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[vsnet-grb-info 43661] IceCube-Cascade 260824A: Upper limits from a search for additional neutrino events in IceCube
by GCN Circulars 25 Aug '26

25 Aug '26

TITLE: GCN CIRCULAR NUMBER: 45440 SUBJECT: IceCube-Cascade 260824A: Upper limits from a search for additional neutrino events in IceCube DATE: 26/08/25 15:35:18 GMT FROM: Alicia Mand at IceCube/UW-Madison <aemand(a)wisc.edu> The IceCube Collaboration (http://icecube.wisc.edu/) reports: IceCube has performed a search [1] for additional track-like muon neutrino events arriving from the direction of IceCube-Cascade 260824A (https://gcn.gsfc.nasa.gov/notices_amon_icecube_cascade/143029_33795562.amon) in a time range of 1000 seconds centered on the alert event time (2026-08-24 01:31:48.903 UTC to 2026-08-24 01:48:28.903 UTC) during which IceCube was collecting good quality data. Excluding the event that prompted the alert, zero track-like events are found within the 90% containment region of IceCube-Cascade 260824A. We report a p-value of 1.00 in this time window. IceCube’s sensitivity to neutrino point sources with an E^-2.5 spectrum, expressed as E^2 dN/dE evaluated at 1 TeV, ranges from 1.4e-01 to 1.6e-01 GeV cm^-2 within the 90% spatial containment region of IceCube-Cascade 260824A in a 1000 second time window. 90% of events IceCube would detect from a source at this declination with an E^-2.5 spectrum have energies in the approximate energy range between 2e+02 GeV and 6e+04 GeV. A subsequent search was performed including 2 days of data centered on the alert event time (2026-08-23 01:40:08.903 UTC to 2026-08-25 01:40:08.903 UTC). In this case, we report a p-value of 0.86, consistent with no significant excess of track events. IceCube’s sensitivity to neutrino point sources with an E^-2.5 spectrum, expressed as E^2 dN/dE evaluated at 1 TeV, ranges from 1.6e-01 to 1.9e-01 GeV cm^-2 within the 90% spatial containment region of IceCube-Cascade 260824A in a 2 day time window. The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the geographic South Pole, Antarctica. The IceCube realtime alert point of contact can be reached at roc(a)icecube.wisc.edu. [1] IceCube Collaboration, R. Abbasi et al., ApJ 910 4 (2021) View this GCN Circular online at https://gcn.nasa.gov/circulars/45440. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 43660] GRB 260825A: Fermi GBM Final Real-time Localization
by GCN Circulars 25 Aug '26

25 Aug '26

TITLE: GCN CIRCULAR NUMBER: 45439 SUBJECT: GRB 260825A: Fermi GBM Final Real-time Localization DATE: 26/08/25 13:17:43 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply(a)GIOC.nsstc.nasa.gov> The Fermi GBM team reports the detection of a likely LONG GRB At 13:07:15 UT on 25 Aug 2026, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 260825A (trigger 809356040.919172 / 260825547). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 88.3, Dec = -1.2 (J2000 degrees, equivalent to J2000 05h 53m, -1d 11'), with a statistical uncertainty of 5.7 degrees. The angle from the Fermi LAT boresight is 95.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260825547/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260825547/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2026/bn260825547/… View this GCN Circular online at https://gcn.nasa.gov/circulars/45439. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 43659] IceCube-260825A - IceCube observation of a high-energy neutrino candidate track-like event
by GCN Circulars 25 Aug '26

25 Aug '26

TITLE: GCN CIRCULAR NUMBER: 45438 SUBJECT: IceCube-260825A - IceCube observation of a high-energy neutrino candidate track-like event DATE: 26/08/25 12:35:54 GMT FROM: Cristobal Zilleruelo Cañas at DESY <cristobal.zilleruelo.canas(a)desy.de> The IceCube Collaboration (http://icecube.wisc.edu/) reports: On 26-08-25 at 10:53:33.63 UT IceCube detected a track-like event with a moderate probability of being of astrophysical origin. The event was selected by the ICECUBE_Astrotrack_BRONZE alert stream. Documentation regarding the alert streams and their astrophysical purity can be found here: https://gcn.nasa.gov/missions/icecube. This alert has an estimated false alarm rate of 0.5733 events per year due to atmospheric backgrounds. The IceCube detector was in a normal operating state at the time of detection. After the initial automated alert (https://gcn.gsfc.nasa.gov/notices_amon_g_b/143033_44905242.amon) more sophisticated reconstruction algorithms have been applied offline, with the direction refined to: Date: 26-08-25 Time: 10:53:33.63 UT RA: 91.95 (+0.75/-0.74 deg 90% PSF containment) J2000 Dec: 45.73 (+0.52/-0.51 deg 90% PSF containment) J2000 As announced in GCN Circular 43419 (https://gcn.nasa.gov/circulars/43419) IceCube alert notices for high-energy track alerts are now also streamed via Kafka. IceCube Gold/Bronze track alerts are available on the Kafka topic 'gcn.notices.icecube.gold_bronze_track_alerts'. The probability distribution of the true neutrino direction, allowing the extraction of precise 90% containment regions around the best-fit direction, is now available for revised reconstruction of high-energy track alerts. The corresponding sky map is distributed as a FITS file and follows the explicit naming convention IceCube-YYMMDDX, where YYMMDD indicates the date of the event and X is a letter distinguishing multiple alerts on the same day. The download link is provided through the GCN schema distributed via Kafka. Detailed documentation describing the alert distribution, schemas, and probability maps is available at: https://gcn.nasa.gov/missions/icecube. No known gamma-ray sources listed in the Fermi LAT 16-year Source List (FL16Y) are located within the 90% uncertainty region of this event. The IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the geographic South Pole, Antarctica. The IceCube realtime alert point of contact can be reached at roc(a)icecube.wisc.edu View this GCN Circular online at https://gcn.nasa.gov/circulars/45438. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 43658] GRB 260822A: PRIME near-infrared upper limits from multiple epochs
by GCN Circulars 24 Aug '26

24 Aug '26

TITLE: GCN CIRCULAR NUMBER: 45437 SUBJECT: GRB 260822A: PRIME near-infrared upper limits from multiple epochs DATE: 26/08/25 05:45:24 GMT FROM: Joe Durbak at UMD <gcn.joedurbak(a)gmail.com> J. Durbak (UMD, NASA GSFC), O. Guiffreda (UMD, NASA GSFC), F. McDaniel (UMD, NASA GSFC), R. Hamada (UOsaka), N. Passaleva (U Rome), M. El Kabir (U Rome), E. Troja (U Rome), A. S. Kutyrev (NASA/GSFC), S. B. Cenko (NASA/GSFC) Following the SVOM (GCN 45422) detection, we observed the transient field in J and H-filters with PRIME starting ~5.5 hours and ~30 hours after SVOM detection. Within the localization region reported by SVOM (GCN 45422) and the regions of interest reported by Einstein Probe (GCN 45436), we find no significant varying sources during the 24 hour period between follow-up observations. The limiting magnitudes (SNR>6) for each filter and epoch are given below using Vista Hemispherical Survey (VHS) and UKIRT Infrared Deep Sky Survey Large Area Survey (UKIDSS LAS) stars for calibration. | Epoch | Filter | Mag(AB) | Calibration Survey | |-------|--------|---------|--------------------| | 1 | J | > 21.4 | VHS | | 1 | H | > 21.2 | UKIDSS LAS | | 2 | J | > 21.7 | VHS | | 2 | H | > 21.3 | VHS | PRIME is a 1.8m telescope with 1.56 square degree FOV (0.5 arcsec/pixel) located in Sutherland, South Africa at the South African Astronomical Observatory (SAAO) (Kutyrev et al. 2023, Yama et al. 2023, Durbak et al. 2024, Sumi et al. 2025). We thank the University of Osaka observers at PRIME and the staff at SAAO for their support with these observations. View this GCN Circular online at https://gcn.nasa.gov/circulars/45437. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 43657] GRB 260822A: EP/FXT follow-up observations
by GCN Circulars 24 Aug '26

24 Aug '26

TITLE: GCN CIRCULAR NUMBER: 45436 SUBJECT: GRB 260822A: EP/FXT follow-up observations DATE: 26/08/24 15:20:24 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> D. Turpin, S. Schanne (CEA/Irfu), D. B. Malesani (DAWN/NBI and Radboud) and J. P. Feng (USTC) report on behalf of the SVOM and Einstein Probe teams: EP-FXT performed a follow-up observation of GRB 260822A detected by SVOM/ECLAIRs (Schanne et al., GCN 45422). The observation started at 2026-08-23T12:00:29.920 (UTC), about 19.2 hr after the SVOM trigger, with a total exposure time of around 5.8 ks. On-ground analysis of the FXT data found several uncataloged sources inside the ECLAIRs error region. Detected both in FXT A and B: ============================================================= Name | RA | DEC | dist from ECL position | Flux [0.5-10keV] | | | (arcmin) | (erg/cm^2/s) ============================================================= EPF_J000959.8+012409 | 2.4997 | 1.4010 | 4.6072 | 1.2304e-13 EPF_J000926.2+012804 | 2.3576 | 1.4675 | 6.2141 | 7.2405e-14 Detected in FXT A only: ============================================================= Name | RA | DEC | dist from ECL position | Flux [0.5-10keV] | | | (arcmin) | (erg/cm^2/s) ============================================================= EPF_J001001.7+011925 | 2.5071 | 1.3237 | 6.3032 | 5.673e-14 EPF_J000930.4+012950 | 2.3758 | 1.4964 | 7.1176 | 6.5814e-14 EPF_J001016.0+012360 | 2.5668 | 1.3999 | 8.5952 | 5.3425e-14 Detected in FXT B only: ============================================================= Name | RA | DEC | dist from ECL position | Flux [0.5-10keV] | | | (arcmin) | (erg/cm^2/s) ============================================================= EPF_J000951.2+011738 | 2.4632 | 1.2940 | 6.1105 | 4.1612e-14 EPF_J001002.6+011947 | 2.5108 | 1.3271 | 6.3608 | 4.8955e-14 EPF_J000915.7+012111 | 2.3155 | 1.3529 | 6.8404 | 2.1891e-14 EPF_J000930.4+012948 | 2.3757 | 1.4971 | 7.1584 | 5.1928e-14 EPF_J000947.5+013106 | 2.4477 | 1.5183 | 7.9462 | 2.6114e-14 EPF_J000928.0+013037 | 2.3667 | 1.5103 | 8.1030 | 4.2864e-14 with uncertainties of 10 arcsec (radius, 90% C.L. statistical and systematic). At this stage, we can not identify any significant flux variability from these sources. A second EP/FXT ToO has been requested in order to conclude about the association of the EP/FXT sources with GRB 260822A. 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/45436. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 43656] GRB 260822A: the candidate optical afterglow is an unrelated type-Ia SN
by GCN Circulars 24 Aug '26

24 Aug '26

TITLE: GCN CIRCULAR NUMBER: 45435 SUBJECT: GRB 260822A: the candidate optical afterglow is an unrelated type-Ia SN DATE: 26/08/24 14:07:25 GMT FROM: Daniele Bjørn Malesani at Cosmic Dawn Center, Niels Bohr Institute <daniele.malesani(a)nbi.ku.dk> L. Izzo (INAF/OAC), A. Saccardi (CEA/Irfu), G. Corcoran (UCD), A. Martin-Carrillo (UCD), A. J. Levan (Radboud and Warwick), D. O’Neill (Birmingham), A. L. Thakur (INAF/IAPS), D. B. Malesani (DAWN/NBI and Radboud), N. Globus (UNAM), S. Basa (UAR Pytheas), on behalf of the Stargate collaboration, J. H. Gillanders (Oxford), K. W. Smith, S. J. Smartt (Oxford/QUB), M. Huber, K. C. Chambers (IfA, Univ. Hawaii), on behalf of the Pan-STARRS collaboration, report: We observed the candidate optical afterglow (Globus et al., GCN 45429; Li et al., GCN 45430) of the short GRB 260822A (Schanne et al., GCN 45422) using the ESO VLT UT4 (Yepun) equipped with the MUSE integral field unit spectrograph. Observations began on 2026 August 23 at 09:31:23 UT (0.69 days after the SVOM/ECLAIRs trigger), and consisted of four observations of about 12 min exposure time each. The optical transient lies close to a system of two galaxies, visible in both our data and in archival images. This could be plausibly the host system of the transient. We measure for them the following redshifts: RA = 00:09:45.94, Dec = +01:23:29.8: z = 0.290 from Halpha, [N II], [O III], Hbeta; RA = 00:09:45.91, Dec = +01:23:24.8: z = 0.296 from Halpha, [N II], [O III], Hbeta. At the position of the candidate optical afterglow (Globus et al., GCN 45429), a faint source is detected. Following preliminary extraction and flux calibration, the transient spectrum shows a continuum with a number of broad undulations, typical of supernovae. Template matching via SNID (Blondin & Tonry 2007, doi:10.1086/520494), leaving the redshift free, provides a match with a type-Ia SN post peak at redshift z = 0.291 +- 0.010. Good matches to post-peak type-Ia SNe are also obtained using SNID-SAGE (Stoppa et al. 2026, doi:10.1093/mnras/stag1066). Given the timing of our observation, the SN exploded well before the SVOM/ECLAIRs trigger. Examining recent data obtained during ordinary Pan-STARRS survey coverage (see Fulton et al. 2025, doi:10.1093/mnras/staf1165), we report the following archival detections of the transient: | MJD | Filter | Magnitude (AB) | | -------- | ------ | ------------------ | | 61020.23 | w | >22.8 (3-sigma UL) | | 61247.54 | i | 21.4 +/- 0.2 | | 61263.54 | w | 22.5 +/- 0.4 | These archival detections predate the GRB trigger (MJD 61274.7). Both the photometric and the spectroscopic data thus support the interpretation that this source is a pre-existing transient, unrelated to GRB 260822A. We acknowledge expert support from the observing staff at Paranal, in particular Zahed Wahhaj, Thomas Szeifert and Marcelo Lopez. The Pan-STARRS system comprises 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 (Chambers et al., 2016, ArXiv e-prints, 1612.05560) 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). Discoveries from this program are a byproduct of the Panoramic Survey Telescope and Rapid Response System (Pan-STARRS) NEO survey observations. Operation of the Pan-STARRS1 and Pan-STARRS2 telescopes is primarily supported by the National Aeronautics and Space Administration under Grant No. NNX12AR65G and Grant No. NNX14AM74G issued through the SSO Near-Earth Object Observations Program. Data are processed at Queen's University Belfast enabled through the STFC grants ST/P000312/1 and ST/T000198/1. View this GCN Circular online at https://gcn.nasa.gov/circulars/45435. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 43655] GRB 260818A: further EP-FXT observations and X-ray afterglow confirmation
by GCN Circulars 24 Aug '26

24 Aug '26

TITLE: GCN CIRCULAR NUMBER: 45434 SUBJECT: GRB 260818A: further EP-FXT observations and X-ray afterglow confirmation DATE: 26/08/24 06:29:10 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> C. Plasse (HKU), Z.M. Wang (BNU) and H. Goto (RIKEN, CEA) report on behalf of the SVOM and Einstein Probe teams: We performed two additional observations at the location of the SVOM/ECLAIRs GRB 260818A (Yin et al., GCN 45391) with the Follow-up X-ray Telescope (FXT) on board the Einstein Probe (EP) mission. The observations started on 2026-08-18 at 18:10:40 UT (0.76 days after the trigger) and on 2026-08-20 at 18:05:05 UTC (2.75 days after the trigger), both with a total exposure time of ~6000 s. The source EPF_J232025.8-320549, detected by EP/FXT about 1.67 hr after the SVOM trigger, reported in GCN 45400, fades by a factor 2 in the second observation, from a flux of (13.1 +/- 2.6) x 10^-14 erg/s/cm^-2 down to a flux of (6.7 +/- 1.9) x 10^-14 erg/s/cm^-2 (0.3-10 keV; 1-sigma uncertainty). At this source position of RA, Dec: 350.1064 -32.0978 (with an error radius of 10 arcsec ), 5.9 arcmin from ECLAIRs position, no X-ray source is detected in the third observation. The fading behaviour of this X-ray source confirms it as the afterglow of GRB 260818A. We encourage further multi-wavelength follow-up of this source. 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/45434. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 43654] EP260822a: EP-FXT non-detection and upper limit
by GCN Circulars 23 Aug '26

23 Aug '26

TITLE: GCN CIRCULAR NUMBER: 45433 SUBJECT: EP260822a: EP-FXT non-detection and upper limit DATE: 26/08/24 05:19:05 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> J. P. Feng, B. Zhang (USTC), Y. Q. Zhao (PRIC, USTC) and H. Sun (NAO, CAS) on behalf of the Einstein Probe (EP) team: EP-FXT observed the field of EP260822a (Feng et al., GCN 45428) for 2825 seconds starting at 2026-08-23T05:39:06, around 13.5 hours after the detection by EP-WXT. No significant X-ray source is detected within the 2.6 arcmin radius of the EP-WXT position (Feng et al., GCN 45428) . The derived 0.5-10 keV flux upper limit is 7.55e-14 erg/cm^2/s, assuming a powerlaw intrinsic emission with a photon index of 2 and fixed galactic absorption. 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/45433. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 43653] GRB 260822A: Retraction of GOTO optical counterpart detection GCN 45431
by GCN Circulars 23 Aug '26

23 Aug '26

TITLE: GCN CIRCULAR NUMBER: 45432 SUBJECT: GRB 260822A: Retraction of GOTO optical counterpart detection GCN 45431 DATE: 26/08/23 22:49:28 GMT FROM: d.s.oneill(a)bham.ac.uk D. O'Neill on behalf of GOTO collaboration: Upon further examination, the GOTO optical detection is approximately 6" offset from the optical counterpart reported by Globus et al., GCN 45429 and Li et al. GCN 45430. Using MPChecker (https://minorplanetcenter.net/cgi-bin/checkmp.cgi) we find that the optical detection is consistent with a known MP object 2016 CP289 which is estimated to have a brightness of 20.8 mag, consistent with the GOTO detection. We apologise for any inconvenience caused. 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, the University of Birmingham and the Instituto de Astrofisica de Canarias (IAC). View this GCN Circular online at https://gcn.nasa.gov/circulars/45432. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 43652] GRB 260822A: GOTO optical counterpart detection
by GCN Circulars 23 Aug '26

23 Aug '26

TITLE: GCN CIRCULAR NUMBER: 45431 SUBJECT: GRB 260822A: GOTO optical counterpart detection DATE: 26/08/23 12:55:36 GMT FROM: d.s.oneill(a)bham.ac.uk D. O'Neill, S. Moran, M. Kennedy, R. Starling, B. Gompertz, K. Ackley, M. Dyer, G. Ramsay, J. Lyman, K. Ulaczyk, D. Steeghs, D. Galloway, V. Dhillon, P. O'Brien, K. Noysena, R. Kotak, R. Breton, J. Casares, L. Nuttall, B. Godson, T. Killestein, A. Kumar, M. Pursiainen, on behalf of 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 SVOM/ECLAIRS alert for GRB 260822A (Schanne et al.; GCN #45422). Following the detection of an optical counterpart candidate of GRB 260822A (Globus et al., GCN #45429; Li et al., GCN #45430), we checked the position of the candidate in the targeted GOTO data (O'Neill et al. GCN #45423) and identify the counterpart at a 4-sigma level with magnitude L = 21.00 ± 0.25 AB mag at 2026-08-22 18:28:33 (+1.63h). We note an earlier non-detection with 3-sigma limiting magnitude L > 21.26 AB mag at 2026-08-22 17:21:22 (+0.51h). 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, the University of Birmingham and the Instituto de Astrofisica de Canarias (IAC). View this GCN Circular online at https://gcn.nasa.gov/circulars/45431. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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