (21h 51m 37.44s , -38d 54m 31.8s) | C | 30 | 12.8 | 9722 | 2026-02-09 00:24:32 | MASTER-OAFA | (21h 51m 33.51s , -38d 53m 25.2s) | C | 30 | 13.1 | 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/43654. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41758] Fermi GRB 260208D: Global MASTER-Net observations report
by GCN Circulars 09 Feb '26

09 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43654 SUBJECT: Fermi GRB 260208D: Global MASTER-Net observations report DATE: 26/02/09 00:30:26 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 260208D ( Fermi GBM team, GCN 43653) errorbox 9638 sec after notice time and 9659 sec after trigger time at 2026-02-09 00:23:45 UT, with upper limit up to 13.1 mag. Observations started at twilight. The observations began at zenith distance = 83 deg. The sun altitude is -11.6 deg. The galactic latitude b = -51 deg., longitude l = 4 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3126729 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 9675 | 2026-02-09 00:23:45 | MASTER-OAFA | (21h 51m 37.44s , -38d 54m 31.8s) | C | 30 | 12.8 | 9722 | 2026-02-09 00:24:32 | MASTER-OAFA | (21h 51m 33.51s , -38d 53m 25.2s) | C | 30 | 13.1 | 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/43654. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41757] GRB 260208D: Fermi GBM Final Real-time Localization
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43653 SUBJECT: GRB 260208D: Fermi GBM Final Real-time Localization DATE: 26/02/08 21:53:17 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 21:42:45 UT on 8 Feb 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260208D (trigger 792279770.48211 / 260208905). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 327.7, Dec = -39.0 (J2000 degrees, equivalent to J2000 21h 50m, -39d 00'), with a statistical uncertainty of 6.9 degrees. The angle from the Fermi LAT boresight is 51.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260208905/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260208905/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260208905/… View this GCN Circular online at https://gcn.nasa.gov/circulars/43653. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41756] GRB 260208A: Swift-XRT observations
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43652 SUBJECT: GRB 260208A: Swift-XRT observations DATE: 26/02/08 21:51:33 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> S. Dichiara (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), T. Sbarrato (INAF-OAB), P. D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), J.A. Kennea (PSU), D.N. Burrows (PSU) and P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the Fermi/LAT-detected burst GRB 260208A, collecting 3.4 ks of Photon Counting (PC) mode data between T0+35.1 ks and T0+42.2 ks. Six uncatalogued X-ray sources have been detected, with Source 1 located 2.2 arcsec from the new optical source seen by MASTER and GOTO (GCN Circ. 43640 and 43641) and, therefore, consistent with that source. The details of this new X-ray source are: RA (J2000.0): 204.73150 = 13h 38m 55.56s Dec (J2000.0): +33.80112 = +33d 48' 04.0" Error: 2.5 arcsec (radius, 90% conf. [Enhanced position]) Count-rate: 0.0488 +/- 0.0045 ct s^-1 Flux: (1.55 +/- 0.14)e-12 erg cm^-2 s^-1 (observed, 0.3-10 keV) However, we cannot presently determine if the source is fading. The results of the XRT-team automatic analysis of the XRT observations, including a position-specific upper limit calculator, are available at https://www.swift.ac.uk/ToO_GRBs/00021908. This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/43652. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41755] GRB 260208B: Swift ToO observations
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43651 SUBJECT: GRB 260208B: Swift ToO observations DATE: 26/02/08 18:58:32 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a ToO observation of the Fermi/LAT-detected event GRB 260208B. Automated analysis of the XRT data will be presented online at https://www.swift.ac.uk/ToO_GRBs/00021909 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. These are not necessarily related to the Fermi/LAT event. Any X-ray source considered to be a probable afterglow candidate will be reported via a GCN Circular after manual consideration. Details of the XRT automated analysis methods are detailed in Evans et al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8). This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/43651. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41754] GRB 260208B: SVOM/GRM observation of a bright burst
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43650 SUBJECT: GRB 260208B: SVOM/GRM observation of a bright burst DATE: 26/02/08 17:40:27 GMT FROM: Chenwei Wang at IHEP <cwwang(a)ihep.ac.cn> SVOM/GRM team: Xing-Hao Luo, Wen-Jun Tan, Chen-Wei Wang, Zheng-Hang Yu, Yue Huang, Shi-Jie Zheng, Shao-Lin Xiong, Shuang-Nan Zhang (IHEP) SVOM/ECLAIRs team: Hui Yang (IRAP) Report on behalf of the SVOM team: SVOM/GRM was triggered in-flight by GRB 260208B (SVOM trigger reference: sb26020804) at 2026-02-08T09:52:48.000 UTC (T0), which is also detected by Fermi/GBM (Fermi GBM team, GCN #43638) and Fermi/LAT (F. Longo et al., GCN #43647). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of multi-pulses with a T90 of 147 +1/-1 s in the 15-5000 keV band. The SVOM/GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb260208B.png In addition, the position of this burst, as determined by Fermi/GBM (RA=99.9 , DEC=-13.1, Fermi GBM team, GCN #43638), is located at about 64 degrees form the SVOM optical axis, which is outside the ECLAIRs field of view, but this burst is still clearly detected by ECLAIRs through the shield. With this localization, the time-averaged spectrum from T0-12 to T0+166 s is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -1.01 +0.04/-0.04 and the cutoff energy parameterized as Epeak, is 830 +105/-89 keV. The event fluence (10-1000keV) in this time interval is (1.09 +0.024/-0.025)E-04 erg/cm^2. The 1s peak spectrum, measured from T0+11 to T0+12 s, is also best fitted by a power law function with an exponential high-energy cutoff. The power law index is -0.81 +0.03/-0.03 and the cutoff energy, parameterized as Epeak, is 1520 +130/-120 keV. The flux (10-1000 keV) in this time interval is (1.011 + 0.019/-0.019)E-05 erg/cm^2/s. The localization of GRB 260208B in the 'Amati' relation diagram is shown at: https://www.bursthub.cn//admin/static/svgrb260208B_amati.png The localization of GRB 260208B in the 'Yonetoku' relation diagram is shown at: https://www.bursthub.cn//admin/static/svgrb260208B_yonetoku.png The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. GRM is developed by the Institute of High Energy Physics (IHEP) of CAS. The SVOM point of contact for this burst is: Xing-Hao Luo (luoxh(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/43650. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41753] GRB 260208B: Fermi GBM Detection
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43649 SUBJECT: GRB 260208B: Fermi GBM Detection DATE: 26/02/08 17:38:17 GMT FROM: Rushikesh Sonawane at IISER, TVM <rushikesh23(a)iisertvm.ac.in> R. Sonawane (IISER, TVM) reports on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 09:52:44.91 UT on 08 February 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260208B (trigger 792237169/260208412). which was also detected by Fermi LAT (A. H. Airasca et al. 2026, GCN 43647). The Fermi GBM final real-time Localization (GCN 43638) is consistent with the Fermi LAT position. The angle from the Fermi LAT boresight is 16 degrees. The GBM light curve consists of two emission episodes with multiple spikes for a duration (T90) of about 145 s (50-300 keV). The time-averaged spectrum from T0-8.2 to T0+172.0 s is best fit by a Band function with Epeak = 855 +/- 61 keV, alpha = -1.0 +/- 0.02, and beta = -2.12 +/- 0.08. The event fluence (10-1000 keV) in this time interval is (9.1 +/- 0.1)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+14 s in the 10-1000 keV band is 23 +/- 0.4 ph/s/cm^2. 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/43649. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41752] LAT GRB260208.41: Global MASTER-Net observations report
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43648 SUBJECT: LAT GRB260208.41: Global MASTER-Net observations report DATE: 26/02/08 16:44:32 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 LAT GRB260208.41 (trigger No 792237169,06h 38m 33.12s , -13d 50m 16.8s, R=0.0598333) errorbox 6014 sec after notice time and 24109 sec after trigger time at 2026-02-08 16:34:34 UT, with upper limit up to 16.4 mag. The observations began at zenith distance = 70 deg. The sun altitude is -52.8 deg. The galactic latitude b = -9 deg., longitude l = 224 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3126408 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 24140 | 2026-02-08 16:34:34 | MASTER-Tunka | (06h 37m 00.05s , -13d 24m 07.8s) | C | 60 | 15.9 | 24212 | 2026-02-08 16:35:47 | MASTER-Tunka | (06h 36m 53.46s , -13d 23m 06.3s) | C | 60 | 15.9 | 24284 | 2026-02-08 16:36:59 | MASTER-Tunka | (06h 36m 52.89s , -13d 21m 12.6s) | C | 60 | 16.4 | 24358 | 2026-02-08 16:38:12 | MASTER-Tunka | (06h 36m 59.13s , -13d 21m 17.5s) | C | 60 | 16.4 | 24431 | 2026-02-08 16:39:25 | MASTER-Tunka | (06h 36m 53.87s , -13d 21m 24.3s) | C | 60 | 16.4 | 24505 | 2026-02-08 16:40:40 | MASTER-Tunka | (06h 37m 00.18s , -13d 21m 29.5s) | C | 60 | 16.0 | 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/43648. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41751] GRB 260208B: Fermi-LAT detection
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43647 SUBJECT: GRB 260208B: Fermi-LAT detection DATE: 26/02/08 16:31:58 GMT FROM: A. Holzmann Airasca at University of Trento and INFN Bari <a.holzmannairasca(a)unitn.it> F. Longo (University and INFN, Trieste), D. Depalo (Politecnico and INFN Bari), A. Holzmann Airasca (UniTrento and INFN Bari) and R. Gupta (NASA/GSFC) report on behalf of the Fermi-LAT team: At 09:52:44.91 UT on February 8th, 2026 Fermi-LAT detected high-energy emission from GRB 260208B, which was also detected by Fermi-GBM (trigger 792237169 / 260208412, GCN #43638). The best LAT on-ground location is found to be RA, Dec = 99.64, -13.84 (J2000) with an error radius of 0.06 deg (90 % containment, statistical error only). This was 13 deg from the LAT boresight at the time of the trigger. The data from the Fermi-LAT show a significant increase in the event rate that is spatially and temporally correlated with the trigger with high significance. The photon flux above 100 MeV in the time interval 0 - 2 ks after the GBM trigger is (8.7 ± 1.2)E-6 ph/cm2/s. The estimated photon index above 100 MeV is -2.03 ± 0.12. The highest energy photon has an energy of 2.6 GeV and occurs at 20 s after trigger time. A Swift ToO request has been sent for this burst. The Fermi-LAT point of contact for this burst is Chiara Bartolini (chiara.bartolini(a)ba.infn.it) The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden. View this GCN Circular online at https://gcn.nasa.gov/circulars/43647. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41750] GRB 260208C: Fermi GBM Final Real-time Localization
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43646 SUBJECT: GRB 260208C: Fermi GBM Final Real-time Localization DATE: 26/02/08 15:22:56 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 15:12:18 UT on 8 Feb 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260208C (trigger 792256343.59123 / 260208634). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 281.3, Dec = -49.2 (J2000 degrees, equivalent to J2000 18h 45m, -49d 12'), with a statistical uncertainty of 2.3 degrees. The angle from the Fermi LAT boresight is 82.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260208634/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260208634/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260208634/… View this GCN Circular online at https://gcn.nasa.gov/circulars/43646. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41749] GRB 260208A: Fermi-LAT detection
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43645 SUBJECT: GRB 260208A: Fermi-LAT detection DATE: 26/02/08 15:21:39 GMT FROM: Davide Depalo at Politecnico and INFN Bari <davide.depalo(a)ba.infn.it> F. Longo (University and INFN, Trieste), D. Depalo (Politecnico and INFN Bari), A. Holzmann Airasca (UniTrento and INFN Bari) and R. Gupta (NASA/GSFC) report on behalf of the Fermi-LAT team: At 05:07:28.24 UT on February 8th, 2026 Fermi-LAT detected high-energy emission from GRB 260208A, which was also detected by Fermi-GBM (trigger 792220053 / 260208214, GCN #43635), MASTER (GCN #43640) and GOTO (GCN #43641). The best LAT on-ground location is found to be RA, Dec = 204.57, 33.77 (J2000) with an error radius of 0.15 deg (90 % containment, statistical error only). This was 80 deg from the LAT boresight at the time of the trigger. The data from the Fermi-LAT show a significant increase in the event rate that is spatially and temporally correlated with the trigger with high significance. The photon flux above 100 MeV in the time interval 400 - 2500 s after the GBM trigger is (2.86 ± 0.65)E-6 ph/cm2/s. The estimated photon index above 100 MeV is -1.99 ± 0.19. The highest-energy photon is a 5.3 GeV event which is observed 1168 seconds after the GBM trigger. A Swift ToO request has been approved for this burst. The Fermi-LAT point of contact for this burst is Chiara Bartolini (chiara.bartolini(a)ba.infn.it) The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden. View this GCN Circular online at https://gcn.nasa.gov/circulars/43645. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41748] GRB 260207B: GECAM-B observation
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43644 SUBJECT: GRB 260207B: GECAM-B observation DATE: 26/02/08 14:58:40 GMT FROM: xueyuan zao <zaoxueyuan(a)gmail.com> Xue-Yuan Zao, Xing-Hao Luo, Chen-Wei Wang, Shao-Lin Xiong (IHEP) report on behalf of GECAM team: GECAM-B was triggered in-flight and on-ground by GRB 260207B, at 2026-02-07T13:12:10.850 UTC, which is also detected by Fermi/GBM (Fermi GBM team, GCN #43629). According to the GECAM-B light curves in about 70-6000 keV, this burst mainly consists of a short spike (Main Emission, ME) followed by an extended emission (EE) with a total duration (T90) of 65 +23/-9.5 s. The GECAM-B light curve can be found here: https://www.bursthub.cn//admin/static/gecambgrb260207B.png The ME from T0 - 0.07 to T0 + 0.19 s is best fitted by a power law function with an exponential high-energy cutoff. The power law index is -1.15 +0.29/-0.32 and the cutoff energy, parameterized as Epeak, is 345 +151/-70 keV. The event fluence (10-1000 keV) in this time interval is (2.04 +/-0.22)E-06 erg/cm^2. Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM) mission originally consists of two micro-satellites (GECAM-A and GECAM-B) launched in Dec. 2020. As the third member of GECAM constellation, GECAM-C was launched onboard SATech-01 experimental satellite in July 2022. GECAM mission is funded by the Chinese Academy of Sciences (CAS). View this GCN Circular online at https://gcn.nasa.gov/circulars/43644. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41747] GRB 260208A: Swift ToO observations
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43643 SUBJECT: GRB 260208A: Swift ToO observations DATE: 26/02/08 14:50:32 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a ToO observation of the Fermi/LAT-detected event GRB 260208A. Automated analysis of the XRT data will be presented online at https://www.swift.ac.uk/ToO_GRBs/00021908 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. These are not necessarily related to the Fermi/LAT event. Any X-ray source considered to be a probable afterglow candidate will be reported via a GCN Circular after manual consideration. Details of the XRT automated analysis methods are detailed in Evans et al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8). This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/43643. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41746] GRB 260208A: Fermi GBM Classification Correction
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43642 SUBJECT: GRB 260208A: Fermi GBM Classification Correction DATE: 26/02/08 14:07:05 GMT FROM: Rushikesh Sonawane at IISER, TVM <rushikesh23(a)iisertvm.ac.in> R. Sonawane (IISER, TVM), O.J. Roberts (Uni. of Galway, Ireland), and R. Hamburg (USRA) reports on behalf of the Fermi Gamma-ray Burst Monitor Team: "The Fermi Gamma-ray Burst Monitor (GBM) trigger 792220053/260208214 at 05:07:28.24 UT on 08 February 2026, is in fact a GRB. The GBM localization for this GRB is valid (GCN 43635). The GRB was confirmed with an optical afterglow detection by MASTER (GCN 43640). This trigger was misclassified as a particle trigger (GCN 43636)." View this GCN Circular online at https://gcn.nasa.gov/circulars/43642. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41745] GRB 260208A: GOTO detection of a potential optical counterpart (GOTO26aob)
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43641 SUBJECT: GRB 260208A: GOTO detection of a potential optical counterpart (GOTO26aob) DATE: 26/02/08 14:01:53 GMT FROM: MEW020(a)student.bham.ac.uk M. E. Wortley, D. O'Neill, A. Kumar, G. Ramsay, B. P. Gompertz, K. Ackley, M. Dyer, J. Lyman, K. Ulaczyk, D. Steeghs, D. Galloway, V. Dhillon, P. O'Brien, K. Noysena, R. Kotak, R. Breton, J. Casares, L. Nuttall, R. Starling, B. Godson, T. Killestein, M. Pursiainen, on behalf of GOTO collaboration We report on optical observations with the Gravitational-wave Optical Transient Observer (GOTO; Steeghs et al. 2022, Dyer et al. 2024) in response to the Fermi/GBM GRB 260208A (trigger GBM792220053; Fermi GBM team, GCN 43638). Observations covering the localisation area began at 2026-02-08 05:19:32 UT (+0.20h post trigger) and continued through to 2026-02-08 06:31:29 UT (+1.4h post trigger). All observations were performed with 90s integrations using the GOTO L-band filter (400–700 nm). Images were processed immediately after acquisition using the GOTO pipeline. Source candidates were initially filtered using a classifier (Killestein et al. 2021) and cross-matched against a variety of contextual and minor planet catalogs. Human vetting was carried out in real time on any candidates that passed the above checks. We detect the source reported by R. Podesta et al. (GCN 43640) with an L-band = 13.78 ± 0.01 AB mag at 2026-02-08 05:19:32 UT (t0+0.20h) before it faded to L=16.72 ± 0.01 AB mag at 2026-02-08 06:29:16 UT (t0+1.36h). We find no evidence of this source prior to the GRB trigger time in previous GOTO observations taken at 2026-02-08 03:33:31 UT (t0-1.57h pre-trigger) down to a 5-sigma depth of L>19.07 AB mag. GOTO (https://goto-observatory.org) is a network of telescopes that is principally funded by the STFC and operated at the Roque de los Muchachos Observatory on La Palma, Spain, and Siding Spring Observatory in NSW, Australia, on behalf of a consortium including the University of Warwick, Monash University, Armagh Observatory & Planetarium, the University of Leicester, the University of Sheffield, the National Astronomical Research Institute of Thailand (NARIT), the University of Turku, the University of Portsmouth, the University of Manchester, the University of Birmingham and the Instituto de Astrofisica de Canarias (IAC). View this GCN Circular online at https://gcn.nasa.gov/circulars/43641. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41744] GRB 260208A : MASTER bright optical transient inside retracted Fermi error-box
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43640 SUBJECT: GRB 260208A : MASTER bright optical transient inside retracted Fermi error-box DATE: 26/02/08 12:35:14 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> R.Podesta (OAFA), V.M.Lipunov (Lomonosov MSU), C. Francile, F.Podesta (OAFA), I.Panchenko (Lomonosov MSU), V.Shumkov (Ozersk), P.Balanutsa, G.Antipov, A.Kuznetsov, E.Gorbovskoy, D.Vlasenko, N. Tiurina, Ya.Kechin, A.Chasovnikov (Lomonosov MSU), D.Svinkin (Ioffe Institute), O.Gress, N.Budnev, R.Mirgazov, A.Diachok, O.Ershova (Irkutsk State University), E. Gonzalez (OAFA, San JuanUni.,Argentina); D.Buckley (SAAO), V.A.Senik, I.Ionov,Yu.Tselik(Lomonosov MSU), A. Sosnovskij (CrAO RAS), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino, J.Martinez, A.R.Corella, J.G.Tanori, L. F. Villalobos, L.H.Rodriguez (INAOE, Guillermo Haro AstrophysicObservatory, Mexico), V.M.Pillet, R.Rebolo Lopez (The Instituto de Astrofisica de Canarias,Spain) MASTER Global Robotic Net started (Lipunov et al. GCN 43637) Fermi GRB 260208A (GCN 43635) MASTER OT J133855.59+334806.2 discovery MASTER-OAFA auto-detection system ( Lipunov et al., "MASTER Global Robotic Net", Advances in Astronomy, 2010, 30L ) discovered OT source at (RA, Dec) = 13h 38m 55.59s +33d 48m 06.2s during Fermi trigger 792220053 inspection (also known as GRB 260208A, retracted by Fermi team) The OT unfiltered magnitude is 15.2m at 05:33:36UT with GRB decay t^-alpha low at light curve (alpha ~ 1). We observed OT in MASTER-OAFA (Argentina) and MASTER-OAGH (Mexico) (Shumkov et al. https://www.wis-tns.org/object/2026ciw ). We have reference image on 2019-05-24.09972 UT with unfiltered 20.7m. Deep photometry and spectral observations are required. [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/43640. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41743] GRB 260208B: BALROG localization (Fermi Trigger 792237169 / GRB 260208412)
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43639 SUBJECT: GRB 260208B: BALROG localization (Fermi Trigger 792237169 / GRB 260208412) DATE: 26/02/08 10:54:01 GMT FROM: Jochen Greiner at MPE <jcgrog(a)mpe.mpg.de> T. Preis (University of Innsbruck) & J. Greiner (MPE Garching) report: The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger 792237169 at 09:52:44 on 08 Feb. 2026 were automatically fitted for spectrum and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427; Berlato et al. 2019, ApJ 873, 60). The best-fit position is: RA(2000.0) = 96.2 deg Decl.(2000.0) = -14.5 deg The 1 sigma statistical error radius is 0.8 deg. We estimate an additional systematic error of 1 deg. Further details are available at: https://grb.mpe.mpg.de/grb/GRB260208412/ The Healpix map can be downloaded from: https://grb.mpe.mpg.de/grb/GRB260208412/healpix The location parameters are available as JSON at: https://grb.mpe.mpg.de/grb/GRB260208412/json View this GCN Circular online at https://gcn.nasa.gov/circulars/43639. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41742] GRB 260208B: Fermi GBM Final Real-time Localization
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43638 SUBJECT: GRB 260208B: Fermi GBM Final Real-time Localization DATE: 26/02/08 10:03:19 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 09:52:44 UT on 8 Feb 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260208B (trigger 792237169.910408 / 260208412). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 99.9, Dec = -13.1 (J2000 degrees, equivalent to J2000 06h 39m, -13d 05'), with a statistical uncertainty of 1.0 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/bn260208412/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260208412/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260208412/… View this GCN Circular online at https://gcn.nasa.gov/circulars/43638. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 41741] Fermi GRB 260208A: Global MASTER-Net observations report
by GCN Circulars 08 Feb '26

08 Feb '26

TITLE: GCN CIRCULAR NUMBER: 43637 SUBJECT: Fermi GRB 260208A: Global MASTER-Net observations report DATE: 26/02/08 06:45:32 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 260208A ( Fermi GBM team, GCN 43635) errorbox 829 sec after notice time and 866 sec after trigger time at 2026-02-08 05:21:55 UT, with upper limit up to 17.9 mag. The observations began at zenith distance = 82 deg. The sun altitude is -43.2 deg. The galactic latitude b = 78 deg., longitude l = 64 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3125988 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 952 | 2026-02-08 05:21:55 | MASTER-OAFA | (13h 38m 21.97s , +33d 02m 05.7s) | C | 170 | 15.2 | 1073 | 2026-02-08 05:24:51 | MASTER-OAFA | (13h 38m 22.08s , +33d 02m 10.6s) | C | 60 | 15.9 | 1133 | 2026-02-08 05:24:51 | MASTER-OAFA | (13h 38m 22.14s , +33d 02m 11.3s) | C | 180 | 16.9 | Coadd 1139 | 2026-02-08 05:25:57 | MASTER-OAFA | (13h 38m 22.25s , +33d 02m 15.0s) | C | 60 | 16.1 | 1205 | 2026-02-08 05:27:02 | MASTER-OAFA | (13h 38m 22.38s , +33d 02m 19.9s) | C | 60 | 16.5 | 1271 | 2026-02-08 05:28:08 | MASTER-OAFA | (13h 38m 22.48s , +33d 02m 24.1s) | C | 60 | 16.6 | 1331 | 2026-02-08 05:28:08 | MASTER-OAFA | (13h 38m 22.48s , +33d 02m 24.0s) | C | 180 | 17.2 | Coadd 1336 | 2026-02-08 05:29:14 | MASTER-OAFA | (13h 38m 22.62s , +33d 02m 28.3s) | C | 60 | 16.7 | 1401 | 2026-02-08 05:30:19 | MASTER-OAFA | (13h 38m 22.73s , +33d 02m 32.6s) | C | 60 | 16.8 | 1467 | 2026-02-08 05:31:25 | MASTER-OAFA | (13h 38m 22.83s , +33d 02m 36.7s) | C | 60 | 17.0 | 1527 | 2026-02-08 05:31:25 | MASTER-OAFA | (13h 38m 22.83s , +33d 02m 36.7s) | C | 180 | 17.7 | Coadd 1532 | 2026-02-08 05:32:30 | MASTER-OAFA | (13h 38m 22.91s , +33d 02m 40.5s) | C | 60 | 17.1 | 1598 | 2026-02-08 05:33:36 | MASTER-OAFA | (13h 38m 22.99s , +33d 02m 44.5s) | C | 60 | 17.2 | 1664 | 2026-02-08 05:34:42 | MASTER-OAFA | (13h 38m 23.00s , +33d 02m 48.1s) | C | 60 | 17.2 | 1724 | 2026-02-08 05:34:42 | MASTER-OAFA | (13h 38m 23.01s , +33d 02m 48.1s) | C | 180 | 17.9 | Coadd 1730 | 2026-02-08 05:35:48 | MASTER-OAFA | (13h 38m 23.04s , +33d 02m 51.5s) | C | 60 | 17.2 | 1796 | 2026-02-08 05:36:53 | MASTER-OAFA | (13h 38m 23.05s , +33d 02m 54.5s) | C | 60 | 17.3 | 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/43637. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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