June 2025 - vsnet-grb-info - ooruri.kusastro.kyoto-u.ac.jp

[vsnet-grb-info 38687] The EP-WXT trigger 01709178244 is likely a flaring star
by GCN Circulars 08 Jun '25

08 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40649 SUBJECT: The EP-WXT trigger 01709178244 is likely a flaring star DATE: 25/06/08 05:41:59 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> D. F. Hu (PMO, CAS), Q. C. Liu (THU), B. B. Zhang (BNU), Y. Liu (NAO, CAS) on behalf of the Einstein Probe (EP) team: The EP-WXT trigger 01709178244 at the time of 2025-06-08T04:53:30 (UTC), is likely a stellar flare associated with Gaia DR3 6730332160799599744. The estimated flux of the flare is around 1.6 x 10^-10 erg/s/cm^2 in 0.5-4 keV, corresponding to an X-ray luminosity of around 3.3 x 10^32 erg/s. 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/40649. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38686] GRB 250607A: Fermi GBM Final Localization
by GCN Circulars 07 Jun '25

07 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40648 SUBJECT: GRB 250607A: Fermi GBM Final Localization DATE: 25/06/07 15:22:38 GMT FROM: rhamburg(a)usra.edu The Fermi GBM team reports the detection of a likely LONG GRB. "At 14:00:55.64 UT on 07 June 2025, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 250607A (trigger 770997660/250607584). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 243.84, Dec = -24.71 (J2000 degrees, equivalent to J2000 16h 15m, -24d 42'), with a statistical uncertainty of 10.15 degrees. The angle from the Fermi LAT boresight is 90 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2025/bn250607584/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2025/bn250607584/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2025/bn250607584/…" View this GCN Circular online at https://gcn.nasa.gov/circulars/40648. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38685] EP-WXT trigger 01709178069: confirmation of a stellar flare by BOOTES-6 & BOOTES-7
by GCN Circulars 07 Jun '25

07 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40647 SUBJECT: EP-WXT trigger 01709178069: confirmation of a stellar flare by BOOTES-6 & BOOTES-7 DATE: 25/06/07 11:28:27 GMT FROM: I. Perez-Garcia at Institute of Astrophysics of Andalusia <ipg(a)iaa.es> I. Perez-Garcia, S.-Y. Wu, A. J. Castro-Tirado, E. J. Fernandez-Garcia, M.D. Caballero-Garcia, S. Guziy, G. Garcia-Segura, R. Sanchez-Ramirez (IAA-CSIC), Y.-D. Hu (INAF-OAB), C. Perez del Pulgar, A. Castellon, I. Carrasco (Univ. de Malaga), L. Hernandez-Garcia (Univ. de Valparaiso), M. Gritsevich (Univ. of Helsinki), D.-R. Xiong (Yunnan Observatories of CAS), B.-B. Zhang (Nanjing Univ.) and A. Maury (Space, San Pedro de Atacama), on behalf of a larger collaboration, report: Following the detection of trigger 01709178069 by EP-WXT (Hu et al. GCN 40646), both the 0.6m robotic telescopes BOOTES-6/DPRT 0.6m at Boyden Observatory in Maselspoort (South Africa) and BOOTES-7 at San Pedro de Atacama (Chile) responded to the alert on June 7, 23:45 UT (i.e. 2 min after notification and 7 min after the detection). Within the reported EP-FXT error circle we find the star UCAC4 204-077663 decreasing 0.25 mag in brightness (clear filter) during a 30 min time interval. Subsequent observations using the g filter and starting on June 8, 00:23 we find a decrease in 0.7 mag during a 2 hour time interval, confirming the EP X-ray trigger due to a stellar flare. We thank the staff at San Pedro de Atacama Celestial Observations and Boyden Observatory for their excellent support. View this GCN Circular online at https://gcn.nasa.gov/circulars/40647. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38684] The EP-WXT trigger 01709178069 is likely a flaring star
by GCN Circulars 07 Jun '25

07 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40646 SUBJECT: The EP-WXT trigger 01709178069 is likely a flaring star DATE: 25/06/07 01:58:34 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> D. F. Hu, Y. Wang (PMO, CAS), H. Sun, W. D. Zhang (NAO, CAS) on behalf of the Einstein Probe (EP) team: The EP-WXT trigger 01709178069 at the time of 2025-06-06T23:38:19 (UTC), is likely a stellar flare associated with UCAC4 204-077663. The estimated flux of the flare is around 8 x 10^-11 erg/s/cm^2 in 0.5-4 keV, corresponding to an X-ray luminosity of around 1.1 x 10^32 erg/s. 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/40646. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38682] GRB 250605A: VT optical upper limit
by GCN Circulars 06 Jun '25

06 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40645 SUBJECT: GRB 250605A: VT optical upper limit DATE: 25/06/06 15:40:20 GMT FROM: Huali Li at at NAOC, SVOM <lhl(a)nao.cas.cn> L. P. Xin, Y. L. Qiu, H. L. Li, C. Wu, X. H. Han, J. Wang, Y. Xu, P. P. Zhang, Z. H. Yao, Y. N. Ma, 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 conducted ToO follow-up observations of the GRB 250605A (Gupta et al., GCN 40633, Melandri et al., GCN 40644). The observation started on 2025-06-06T05:02:39 UT in VT_B (400nm-650nm) and VT_R (650nm-1000nm) channels simultaneously. No uncatalogued sources are detected in single or stacked images within the Swift/XRT error box (Evans et al., GCN 40642) and the possible optical candidate reported by Gompertz et al. (GCN 40634). The 3 sigma limit magnitudes are derived as below: Mid time | Band | Exposure Time | 3 sigma limit magnitude 11.28 hour VT_B 59*70 sec >23.6 mag 11.28 hour VT_R 59*70 sec >23.6 mag 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/40645. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38683] GRB 250605A: VT optical upper limit
by GCN Circulars 06 Jun '25

06 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40645 SUBJECT: GRB 250605A: VT optical upper limit DATE: 25/06/06 15:40:20 GMT FROM: Huali Li at at NAOC, SVOM <lhl(a)nao.cas.cn> L. P. Xin, Y. L. Qiu, H. L. Li, C. Wu, X. H. Han, J. Wang, Y. Xu, P. P. Zhang, Z. H. Yao, Y. N. Ma, 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 conducted ToO follow-up observations of the GRB 250605A (Gupta et al., GCN 40633, Melandri et al., GCN 40644). The observation started on 2025-06-06T05:02:39 UT in VT_B (400nm-650nm) and VT_R (650nm-1000nm) channels simultaneously. No uncatalogued sources are detected in single or stacked images within the Swift/XRT error box (Evans et al., GCN 40642) and the possible optical candidate reported by Gompertz et al. (GCN 40634). The 3 sigma limit magnitudes are derived as below: Mid time | Band | Exposure Time | 3 sigma limit magnitude 11.28 hour VT_B 59*70 sec >23.6 mag 11.28 hour VT_R 59*70 sec >23.6 mag 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/40645. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38681] GRB 250605A: Swift-XRT refined Analysis
by GCN Circulars 06 Jun '25

06 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40644 SUBJECT: GRB 250605A: Swift-XRT refined Analysis DATE: 25/06/06 11:02:50 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> A. Melandri (INAF-OAR), T. Sbarrato (INAF-OAB), P. D'Avanzo (INAF-OAB), M.A. Williams (PSU), S. Dichiara (PSU), J.A. Kennea (PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 7.0 ks of XRT data for GRB 250605A, from 90 s to 50.2 ks after the trigger. The data comprise 149 s in Windowed Timing (WT) mode (the first 6 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The light curve can be modelled with a series of power-law decays. The initial decay index is alpha=4.36 (+0.19, -0.15). At T+164 s the decay flattens to an alpha of 3.19 (+0.29, -0.32) before breaking again at T+326 s to a final decay with index alpha=0.79 (+/-0.07). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.12 (+0.06, -0.05). The best-fitting absorption column is 2.59 (+0.20, -0.19) x 10^21 cm^-2, in excess of the Galactic value of 4.3 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 2.10 (+0.13, -0.12) and a best-fitting absorption column of 2.9 (+/-0.5) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.6 x 10^-11 (5.5 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 2.9 (+/-0.5) x 10^21 cm^-2 Galactic foreground: 4.3 x 10^20 cm^-2 Excess significance: 8.7 sigma Photon index: 2.10 (+0.13, -0.12) If the light curve continues to decay with a power-law decay index of 0.79, the count rate at T+24 hours will be 0.085 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.0 x 10^-12 (4.7 x 10^-12) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01321323. This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/40644. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38680] EP/WXT 01709177873: GOTO observations confirm stellar variability
by GCN Circulars 06 Jun '25

06 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40643 SUBJECT: EP/WXT 01709177873: GOTO observations confirm stellar variability DATE: 25/06/06 10:10:51 GMT FROM: Amit Kumar at Royal Holloway - UoL/ U of Warwick, UK <amitkundu515(a)gmail.com> A. Kumar, D. O'Neill, G. Ramsay, B. P. Gompertz, R. Starling, K. Ackley, M. J. Dyer, J. Lyman, K. Ulaczyk, B. Godson, D. Steeghs, D. K. Galloway, V. Dhillon, P. O'Brien, K. Noysena, R. Kotak, R. P. Breton, L. K. Nuttall, and J. Casares report on behalf of the 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 EP/WXT alert 01709177873. Targeted observations were performed beginning at 2025-06-05 21:27:07 UT (+2.59 hr post trigger) and continued through to 2025-06-05 23:43:10 UT (+4.86 hr post trigger). 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. 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. No new transients associated with the alert were identified, except for one source within the localisation region: RX J1553.0+4457, a low mass star + white binary at RA = 15:53:04.8, Dec = +44:57:44.6. This source exhibited significant variability, brightening by ~0.6 mag relative to the last pre-trigger image taken on 2025-05-30 at 00:18:22 UT (6.77 days pre-trigger), reaching 13.70 ± 0.01 mag in the first post-trigger image at 2025-06-05 21:27:07 UT (+2.59 hr). It then faded to 14.10  ±  0.01 mag by the final observation at 2025-06-05 23:43:10 UT (+4.86 hr post-trigger). All the reported magnitudes are in the GOTO L-band and the AB system. Magnitudes were calibrated using ATLAS-REFCAT2 (Tonry et al. 2018) and are not corrected for Galactic extinction. 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 and the Instituto de Astrofisica de Canarias (IAC). View this GCN Circular online at https://gcn.nasa.gov/circulars/40643. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38679] GRB 250605A: Enhanced Swift-XRT position
by GCN Circulars 06 Jun '25

06 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40642 SUBJECT: GRB 250605A: Enhanced Swift-XRT position DATE: 25/06/06 08:44:00 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) report on behalf of the Swift-XRT team. Using 3740 s of XRT Photon Counting mode data and 7 UVOT images for GRB 250605A, we find an astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 166.95715, -19.78841 which is equivalent to: RA (J2000): 11h 07m 49.72s Dec (J2000): -19d 47' 18.3" with an uncertainty of 2.0 arcsec (radius, 90% confidence). This position may be improved as more data are received. The latest position can be viewed at http://www.swift.ac.uk/xrt_positions. Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular was automatically generated, and is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/40642. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38678] Fermi GRB 250606A: Global MASTER-Net observations report
by GCN Circulars 06 Jun '25

06 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40641 SUBJECT: Fermi GRB 250606A: Global MASTER-Net observations report DATE: 25/06/06 06:31:54 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-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 250606A ( Fermi GBM team, GCN 40640) errorbox 91 sec after trigger time at 2025-06-06 04:30:12 UT, with upper limit up to 19.3 mag. Observations started at twilight. The observations began at zenith distance = 50 deg. The sun altitude is -13.2 deg. MASTER-OAFA robotic telescope located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 250606A errorbox 133 sec after trigger time at 2025-06-06 04:30:55 UT, with upper limit up to 19.0 mag. The observations began at zenith distance = 69 deg. The sun altitude is -81.6 deg. The galactic latitude b = -38 deg., longitude l = 298 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2894070 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 101 | 2025-06-06 04:30:12 | MASTER-SAAO | (02h 08m 41.74s , -77d 25m 10.8s) | C | 20 | 18.5 | 136 | 2025-06-06 04:30:12 | MASTER-SAAO | (02h 08m 41.71s , -77d 25m 10.8s) | C | 90 | 19.3 | Coadd 101 | 2025-06-06 04:30:12 | MASTER-SAAO | (02h 17m 05.10s , -77d 40m 08.2s) | C | 20 | 18.4 | 136 | 2025-06-06 04:30:12 | MASTER-SAAO | (02h 17m 05.14s , -77d 40m 08.2s) | C | 90 | 19.2 | Coadd 145 | 2025-06-06 04:30:51 | MASTER-SAAO | (02h 08m 41.54s , -77d 25m 10.8s) | C | 30 | 18.7 | 145 | 2025-06-06 04:30:51 | MASTER-SAAO | (02h 17m 04.94s , -77d 40m 08.4s) | C | 30 | 18.6 | 149 | 2025-06-06 04:30:55 | MASTER-OAFA | (02h 17m 57.07s , -77d 44m 13.6s) | C | 30 | 16.1 | 185 | 2025-06-06 04:31:31 | MASTER-OAFA | (02h 17m 56.58s , -77d 44m 12.6s) | C | 30 | 15.8 | 199 | 2025-06-06 04:31:40 | MASTER-SAAO | (02h 08m 41.15s , -77d 25m 10.8s) | C | 40 | 18.9 | 199 | 2025-06-06 04:31:40 | MASTER-SAAO | (02h 17m 04.63s , -77d 40m 08.5s) | C | 40 | 18.8 | 226 | 2025-06-06 04:32:07 | MASTER-OAFA | (02h 17m 56.05s , -77d 44m 11.8s) | C | 40 | 16.1 | 263 | 2025-06-06 04:32:40 | MASTER-SAAO | (02h 08m 40.59s , -77d 25m 10.4s) | C | 50 | 18.9 | 263 | 2025-06-06 04:32:40 | MASTER-SAAO | (02h 17m 04.32s , -77d 40m 08.4s) | C | 50 | 18.8 | 277 | 2025-06-06 04:32:53 | MASTER-OAFA | (02h 17m 55.51s , -77d 44m 10.8s) | C | 50 | 17.0 | 337 | 2025-06-06 04:33:48 | MASTER-SAAO | (02h 08m 40.02s , -77d 25m 10.1s) | C | 60 | 18.9 | 337 | 2025-06-06 04:33:48 | MASTER-SAAO | (02h 17m 03.91s , -77d 40m 08.3s) | C | 60 | 18.8 | 376 | 2025-06-06 04:34:22 | MASTER-OAFA | (02h 17m 54.36s , -77d 44m 09.3s) | C | 70 | 16.6 | 457 | 2025-06-06 04:35:38 | MASTER-OAFA | (02h 17m 53.34s , -77d 44m 08.1s) | C | 80 | 16.0 | 552 | 2025-06-06 04:37:04 | MASTER-OAFA | (02h 17m 52.34s , -77d 44m 06.6s) | C | 100 | 17.2 | 633 | 2025-06-06 04:38:44 | MASTER-SAAO | (02h 01m 01.33s , -78d 21m 33.4s) | C | 60 | 18.4 | 693 | 2025-06-06 04:38:44 | MASTER-SAAO | (02h 01m 01.32s , -78d 21m 33.4s) | C | 180 | 18.9 | Coadd 633 | 2025-06-06 04:38:44 | MASTER-SAAO | (02h 10m 05.68s , -78d 36m 27.8s) | C | 60 | 18.2 | 693 | 2025-06-06 04:38:44 | MASTER-SAAO | (02h 10m 05.70s , -78d 36m 27.8s) | C | 180 | 18.9 | Coadd 702 | 2025-06-06 04:39:19 | MASTER-OAFA | (02h 10m 51.22s , -78d 38m 24.3s) | C | 130 | 17.1 | 712 | 2025-06-06 04:40:03 | MASTER-SAAO | (02h 01m 00.54s , -78d 21m 33.2s) | C | 60 | 18.2 | 712 | 2025-06-06 04:40:03 | MASTER-SAAO | (02h 10m 05.03s , -78d 36m 27.9s) | C | 60 | 18.1 | 791 | 2025-06-06 04:41:22 | MASTER-SAAO | (02h 00m 59.70s , -78d 21m 32.7s) | C | 60 | 18.1 | 791 | 2025-06-06 04:41:22 | MASTER-SAAO | (02h 10m 04.49s , -78d 36m 27.5s) | C | 60 | 17.9 | 849 | 2025-06-06 04:41:35 | MASTER-OAFA | (02h 10m 49.35s , -78d 38m 22.1s) | C | 150 | 17.0 | 870 | 2025-06-06 04:42:41 | MASTER-SAAO | (02h 00m 58.99s , -78d 21m 32.4s) | C | 60 | 17.8 | 870 | 2025-06-06 04:42:41 | MASTER-SAAO | (02h 10m 03.94s , -78d 36m 27.3s) | C | 60 | 17.8 | 1020 | 2025-06-06 04:44:12 | MASTER-OAFA | (02h 10m 47.45s , -78d 38m 19.3s) | C | 180 | 17.4 | 1206 | 2025-06-06 04:47:18 | MASTER-OAFA | (02h 10m 44.99s , -78d 38m 15.8s) | C | 180 | 14.2 | 3930 | 2025-06-06 05:32:42 | MASTER-OAFA | (02h 02m 27.41s , -77d 24m 58.8s) | C | 180 | 18.4 | 4117 | 2025-06-06 05:35:48 | MASTER-OAFA | (02h 02m 25.46s , -77d 24m 53.1s) | C | 180 | 18.4 | 4304 | 2025-06-06 05:38:55 | MASTER-OAFA | (02h 02m 23.74s , -77d 24m 48.4s) | C | 180 | 19.0 | 4490 | 2025-06-06 05:42:01 | MASTER-OAFA | (02h 02m 21.86s , -77d 24m 43.4s) | C | 180 | 18.9 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited. View this GCN Circular online at https://gcn.nasa.gov/circulars/40641. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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