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

[vsnet-grb-info 39000] GRB 250704A: VLT/X-shooter afterglow discovery and spectroscopic redshift z = 1.091
by GCN Circulars 04 Jul '25

04 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40953 SUBJECT: GRB 250704A: VLT/X-shooter afterglow discovery and spectroscopic redshift z = 1.091 DATE: 25/07/04 14:56:37 GMT FROM: Benjamin Schneider at MIT <bschn(a)mit.edu> B. Schneider (LAM), A. Saccardi (CEA/Irfu), M. Garnichey (LUX-Paris Obs.), G. Corcoran (UCD), V. D’Elia (ASI/SSDC), M. De Pasquale (Univ. Messina), D. B. Malesani (DAWN/NBI and Radboud), A. L. Thakur (INAF-IAPS), S. D. Vergani (LUX-Paris Obs.) report on behalf of the Stargate collaboration: We observed the field of GRB 250704A detected by SVOM/ECLAIRs (Cao et al., GCN 40934) with ESO VLT UT3 (Melipal) equipped with the X-shooter spectrograph. Our spectra cover the wavelength range 3000-21000 AA, and consist of 4 exposures of 600 s each. The observation mid time was 2025 Jul 4.41 UT (6.10 hr after the GRB). In images taken with the acquisition camera, we clearly detect a source inside the error circle of the Swift/XRT X-ray afterglow (Osborne et al., GCN 40950) at coordinates (J2000): RA = 01:08:46.69 Dec = -17:19:25.87 The source is well detected in the g, r, and z bands, and we measure a magnitude r = 20.48 +- 0.05 AB, at a mid time Jul 4.39 UT (5.59 hr after trigger). The photometric calibration is preliminary as it was performed using a single nearby star from the Pan-STARRS catalog. This source is significantly brighter than existing archival imaging, and we thus conclude that this is the optical afterglow of GRB 250704A. In a preliminary reduction of the spectra, we detect a continuum over the entire covered wavelength range. From detection in the blue down to 3080 AA, and the lack of hydrogen absorption, we set a redshift upper limit z < 1.53. Furthermore, we detect multiple absorption lines, which we interpret as Al II, Fe II and the Mg II doublet, at a common redshift of z = 1.091. Three intervening Mg II absorbers are also detected at z = 0.65, z = 0.71, and z = 0.91. No emission lines are observed across the spectrum. Due to the lack of detection of fine-structure transitions, z = 1.091 is strictly a lower limit to the GRB redshift, but the absence of unidentified features and the reasonable S/N over the whole continuum suggest z = 1.091 as the actual value of the redshift. We acknowledge excellent support from the ESO observing staff in Paranal, in particular Robert Klement, Diego Parraguez, and Leonel Rivas. View this GCN Circular online at https://gcn.nasa.gov/circulars/40953. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38999] GRBs 250702B/C/D/E / EP250702a: Swift/UVOT Upper Limits
by GCN Circulars 04 Jul '25

04 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40952 SUBJECT: GRBs 250702B/C/D/E / EP250702a: Swift/UVOT Upper Limits DATE: 25/07/04 14:09:07 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 Einstein Probe (GCN Circ. 40906) location of the source that showed repeated outbursts detected by Fermi/GBM (GCN Circ. 40883, 40885, 40886, 40890, 40891) and Swift/BAT-GUANO (GCN #40903) 82 ks after the initial EP detection. No optical afterglow consistent with the XRT position (Kennea et al., GCN Circ. 40919) is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) using the initial EP detection as T_0 are: Filter T_start(s) T_stop(s) Exp(s) Mag b 82576 99156 235 >19.83 uvm2 99570 99822 247 >19.33 u 82491 104859 302 >19.73 v 82985 99566 115 >18.44 uvw1 82327 104787 628 >19.93 uvw2 82661 99481 663 >20.12 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.27 in the direction of the burst (Schlegel et al. 1998). View this GCN Circular online at https://gcn.nasa.gov/circulars/40952. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38998] EP250704a / GRB250704B: Swift-XRT counterpart detection
by GCN Circulars 04 Jul '25

04 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40951 SUBJECT: EP250704a / GRB250704B: Swift-XRT counterpart detection DATE: 25/07/04 14:06:18 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 Einstein Probe/WXT-detected source EP250704a (temporally coincident with the SVOM GRB 250704B, Wang et al., GCN 40940), collecting 1.7 ks of Photon Counting (PC) mode data between T0+1.8 ks and T0+3.7 ks after the trigger. A candidate counterpart has been found. The details of this source are: Source 2 (SWIFT J200329.1+120123): ================================== RA (J2000.0): 300.8716 = 20h 03m 29.18s Dec (J2000.0): +12.0233 = +12d 01' 23.9" Error: 3.6 (arcsec, radius, 90% confidence). Detect flag: REASONABLE Distance: 24 arcsec from the Einstein Probe/WXT position. Mean rate: 0.247 +/- 0.017 ct s^-1 Mean flux: (8.79 +/- 0.59)e-12 erg cm^-2 s^-1 Peak rate: 0.389 +/- 0.088 ct s^-1 Peak flux: (1.39 +/- 0.31)e-11 erg cm^-2 s^-1 ECF: 3.56e-11 erg cm^-2 ct^-1, assuming NH=1.47e+21 cm^-2, gamma=1.97; determined from a spectral fit. RASS UL: 2.9e-02 ct s^-1 (converted to XRT; 0.3-10 keV) so the source is not above this 3-sigma upper limit. The source may be fading, at the 1.7-sigma level. There is 1 2MASS object within the source's 3-sigma error radius. 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. 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/EP. The detected afterglow position is consistent with the optical counterpart of the EP trigger, reported by Schneider et al. (GCN 40942). This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/40951. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38997] GRB 250704A: Swift-XRT afterglow detection
by GCN Circulars 04 Jul '25

04 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40950 SUBJECT: GRB 250704A: Swift-XRT afterglow detection DATE: 25/07/04 14:00:05 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> J.P. Osborne (U. Leicester), B. Sbarufatti (INAF-OAB), C. Salvaggio (INAF-OAB), M. Ferro (INAF-OAB), M.A. Williams (PSU), S. Dichiara (PSU), J.A. Kennea (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester) and P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: We have analysed 2.0 ks of XRT data for GRB 250704A, from 2.9 ks to 8.7 ks after the SVOM/ECLAIRs trigger. The data are entirely in Photon Counting (PC) mode. A bright, fading source is detected inside the SVOM/ECLAIRs error region (Cao et al., GCN 40934), which we propose as the GRB afterglow. Using 2029 s of PC mode data and 2 UVOT images, we find an enhanced XRT position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 17.19414, -17.32397 which is equivalent to: RA (J2000): 01h 08m 46.59s Dec(J2000): -17d 19' 26.3" with an uncertainty of 2.8 arcsec (radius, 90% confidence). The light curve can be modelled with a power-law decay with a decay index of alpha=1.3 (+0.6, -0.5). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.03 (+0.31, -0.28). The best-fitting absorption column is 6.0 (+6.7, -4.5) x 10^20 cm^-2, consistent with the Galactic value of 1.6 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.2 x 10^-11 (3.8 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 6.0 (+6.7, -4.5) x 10^20 cm^-2 Galactic foreground: 1.6 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 2.03 (+0.31, -0.28) If the light curve continues to decay with a power-law decay index of 1.3, the count rate at T+24 hours will be 2.4 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 7.9 x 10^-14 (9.1 x 10^-14) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00019907. This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/40950. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38996] GRB 250702B / EP2050702a: FTW optical and NIR observations
by GCN Circulars 04 Jul '25

04 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40949 SUBJECT: GRB 250702B / EP2050702a: FTW optical and NIR observations DATE: 25/07/04 13:59:08 GMT FROM: Malte Busmann at Ludwig-Maximilians-Universität München <m.busmann(a)physik.lmu.de> Malte Busmann (LMU), Xander J. Hall (Carnegie Mellon U.), Brendan O’Connor (Carnegie Mellon U.), Daniel Gruen (LMU), Julian Sommer (LMU), and Antonella Palmese (Carnegie Mellon U.) report: We observed the location of GRB 250702B / EP250702a (Fermi GBM Team, GCNs 40883, 40886, 40890; Neights et al., GCNs 40891, 40931; DeLaunay et al., GCN 40903; Cheng et al., GCNs 40906, 40917; Kawakubo et al, GCN 40910; Frederiks et al., GCN 40914; Wang et al., GCN GCN 40923) with the Three Channel Imager (3KK) at the Fraunhofer Telescope at Wendelstein Observatory (FTW) in the r, i and J band simultaneously for 40 x 180 s starting at 2025-07-03T21:52:47 UT. We do not detect the source seen by Martin-Carrillo et al. (GCN 40924) or any other new source in the Swift/XRT localization (Kennea at al., GCN 40919) to 3 sigma limiting magnitudes of r > 23.6 AB mag i > 22.7 AB mag J > 21.7 AB mag. Compared to the K-band magnitude reported by Martin-Carrilo et al. (GCN 40924) this implies an extremely red color of the source, which implies a dusty environment, as also supported by the hydrogen column density inferred from the Swift/XRT observations (Kennea at al., GCN 40919). This is consistent with previous observations by Lipunov et al. (GCNs 40904, 40905, 40912), Kumar et al. (GCN 40908), Becerra et al. (GCN 40918), and Pérez-García et al. (GCN 40929). The r and i band magnitudes are calibrated against the PS1 catalog and the J band is calibrated with the 2MASS Catalog. The magnitudes 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/40949. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38995] Konus-Wind detection of GRB 250702F
by GCN Circulars 04 Jul '25

04 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40948 SUBJECT: Konus-Wind detection of GRB 250702F DATE: 25/07/04 13:22:06 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 250702F (Fermi-GBM detection: The Fermi GBM team, GCN 40892; Mukherjee & Meegan, GCN 40927; Swift detection: Klingler et al., GCN 40894) triggered Konus-Wind (KW) at T0=76042.205 s UT (21:07:22.205). The burst shows multiple emission pulses and has a total duration of ~46 s. The emission is seen up to ~3 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB250702_T76042/ As observed by Konus-Wind, the burst had a fluence of (1.60 ± 0.25)x10^-5 erg/cm^2 and a 64-ms peak energy flux, measured from T0 + 0.512 s, of (5.02 ± 1.15)x10^-6 erg/cm^2/s (both in the 20 keV - 10 MeV energy range). Modeling the time-integrated spectrum of the burst by a power law with exponential cutoff (CPL) model dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) yields alpha = -1.47 (-0.10, + 0.10) and Ep = 480(-130,+250) keV. The spectrum near the peak count rate (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 = -1.22 (-0.12,+0.17), the high energy photon index beta = -2.20 (-7.8,+0.29), the peak energy Ep = 505 (-155,+326) keV, chi2 = 85/94 dof. Assuming the redshift z=1.520 (de Ugarte Postigo et al., GCN 40896) and a standard cosmology with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315, and Omega_Lambda = 0.685 (Planck Collaboration, 2014), we estimate the burst isotropic energy release E_iso to (9.9 ± 1.5)x10^52 erg, the isotropic peak luminosity L_iso to (7.8 ± 1.8)x10^52 erg/s, and the rest-frame peak spectral energy Ep,z to ~1250 keV. With the obtained estimates, GRB 250702F is consistent with 90% prediction bands of both 'Amati' and 'Yonetoku' relations for the sample of >300 long KW GRBs with known redshifts (Tsvetkova et al., 2017; Tsvetkova et al., 2021), see http://www.ioffe.ru/LEA/GRBs/GRB250702_T76042/GRB250702F_rest_frame.pdf 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/40948. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38994] EP250704a / GRB 250704B - REM observations
by GCN Circulars 04 Jul '25

04 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40947 SUBJECT: EP250704a / GRB 250704B - REM observations DATE: 25/07/04 13:08:04 GMT FROM: Matteo Ferro at INAF-OAB <matteo.ferro(a)inaf.it> R. Brivio, M. Ferro, P. D'Avanzo, S. Covino, D. Fugazza (INAF-OAB) report on behalf of the REM team: We observed the field of EP250704a (Li et al., GCN 40941) / GRB 250704B (Wang et al., GCN 40940) with the REM 60 cm robotic telescope located at the ESO observatory of La Silla (Chile). The observations were carried in the g, r, i, z, and H bands, started on 2025 July 04 at 08:28:07 UT (i.e. 11.3 min after the burst), and lasted for about 2 hours. From preliminary inspection, we do not detect any counterpart at the position of the optical afterglow candidate (Schneider et al., GCN 40942, Malesani et al., GCN 40945) down to the following 3sigma limits: r > 18.7 (AB; calibrated against the Pan-STARRS catalogue), at a mid-time of 11.4 min after the trigger; H > 14.8 (Vega; calibrated against the 2MASS catalogue), at a mid-time of 11.3 min after the trigger. View this GCN Circular online at https://gcn.nasa.gov/circulars/40947. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38993] GRB 250702F: GROWTH-India Telescope optical observations
by GCN Circulars 04 Jul '25

04 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40946 SUBJECT: GRB 250702F: GROWTH-India Telescope optical observations DATE: 25/07/04 12:52:24 GMT FROM: V. Swain at IIT Bombay <vishwajeet.s(a)iitb.ac.in> T. Mohan, V. Swain, A. Salgundi, A.P. Saikia, V. Bhalerao (IITB), G.C. Anupama, S. Barway (IIA) and K. Angail (IAO) report on behalf of the GIT team: We observed the field of GRB 250702F (Klingler et al., GCN 40894, Fermi GBM, GCN 40892), with 0.7m GROWTH-India Telescope (GIT). We started the observation at 2025-07-03 16:43:24 UT, i.e., 19.6 hours after the Fermi/Swift trigger. We obtained multiple exposures in r' and i' filters. We detected the optical afterglow in our stacked image of r' filter at position reported by Swift UVOT (Siegel et al., GCN 40933). The photometry results are as follows: | MJD (mid) | Filter | t-t0 (in hours) |Total Exposure Time (sec) | Magnitude (AB) | | ------------- | ------ |-----| ------------------ | -------------- | | 60859.721180 | r' | 20.2 | 6 x 300 | 20.57 +/- 0.09 | | 60859.727245 | i' | 20.34 |3 x 300 | >19.4 | The measurement is calibrated against PanSTARRS DR1 (Chambers et al., 2016) and not corrected for Galactic extinction. Our magnitude is consistent with other optical observations (Jeliken et al., GCN 40895, Kumar et al., GCN 40896, Lipunov et al., GCN 40899, 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, Ma et al., GCN 40936, Vinko et al., GCN 40939). The GROWTH India Telescope (GIT; Kumar et al. 2022) is a 70-cm telescope with a 0.7-degree field of view, set up by the Indian Institute of Astrophysics (IIA) and the Indian Institute of Technology Bombay (IITB) with funding from DST-SERB and IUSSTF. It is located at the Indian Astronomical Observatory (Hanle), operated by IIA. We acknowledge funding by the IITB alumni batch of 1994, which partially supports the operations of the telescope. Telescope technical details are available at https://sites.google.com/view/growthindia/. View this GCN Circular online at https://gcn.nasa.gov/circulars/40946. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38992] EP250704a / GRB 250704B: VLT/FORS2 optical afterglow detection
by GCN Circulars 04 Jul '25

04 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40945 SUBJECT: EP250704a / GRB 250704B: VLT/FORS2 optical afterglow detection DATE: 25/07/04 11:22:17 GMT FROM: Daniele Bjørn Malesani at Cosmic Dawn Center, Niels Bohr Institute <daniele.malesani(a)nbi.ku.dk> Daniele B. Malesani (DAWN/NBI and Radboud), Rob Eyles-Ferris (U. of Leicester), Gregory Corcoran (UCD), Massimiliano De Pasquale (University of Messina), Peter G. Jonker (Radboud), Andrew J. Levan (Radboud), Antonio Martin-Carrillo (UCD), Aishwarya L. Thakur (INAF-IAPS), Dong Xu (NAOC) report on behalf of the Stargate collaboration: We observed the field of EP250704a (Li et al., GCN 40941) / GRB 250704B (Wang et al., GCN 40940) using the ESO VLT UT1 (Antu) equipped with the FORS2 camera. Observations were carried out in the z band and were executed in rapid response mode (RRM). The optical counterpart reported by Schneider et al. (GCN 40942) using COLIBRÍ/DDRAGO is clearly detected in our images. From a single 60-s exposure taken in the z band at a mean epoch of 2025 Jul 4.375 UT (42.8 min after the trigger), we measure z = 20.12 +- 0.05 AB. This is significantly brighter than the limit of the Pan-STARRS catalog, and well within the EP/FXT error circle. We thus concur with Schneider et al. (GCN 40942) that this is the likely afterglow of EP250704a. We acknowledge expert support from the observing staff in Paranal, in particular Sam Kim, Robert Klement and Leonel Rivas. View this GCN Circular online at https://gcn.nasa.gov/circulars/40945. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 38991] GRB 250704A: REM retraction of optical afterglow detection and updated limit
by GCN Circulars 04 Jul '25

04 Jul '25

TITLE: GCN CIRCULAR NUMBER: 40944 SUBJECT: GRB 250704A: REM retraction of optical afterglow detection and updated limit DATE: 25/07/04 10:52:18 GMT FROM: Riccardo Brivio at INAF-OAB <riccardo.brivio(a)inaf.it> R. Brivio, M. Ferro (INAF-OAB), A. Rossi (INAF-OAS), P. D'Avanzo, S. Covino, D. Fugazza (INAF-OAB) report on behalf of the REM team: Further analysis of the optical data obtained with REM (Brivio et al. GCN Circ. 40938) reveals that the source identified as the optical afterglow of GRB 250704A (Cao et al., GCN Circ. 40934) is spurious, likely resulting from a cosmic ray. From further analysis of the field, we obtain a 3sigma upper limit of: r > 18.1 (AB; calibrated against the Pan-STARRS catalogue), at a mid-time of 1.7 hr after the trigger. We apologize for any confusion this may have caused. View this GCN Circular online at https://gcn.nasa.gov/circulars/40944. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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