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

[vsnet-grb-info 39030] GRB 250704A: Swift/UVOT Detection
by GCN Circulars 05 Jul '25

05 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40981 SUBJECT: GRB 250704A: Swift/UVOT Detection DATE: 25/07/05 18:25:39 GMT FROM: Mike Siegel at PSU/Swift MOC <mhs18(a)psu.edu> M. H. Siegel (PSU) reports on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 250704A 2.9 ks after the SVOM/ECLAIRs trigger (Cao et al., GCN Circ. 40934). A source consistent with the XRT position (Osborne et al., GCN Circ. 40950) and the optical transient (Schneider et al., GCN Circ. 40953; Cao et al., GCN Circ. 40964) is detected in the UVOT exposures. The preliminary UVOT position is: RA (J2000) = 01:08:44.62 = 17.19427 (deg.) Dec (J2000) = -17:19:26.3 = -17.32398 (deg.) with an estimated uncertainty of 0.42 arc sec. (radius, 90% confidence). Preliminary detections and 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag u 2933 8704 1993 18.38+/-0.05 u 70704 76996 2879 20.77+/-0.28 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.015 in the direction of the burst (Schlegel et al. 1998). View this GCN Circular online at https://gcn.nasa.gov/circulars/40981. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39029] LIGO/Virgo/KAGRA S250705cb: Identification of a GW compact binary merger candidate
by GCN Circulars 05 Jul '25

05 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40980 SUBJECT: LIGO/Virgo/KAGRA S250705cb: Identification of a GW compact binary merger candidate DATE: 25/07/05 16:58:35 GMT FROM: Mayara Hilgert Pacheco at LIGO <mayara.pacheco(a)inpe.br> The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We identified the compact binary merger candidate S250705cb during real-time processing of data from LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) at 2025-07-05 16:29:56.842 UTC (GPS time: 1435768214.842). The candidate was found by the GstLAL [1], MBTA [2], and PyCBC Live [3] analysis pipelines. S250705cb is an event of interest because its false alarm rate, as estimated by the online analysis, is 9.5e-10 Hz, or about one in 33 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S250705cb The classification of the GW signal, in order of descending probability, is BBH (>99%), Terrestrial (<1%), BNS (<1%), or NSBH (<1%). Assuming the candidate is astrophysical in origin, the probability that at least one of the compact objects is consistent with a neutron star mass (HasNS) is <1%. [4] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [4] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%. The source chirp mass falls with highest probability in the bin (5.5, 11.0) solar masses, assuming the candidate is astrophysical in origin. Two sky maps are available at this time and can be retrieved from the GraceDB event page: * bayestar.multiorder.fits,0, an initial localization generated by BAYESTAR [5], distributed via GCN and SCiMMA notices about 27 seconds after the candidate event time. * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [5], distributed via GCN and SCiMMA notices about 5 minutes after the candidate event time. The preferred sky map at this time is bayestar.multiorder.fits,1. For the bayestar.multiorder.fits,1 sky map, the 90% credible region is 510 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1209 +/- 336 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/. [1] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. PRD 109, 042008 (2024) doi:10.1103/PhysRevD.109.042008 [2] Alléné et al. CQG 42, 105009 (2025) doi:10.1088/1361-6382/add234 [3] Dal Canton et al. ApJ 923, 254 (2021) doi:10.3847/1538-4357/ac2f9a [4] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe [5] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013 View this GCN Circular online at https://gcn.nasa.gov/circulars/40980. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39028] LIGO/Virgo/KAGRA S250705cb: Identification of a GW compact binary merger candidate
by GCN Circulars 05 Jul '25

05 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40980 SUBJECT: LIGO/Virgo/KAGRA S250705cb: Identification of a GW compact binary merger candidate DATE: 25/07/05 16:58:35 GMT FROM: Mayara Hilgert Pacheco at LIGO <mayara.pacheco(a)inpe.br> The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We identified the compact binary merger candidate S250705cb during real-time processing of data from LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) at 2025-07-05 16:29:56.842 UTC (GPS time: 1435768214.842). The candidate was found by the GstLAL [1], MBTA [2], and PyCBC Live [3] analysis pipelines. S250705cb is an event of interest because its false alarm rate, as estimated by the online analysis, is 9.5e-10 Hz, or about one in 33 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S250705cb The classification of the GW signal, in order of descending probability, is BBH (>99%), Terrestrial (<1%), BNS (<1%), or NSBH (<1%). Assuming the candidate is astrophysical in origin, the probability that at least one of the compact objects is consistent with a neutron star mass (HasNS) is <1%. [4] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [4] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%. The source chirp mass falls with highest probability in the bin (5.5, 11.0) solar masses, assuming the candidate is astrophysical in origin. Two sky maps are available at this time and can be retrieved from the GraceDB event page: * bayestar.multiorder.fits,0, an initial localization generated by BAYESTAR [5], distributed via GCN and SCiMMA notices about 27 seconds after the candidate event time. * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [5], distributed via GCN and SCiMMA notices about 5 minutes after the candidate event time. The preferred sky map at this time is bayestar.multiorder.fits,1. For the bayestar.multiorder.fits,1 sky map, the 90% credible region is 510 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1209 +/- 336 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/. [1] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. PRD 109, 042008 (2024) doi:10.1103/PhysRevD.109.042008 [2] Alléné et al. CQG 42, 105009 (2025) doi:10.1088/1361-6382/add234 [3] Dal Canton et al. ApJ 923, 254 (2021) doi:10.3847/1538-4357/ac2f9a [4] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe [5] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013 View this GCN Circular online at https://gcn.nasa.gov/circulars/40980. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39027] Radio observation of GRBs 250702B,C,E / EP250702a with the Allen Telescope Array
by GCN Circulars 05 Jul '25

05 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40979 SUBJECT: Radio observation of GRBs 250702B,C,E / EP250702a with the Allen Telescope Array DATE: 25/07/05 16:16:46 GMT FROM: Itai Sfaradi at University of California, Berkeley <itai.sfaradi(a)mail.huji.ac.il> Authors: I. Sfaradi (UC Berkeley), R. Margutti (UC Berkeley), W. Farah (SETI Institute, UC Berkeley), S. Sheikh (SETI Institute, UC Berkeley), R. Chornock (UC Berkeley), V. Garcia Lopez (SETI Institute), J. Bright (Oxford), K. Alexander (University of Arizona), A. Siemion (Oxford, SETI Institute), A. Pollak (SETI Institute), Y. Yao (UC Berkeley), Nayana A.J. (UC Berkeley), H. Sears (Rutgers U) We observed the field of the Einstein Probe source EP250702a (GCN 40906) with the Allen Telescope Array (ATA) on July 4, 2025, between 04:25:12 to 10:48:50 (UTC) about 2 days after first discovery. Our observation was carried out with four spectral windows centered around 1.5 and 3, 5, and 8 GHz, each with a bandwidth of 672 MHz. Calibration and imaging were performed using CASA with 3C286 as a bandpass and absolute flux scale calibrator, and 1822-096 as a complex gain calibrator. No radio emission was detected at the position of EP250702a and we report here a flux density upper limit (3 sigma image RMS) of 1.1 mJy/beam in 5 GHz. For comparison, while the distance of this EP source is not known, we note that the level of emission in GRB 221009A was ~18 mJy at 5 GHz, ~2 days after discovery (Bright et al. 2023). The Allen Telescope Array refurbishment program and its ongoing operations are being substantially funded through the Franklin Antonio Bequest. Additional contributions from Frank Levinson, Greg Papadopoulos, the Breakthrough Listen Initiative and other private donors have been instrumental in the renewal of the ATA. Breakthrough Listen is managed by the Breakthrough Initiatives, sponsored by the Breakthrough Prize Foundation. The Paul G. Allen Family Foundation provided major support for the design and construction of the ATA, alongside contributions from Nathan Myhrvold, Xilinx Corporation, Sun Microsystems, and other private donors. The ATA has also been supported by contributions from the US Naval Observatory and the US National Science Foundation. View this GCN Circular online at https://gcn.nasa.gov/circulars/40979. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39026] GRB 250704B: Insight-HXMT detection
by GCN Circulars 05 Jul '25

05 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40978 SUBJECT: GRB 250704B: Insight-HXMT detection DATE: 25/07/05 15:09:12 GMT FROM: Chenwei Wang at IHEP <cwwang(a)ihep.ac.cn> Chen-Wei Wang, Shao-Lin Xiong, Cheng-Kui Li, and Chao Zheng report on behalf of the Insight-HXMT team: At 2025-07-04T08:16:27.100 (T0), Insight-HXMT/HE detected the short burst GRB 250704B/ EP250704a, which is also detected by SVOM/GRM (Wang et al., GCN #40940), Konus-Wind (Dmitry Frederiks et al., GCN # 40972) and EP (Li et al., GCN # 40941). The Insight-HXMT/HE light curve mainly consists of double pulses with a T90 of 0.68 +0.34/-0.48 s. The total counts from this burst is 2046 counts. The HXMT/HE light curve can be found here: https://www.bursthub.cn//admin/static/hxmtgrb250704B.png All measurements above are made with the CsI detectors operating in the regular mode with the energy range of about 60-900 keV (deposited energy). Only gamma-rays with energy greater than about 200 keV can penetrate the spacecraft and leave signals in the CsI detectors installed inside of the telescope. Insight-HXMT is the first Chinese space X-ray telescope, which was funded jointly by the China National Space Administration (CNSA) and the Chinese Academy of Sciences (CAS). More information about it could be found at: http://www.hxmt.org. View this GCN Circular online at https://gcn.nasa.gov/circulars/40978. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39025] Konus-Wind detection of GRB 250703A
by GCN Circulars 05 Jul '25

05 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40977 SUBJECT: Konus-Wind detection of GRB 250703A DATE: 25/07/05 14:50:15 GMT FROM: Dmitry Frederiks at Ioffe Institute <fred(a)mail.ioffe.ru> D. Frederiks, A.Lysenko, A. Ridnaia, D. Svinkin, A. Tsvetkova, M. Ulanov, and T. Cline, on behalf of the Konus-Wind team, report: The long-duration GRB 250703A (Fermi-GBM detection: The Fermi GBM team, GCN 40909; IPN localization Kozyrev et al., GCN 40976) triggered Konus-Wind (KW) at T0=32851.983 s UT (09:07:31.983). The burst light curve shows a single multi-peaked emission pulse with a total duration of ~4.5 s. The emission is seen up to ~5 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB250703_T32851/ As observed by Konus-Wind, the burst had a fluence of (5.86 ± 0.66)x10^-6 erg/cm^2 and a 64-ms peak energy flux, measured from T0 + 0.960 s, of (3.81 ± 0.43)x10^-6 erg/cm^2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum (measured from T0 to T0+8.448 s) is best fit in the 20 keV - 15 MeV range by a GRB (Band) function with the following model parameters: the low-energy photon index alpha = -0.36 (-0.22,+0.28), the high energy photon index beta = -2.76 (-0.49,+0.27), the peak energy Ep = 147(-15,+15) keV, chi2 = 84/94 dof. All the quoted errors are estimated at the 68% confidence level. All the presented results are preliminary. View this GCN Circular online at https://gcn.nasa.gov/circulars/40977. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39024] IPN triangulation of GRB 250703A
by GCN Circulars 05 Jul '25

05 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40976 SUBJECT: IPN triangulation of GRB 250703A DATE: 25/07/05 14:48:05 GMT FROM: Anna Ridnaia at Ioffe Institute <ridnaia(a)mail.ioffe.ru> A.S. Kozyrev, D.V. Golovin, M.L. Litvak, I.G. Mitrofanov, and A.B. Sanin on behalf of the HEND/Mars Odyssey team, A. Ridnaia, D. Frederiks, A. Lysenko, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, A. Goldstein, M. S. Briggs, C. Wilson-Hodge, and E. Burns on behalf of the Fermi GBM team, and W. Boynton, C. Fellows, K. Harshman, H. Enos, R. Starr, and A.S. Gardner on on behalf of the GRS-Odyssey GRB team, report: The long-duration GRB 20250703A (Fermi-GBM detection: Fermi GBM team, GCN Circ. 40909) was detected by Fermi (GBM trigger 773226456), Konus-Wind, and Mars-Odyssey (HEND) at about 32851 s UT (09:07:31). We have triangulated it to a preliminary, 3 sigma error box whose coordinates are: --------------------------------------------- RA(2000), deg Dec(2000), deg --------------------------------------------- Center: 351.240 (23h 24m 58s) +28.375 (+28d 22' 31") Corners: 352.362 (23h 29m 27s) +28.111 (+28d 06' 39") 350.071 (23h 20m 17s) +28.695 (+28d 41' 42") 350.131 (23h 20m 32s) +28.603 (+28d 36' 11") 352.423 (23h 29m 41s) +28.013 (+28d 00' 47") --------------------------------------------- The error box area is 0.16 sq. deg, and its maximum dimension is 2.2 deg (the minimum one is 5 arcmin). The Sun distance was 96 deg. The IPN localization is consistent with, but reduces the area of, the Fermi-GBM localization. A triangulation map and HEALPix FITS file are posted at http://www.ioffe.ru/LEA/GRBs/GRB250703_T32851/IPN The HEALPix triangulation map is the multi-order HEALPix in units of probability density. The Konus-Wind time history and spectrum will be given in a forthcoming GCN Circular. View this GCN Circular online at https://gcn.nasa.gov/circulars/40976. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39023] EP250704a/GRB 250704B: GSP observations of the optical counterpart
by GCN Circulars 05 Jul '25

05 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40975 SUBJECT: EP250704a/GRB 250704B: GSP observations of the optical counterpart DATE: 25/07/05 12:56:03 GMT FROM: Wenxiong Li at NAOC <liwenxiong1992(a)gmail.com> W. X. Li, S. J. Xue (NAOC), M. Andrews, J. Farah, D. A. Howell, M. Newsome, E. Padilla Gonzalez, C. McCully, and G. Terreran (Las Cumbres Observatory), on behalf of a larger collaboration, report: Following the detection of the fast X-ray transient EP250704a/GRB 250704B (Li et al., GCN 40491, 40956; Wang et al., GCN 40940; Frederiks et al., GCN 40972), we initiated observations of the fast X-ray transient location starting on July 05 at 4:16 UT (~20 hours after the EP/WXT trigger) in the g, r and i bands. These observations were conducted using the 1-meter telescope at the Las Cumbres Observatory node located at the Cerro Tololo Inter-American Observatory in Chile. The optical counterpart, detected by COLIBRÍ (Schneider et al., GCN 40942), VLT/FORS2 (Malesani et al., GCN 40945), BOOTES-5 (Pérez-García et al., GCN 40957), Pan-STARRS (Gillanders et al., GCN 40958), SVOM/VT (Xin et al., GCN 40960), GROWTH-India (Mohan et al., GCN 40962), SAO RAS (Moskvitin et al., GCN 40963), JinShan (Liu et al., GCN 40965), VLT/X-shooter (An et al., GCN 40966), VLT/HAWK-I (Yang et al., GCN 40970), and NOT (Ricci et al., GCN 40970), is clearly detected in all LCO exposures, with preliminary magnitudes of g ≈ 20.2, r ≈ 20.1, and i ≈ 20.0 (AB mag). These observations were taken as part of the Global Supernova Project. View this GCN Circular online at https://gcn.nasa.gov/circulars/40975. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39022] EP250704a/GRB 250704B: FTW optical and NIR observations of the counterpart
by GCN Circulars 05 Jul '25

05 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40974 SUBJECT: EP250704a/GRB 250704B: FTW optical and NIR observations of the counterpart DATE: 25/07/05 12:53:11 GMT FROM: Malte Busmann at Ludwig-Maximilians-Universität München <m.busmann(a)physik.lmu.de> Malte Busmann (LMU), Xander Hall (Carnegie Mellon U.), Brendan O’Connor (Carnegie Mellon U.), Daniel Gruen (LMU), and Antonella Palmese (Carnegie Mellon U.) report: We observed the counterpart of EP250704a/GRB 250704B (Wang et al., GCN 40940; Li et al., GCNs 40941, 40956; Schneider et al., GCN 40942; Malesani et al., GCN 40945; Brivio et al., GCN 40947; Evans et al., GCN 40951; Perez-Garcia et al., GCN 4957; Gillanders et al., GCN 40958; Xin et al., GCN 40960; Mohan et al., GCN 40962; Moskvin et al., GCN 40963; Liu et al., GCN 40965; An et al., GCN 40966; Yang et al., GCN 4970; Martin-Carillo et al., GCN 40971; Frederiks et al., GCN 40972) with the Three Channel Imager (3KK) at the Fraunhofer Telescope at Wendelstein Observatory (FTW) in the r, i and J band simultaneously for 10 x 180 s starting at 2025-07-04T20:50:45 UT and again at 2025-07-05T01:28:10 UT (0.52 and 0.72 days after the trigger). The counterpart is detected in the individual images. In our second observation we detect it at: r = (20.2 +/- 0.1) mag, i = (19.9 +/- 0.1) mag, J = (19.4 +/- 0.2) mag. Consistent with previous observations, we do not see a significant evolution in time or color between our two epochs. The r and i band magnitudes are calibrated against the PS1 catalog and the J band is calibrated with the 2MASS Catalog. All magnitudes are provided in the AB system and are not corrected for Galactic extinction. We thank Silona Wilke from the Wendelstein Observatory staff for obtaining these observations. View this GCN Circular online at https://gcn.nasa.gov/circulars/40974. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39021] GRB 250702F: Calapai Observatory, Massa S. Giorgio (Messina), optical observation.
by GCN Circulars 05 Jul '25

05 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40973 SUBJECT: GRB 250702F: Calapai Observatory, Massa S. Giorgio (Messina), optical observation. DATE: 25/07/05 11:42:59 GMT FROM: Giovanni Calapai at Calapai Astronomical Observatory, Massa S. Giorgio, Messina, Italy <giovannicalapai(a)tiscali.it> Giovanni Calapai at Calapai Astronomical Observatory, Massa S. Giorgio, (Messina) Italy Member of: GRB/UAI Gamma Ray Burst Section of Unione Astrofili Italiani. Report: We observed the field of GRB 250702F detected by Swift/BAT (Klingler et al., GCN 40894) and Fermi/GBM (Fermi GBM Team, GCN 40892) with the 11 inches Schmidt-Cassegrain (Celestron 11) telescope F/D=6,3. The observations were started at 2025-07-02 21:32:30 UT (approximately 0.43 hours after burst) stacking two consecutive sets of unfiltered CCD image. The observations were carried out with clear skies and good visibility conditions. The OT was detected at the following position: RA (J2000.0) 14h 11m 44.68s Decl. (J2000.0) +16° 44' 55.0" Photometry was obtained using nearby PanSTARRS stars as follows: Observation Mid-Time T-T0 (hr) Exposure Filter Mag. Mag. err. 2025-07-02 22:03:02 UT 0.94 60x60s CR 17.13 +/-0.02 2025-07-02 23:05:09 UT 1.97 60x60s CR 18.07 +/-0.05 Magnitude was calibrated with the nearby PanSTARRS stars converted using Lupton (2005) equations. No correction for galactic dust extinction was applied. Our observations are consistent with other already reported Jelinek et al. (GCN 40895); Kumar et al. (GCN 40896); Lipunov et al. (GCN 40898); Martin-Carrillo et al. (GCN 40900); Angulo et al. (GCN 40907); Becerra et al. (GCN 40911); Brivio et al. (GCN 40913); An et al. (GCN 40916); Dutton et al. (GCN 40921); Odeh et al. (GCN 40925); Moretti et al. (GCN 40926); Siegel et al. (GCN 40933); Ma et al. (GCN 40936); Vinko et al. (GCN 40939); Mohan et al. (GCN 40946); Ciabattari et al. (GCN 40968); Broens et al. (GCN 40969). The message may be cited. View this GCN Circular online at https://gcn.nasa.gov/circulars/40973. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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