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

[vsnet-grb-info 38648] GRB 250602A: Fermi GBM Observation
by GCN Circulars 03 Jun '25

03 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40612 SUBJECT: GRB 250602A: Fermi GBM Observation DATE: 25/06/03 01:47:35 GMT FROM: Jacob Smith at Fermi-GBM Team <jrs0118(a)uah.edu> Jacob Smith (UAH) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: At 03:04:31.31 UT on 02 June 2025, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 250602A (trigger 770526276/250602128). which was also detected by Fermi-LAT (A. Holzmann Airasca, et al. 2025, GCN 40611). The Fermi GBM on-ground location is consistent with the Fermi-LAT position. The angle from the Fermi LAT boresight is 111 degrees. The GBM light curve consists of a single emission episode with a duration (T90) of about 14.6 s (50-300 keV). The time-averaged spectrum from T0+0.003 to T0+8.768 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.9 +/- 0.1 and the cutoff energy, parameterized as Epeak, is 120 +/- 10 keV. The event fluence (10-1000 keV) in this time interval is (1.7 +/- 0.1)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+0.0 s in the 10-1000 keV band is 5.8 +/- 0.3 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 102 +/- 22 keV, alpha = -0.7 +/- 0.3 and beta = -2.2 +/- 0.2. 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/40612. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38647] GRB 250602A: Fermi-LAT detection
by GCN Circulars 02 Jun '25

02 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40611 SUBJECT: GRB 250602A: Fermi-LAT detection DATE: 25/06/02 20:13:59 GMT FROM: Rahul Gupta at NASA GSFC <rahul.gupta(a)nasa.gov> A. Holzmann Airasca (UniTrento and INFN Bari), S. Lopez (CNRS / IN2P3), R. Gupta (NASA GSFC), F. Longo (University and INFN, Trieste), N. Di Lalla (Stanford Univ.), and J. Racusin (NASA GSFC) report on behalf of the Fermi-LAT Collaboration: On June 02, 2025, Fermi-LAT detected high-energy emission from GRB 250602A, which was also detected by Fermi-GBM (trigger 770526276 / 250602128, GCN 40602). The best LAT on-ground location is found to be: RA, Dec = 111.9, 56.9 (J2000) with an error radius of 0.4 deg (90 % containment, statistical error only). This was 111 deg from the LAT boresight at the time of the GBM trigger (T0 = 03:04:31.31 UT). The data from the Fermi-LAT shows a significant increase in the event rate that is spatially and temporally correlated with the GBM emission with high significance. The photon flux above 100 MeV in the time interval 3000 - 8000 s after the GBM trigger is (8.2 ± 3.2) E-7 ph/cm2/s. The estimated photon index above 100 MeV is -2.17 ± 0.33. The highest-energy photon is a 1.6 GeV event which is observed ~ 4800 seconds after the GBM trigger. The Fermi-LAT point of contact for this burst is Rahul Gupta (rahul.gupta(a)nasa.gov). 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/40611. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38646] GRB 250602A: DDOTI Optical Upper Limit
by GCN Circulars 02 Jun '25

02 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40610 SUBJECT: GRB 250602A: DDOTI Optical Upper Limit DATE: 25/06/02 19:56:39 GMT FROM: sahil.atri(a)students.uniroma2.eu Sahil Atri (U Roma), Rosa L. Becerra (U Roma), Alan M. Watson (UNAM), Camila Angulo Valdez (UNAM), Nat Butler (ASU), Simone Dichiara (Penn State University), Tsvetelina Dimitrova (ASU), Alexander Kutyrev (GSFC/UMD), William H. Lee (UNAM), Océlotl López (UNAM), Margarita Pereyra (UNAM) and Eleonora Troja (U Roma) report: We observed the field of GRB 250602A detected by Fermi/GBM (Fermi GBM Team, GCN Circ. 40602) with the DDOTI/OAN wide-field imager at the Observatorio Astronómico Nacional on Sierra San Pedro Mártir (http://ddoti.astroscu.unam.mx) on the night of 2025-06-02 UTC. DDOTI observed the Fermi/GBM error region, covering about 88% of the statistical error region (Fermi GBM Team, GCN Circ. 40602). DDOTI observed the field of GRB 250602A from 04:05 UTC to 06:05 UTC (from T+1.01 h to T+ 3.02 h after the trigger) and obtained a total exposure of 50 minutes, alternating with other scientific programs. Comparing our observations to the USNO-B1 and Pan-STARRS PS1 DR2 catalogues, we detect no uncatalogued fading sources within the observed field down to a 10-sigma limiting AB magnitude of: w > 20.0 This value is not corrected for the Galactic extinction. We thank the staff of the Observatorio Astronómico Nacional on the Sierra of San Pedro Mártir. View this GCN Circular online at https://gcn.nasa.gov/circulars/40610. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38645] GRB 250530C: Swift-BAT refined analysis
by GCN Circulars 02 Jun '25

02 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40609 SUBJECT: GRB 250530C: Swift-BAT refined analysis DATE: 25/06/02 19:11:33 GMT FROM: Mike Moss at NASA GSFC <mikejmoss3(a)gmail.com> D. Sadaula (GSFC/UMBC), S. D. Barthelmy (GSFC), R. Caputo (NASA/GSFC), R. Gupta (GSFC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), C. B. Markwardt (GSFC), M. J. Moss (GSFC), D. M. Palmer (LANL), T. Parsotan (GSFC), T. Sakamoto (AGU) (i.e. the Swift-BAT team): Using the data set from T-240 to T+885 sec from the recent telemetry downlink, we report further analysis of BAT GRB 250530C (trigger #1319125) (Caputo, et al., GCN Circ. 40585). The BAT ground-calculated position is RA, Dec = 55.146, -22.457 deg which is RA(J2000) = 03h 40m 35.1s Dec(J2000) = -22d 27' 26.1" with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment). The partial coding was 96%. The mask-weighted light curve displays a complex structure with multiple dim pulses. The T90 (15-350 keV) is 42.86 +- 6.04 sec (estimated error including systematics). The time-averaged spectrum from T-29.77 to T+21.26 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.32 +- 0.17. The fluence in the 15-150 keV band is 8.5 +- 0.9 x 10^-07 erg/cm2. The 1-sec peak photon flux measured from T-0.28 sec in the 15-150 keV band is 0.8 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at https://swift.gsfc.nasa.gov/results/batgrbcat/BAT_refined_circular/1319125 View this GCN Circular online at https://gcn.nasa.gov/circulars/40609. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38644] GRB 250521C: NOT spectroscopic observations exclude the afterglow candidate AT2025mgj
by GCN Circulars 02 Jun '25

02 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40608 SUBJECT: GRB 250521C: NOT spectroscopic observations exclude the afterglow candidate AT2025mgj DATE: 25/06/02 16:07:14 GMT FROM: Antonio Martin-Carrillo at UCD,Space Science Group <antonio.martin-carrillo(a)ucd.ie> A. Martin-Carrillo (UCD), B. Schneider (LAM), L. Izzo (INAF/OACN and DARK/NBI), A. de Ugarte Postigo (LAM), G. Corcoran (UCD), B. Gompertz (U. Birmingham), D. B. Malesani (DAWN/NBI and Radboud), R. H. Rasmussen (NOT and Aarhus Univ.), report on behalf of a larger collaboration. We carried out spectroscopic observations of AT2025mgj (Andreoni et al., GCN 40566), a candidate optical counterpart to GRB 250521C (Fermi GBM team, GCN 40515), using the ALFOSC camera mounted on the Nordic Optical Telescope (NOT). We obtained 4x900 s exposures starting at 21:16 UT on 2025-05-31 (10.3 days after the Fermi trigger) with a wavelength coverage of 3800-9500 AA. The spectrum shows a blue, featureless continuum, peaking at around 4500 AA. Redward of the peak, the continuum is consistent with a power law F_lambda propto lambda^-2.7. The overall shape does not resemble a power-law spectrum, which would be typical of GRB afterglows, nor a SN spectrum, given the lack of any features. Although the spectrum does not fully resemble those of dwarf novae in outbursts, the spectral energy distribution is overall consistent with previous examples (e.g. Aviles et al. 2018, doi:10.14482/INDES.30.1.303.661). In summary, our spectroscopic observations confirm that AT2025mgj is not associated with GRB250521C, as already suggested by Busmann et al. (GCN 40597) and Gillanders et al. (GCN 40605) based on photometric observations. View this GCN Circular online at https://gcn.nasa.gov/circulars/40608. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38643] GRB 250601A: EP-FXT follow-up observation and afterglow candidates
by GCN Circulars 02 Jun '25

02 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40607 SUBJECT: GRB 250601A: EP-FXT follow-up observation and afterglow candidates DATE: 25/06/02 15:46:51 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> Q. C. Liu (THU), X. Y. Zhou (PRIC), H. L. Peng (NNU), B. B. Zhang (BNU) and Y. Liu (NAO,CAS) report on behalf of the Einstein Probe (EP) team : We performed a follow-up observation of GRB 250601A (detected through on-broad trigger of Fermi/GBM, Fermi, GCN #40596, and localized by Swift/BAT, DeLaunay, GCN #40600; followed by Swift/XRT, Page et al., GCN #40604), with the Follow-up X-ray Telescope (FXT) on board the Einstein Probe (EP) mission. The observation began at 2025-06-02T02:10:26 (T-TGRB ~ 8.7 hrs) with an exposure time of about 5.8 ks. Two uncatalogued sources were detected by FXT-A and FXT-B in the 3-sigma Swift/BAT error circle with a radius of 493 arcsecond centered at RA, DEC = 90.0709 deg, -57.2892 deg, as listed below (the FXT flux is taken from FXT-B module). EP J060023.3-571631 has a separation of 11.6 arcsecond from the XRT source 3, and EP J060048.7-571413 has a separation of 4.8 arcsecond from the XRT source 2. Source name | RA | DEC | Estimated Flux | SNR | Dist from Swift/BAT | | deg | deg | (erg/s/cm^2) | | offset (in arcmin) | EP J060023.3-571631 | 90.0971 | -57.2752 | 3.2(+/-1.2) x 10^-14 | 4.1 | 1.19 | EP J060048.7-571413 * | 90.2037 | -57.2368 | 1.0(+/-0.2) x 10^-13 | 9.4 | 5.33 | Note: * EP J060048.7-571413 was also detected by Swift/XRT (GCN #40604) in a ~4.6 ks observation conducted at T-TGRB ~ 4.8 hrs, with a flux of ~ 4e-13 erg/s/cm^2. The source thus exhibits a decreasing trend in the X-ray flux within the two epochs. The above observation was made with the EP-FXT instrument. 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). EP is a mission of the Chinese Academy of Sciences in collaboration with ESA, MPE and CNES. View this GCN Circular online at https://gcn.nasa.gov/circulars/40607. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38642] GRB 250601A: Swift/XRT candidate afterglow
by GCN Circulars 02 Jun '25

02 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40606 SUBJECT: GRB 250601A: Swift/XRT candidate afterglow DATE: 25/06/02 15:13:44 GMT FROM: Chiara Salvaggio at INAF OABrera <chiara.salvaggio(a)inaf.it> C. Salvaggio (INAF-OAB), S. B. Cenko (GSFC), B. Sbarufatti (INAF-OAB) report on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the Fermi/GBM, Swift/BAT-GUANO detected burst GRB 250601A (GCN 40596, 40600). Two XRT sources have been previously reported in GCN 40604. One of the two sources (source 2) has an eROSITA counterpart, while XRT source 3 is a new transient. Therefore we consider source 3 a candidate afterglow for GRB 250601A. Source 3: RA (J2000.0): 90.0936 = 06:00:22.47 Dec (J2000.0): -57.2778 = -57:16:40.0 Error: 5.7 arcsec (radius, 90% conf.) Count-rate: (3.6 [+1.6, -1.3])e-3 ct s^-1 Distance: 60 arcsec from Swift/BAT position. Flux: (1.00 [+0.45, -0.35])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV) More Swift/XRT observations are planned to (un)confirm the afterglow detection. 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/00021844. This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/40606. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38641] GRB 250521C / AT2025mgj: Pan-STARRS multi-band and multi-epoch imaging and photometry
by GCN Circulars 02 Jun '25

02 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40605 SUBJECT: GRB 250521C / AT2025mgj: Pan-STARRS multi-band and multi-epoch imaging and photometry DATE: 25/06/02 15:01:40 GMT FROM: James Gillanders at University of Oxford <jhgillanders.astro(a)gmail.com> J. H. Gillanders (Oxford), M. Huber, K. C. Chambers (IfA, Univ. Hawaii), S. J. Smartt, K. W. Smith, (Oxford/QUB), S. Srivastav (Oxford), M. Nicholl, D. Young, M. Fulton (QUB), T.-W. Chen (NCU, Taiwan) A. S. B. Schultz, T. de Boer, J. Fairlamb, G. Paek, C. C. Lin, T. Lowe, E. Magnier, P. Minguez, I. A. Smith, R. J. Wainscoat (IfA, Univ. Hawaii). We observed the fast-fading transient AT2025mgj (Andreoni et al., GCN 40566), tentatively associated with the short-GRB 250521C (Fermi GBM Team, GCN 40515) using the Pan-STARRS telescope system (Chambers et al., 2016, arXiv e-prints, 1612.05560) on MJDs 60825.26 and 60827.26 (approximately 8.7 and 10.7 days post-GRB, respectively). The Pan-STARRS system consists of two 1.8m telescope units located at the summit of Haleakala on the Hawaiian island of Maui, employing an SDSS-like filter system denoted as grizy, and a broad w-filter, which is a composite of the gri-filters. Our observations consisted of 120s (MJD 60825.26) and 200s exposures (MJD 60827.26) in grizy-bands. All images were processed with the Pan-STARRS pipeline. After astrometric and photometric calibration, reference images were subtracted from the target images (Magnier et al., 2020a, ApJS, 251, 3; Magnier et al., 2020b, ApJS, 251, 6; Waters et al., 2020, ApJS, 251, 4). From these difference images, we recover the following photometry measurements: MJD Filter AB mag 60825.26 g 18.97 +/- 0.06 60825.26 r 19.18 +/- 0.08 60825.26 i 19.29 +/- 0.08 60825.26 z 19.5 +/- 0.2 60827.26 g 19.29 +/- 0.05 60827.26 r 19.39 +/- 0.06 60827.26 i 19.62 +/- 0.06 60827.26 z 19.57 +/- 0.08 From our multi-band Pan-STARRS photometry, we estimate a fade rate of ~0.1 mag/day in r-band. Our rate of fading across our photometric bands match those reported previously by Martin-Carrillo et al. (GCN 40584), Becerra et al. (GCN 40590), and Busmann et al. (GCN 40597). The rate of fading and persistent blue colour, with some indication of cooling, are all reminiscent of typical CV behaviour. While the connection to GRB 250521C cannot be definitively ruled out, the data match the lightcurve behaviour of CVs. Late-time, deep imaging is required to unambiguously uncover the nature of AT2025mgj. A point source would confirm AT2025mgj is indeed a CV, whereas an extended source in its vicinity would indicate that it was the afterglow of GRB 250521C. View this GCN Circular online at https://gcn.nasa.gov/circulars/40605. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38640] GRB 250601A: Swift-XRT observations
by GCN Circulars 02 Jun '25

02 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40604 SUBJECT: GRB 250601A: Swift-XRT observations DATE: 25/06/02 08:18:00 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), R. Brivio (INAF-OAB), A. D'Ai (INAF-IASFPA), S. Campana (INAF-OAB), S. Dichiara (PSU), 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 Swift/BAT-detected burst GRB 250601A, collecting 4.6 ks of Photon Counting (PC) mode data between T0+17.2 ks and T0+35.3 ks. Two uncatalogued X-ray sources have been detected within the estimated 3-sigma Swift/BAT error region (493 arcsec), however none of them is above the RASS limit or shows definitive signs of fading. Therefore, at the present time we cannot identify which, if any, is the afterglow. Details of these sources are given below: Source 2: RA (J2000.0): 90.2023 = 06:00:48.56 Dec (J2000.0): -57.2379 = -57:14:16.6 Error: 7.3 arcsec (radius, 90% conf. [Enhanced position]) Count-rate: (7.8 +/- 1.9)e-3 ct s^-1 Distance: 315 arcsec from Swift/BAT position. Flux: (4.2 +/- 1.0)e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV) Source 3: RA (J2000.0): 90.0936 = 06:00:22.47 Dec (J2000.0): -57.2778 = -57:16:40.0 Error: 5.7 arcsec (radius, 90% conf.) Count-rate: (3.6 [+1.6, -1.3])e-3 ct s^-1 Distance: 60 arcsec from Swift/BAT position. Flux: (1.00 [+0.45, -0.35])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV) Another uncatalogued source was also detected, however this was too far from the GRB position to be the 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/00021844. This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/40604. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38639] Fermi GRB 250601A: Global MASTER-Net observations report
by GCN Circulars 02 Jun '25

02 Jun '25

TITLE: GCN CIRCULAR NUMBER: 40603 SUBJECT: Fermi GRB 250601A: Global MASTER-Net observations report DATE: 25/06/02 04:45:45 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 250601A ( Fermi GBM team, GCN 40596) errorbox 31266 sec after notice time and 31297 sec after trigger time at 2025-06-02 02:11:13 UT, with upper limit up to 18.8 mag. The observations began at zenith distance = 80 deg. The sun altitude is -41.7 deg. The galactic latitude b = -31 deg., longitude l = 264 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2888853 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 31328 | 2025-06-02 02:11:13 | MASTER-SAAO | (05h 23m 33.62s , -61d 25m 21.7s) | C | 60 | 18.1 | 31328 | 2025-06-02 02:11:13 | MASTER-SAAO | (05h 27m 12.25s , -61d 40m 47.0s) | C | 60 | 16.8 | 32079 | 2025-06-02 02:23:44 | MASTER-SAAO | (05h 23m 32.93s , -61d 25m 26.3s) | C | 60 | 18.2 | 32079 | 2025-06-02 02:23:44 | MASTER-SAAO | (05h 27m 11.81s , -61d 40m 51.9s) | C | 60 | 16.9 | 32832 | 2025-06-02 02:36:17 | MASTER-SAAO | (05h 23m 35.76s , -61d 24m 34.2s) | C | 60 | 18.2 | 32832 | 2025-06-02 02:36:17 | MASTER-SAAO | (05h 27m 14.94s , -61d 39m 58.9s) | C | 60 | 16.9 | 32926 | 2025-06-02 02:37:51 | MASTER-SAAO | (05h 01m 57.98s , -57d 37m 48.3s) | C | 60 | 18.3 | 32926 | 2025-06-02 02:37:51 | MASTER-SAAO | (05h 05m 13.56s , -57d 53m 13.1s) | C | 60 | 16.9 | 33492 | 2025-06-02 02:47:17 | MASTER-SAAO | (05h 23m 29.69s , -61d 25m 33.6s) | C | 60 | 18.3 | 33492 | 2025-06-02 02:47:17 | MASTER-SAAO | (05h 27m 09.27s , -61d 40m 57.8s) | C | 60 | 16.9 | 33586 | 2025-06-02 02:48:51 | MASTER-SAAO | (05h 01m 58.51s , -57d 38m 06.3s) | C | 60 | 18.6 | 33586 | 2025-06-02 02:48:51 | MASTER-SAAO | (05h 05m 14.44s , -57d 53m 30.3s) | C | 60 | 17.1 | 33679 | 2025-06-02 02:50:24 | MASTER-SAAO | (05h 17m 04.95s , -57d 38m 12.0s) | C | 60 | 18.3 | 33679 | 2025-06-02 02:50:24 | MASTER-SAAO | (05h 20m 20.73s , -57d 53m 36.1s) | C | 60 | 17.0 | 34244 | 2025-06-02 02:59:49 | MASTER-SAAO | (05h 23m 26.94s , -61d 25m 56.2s) | C | 60 | 18.2 | 34348 | 2025-06-02 03:01:33 | MASTER-SAAO | (05h 01m 56.88s , -57d 38m 26.6s) | C | 60 | 18.6 | 34348 | 2025-06-02 03:01:33 | MASTER-SAAO | (05h 05m 13.07s , -57d 53m 50.3s) | C | 60 | 17.2 | 34441 | 2025-06-02 03:03:06 | MASTER-SAAO | (05h 17m 02.63s , -57d 38m 31.9s) | C | 60 | 18.3 | 34441 | 2025-06-02 03:03:06 | MASTER-SAAO | (05h 20m 18.63s , -57d 53m 56.0s) | C | 60 | 17.0 | 35007 | 2025-06-02 03:12:32 | MASTER-SAAO | (05h 23m 27.32s , -61d 26m 18.0s) | C | 60 | 18.4 | 35101 | 2025-06-02 03:14:06 | MASTER-SAAO | (05h 01m 55.99s , -57d 38m 46.4s) | C | 60 | 18.6 | 35101 | 2025-06-02 03:14:06 | MASTER-SAAO | (05h 05m 12.55s , -57d 54m 10.0s) | C | 60 | 17.2 | 35194 | 2025-06-02 03:15:39 | MASTER-SAAO | (05h 17m 02.39s , -57d 38m 52.0s) | C | 60 | 18.4 | 35194 | 2025-06-02 03:15:39 | MASTER-SAAO | (05h 20m 18.72s , -57d 54m 16.2s) | C | 60 | 17.0 | 35288 | 2025-06-02 03:17:13 | MASTER-SAAO | (05h 02m 24.56s , -54d 08m 10.8s) | C | 60 | 17.0 | 35381 | 2025-06-02 03:18:46 | MASTER-SAAO | (05h 12m 59.55s , -53d 50m 37.6s) | C | 60 | 18.5 | 35381 | 2025-06-02 03:18:46 | MASTER-SAAO | (05h 15m 57.34s , -54d 06m 02.3s) | C | 60 | 16.7 | 35661 | 2025-06-02 03:23:26 | MASTER-SAAO | (05h 11m 01.98s , -51d 56m 40.6s) | C | 60 | 18.5 | 35661 | 2025-06-02 03:23:26 | MASTER-SAAO | (05h 13m 52.04s , -52d 12m 05.7s) | C | 60 | 16.8 | 35757 | 2025-06-02 03:25:02 | MASTER-SAAO | (05h 01m 55.75s , -57d 41m 01.1s) | C | 60 | 18.6 | 35757 | 2025-06-02 03:25:02 | MASTER-SAAO | (05h 05m 12.76s , -57d 56m 25.1s) | C | 60 | 17.3 | 35851 | 2025-06-02 03:26:36 | MASTER-SAAO | (05h 17m 02.21s , -57d 39m 55.6s) | C | 60 | 18.5 | 35851 | 2025-06-02 03:26:36 | MASTER-SAAO | (05h 20m 18.88s , -57d 55m 20.0s) | C | 60 | 17.2 | 36038 | 2025-06-02 03:29:43 | MASTER-SAAO | (05h 12m 58.98s , -53d 52m 22.2s) | C | 60 | 18.4 | 36038 | 2025-06-02 03:29:43 | MASTER-SAAO | (05h 15m 56.70s , -54d 07m 48.0s) | C | 60 | 17.0 | 36318 | 2025-06-02 03:34:23 | MASTER-SAAO | (05h 11m 01.70s , -51d 56m 54.3s) | C | 60 | 18.7 | 36318 | 2025-06-02 03:34:23 | MASTER-SAAO | (05h 13m 51.53s , -52d 12m 20.2s) | C | 60 | 17.0 | 36411 | 2025-06-02 03:35:56 | MASTER-SAAO | (05h 24m 08.15s , -51d 57m 10.8s) | C | 60 | 18.4 | 36411 | 2025-06-02 03:35:56 | MASTER-SAAO | (05h 26m 57.92s , -52d 12m 36.4s) | C | 60 | 17.0 | 36504 | 2025-06-02 03:37:29 | MASTER-SAAO | (05h 05m 10.11s , -57d 56m 43.4s) | C | 60 | 17.4 | 36504 | 2025-06-02 03:37:29 | MASTER-SAAO | (05h 01m 53.17s , -57d 41m 19.2s) | C | 60 | 18.7 | 36597 | 2025-06-02 03:39:02 | MASTER-SAAO | (05h 20m 17.51s , -57d 55m 46.9s) | C | 60 | 17.3 | 36597 | 2025-06-02 03:39:02 | MASTER-SAAO | (05h 17m 00.88s , -57d 40m 22.3s) | C | 60 | 18.6 | 36784 | 2025-06-02 03:42:09 | MASTER-SAAO | (05h 15m 55.94s , -54d 07m 49.4s) | C | 60 | 17.0 | 36784 | 2025-06-02 03:42:09 | MASTER-SAAO | (05h 12m 57.97s , -53d 52m 23.8s) | C | 60 | 18.6 | 36973 | 2025-06-02 03:45:18 | MASTER-SAAO | (05h 04m 12.35s , -56d 01m 02.3s) | C | 60 | 17.5 | 36973 | 2025-06-02 03:45:18 | MASTER-SAAO | (05h 01m 05.36s , -55d 45m 37.7s) | C | 60 | 18.8 | 37066 | 2025-06-02 03:46:51 | MASTER-SAAO | (05h 13m 57.11s , -52d 13m 36.4s) | C | 60 | 17.2 | 37066 | 2025-06-02 03:46:51 | MASTER-SAAO | (05h 11m 06.80s , -51d 58m 10.9s) | C | 60 | 18.7 | 37159 | 2025-06-02 03:48:24 | MASTER-SAAO | (05h 26m 51.17s , -52d 13m 53.2s) | C | 60 | 17.1 | 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/40603. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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