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[vsnet-grb-info 42617] EP260507a: Kinder optical counterpart candidate
by GCN Circulars 07 May '26

07 May '26

TITLE: GCN CIRCULAR NUMBER: 44490 SUBJECT: EP260507a: Kinder optical counterpart candidate DATE: 26/05/07 15:19:55 GMT FROM: Janet Chen at National Central University <janetstars(a)gmail.com> A. Sankar.K, A. Aryan, Y.-H. Lee, T.-W. Chen, W.-J. Hou (all NCU), A. K. H. Kong (NTHU), S. J. Smartt, J. Gillanders (both Oxford), S. Yang(HNAS), M.-H. Lee, A. Dutta, K. N.-T. Ho, Y.-C. Pan, C.-C. Ngeow, C.-H. Lai, H.-C. Lin, H.-Y. Hsiao, C.-S. Lin, J.-K. Guo (all NCU), Z. N. Wang, D. C. Qiang, L. L. Fan (all HNAS), Y. J. Yang (NYUAD), H.-W. Lin (UMich), H. F. Stevance, S. Srivastav, L. Rhodes (all Oxford), M. Nicholl, M. Fulton, K. W. Smith, C. Angus, A. Aamer (all QUB), T. Moore (STScI), A. Schultz and M. Huber (both IfA, Hawaii) report: We observed the field of the fast X-ray transient EP260507a (Fu et al., GCN 44488) using the 40cm SLT at the Lulin Observatory in Taiwan as part of the Kinder collaboration (Chen & Yang et al., 2025, ApJ, 983, 86). The first SLT epoch of observations started at 14:06 UTC on 7th May 2026 (MJD 61167.5837), 0.30 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 using the 'SFFT' (Hu et al. 2022, ApJ, 936, 157) algorithm. In the stacked frame as well as in the difference image, we detect an uncatalogued optical counterpart candidate at RA, DEC = 13:47:35.567, -22:14:08.38 with an uncertainty of 1". The optical counterpart candidate is well inside the EP-FXT error circle of 20". The details of the observations and measured PSF magnitude with template subtraction (in the AB system) of the possible counterpart of EP260507a are as follows: -------------------------------------------------------------------------------------------------- Telescope | Filter | MJD (start) | t-t0 (hr) | Exposure (s) | Magnitude | avg. Seeing | med. Airmass SLT | r | 61167.5837 | 0.30 | 300 * 6 | 20.64 +/- 0.07 | 2".07 | 1.44 The presented magnitudes are calibrated using the field stars from ATLAS-RefCat2 catalog from MAST (Tonry J. L. et al. 2018, ApJ, 867, 105). The reported magnitudes/upper-limits are not corrected for an expected galactic extinction of A_r = 0.16 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/44490. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42616] EP260507a: LCO optical counterpart
by GCN Circulars 07 May '26

07 May '26

TITLE: GCN CIRCULAR NUMBER: 44489 SUBJECT: EP260507a: LCO optical counterpart DATE: 26/05/07 15:16:19 GMT FROM: Rob Eyles-Ferris at U of Leicester <raje1(a)leicester.ac.uk> G. Corcoran (UCD), R. A. J. Eyles-Ferris (Leicester), J. A. Chácon (PUC), J. N. D. van Dalen (Radboud), F. E. Bauer (SSI and UTA), P. G. Jonker (Radboud), A. J. Levan (Radboud & Warwick) and D. B. Malesani (DAWN/NBI and Radboud) report on behalf of a larger collaboration: We observed the field of the fast X-ray transient EP260507a (Fu et al., GCN 44488) using an LCO 1m telescope located at the Siding Spring Observatory (Australia) equipped with the SINISTRO instrument. We obtained 6x300s exposures in the SDSS-r filter starting at 2026-05-07 14:34:48 (~47 minutes after the trigger). Within the EP/FXT error region (Fu et al., GCN 44488), we detect a likely optical counterpart at a position of (J2000): RA 13:47:35.57 (206.89822) Dec -22:14:08.40 (-22.23566) We measure a magnitude of r = 21.21 +/- 0.07 (AB) calibrated to PanSTARRS and not corrected for Galactic extinction. View this GCN Circular online at https://gcn.nasa.gov/circulars/44489. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42615] EP260507a: Einstein Probe detection of an X-ray transient
by GCN Circulars 07 May '26

07 May '26

TITLE: GCN CIRCULAR NUMBER: 44488 SUBJECT: EP260507a: Einstein Probe detection of an X-ray transient DATE: 26/05/07 14:40:02 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> S. Y. Fu (HUST), Y. L. Wang (NAO, CAS; ICE, CSIC), C. L. Guo (NAO, CAS), X. Tian (GXU), 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 EP260507a. The transient triggered EP-WXT (ID: 01709261593) at 2026-05-07T13:47:57 (UTC). The WXT position of the source is R.A. = 206.895 deg, DEC = -22.243 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. = 206.8963 deg, DEC = -22.2361 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/44488. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42614] GRB 260504B: AstroSat CZTI detection
by GCN Circulars 07 May '26

07 May '26

TITLE: GCN CIRCULAR NUMBER: 44487 SUBJECT: GRB 260504B: AstroSat CZTI detection DATE: 26/05/07 14:19:14 GMT FROM: Anuraag Arya at IIT Bombay <aryaanuraag910(a)gmail.com> A. Goyal (IITB), A. Arya (IITB), Harsha K. H. (IUCAA), S. Salunke (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 GRB 260504B which is also detected by SVOM/GRM (Saccardi et al., GCN Circ. 44454), GECAM-B (Wang et al., GCN Circ. 44473), and Konus-Wind (Frederiks et. al., GCN Circ. 44474). The source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve peaks at 2026-05-04 09:31:16.450 UTC. The measured peak count rate associated with the burst is 1150 (+201, -203) counts/s above the background in the combined data of all four quadrants, with a total of 162 (+33, -36) counts. The local mean background count rate was 319 (+9, -11) counts/s. Using cumulative rates, we measure a T90 of 0.22 (+0.11, -0.07) 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/44487. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42613] GRB 260504B: SVOM/ECLAIRs refined analysis
by GCN Circulars 06 May '26

06 May '26

TITLE: GCN CIRCULAR NUMBER: 44486 SUBJECT: GRB 260504B: SVOM/ECLAIRs refined analysis DATE: 26/05/06 16:54:33 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> F. Piron (LUPM), M. Brunet (IRAP), N. Dagoneau (CEA), Y. Wang (PMO,CAS; UCB), W. J. Xie (NAO,CAS), 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 260504B (SVOM burst-id sb26050402 – GCN 44454, trigger time T0 = 2026-05-04T09:31:19 UTC), which was also detected by SVOM/GRM (GCN 44470), GECAM-B (GCN 44473) and Konus-Wind (GCN 44474). The burst that triggered ECLAIRs onboard shows a single peak lightcurve. The burst duration is T90 = 0.46 -0.06/+0.09 s in the 4-120 keV energy band. The time-averaged spectrum from T0+0.40 s to T0+0.86 s in the energy range 5-120 keV is best fitted by a powerlaw model with best-fit parameters: alpha = -0.72 +/-0.06. With this model, the 4-120 keV fluence is (1.87 ± 0.09) e-7 erg/cm^2 and the 4-120 keV photon flux is 6.0 ± 0.3 ph/cm²/s. We note that the photon index is consistent with the one found by SVOM/GRM (GCN 44470). 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: Frédéric Piron (LUPM) (piron at in2p3.fr) View this GCN Circular online at https://gcn.nasa.gov/circulars/44486. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42612] GRB 260506B: BALROG localization (Fermi Trigger 799765648 / GRB 260506547)
by GCN Circulars 06 May '26

06 May '26

TITLE: GCN CIRCULAR NUMBER: 44485 SUBJECT: GRB 260506B: BALROG localization (Fermi Trigger 799765648 / GRB 260506547) DATE: 26/05/06 14:01:40 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 799765648 at 13:07:23 on 06 May 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) = 280.7 deg Decl.(2000.0) = -6.1 deg The 1 sigma statistical error radius is 1.5 deg. We estimate an additional systematic error of 1 deg. Further details are available at: https://grb.mpe.mpg.de/grb/GRB260506547/ The Healpix map can be downloaded from: https://grb.mpe.mpg.de/grb/GRB260506547/healpix The location parameters are available as JSON at: https://grb.mpe.mpg.de/grb/GRB260506547/json View this GCN Circular online at https://gcn.nasa.gov/circulars/44485. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42611] GRB 260506B: BALROG localization (Fermi Trigger 799765648 / GRB 260506547)
by GCN Circulars 06 May '26

06 May '26

TITLE: GCN CIRCULAR NUMBER: 44485 SUBJECT: GRB 260506B: BALROG localization (Fermi Trigger 799765648 / GRB 260506547) DATE: 26/05/06 14:01:40 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 799765648 at 13:07:23 on 06 May 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) = 280.7 deg Decl.(2000.0) = -6.1 deg The 1 sigma statistical error radius is 1.5 deg. We estimate an additional systematic error of 1 deg. Further details are available at: https://grb.mpe.mpg.de/grb/GRB260506547/ The Healpix map can be downloaded from: https://grb.mpe.mpg.de/grb/GRB260506547/healpix The location parameters are available as JSON at: https://grb.mpe.mpg.de/grb/GRB260506547/json View this GCN Circular online at https://gcn.nasa.gov/circulars/44485. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42610] GRB 260506B: Fermi GBM Final Real-time Localization
by GCN Circulars 06 May '26

06 May '26

TITLE: GCN CIRCULAR NUMBER: 44484 SUBJECT: GRB 260506B: Fermi GBM Final Real-time Localization DATE: 26/05/06 13:18:06 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 13:07:23 UT on 6 May 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260506B (trigger 799765648.964258 / 260506547). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 280.5, Dec = -0.5 (J2000 degrees, equivalent to J2000 18h 41m, 0d 30'), with a statistical uncertainty of 1.8 degrees. The angle from the Fermi LAT boresight is 44.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260506547/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260506547/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260506547/… View this GCN Circular online at https://gcn.nasa.gov/circulars/44484. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42609] EP260502a is likely a flaring star
by GCN Circulars 06 May '26

06 May '26

TITLE: GCN CIRCULAR NUMBER: 44483 SUBJECT: EP260502a is likely a flaring star DATE: 26/05/06 10:24:37 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> T.Y. Liu (NAO,CAS), Y. Q. Zhao(PRIC,USTC), Y. F. Liang (PMO, CAS), Y. Wang (PMO, CAS; UCB), H. W. Pan (NAO,CAS) on behalf of the Einstein Probe (EP) team: The fast X-ray transient EP260502a (GCN #44440) at the time of 2026-05-02T06:08:51, is likely a stellar flare associated with SIPS J1809-7613. The estimated flux of the flare is around 1.1×10^(-9) erg/s/cm^2 in 0.5-4.0 keV, corresponding to an X-ray luminosity of around 9.8×10^(30) erg/s. The telemetry WXT data show that the flare started around 2026-05-02T05:58:08 (UTC) and exhibits no obvious flux variation later in the WXT exposure. The average WXT 0.5-4 keV spectrum of the burst period can be fitted with an absorbed power law with a hydrogen column density of 3.68×10^(-9)（-3.68×10^(-9)/+0.361 ）×10^22 cm^-2 and a photon index of 0.52(-0.52/+1.70). The derived average unabsorbed 0.5-4 keV flux is 9.96 (-3.89/+11.51) ×10^(-11) erg/s/cm^2. The Follow-up X-ray Telescope (FXT) on board EP observed this source at 2026-05-02T06:19:45 (UTC). The exposure time of this observation is 3.0ks. The flux show a rapid fading of around 5 times in 1ks. The average 0.5-10 keV spectrum can be fitted with an absorbed power law with a Galactic hydrogen column density of 0.66 (-0.21/+0.25) × 10^22 cm^-2 and a photon index of 5.44 (-1.02/+1.23). The derived average unabsorbed 0.5-10 keV flux is 8.29 (-4.61/+15.56) × 10^(-12) erg/s/cm^2. The optical follow-up observations were performed by Li et al. (GCN 44441), Sharma et al. (GCN 44442, GCN 44444), and catch a fading of 0.7mag of SIPS J1809-7613 in 30min starting from 2026-05-02 06:24:42, consistent with the X-ray fading detected by the FXT autumatic follow-up. A follow-up observation around 3ks with the EP/FXT was carried out starting at 2026-05-02T06:19:45, and no FXT trigger was received during the observation. 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/44483. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 42608] Fermi GRB 260506A: Global MASTER-Net observations report
by GCN Circulars 06 May '26

06 May '26

TITLE: GCN CIRCULAR NUMBER: 44482 SUBJECT: Fermi GRB 260506A: Global MASTER-Net observations report DATE: 26/05/06 07:00:25 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-OAGH robotic telescope [1] located in Mexico (OAGH National Institute for Astrophysics, Optics and Electronics) started inspect of the Fermi GRB 260506A ( Fermi GBM team, GCN 44481) errorbox 224 sec after notice time and 230 sec after trigger time at 2026-05-06 06:32:38 UT, with upper limit up to 19.3 mag. The observations began at zenith distance = 58 deg. The sun altitude is -41.5 deg. The galactic latitude b = 36 deg., longitude l = 136 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=3296217 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 260 | 2026-05-06 06:32:38 | MASTER-OAGH | (08h 44m 39.72s , +75d 23m 45.7s) | C | 60 | 18.5 | 260 | 2026-05-06 06:32:38 | MASTER-OAGH | (08h 37m 44.58s , +75d 59m 45.8s) | C | 60 | 18.7 | 333 | 2026-05-06 06:33:51 | MASTER-OAGH | (09h 16m 22.00s , +75d 24m 42.7s) | C | 60 | 18.8 | 333 | 2026-05-06 06:33:51 | MASTER-OAGH | (09h 09m 15.33s , +76d 01m 00.1s) | C | 60 | 18.9 | 406 | 2026-05-06 06:35:04 | MASTER-OAGH | (08h 52m 23.52s , +77d 19m 08.0s) | C | 60 | 19.1 | 406 | 2026-05-06 06:35:04 | MASTER-OAGH | (08h 44m 14.66s , +77d 55m 18.4s) | C | 60 | 19.3 | 479 | 2026-05-06 06:36:17 | MASTER-OAGH | (09h 28m 38.58s , +77d 18m 24.2s) | C | 60 | 18.3 | 479 | 2026-05-06 06:36:17 | MASTER-OAGH | (09h 20m 26.78s , +77d 54m 22.8s) | C | 60 | 18.6 | 553 | 2026-05-06 06:37:31 | MASTER-OAGH | (09h 32m 43.22s , +73d 30m 24.2s) | C | 60 | 18.8 | 553 | 2026-05-06 06:37:31 | MASTER-OAGH | (09h 26m 27.66s , +74d 06m 31.2s) | C | 60 | 18.9 | 626 | 2026-05-06 06:38:44 | MASTER-OAGH | (10h 00m 45.91s , +73d 28m 55.8s) | C | 60 | 18.7 | 626 | 2026-05-06 06:38:44 | MASTER-OAGH | (09h 54m 25.86s , +74d 05m 06.5s) | C | 60 | 19.0 | 699 | 2026-05-06 06:39:57 | MASTER-OAGH | (09h 44m 54.95s , +75d 25m 08.4s) | C | 60 | 19.0 | 699 | 2026-05-06 06:39:57 | MASTER-OAGH | (09h 37m 45.79s , +76d 01m 15.0s) | C | 60 | 19.2 | 773 | 2026-05-06 06:41:11 | MASTER-OAGH | (10h 16m 39.45s , +75d 23m 04.3s) | C | 60 | 19.0 | 773 | 2026-05-06 06:41:11 | MASTER-OAGH | (10h 09m 25.61s , +75d 59m 15.1s) | C | 60 | 19.2 | 1010 | 2026-05-06 06:45:08 | MASTER-OAGH | (08h 44m 32.03s , +75d 26m 03.2s) | C | 60 | 18.9 | 1010 | 2026-05-06 06:45:08 | MASTER-OAGH | (08h 37m 39.30s , +75d 57m 59.1s) | C | 60 | 18.9 | 1083 | 2026-05-06 06:46:21 | MASTER-OAGH | (09h 16m 23.42s , +75d 24m 39.6s) | C | 60 | 18.8 | 1083 | 2026-05-06 06:46:21 | MASTER-OAGH | (09h 09m 18.88s , +76d 00m 58.5s) | C | 60 | 19.0 | 1156 | 2026-05-06 06:47:34 | MASTER-OAGH | (08h 52m 15.20s , +77d 18m 04.3s) | C | 60 | 19.1 | 1156 | 2026-05-06 06:47:34 | MASTER-OAGH | (08h 44m 14.12s , +77d 54m 09.0s) | C | 60 | 19.1 | 1230 | 2026-05-06 06:48:47 | MASTER-OAGH | (09h 28m 45.20s , +77d 17m 37.2s) | C | 60 | 18.7 | 1230 | 2026-05-06 06:48:47 | MASTER-OAGH | (09h 20m 32.90s , +77d 53m 53.1s) | C | 60 | 19.0 | 1303 | 2026-05-06 06:50:00 | MASTER-OAGH | (09h 32m 40.96s , +73d 31m 11.3s) | C | 60 | 18.9 | 1303 | 2026-05-06 06:50:00 | MASTER-OAGH | (09h 26m 24.09s , +74d 07m 34.1s) | C | 60 | 19.0 | 1376 | 2026-05-06 06:51:14 | MASTER-OAGH | (10h 00m 49.53s , +73d 29m 34.1s) | C | 60 | 18.9 | 1376 | 2026-05-06 06:51:14 | MASTER-OAGH | (09h 54m 31.45s , +74d 05m 45.0s) | C | 60 | 19.2 | 1448 | 2026-05-06 06:52:26 | MASTER-OAGH | (09h 44m 56.50s , +75d 25m 43.2s) | C | 60 | 19.0 | 1448 | 2026-05-06 06:52:26 | MASTER-OAGH | (09h 37m 49.83s , +76d 01m 49.5s) | C | 60 | 19.1 | 1523 | 2026-05-06 06:53:41 | MASTER-OAGH | (10h 16m 36.92s , +75d 24m 10.7s) | C | 60 | 18.9 | 1523 | 2026-05-06 06:53:41 | MASTER-OAGH | (10h 09m 24.89s , +76d 00m 21.4s) | C | 60 | 19.3 | 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/44482. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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