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[vsnet-grb-info 42363] GRB 260407A: CALET Gamma-Ray Burst Monitor detection
by GCN Circulars 09 Apr '26

09 Apr '26

TITLE: GCN CIRCULAR NUMBER: 44242 SUBJECT: GRB 260407A: CALET Gamma-Ray Burst Monitor detection DATE: 26/04/09 03:43:44 GMT FROM: Yuta Kawakubo at Aoyama Gakuin University <kawakubo(a)phys.aoyama.ac.jp> M. L. Cherry (LSU), A. Yoshida, T. Sakamoto, S. Sugita, Y. Kawakubo (AGU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA), Y. Asaoka (ICRR), S. Torii, Y. Akaike, K. Kobayashi (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), N. Cannady (GSFC), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena), and the CALET collaboration: The long GRB 260407A (Fermi GBM Final Real-time Localization: Fermi GBM team, GCN Circ. 44226; Glowbug gamma-ray detection: Cheung et al., GCN Circ 44237) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 09:11:06.11 UTC on 7 April 2026 (https://cgbm.calet.jp/cgbm_trigger/flight/1459588274/index.html) The burst signal was seen by all CGBM detectors. The burst light curve shows a single pulse that starts at T-0.5 sec, peaks at T+1.6 sec, and ends at T+27.1 sec. The T90 and T50 durations measured by the SGM data are 22.6 +/- 5.0 sec and 7.0 +/- 1.0 sec (40-1000 keV), respectively. The ground-processed light curve is available at https://cgbm.calet.jp/cgbm_trigger/ground/1459588274 The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at Waseda University. View this GCN Circular online at https://gcn.nasa.gov/circulars/44242. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42362] EP260409a: Global MASTER-Net observations report
by GCN Circulars 09 Apr '26

09 Apr '26

TITLE: GCN CIRCULAR NUMBER: 44241 SUBJECT: EP260409a: Global MASTER-Net observations report DATE: 26/04/09 02:00:29 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) was pointed to the EP260409a ( EP Team et al., GCN 44240) errorbox 2305 sec after trigger time at 2026-04-09 00:56:46 UT, with upper limit up to 19.7 mag. The observations began at zenith distance = 36 deg. The sun altitude is -33.7 deg. The galactic latitude b = 49 deg., longitude l = 273 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3241458 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 2335 | 2026-04-09 00:56:46 | MASTER-OAFA | (11h 31m 41.72s , -09d 16m 57.1s) | C | 60 | 19.5 | 2401 | 2026-04-09 00:57:52 | MASTER-OAFA | (11h 31m 41.64s , -09d 16m 56.1s) | C | 60 | 19.7 | 2467 | 2026-04-09 00:58:58 | MASTER-OAFA | (11h 31m 41.57s , -09d 16m 55.4s) | C | 60 | 19.6 | 2533 | 2026-04-09 01:00:04 | MASTER-OAFA | (11h 31m 41.51s , -09d 16m 54.5s) | C | 60 | 19.7 | 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/44241. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42361] EP260409a: Einstein Probe detection of an X-ray transient
by GCN Circulars 09 Apr '26

09 Apr '26

TITLE: GCN CIRCULAR NUMBER: 44240 SUBJECT: EP260409a: Einstein Probe detection of an X-ray transient DATE: 26/04/09 01:55:16 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> S. Q. Jiang (NAO, CAS), G. L. Huang, Z. X. Li, J. Y. Cao (IHEP, CAS), W. D. Zhang (NAO, CAS) on behalf of the Einstein Probe (EP) team: We report on the detection of an X-ray transient by the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) mission, designated EP260409a. The transient triggered EP-WXT (ID: 01709259735) at 2026-04-09T00:18:21 (UTC). The WXT position of the source is R.A. = 172.895 deg, DEC = -9.348 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. = 172.9080 deg, DEC = -9.3442 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/44240. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42360] EP260321a: VLA radio detection
by GCN Circulars 09 Apr '26

09 Apr '26

TITLE: GCN CIRCULAR NUMBER: 44239 SUBJECT: EP260321a: VLA radio detection DATE: 26/04/09 01:06:49 GMT FROM: todwyer1(a)jh.edu Tanner O'Dwyer (JHU), Alessandra Corsi (JHU), Gokul Srinivasaragavan (UMD), S. Bradley Cenko (NASA GSFC), Shreya Anand (Stanford.U), Anna Ho (Cornell), Jesper Sollerman (U.Stockholm), Bei Zhou (FemiLab & U.Chicago), Marc Kamionkowski (JHU), Jillian Rastinejad (UMD) We observed the field of EP260321a (Huang et al., GCN 44068) with the Karl G. Jansky Very Large Array (VLA) in its A-configuration. Our observations were conducted at about 13.6 days post trigger at a nominal central frequency of 6 GHz. We report the detection of a radio source with a S/N of about 4 at a position compatible with that of SN 2026gzf (Corcoran et al., GCN 44105, Rastinejad et al., GCN 44107). Our image RMS is about 5 uJy. Further observations are planned to also evaluate potential contribution of the host galaxy to the observed emission. View this GCN Circular online at https://gcn.nasa.gov/circulars/44239. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42359] GRB 260404A: Fermi GBM Final Localization
by GCN Circulars 08 Apr '26

08 Apr '26

TITLE: GCN CIRCULAR NUMBER: 44238 SUBJECT: GRB 260404A: Fermi GBM Final Localization DATE: 26/04/08 19:07:24 GMT FROM: atrigg2(a)lsu.edu The Fermi GBM team reports the detection of a likely SHORT GRB "At 23:57:08.96 UT on 04 April 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260404A (trigger 797039833/260404998). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 165.79, Dec = -48.56 (J2000 degrees, equivalent to J2000 11h 03m, -48d 33'), with a statistical uncertainty of 18.12 degrees. The angle from the Fermi LAT boresight is 113 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260404998/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260404998/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260404998/…" View this GCN Circular online at https://gcn.nasa.gov/circulars/44238. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42358] GRB 260407A: Glowbug gamma-ray detection
by GCN Circulars 08 Apr '26

08 Apr '26

TITLE: GCN CIRCULAR NUMBER: 44237 SUBJECT: GRB 260407A: Glowbug gamma-ray detection DATE: 26/04/08 14:32:22 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 260407A, which was detected by Fermi/GBM (GCN 44226). Using an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2026-04-07 09:11:06.112 with a duration of 4.1 s and a total significance of about 9.6 sigma. The light curve comprises a single peak. Additional lower-level emission up to ~T0+10s, as well as earlier emission beginning ~T0-2s, may be present in the Glowbug light curve at low significance. 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 telescopes 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/44237. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42357] GRB 260402A: SVOM/ECLAIRs refined analysis
by GCN Circulars 08 Apr '26

08 Apr '26

TITLE: GCN CIRCULAR NUMBER: 44236 SUBJECT: GRB 260402A: SVOM/ECLAIRs refined analysis DATE: 26/04/08 13:04:28 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> M. Brunet, O.Godet (IRAP), W.-J. Xie (NAOC), W. Tan, R. Li (IHEP), report on behalf of the SVOM/ECLAIRs team Using the event-by-event data downloaded through the X-band ground station, we report further analysis of SVOM/ECLAIRs observations of GRB 260402A(SVOM burst-id sb26040203– GCN 44181, trigger time T0 = 2026-04-02T10:30:17 UTC), which was also detected by EP/WXT (GCN 44186). The burst that triggered ECLAIRs onboard shows a multiple peak lightcurve. The burst duration is T90 = (15.2 -3.9/+3.1) s in the 4-120 keV energy band. However, some emission is seen for 41 s from T0 up to T0 + 41 s in the 4-20 keV energy band through imaging. The time-averaged spectrum from T0 to T0+41s in the energy range 5-120 keV is best fitted by a powerlaw model with a photon index of -2.18 +0.09/-0.10. With this model, the 4-120 keV fluence is (5.40 +0.33/-0.57)e-7 erg/cm^2 and the 4-120 keV photon flux is 0.67 +0.03/-0.04 ph/cm^2/s. This GRB shows some spectral evolution. The spectrum from T0 to T0 + 1 s in the 5-120 keV energy range is best fitted by a power-law model with a photon index of -1.37 +/-0.12. With this model, the 4-120 keV flux is (8.9 +0.6/-1.7)e-8 erg/cm²/s. The spectrum from T0 + 1 s to T0 + 5 s in the 5-120 keV energy range is best fitted by a broken power-law model with the second photon index fixed at -3, which gives a first photon index of -0.85 +0.23/-0.20 and a break energy of 17.3 +2.0/-1.6 keV. With this model, the 4-120 keV flux is (4.6 +0.1/-1.1)e-8 erg/cm²/s. The spectrum from T0 + 5 s to T0 + 10 s in the 5-120 keV energy range is best fitted by a broken power-law model with the first photon index fixed at -0.85 and the second one fixed at -3, which gives a break energy of 8.6 +1.2/-0.8 keV. With this model, the 4-120 keV flux is (2.3 +0.1/-0.2)e-8 erg/cm²/s. The spectrum from T0 + 10 s to T0 + 41 s in the 5-50 keV energy range is best fitted by a power-law model with a photon index of -2.9 +0.3/-0.4. With this model, the 4-120 keV flux is (4.8 +0.3/-2.0)e-9 erg/cm²/s. 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) (mbrunet at utoulouse.fr) View this GCN Circular online at https://gcn.nasa.gov/circulars/44236. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42356] GRB 260310A: Continued VLA Multi-frequency Radio Observations
by GCN Circulars 08 Apr '26

08 Apr '26

TITLE: GCN CIRCULAR NUMBER: 44235 SUBJECT: GRB 260310A: Continued VLA Multi-frequency Radio Observations DATE: 26/04/08 02:27:55 GMT FROM: Genevieve Schroeder at Cornell University <genevieveschroeder(a)u.northwestern.edu> G. Schroeder (Cornell), D. A. Perley (LJMU), and T. Laskar (Utah) report on behalf of a larger collaboration: The Karl G. Jansky Very Large Array observed the location of the afterglow (Hinds et al., TNS AstroNote 2026-65; Konno et al., GCN 43974) associated with GRB 260310A (Fermi GBM Team, GCN 43951; Hamburg & Meegan, GCN 43975) using all available receivers from L-band to Q-band, providing nearly continuous spectral coverage from 1 to 50 GHz, as a part of our multi-frequency public campaign (Perley et al., GCN 44160). Observations were carried out on UT 2026-04-04 between 08:42 and 12:19 UT, approximately 25.2 days after the GRB. Preliminary flux densities are: | freq(GHz) | flux(mJy) | |-----------|----------------| | 1.5 | 1.74 +/- 0.06 | | 3 | 5.00 +/- 0.04 | | 6 | 8.39 +/- 0.05 | | 10 | 8.93 +/- 0.12 | | 15 | 8.16 +/- 0.22 | | 22 | 7.34 +/- 0.23 | | 33 | 6.14 +/- 0.19 | | 45 | 5.25 +/- 0.19 | Compared to previous radio observations (Rhodes et al., GCN 44005; Giarratana et al., GCN 44045; Ho et al., GCN 44057; Ho et al., GCN 44134, Perley et al., GCN 44160), the afterglow is brightening at lower frequencies (< 10 GHz) and fading at higher frequencies (> 10 GHz). We thank the NRAO staff for scheduling and executing these observations. Further observations are planned. View this GCN Circular online at https://gcn.nasa.gov/circulars/44235. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42355] GRB 260310A / AT2026fgk: X-ray rebrightening
by GCN Circulars 07 Apr '26

07 Apr '26

TITLE: GCN CIRCULAR NUMBER: 44234 SUBJECT: GRB 260310A / AT2026fgk: X-ray rebrightening DATE: 26/04/07 17:22:52 GMT FROM: Rahul Jayaraman at Cornell University <rj438(a)cornell.edu> Rahul Jayaraman (Cornell), K-Ryan Hinds (Caltech), Gaurav Waratkar (Caltech), S. Y. Fu (HUST), R. D. Liang, M. J. Liu, Z. X. Ling, Hui Sun, Weimin Yuan (NAO, CAS), Anna Y. Q. Ho (Cornell), Genevieve Schroeder (Cornell) report: The Follow-up X-ray Telescope (FXT) on board the Einstein Probe has continued to monitor the X-ray afterglow of GRB 260310A (Fermi GBM team, GCN 43951; Arya et al., GCN 43958; Jayaraman et al., GCN 43994), associated with the optical transient AT2026fgk (Konno et al., GCN 43974; Hinds et al., AstroNote 2026-65), with 10 epochs of observations since the GRB. After the detection of a clear break (near-simultaneous steepening in both the X-ray and optical; Jayaraman et al., GCN 44095; Perley et al., GCN 44096), we observed two further epochs that were consistent with the steeper slope of -1.6 reported in GCN 44095. However, the most recent three epochs (which span 3 days) show a clear rebrightening, with a power-law index of α = 2.9 ± 0.5, where f ~ t^α. Further follow-up with FXT is planned. Launched on January 9, 2024, the Einstein Probe is a space X-ray observatory to monitor the soft X-ray sky with X-ray follow-up capability (Yuan et al. 2022, Handbook of X-ray and Gamma-ray Astrophysics). EP is supported by the Strategic Priority Program on Space Sciénce of the Chinese Academy of Sciences, in collaboration with the European Space Agency, the Max-Planck-Institute for Extraterrestrial Physics (Germany), and the Centre National d'études Spatiales (France). View this GCN Circular online at https://gcn.nasa.gov/circulars/44234. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42354] EP260402a / GRB 260402A: Mephisto optical upper limits
by GCN Circulars 07 Apr '26

07 Apr '26

TITLE: GCN CIRCULAR NUMBER: 44233 SUBJECT: EP260402a / GRB 260402A: Mephisto optical upper limits DATE: 26/04/07 15:20:03 GMT FROM: Chenxu Liu at Mephisto Team <cxliu(a)ynu.edu.cn> Chenxi Shang, Chenxu Liu, Guowang Du (SWIFAR, YNU), Jinghang Xue (NJU), Yuhui Zhang, Jialei Zheng, Tao Wang, Brajesh Kumar, Xueling Du, Xufeng Zhu, Yu Pan, Xingzhu Zou, Xinlei Chen, Yuan Fang, Jinghua Zhang (SWIFAR, YNU), Chao Wu (NAOC), Yuanpei Yang, Xiangkun Liu, Xiaowei Liu (SWIFAR, YNU) report on behalf of the Mephisto Team: The 1.6-m Multi-channel Photometric Survey Telescope (Mephisto) of Yunnan University, located at the Lijiang Observatory, was triggered at 2026-04-02 19:52:10 UT (~9.4 hours after the Einstein Probe/WXT trigger; Zhao et al., GCN 44186) to observe the field of EP260402a. A set of simultaneous multi-band (u, g, v, r, i, z) images were collected with individual exposure times of 45 s per frame. Multiple exposures were obtained in each band and later stacked for analysis. The refined EP/FXT position (Zhao et al., GCN 44201) is fully covered by our field of view. Due to relatively poor seeing conditions during the observations (FWHM ~2.5–4.0 arcsec), the image quality is degraded compared to nominal performance, resulting in shallower limiting magnitudes. In our stacked images, no uncatalogued optical source is detected at the FXT position or within its error circle (radius ~10–20 arcsec). The corresponding 5-sigma limiting magnitudes (AB system, not corrected for Galactic extinction) are listed below: ---------------------------------------------------------------------------------------------- Start Time (UT) | Band | Exposure (s) | Mag / Limiting Mag ---------------------------------------------------------------------------------------------- 2026-04-02T19:52:10 | u | 45.0*2 | >19.77 2026-04-02T19:54:55 | v | 45.0*2 | >18.81 2026-04-02T19:52:23 | g | 45.0*2 | >20.21 2026-04-02T19:55:08 | r | 45.0*2 | >20.33 2026-04-02T19:52:13 | i | 45.0*2 | >20.23 2026-04-02T19:54:58 | z | 45.0*2 | >19.48 ---------------------------------------------------------------------------------------------- Our non-detection is consistent with previous optical and near-infrared upper limits reported by SVOM/COLIBRÍ (Antier et al., GCN 44183), MASTER (Carrasco et al., GCN 44184), Kilonova-Catcher (Freeberg et al., GCN 44185), SVOM/C-GFT (Wu et al., GCN 44189), SVOM/VT (Li et al., GCN 44190), WINTER (Schneider et al., GCN 44192), and Jinshan (He et al., GCN 44199). Mephisto (Multi-channel Photometric Survey Telescope) is a 1.6-m wide-field multi-channel telescope, the first of its type in the world, capable of imaging the same field of view in three optical bands simultaneously. The facility is operated by the South-Western Institute for Astronomy Research (SWIFAR), Yunnan University. It provides real-time, high-quality colors of stellar objects. The Mephisto mosaic cameras were installed in October 2025. The first light was achieved in all three channels on 10 October 2025 and presently, these are under the commissioning phase. All the data have been reduced by the Mephisto data processing pipeline. We note that the current data-processing pipeline is still at a preliminary stage, with flux calibration precision of about 2% in the u and v bands, about 1% in the g and r bands, and better than 1% in the i and z bands. View this GCN Circular online at https://gcn.nasa.gov/circulars/44233. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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