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[vsnet-grb-info 39897] GRB 250912A: Swift-XRT observations
by GCN Circulars 14 Sep '25

14 Sep '25

TITLE: GCN CIRCULAR NUMBER: 41831 SUBJECT: GRB 250912A: Swift-XRT observations DATE: 25/09/14 14:45:17 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> P.A. Evans (U. Leicester), J.A. Kennea (PSU), E. Ambrosi (INAF-IASFPA) , A.P. Beardmore (U. Leicester), M.G. Bernardini (INAF-OAB), R. Brivio (INAF-OAB), D.N. Burrows (PSU), S. Campana (INAF-OAB), M. Capalbi (INAF-OAR), A. D'Ai (INAF-IASFPA), P. D'Avanzo (INAF-OAB), V. D'Elia (SSDC & INAF-OAR), S. Dichiara (PSU), M. Ferro (INAF-OAB), A. Melandri (INAF-OAR), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), M. Perri (SSDC & INAF-OAR), C. Salvaggio (INAF-OAB), T. Sbarrato (INAF-OAB), B. Sbarufatti (INAF-OAB), M.A. Williams (PSU) report on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the SVOM/ECLAIRs-detected source GRB 250912A (Ducoin et al., GCN 41820; Wang et al., GCN 41826; see also Fermi GBM team, GCN 41819), collecting 2.2 ks of Photon Counting (PC) mode data between T0+11 ks and T0+55 ks after the trigger. We have detected 1 source. This has been automatically classified as an uncatalogued X-ray source. Uncatalogued X-ray sources -------------------------- Source 1 (SWIFT J010009.7+111047): ================================== RA (J2000.0): 15.0405 = 01 00 09.72 Dec (J2000.0): +11.1797 = +11 10 46.9 Error: 7.3 (arcsec, radius, 90% confidence). Detect flag: GOOD Distance: 6.8 arcmin from the SVOM/ECLAIRs position. Mean rate: (3.6 [+2.0, -1.5])e-3 ct s^-1 Mean flux: (2.7 [+1.5, -1.1])e-13 erg cm^-2 s^-1 Peak rate: (3.6 [+2.0, -1.5])e-3 ct s^-1 Peak flux: (2.7 [+1.5, -1.1])e-13 erg cm^-2 s^-1 ECF: 7.43e-11 erg cm^-2 ct^-1 assuming NH=5.11e+20 cm^-2, gamma=0.69 determined from a spectral fit. RASS UL: 7.3e-02 ct s^-1 (converted to XRT; 0.3-10 keV) so the source is not above this 3-sigma upper limit. There is no evidence for fading. All fluxes are 0.3-10 keV, observed. For all flux conversions and comparisons with catalogues and upper limits from other missions, we assumed a power-law spectrum with NH=3x10^20 cm^-2 and photon index (Gamma)=1.7 unless otherwise stated. We note that source 1 lies outside the MXT error region reported by Ducoin et al. (GCN 41820), so it is likely unrelated with the GRB. 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/SVOM/SVOM_FIELD00037. This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/41831. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39896] GRB250912A: VLT/HAWK-I follow-up observations
by GCN Circulars 14 Sep '25

14 Sep '25

TITLE: GCN CIRCULAR NUMBER: 41830 SUBJECT: GRB250912A: VLT/HAWK-I follow-up observations DATE: 25/09/14 12:29:31 GMT FROM: Roberto Ricci at INAF-IRA <ricci(a)ira.inaf.it> R. Ricci (U Rome), E. Troja (U Rome), M. Yadav (U Rome) and Y. Yang (U. Rome) report: We observed the field of GRB250912A discovered by Fermi/GBM (Fermi GBM team GCN 41819) and SVOM (Ducoin et al. GCN 41820) and classified as a possible short GRB with extended emission (Wang et al. GCN 41826) using the VLT UT4 (Yepun) telescope equipped with the HAWK-I near-infrared imager. Our observations were centered on the SVOM/MXT position (Ducoin et al. GCN 41820) and were carried out in the J filter for a net exposure time of 15 minutes starting on Sep 14th 03:58 UT (31 hours after the trigger). The source reported by Malesani et al. (GCN 41829) and located at coordinates (J2000): RA = 00:59:44.39 Dec = +11:10:07.0 is detected in our imaging with J ~ 22.20 AB mag, thus not showing significant variability since the previous night. No other obvious counterpart is evident in our observations. Further observations are planned. We thank the VLT Observatory staff for promptly executing the observations. View this GCN Circular online at https://gcn.nasa.gov/circulars/41830. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39895] GRB 250912A: VLT observations
by GCN Circulars 14 Sep '25

14 Sep '25

TITLE: GCN CIRCULAR NUMBER: 41829 SUBJECT: GRB 250912A: VLT observations DATE: 25/09/14 10:06:40 GMT FROM: Daniele Bjørn Malesani at Cosmic Dawn Center, Niels Bohr Institute <daniele.malesani(a)nbi.ku.dk> M. Garnichey (LUX-Paris Obs.), G. Corcoran (UCD), B. Schneider (LAM), L. Izzo (INAF/OACN), A. Saccardi (CEA/Irfu), V. D’Elia (ASI/SSDC), N. Habeeb (Leicester), D. B. Malesani (DAWN/NBI and Radboud), A. Martin-Carrillo (UCD), A. L. Thakur (INAF/IAPS), N. R. Tanvir (Leicester), S. D. Vergani (LUX-Paris Obs.), report on behalf of the Stargate collaboration: Following the reports of deep optical upper limits (Wu et al., GCN 41824; Li et al., GCN 41825), we observed the location of the SVOM GRB 250912A (Ducoin et al., GCN 41820; Wang et al., GCN 41826; see also Smith & Meegan, GCN 41828) using the ESO VLT UT4 (Yepun) equipped with the HAWK-I near-infrared imager. A total of 15 min exposure was secured in the J band, at a mean epoch 2025 Sep 13.130 UT (6.02 hr after the trigger). Image subtraction against archival UKIDSS J-band data reveals no new sources down to the depth of this survey, J ~ 20.6 (AB). As our HAWK-I stack reaches much deeper (limiting magnitude J = 23.9 AB), a more effective search can be carried out by comparison with the Legacy Survey, which is much more sensitive than UKIDSS, but only covers bands different than J. Within the MXT error circle (Ducoin et al., GCN 41820), many objects are visible in our J-band image that are not present in the Legacy Survey. The brightest one has a magnitude J = 22.15 +/- 0.06 (AB), and is located at coordinates (J2000): RA = 00:59:44.39 Dec = +11:10:07.0 For this object, we measure an upper limit z > 23.7 AB in the Legacy Survey, indicating either a remarkably red object or a transient/variable source. Based on the available information, we cannot discriminate between these two possibilities at the moment. Follow-up observations of this source were secured using the ESO VLT UT1 (Antu) equipped with the FORS2 spectrograph. A 3x1000 s spectrum was obtained with the 600z grism (wavelength range 7500 - 10100 AA). No object is detected in the acquisition image (mid time 9.83 hr after trigger) down to a depth of z > 22.7 AB, but a very faint trace is detected in the red part down to ~8550 AA. The very low S/N prevents us from identifying any features, but the continuum detection allows us to set a redshift upper limit z <~ 6. At the present time, no clear afterglow candidate emerges from our observations. A second, deep J-band image is required in order to conclusively identify any faint, variable sources. We acknowledge expert support from the ESO observing staff in Paranal, in particular Robert De Rosa, Juan Carlos Olivares, Jonathan Smoker, Hannah Osborne, and Sam Kim. View this GCN Circular online at https://gcn.nasa.gov/circulars/41829. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39894] GRB 250912A: Fermi GBM Observation
by GCN Circulars 14 Sep '25

14 Sep '25

TITLE: GCN CIRCULAR NUMBER: 41828 SUBJECT: GRB 250912A: Fermi GBM Observation DATE: 25/09/14 00:30:11 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 21:06:23.64 UT on 12 September 2025, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 250912A (trigger 779403988/250912879), which was also detected by SVOM/ECLAIRs (Jean-Grégoire Ducoin et al. 2025, GCN 41820). The Fermi GBM on-ground location is consistent with the SVOM/ECLAIRs position. The angle from the Fermi LAT boresight is 49 degrees. The GBM light curve consists of multiple emission episodes with a duration (T90) of about 15 s (50-300 keV). The time-averaged spectrum from T0 to T0+15.6 s is best fit by a simple power law function with index -1.31 +/- 0.04. A power law function with an exponential high-energy cutoff fits the spectrum equally well with a with power law index = -1.05 +/- 0.12 and Epeak = 783 +/- 359. The event fluence (10-1000 keV) in this time interval is (3.1 +/- 0.1)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0-0.26 s in the 10-1000 keV band is 4 +/- 0.2 ph/s/cm^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/41828. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39893] GRB 250911A: Insight-HXMT detection
by GCN Circulars 13 Sep '25

13 Sep '25

TITLE: GCN CIRCULAR NUMBER: 41827 SUBJECT: GRB 250911A: Insight-HXMT detection DATE: 25/09/13 18:17:46 GMT FROM: Chenwei Wang at IHEP <cwwang(a)ihep.ac.cn> Chen-Wei Wang, Jin-Peng Zhang, Shao-Lin Xiong, and Chao Zheng report on behalf of the Insight-HXMT team: At 2025-09-11T01:29:28.250 (T0), Insight-HXMT/HE detected the burst GRB 250911A, which is also detected by Swift/BAT (Palmer et al., GCN 41781) and GECAM-B (Zhang et al., GCN#41813. The Insight-HXMT/HE light curve mainly consists of multi-pulses with a T90 of 24.5 +2.5/-1.5 s. The 1s peak rate, measured from T0+5.250 s, is 1857 cnts/sec. The total counts from this burst is 11720 counts. The HXMT/HE light curve can be found here: https://www.bursthub.cn//admin/static/hxmtgrb250911A.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/41827. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39892] GRB 250912A: SVOM/GRM analysis suggests a possible short GRB with extended emission
by GCN Circulars 13 Sep '25

13 Sep '25

TITLE: GCN CIRCULAR NUMBER: 41826 SUBJECT: GRB 250912A: SVOM/GRM analysis suggests a possible short GRB with extended emission DATE: 25/09/13 18:17:13 GMT FROM: Chenwei Wang at IHEP <cwwang(a)ihep.ac.cn> SVOM/GRM team: Chen-Wei Wang, Shi-Jie Zheng, Yue Huang, Shao-Lin Xiong, Shuang-Nan Zhang (IHEP) SVOM/ECLAIRs team: Hui Yang, Jean-Luc Atteia (IRAP), Stéphane Schanne (CEA) Report on behalf of the SVOM team: SVOM/GRM detected the burst GRB 250612A at 2025-09-12T21:06:23.700 UTC (T0), which is also detected by SVOM/ECLAIRs (Jean-Grégoire Ducoin et al., GCN #41820) and Fermi/GBM (Fermi GBM team, GCN #41819) With the event-by-event data downloaded through the X-band ground station, we conducted the standard analysis pipeline of GRB 250612A. The GRM light curve shows that this burst consists of a hard pulse followed by extended emission with a T90 of 13.0 +6.5/-2.0 s in the 15-5000 keV band, and there is a weak precursor-like signal at about T0-10 s, which is also clearly detected by ECLAIRs. The SVOM/GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb250912A.png With the localization of ECLAIRs (RA= 14.953, DEC= 11.137), the time-averaged spectrum from T0-1 to T0+16 s can be fitted by a power law function with an exponential high-energy cutoff adequately. The power law index is -1.15 +0.19/- 0.15 and the cutoff energy, parameterized as Epeak, is 520 +692/-203 keV. The event fluence (10-1000 keV) in this time interval is (3.01 +0.40/- 0.44)E-06 erg/cm^2. Thus GRB 250912A is consistent with Type I GRBs in the 'Amati' relation diagram, as shown at: https://www.bursthub.cn//admin/static/svgrb250912A_amati.png Based on the location of this GRB in 'Amati' relation diagram, as well as the shape of the light curve, a possible merger origin is suggested. Follow-up observations are encouraged. We note that the calibration of SVOM/GRM is undergoing thus these results are preliminary. Refined analysis will be reported later. 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. GRM is developed by the Institute of High Energy Physics (IHEP) of CAS. The SVOM/GRM point of contact for this burst is: Chen-Wei Wang (IHEP) (cwwang(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/41826. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39891] GRB 250912A:SVOM/VT optical upper limit
by GCN Circulars 13 Sep '25

13 Sep '25

TITLE: GCN CIRCULAR NUMBER: 41825 SUBJECT: GRB 250912A:SVOM/VT optical upper limit DATE: 25/09/13 06:18:59 GMT FROM: Huali Li at at NAOC, SVOM <lhl(a)nao.cas.cn> H. L. Li, L. P. Xin, Y. N. Ma, Z. H. Yao, Y. L. Qiu, C. Wu, X. H. Han, Y. Xu, J. Wang, P. P. Zhang, W. J. Xie, Y. J. Xiao, H. B. Cai, L. Lan, J. S. Deng, J. Y. Wei, D. H. Zhao (NAOC), J. Palmerio (CEA) report on behalf of the SVOM/VT team. SVOM performed an automatic slew on the burst triggered by SVOM/ECLAIRs (Ducoin et al., GCN 41820). SVOM/VT began observing the field at 2025-09-12T21:10:17 UTC, 233 sec after T0, in the VT_B (400nm-650nm) and VT_R (650nm-1000nm) channels simultaneously. No uncatalogued sources were detected in our single or stacked images at the SVOM/MXT position (Ducoin et al., GCN 41820), compared to the Legacy survey. The 3 sigma limits are: mid-time | exposure time (s) | band | upper limit (AB) -----------|-------------------|------|----------------- 12.8 min | 18*50 | VT_B | 23.0 12.8 min | 18*50 | VT_R | 23.1 Our results are consistent with the reports (Lipunov et al., GCN 41822; Wu et al., GCN 41824). 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/41825. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39890] GRB 250912A: LCO optical upper limit
by GCN Circulars 13 Sep '25

13 Sep '25

TITLE: GCN CIRCULAR NUMBER: 41824 SUBJECT: GRB 250912A: LCO optical upper limit DATE: 25/09/13 03:14:55 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> C. Wu (NAOC), A. Saccardi (CEA/Irfu), L. P. Xin (NAOC), B. Cordier (CEA/Irfu), J.G. Ducoin (CPPM), D. Dornic (CPPM) report on behalf of the SVOM mission team: We observed the field of the GRB 250912A detected by Fermi/GBM(Fermi Team, GCN 41819) and SVOM/ECLAIRs (Ducoin et al., GCN 41820) with the LCO 1m telescope at South African Astronomical Observatory equipped with the Sinistro instrument. Our observation started on 2025-09-12 at 23:43:52 UT (~2.62 hr after the trigger) and we obtained 3x200 s exposures using the SDSS r filter. In the stacked image, we did not detect any new optical source at the SVOM/MXT position (Ducoin et al., GCN 41820). We derived the following upper limit r > 21.4 mag (3-sigma) calibrated using nearby stars from the UCAC4 catalog and not corrected for Galactic extinction. This project is funded by the SVOM collaboration. View this GCN Circular online at https://gcn.nasa.gov/circulars/41824. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39889] The EP-WXT trigger 01709240768 is likely a flaring star
by GCN Circulars 13 Sep '25

13 Sep '25

TITLE: GCN CIRCULAR NUMBER: 41823 SUBJECT: The EP-WXT trigger 01709240768 is likely a flaring star DATE: 25/09/13 02:07:50 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> W.Chen, X. Mao, Z.X. Ling(NAO, CAS) on behalf of the Einstein Probe (EP) team: The EP-WXT trigger 01709240768 at the time of 2025-09-12T23:11:57 is likely a stellar flare associated with LSPM J0011+0227. The estimated flux of the flare is around 6x10^-11 erg/s/cm^2 in 0.5-4.0 keV, corresponding to an X-ray luminosity of around 1.2x10^31 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/41823. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39888] Fermi GRB 250912A: Global MASTER-Net observations report
by GCN Circulars 13 Sep '25

13 Sep '25

TITLE: GCN CIRCULAR NUMBER: 41822 SUBJECT: Fermi GRB 250912A: Global MASTER-Net observations report DATE: 25/09/13 01:30:58 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-Kislovodsk robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB 250912A ( Fermi GBM team, GCN 41819) errorbox 12109 sec after notice time and 12119 sec after trigger time at 2025-09-13 00:28:22 UT, with upper limit up to 17.0 mag. The observations began at zenith distance = 30 deg. The sun altitude is -24.7 deg. The galactic latitude b = -38 deg., longitude l = 125 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2990662 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 12149 | 2025-09-13 00:28:22 | MASTER-Kislovodsk | (00h 49m 11.26s , +24d 09m 10.4s) | C | 60 | 16.9 | 12323 | 2025-09-13 00:31:16 | MASTER-Kislovodsk | (00h 49m 55.02s , +26d 01m 05.3s) | C | 60 | 16.5 | 12820 | 2025-09-13 00:39:33 | MASTER-Kislovodsk | (00h 49m 13.73s , +24d 08m 45.3s) | C | 60 | 17.0 | 12996 | 2025-09-13 00:42:30 | MASTER-Kislovodsk | (00h 49m 58.92s , +26d 02m 34.8s) | C | 60 | 17.0 | 13174 | 2025-09-13 00:45:28 | MASTER-Kislovodsk | (00h 48m 26.82s , +22d 14m 39.0s) | C | 60 | 16.5 | 13353 | 2025-09-13 00:48:26 | MASTER-Kislovodsk | (01h 04m 52.12s , +22d 13m 05.7s) | C | 60 | 13.7 | 13436 | 2025-09-13 00:49:49 | MASTER-Kislovodsk | (00h 49m 14.02s , +24d 06m 49.9s) | C | 60 | 13.8 | 13521 | 2025-09-13 00:51:14 | MASTER-Kislovodsk | (01h 05m 50.94s , +24d 08m 56.8s) | C | 60 | 17.0 | 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/41822. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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