November 2024 - vsnet-grb-info - ooruri.kusastro.kyoto-u.ac.jp

[vsnet-grb-info 36342] LIGO/Virgo/KAGRA S241125n: Swift-UVOT Upper Limits
by GCN Circulars 27 Nov '24

27 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38350 SUBJECT: LIGO/Virgo/KAGRA S241125n: Swift-UVOT Upper Limits DATE: 24/11/27 16:50:48 GMT FROM: N. Klingler at NASA-GSFC/UMBC/CRESST II <noelklingler(a)gmail.com> N.J. Klingler (NASA-GSFC / UMBC / CRESST II), S.R. Oates (Lancaster U.), A. Tohuvavohu (U. Toronto), A.A. Breeveld (UCL-MSSL), C. Gronwall (PSU), N.P.M. Kuin (UCL-MSSL), F.E. Marshall (NASA-GSFC), M. De Pasquale (University of Messina), M.J. Page (UCL-MSSL), S. Shilling (Lancaster U.), M.H. Siegel (PSU), A. D’Aì (INAF-IASFPA), P. D’Avanzo (INAF-OAB), A.P. Beardmore (U. Leicester), M.G. Bernardini (INAF-OAB), S. Campana (INAF-OAB), S.B. Cenko (NASA-GSFC), J.J. Delaunay (PSU), S. Dichiara (PSU), V. D’Elia (ASI-SSDC & INAF-OAR), R.A.J.Eyles-Ferris (U. Leicester), P.A. Evans (U. Leicester), R. Gayathri (PSU), D. Hartmann (Clemson University), J.A. Kennea (PSU), S. Laha (NASA/GSFC), H.A. Krimm (NSF), D. B. Malesani (DTU Space), P. O’Brien (U. Leicester), J.P. Osborne (U. Leicester), T. Partosan (NASA-GSFC), M. Perri (ASDC), K.L. Page (U. Leicester), D.M. Palmer (LANL), S. Ronchini (PSU), T. Sbarrato (INAF-OAB), B. Sbarufatti (INAF-OAB), G. Tagliaferri (INAF-OAB), and E. Troja (U. Tor Vergata, INAF) report on behalf of the Swift Team: Swift has carried out observations of the error region of the BAT-GUANO candidate counterpart, which was detected 11.2641 s after T0 of S241125n (DeLaunay et al., GCN Circ. 38308). Swift-UVOT observations were carried out using the White filter for a total of 4.8 ks, spanning from 55 ks to 74 ks after the LVC trigger. No new/uncatalogued sources were detected within the BAT-GUANO localization (RA, Dec = 58.079, +69.689 deg, r=5', 50% containment; GCN Circ. 38308), with an average 3sigma limit on the magnitude >23.2 (AB; White filter). As reported by Evans et al. (GCN Circ. 38324), 5 X-ray sources were seen. However, none of these sources were detected with UVOT. S241125n_X1 and S241125n_X2 were located outside of UVOT's field of view. S241125n_X3 was not detected, with a 3sigma limit on the magnitude (AB) >23.16. S241125n_X4's position was heavily contaminated by image artifacts and coincidence loss from a bright nearby source. S241125n_X5 was not detected, though its position was also affected by an image artifact from a bright nearby source, though to a lesser degree. The precise upper limit at this location can not be accurately determined, but can be approximated as >23. This circular is an official data product of the Swift-UVOT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/38350. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

1 0

[vsnet-grb-info 36341] IceCube-241127A: IceCube observation of a high-energy neutrino candidate track-like event
by GCN Circulars 27 Nov '24

27 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38349 SUBJECT: IceCube-241127A: IceCube observation of a high-energy neutrino candidate track-like event DATE: 24/11/27 16:03:36 GMT FROM: A. Zegarelli at Ruhr University Bochum <azegarelli(a)icecube.wisc.edu> The IceCube Collaboration (http://icecube.wisc.edu/) reports: On 2024-11-27 at 14:11:14.42 UT IceCube detected a track-like event with a high probability of being of astrophysical origin. The event was selected by the ICECUBE_Astrotrack_GOLD alert stream. The average astrophysical neutrino purity for Gold alerts is 50%. This alert has an estimated false alarm rate of 1.28 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/140125_41215060.amon), more sophisticated reconstruction algorithms have been applied offline, with the direction refined to: Date: 2024-11-27 Time: 14:11:14.42 UT RA: 164.09 (+0.46, -0.52 deg 90% PSF containment) J2000 Dec: 5.38 (+0.58, -0.55 deg 90% PSF containment) J2000 No Fermi 4FGL or 3FHL catalog sources are in the 90% uncertainty region. However, given the promising characteristics of the candidate neutrino event, we encourage follow-up by ground and space-based instruments to help identify a possible astrophysical source associated with it. 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/38349. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

1 0

[vsnet-grb-info 36340] LIGO/Virgo/KAGRA S241127aj: NED Galaxies in the Localization Volume
by GCN Circulars 27 Nov '24

27 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38348 SUBJECT: LIGO/Virgo/KAGRA S241127aj: NED Galaxies in the Localization Volume DATE: 24/11/27 14:52:53 GMT FROM: David Cook at Caltech/IPAC-NED <dcook(a)ipac.caltech.edu> David O. Cook (Caltech/IPAC), Rick Ebert (Caltech/IPAC), George Helou (Caltech/IPAC), Joseph M. Mazzarella (Caltech/IPAC), Marion Schmitz (Caltech/IPAC), and Leo Singer (NASA/GSFC) On behalf of the NASA/IPAC Extragalactic Database (NED) Team. We spatially cross-matched the LVK S241127aj-3-Initial sky localization with the NED Local Volume Sample (NED-LVS; Cook et al. 2023), which is a subset of NED with a redshift or redshift-independent distance less than 1000 Mpc. We find 375 galaxies within the 90% containment volume, and we list here the top 20 galaxies sorted by the joint probability of the 3D localization and the WISE W1 luminosity (an observable proxy for stellar mass). For the full or top 20 list of galaxies in the 90% volume go either to the NED Gravitational Wave Followup service at https://ned.ipac.caltech.edu/uri/NED::GWF/ or click on the following links: Full List Download: https://ned.ipac.caltech.edu/uri/NED::GWFglist/fits/S241127aj/3 Top 20 List Download: https://ned.ipac.caltech.edu/uri/NED::GWFglist/fits/S241127aj/3/20 The NED-GWF service provides downloadable galaxy lists and visualizations for candidate host galaxies. For each GW alert, these products are automatically generated and made available within minutes to expedite efficient electromagnetic follow-up observations. The NED top 20 list is sorted by the joint probability of the 3D localization and the WISE W1 luminosity, but users can sort on additional pre-computed prioritization metrics (star formation rate, P_3D * P_SFR; and specific star formation rate, P_3D * P_sSFR; etc.) which are available via downloading the entire galaxy list inside the event's probability volume. | objname| ra| dec|objtype| DistMpc|DistMpc_unc| m_NUV| m_NUV_unc| m_Ks| m_Ks_unc| m_W1| m_W1_unc| P_3D|P_3D_LumW1| |-------------------------|--------------|--------------|-------|-----------|-----------|------------|------------|------------|------------|------------|------------|--------|----------| |WISEA J132117.98-700426.4| 200.32579| -70.07392| G| 720.76| null| null| null| 12.998| 0.187| 11.042| 0.020|6.83e-08| 1.34e-09| |WISEA J123225.10-303341.2| 188.10458| -30.56150| G| 551.29| null| null| null| 13.457| 0.173| 10.413| 0.006|5.71e-08| 1.13e-09| | WKK 1683| 195.50746| -69.54883| G| 411.98| null| null| null| 12.500| 0.178| 9.939| 0.007|5.95e-08| 1.07e-09| | WKK 1959| 198.11004| -68.33072| G| 315.84| 0.55| null| null| 11.470| 0.130| 10.224| 0.012|8.09e-08| 6.51e-10| |WISEA J125433.99-390111.9| 193.64171| -39.02006| G| 840.17| null| null| null| 13.589| 0.176| 10.727| 0.006|1.59e-08| 5.47e-10| |WISEA J124847.18-695639.9| 192.19642| -69.94439| G| 646.47| null| null| null| 13.521| 0.234| 11.863| 0.029|7.38e-08| 5.47e-10| |WISEA J123747.24-313850.1| 189.44683| -31.64747| G| 781.89| 0.49| null| null| 12.754| 0.134| 12.631| 0.017|9.45e-08| 4.88e-10| |WISEA J124706.30-364934.8| 191.77629| -36.82636| G| 830.06| null| null| null| 13.315| 0.157| 11.553| 0.007|3.01e-08| 4.72e-10| |WISEA J132455.49-693406.5| 201.23112| -69.56850| G| 437.92| null| null| null| 13.260| 0.104| 10.339| 0.009|3.34e-08| 4.65e-10| |WISEA J123740.62-313649.6| 189.41925| -31.61381| G| 722.19| null| null| null| 13.336| 0.152| 12.811| 0.016|1.16e-07| 4.33e-10| |WISEA J124714.84-370926.8| 191.81200| -37.15761| G| 893.44| null| null| null| 13.387| 0.175| 11.189| 0.007|1.69e-08| 4.29e-10| |WISEA J123430.15-321012.3| 188.62558| -32.17014| G| 775.60| null| null| null| 13.235| 0.162| 12.175| 0.007|5.55e-08| 4.29e-10| |WISEA J124147.63-342211.4| 190.44854| -34.36983| G| 793.48| null| null| null| 12.976| 0.155| 12.310| 0.015|5.67e-08| 4.04e-10| |WISEA J123049.72-274538.3| 187.70717| -27.76067| G| 623.50| 0.65| null| null| 12.240| 0.131| 12.326| 0.011|8.32e-08| 3.60e-10| |WISEA J124249.24-333427.7| 190.70513| -33.57442| G| 671.43| null| null| null| 13.549| 0.170| 12.653| 0.011|8.67e-08| 3.23e-10| |WISEA J123504.87-303414.8| 188.77025| -30.57083| G| 649.87| null| null| null| 13.244| 0.154| 12.952| 0.012|1.15e-07| 3.05e-10| |WISEA J123610.19-321649.9| 189.04258| -32.28058| G| 716.32| 0.65| 20.323| 0.327| 13.274| 0.176| 12.858| 0.015|8.44e-08| 2.97e-10| |WISEA J124741.34-362923.6| 191.92217| -36.48997| G| 656.72| null| null| null| 13.403| 0.158| 11.898| 0.007|4.15e-08| 2.96e-10| |WISEA J131211.01-690910.9| 198.04579| -69.15317| G| 437.81| null| null| null| 12.829| 0.149| 12.276| 0.038|1.21e-07| 2.87e-10| |WISEA J124059.32-332226.3| 190.24717| -33.37400| G| 744.09| null| null| null| 13.550| 0.195| 13.093| 0.022|8.89e-08| 2.72e-10| Table 1: Top 20 galaxies in NED-LVS that fall in the 90% probability volume for S241127aj sorted by the joint probability of 3D position and WISE W1 luminosity (P_3D * P_LumW1). Galaxy is the NED preferred name. RA and Dec are the Equatorial coordinates in degrees (J2000). Objtype is the object type of the galaxy candidate. Distance is the distance to the galaxy in Mpc. m_NUV and mErr_NUV are the apparent magnitude and error from GALEX. m_Ks and mErr_Ks are the apparent magnitude and error from 2MASS. m_W1 and mErr_W1 are the apparent magnitude and error from AllWISE. P_3D is the probability that the galaxy is in the volume given the distance of GW event. P_3D_LumW1 is the joint probability within the volume weighted by the WISE1 luminosity of the galaxy (P_3D * P_LumW1). View this GCN Circular online at https://gcn.nasa.gov/circulars/38348. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

1 0

[vsnet-grb-info 36338] LIGO/Virgo/KAGRA S241125n: EP-FXT follow-up observations
by GCN Circulars 27 Nov '24

27 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38347 SUBJECT: LIGO/Virgo/KAGRA S241125n: EP-FXT follow-up observations DATE: 24/11/27 14:24:24 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> Y. L. Wang, S. X. Wen, W. X. Wang (NAO, CAS), B.-T. Wang (YNAO, CAS), T. C. Zheng (PMO, CAS), W. Yuan, D. Y. Li, Y. Liu (NAO, CAS), B. Zhang (UNLV) report on behalf of the Einstein Probe team: Following on the trigger of the detection of the gravitational-wave (GW) event S241125n (LIGO/Virgo/KAGRA collaborations, GCN 38305) and the Swift/BAT-GUANO detection of a candidate counterpart (DeLaunay et al., GCN 38308), we performed a target-of-opportunity observation of the BAT position (RA, Dec = 58.079, +69.689 deg) with the Follow-up X-ray Telescope (FXT) on board the Einstein Probe (EP). The observation started at 2024-11-26 03:08:45 (UTC), about 26 hours after the GW event, with an exposure of ~ 11 ks. Within the 5-arcmin error circle of Swift/BAT (50% containment; DeLaunay et al., GCN 38308), one X-ray source is detected by both modules of the EP-FXT, at an averaged position at R.A. = 58.1097 deg, DEC = 69.6392 deg (J2000), with an uncertainty of 10 arcsec (radius, 90% C.L. statistical and systematic). The average 0.5-10 keV spectrum can be fitted with an absorbed power law with a photon index of 0.43 (+0.76/-0.74) (with a column density fixed at the Galactic value of 3.4 x 10^21 cm^-2). The derived average unabsorbed 0.5-10 keV flux is 1.17 (+1.18/-0.63) x 10^(-13) erg/s/cm^2. The uncertainties are at the 90% confidence level for the above parameters. The location of this source is consistent with S241125n_X3, an uncatalogued X-ray source detected by Swift/XRT (Page et al., GCN 38324). Outside the 5-arcmin error circle of the Swift/BAT source position, EP-FXT detected several other X-ray sources, some of which are consistent with the sources reported by Swift/XRT (Page et al., GCN 38324). We list the sources within the 10-arcmin radius in the followed two tables for FXT-A and FXT-B, respectively, with the seperations from the BAT source given. The observed 0.5-10 keV flux given in the tables is a rough estimate assuming the same spectral paramters as quoted before, and is not corrected for absorption. | FXT-A source | R.A. (deg, J2000) | DEC (deg, J2000) | Sep. (arcmin) | Flux (erg/s/cm^2) | | EPF_J035226.4+693824*| 58.1096 | 69.6383 | 3.11 | 1.05 x 10^(-13) | | EPF_J035109.4+693830*| 57.7917 | 69.6411 | 6.64 | 1.52 x 10^(-13) | | EPF_J035330.7+693812 | 58.3826 | 69.6391 | 7.00 | 1.64 x 10^(-13) | | EPF_J035104.0+693411 | 57.7667 | 69.5698 | 9.68 | 2.34 x 10^(-13) | | EPF_J035318.9+693257*| 58.3287 | 69.5492 | 9.88 | 1.28 x 10^(-13) | | EPF_J035113.2+694926*| 57.8023 | 69.8230 | 9.88 | 5.84 x 10^(-13) | | FXT-A source | R.A. (deg, J2000) | DEC (deg, J2000) | Sep. (arcmin) | Flux (erg/s/cm^2) | | EPF_J035226.4+693824*| 58.1098 | 69.6401 | 3.00 | 1.87 x 10^(-13) | | EPF_J035109.4+693830*| 57.7891 | 69.6418 | 6.68 | 2.45 x 10^(-13) | | EPF_J035330.7+693812 | 58.3779 | 69.6368 | 6.98 | 1.52 x 10^(-13) | | EPF_J035044.0+694519 | 57.6832 | 69.7554 | 9.14 | 2.45 x 10^(-13) | | EPF_J035113.2+694926*| 57.8051 | 69.8238 | 9.89 | 7.71 x 10^(-13) | | EPF_J035028.2+694407 | 57.6174 | 69.7353 | 10.00 | 1.17 x 10^(-13) | * sources also detected by Swift/XRT (Page et al., GCN 38324) Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with onboard 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/38347. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

1 0

[vsnet-grb-info 36337] LIGO/Virgo/KAGRA S241125n: EP-FXT follow-up observations
by GCN Circulars 27 Nov '24

27 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38346 SUBJECT: LIGO/Virgo/KAGRA S241125n: EP-FXT follow-up observations DATE: 24/11/27 14:24:18 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> Y. L. Wang, S. X. Wen, W. X. Wang (NAO, CAS), B.-T. Wang (YNAO, CAS), T. C. Zheng (PMO, CAS), W. Yuan, D. Y. Li, Y. Liu (NAO, CAS), B. Zhang (UNLV) report on behalf of the Einstein Probe team: Following on the trigger of the detection of the gravitational-wave (GW) event S241125n (LIGO/Virgo/KAGRA collaborations, GCN 38305) and the Swift/BAT-GUANO detection of a candidate counterpart (DeLaunay et al., GCN 38308), we performed a target-of-opportunity observation of the BAT position (RA, Dec = 58.079, +69.689 deg) with the Follow-up X-ray Telescope (FXT) on board the Einstein Probe (EP). The observation started at 2024-11-26 03:08:45 (UTC), about 26 hours after the GW event, with an exposure of ~ 11 ks. Within the 5-arcmin error circle of Swift/BAT (50% containment; DeLaunay et al., GCN 38308), one X-ray source is detected by both modules of the EP-FXT, at an averaged position at R.A. = 58.1097 deg, DEC = 69.6392 deg (J2000), with an uncertainty of 10 arcsec (radius, 90% C.L. statistical and systematic). The average 0.5-10 keV spectrum can be fitted with an absorbed power law with a photon index of 0.43 (+0.76/-0.74) (with a column density fixed at the Galactic value of 3.4 x 10^21 cm^-2). The derived average unabsorbed 0.5-10 keV flux is 1.17 (+1.18/-0.63) x 10^(-13) erg/s/cm^2. The uncertainties are at the 90% confidence level for the above parameters. The location of this source is consistent with S241125n_X3, an uncatalogued X-ray source detected by Swift/XRT (Page et al., GCN 38324). Outside the 5-arcmin error circle of the Swift/BAT source position, EP-FXT detected several other X-ray sources, some of which are consistent with the sources reported by Swift/XRT (Page et al., GCN 38324). We list the sources within the 10-arcmin radius in the followed two tables for FXT-A and FXT-B, respectively, with the seperations from the BAT source given. The observed 0.5-10 keV flux given in the tables is a rough estimate assuming the same spectral paramters as quoted before, and is not corrected for absorption. | FXT-A source | R.A. (deg, J2000) | DEC (deg, J2000) | Sep. (arcmin) | Flux (erg/s/cm^2) | | EPF_J035226.4+693824*| 58.1096 | 69.6383 | 3.11 | 1.05 x 10^(-13) | | EPF_J035109.4+693830*| 57.7917 | 69.6411 | 6.64 | 1.52 x 10^(-13) | | EPF_J035330.7+693812 | 58.3826 | 69.6391 | 7.00 | 1.64 x 10^(-13) | | EPF_J035104.0+693411 | 57.7667 | 69.5698 | 9.68 | 2.34 x 10^(-13) | | EPF_J035318.9+693257*| 58.3287 | 69.5492 | 9.88 | 1.28 x 10^(-13) | | EPF_J035113.2+694926*| 57.8023 | 69.8230 | 9.88 | 5.84 x 10^(-13) | | FXT-A source | R.A. (deg, J2000) | DEC (deg, J2000) | Sep. (arcmin) | Flux (erg/s/cm^2) | | EPF_J035226.4+693824*| 58.1098 | 69.6401 | 3.00 | 1.87 x 10^(-13) | | EPF_J035109.4+693830*| 57.7891 | 69.6418 | 6.68 | 2.45 x 10^(-13) | | EPF_J035330.7+693812 | 58.3779 | 69.6368 | 6.98 | 1.52 x 10^(-13) | | EPF_J035044.0+694519 | 57.6832 | 69.7554 | 9.14 | 2.45 x 10^(-13) | | EPF_J035113.2+694926*| 57.8051 | 69.8238 | 9.89 | 7.71 x 10^(-13) | | EPF_J035028.2+694407 | 57.6174 | 69.7353 | 10.00 | 1.17 x 10^(-13) | * sources also detected by Swift/XRT (Page et al., GCN 38324) Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with onboard 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/38346. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

1 0

[vsnet-grb-info 36339] LIGO/Virgo/KAGRA S241125n: EP-FXT follow-up observations
by GCN Circulars 27 Nov '24

27 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38345 SUBJECT: LIGO/Virgo/KAGRA S241125n: EP-FXT follow-up observations DATE: 24/11/27 14:24:16 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> Y. L. Wang, S. X. Wen, W. X. Wang (NAO, CAS), B.-T. Wang (YNAO, CAS), T. C. Zheng (PMO, CAS), W. Yuan, D. Y. Li, Y. Liu (NAO, CAS), B. Zhang (UNLV) report on behalf of the Einstein Probe team: Following on the trigger of the detection of the gravitational-wave (GW) event S241125n (LIGO/Virgo/KAGRA collaborations, GCN 38305) and the Swift/BAT-GUANO detection of a candidate counterpart (DeLaunay et al., GCN 38308), we performed a target-of-opportunity observation of the BAT position (RA, Dec = 58.079, +69.689 deg) with the Follow-up X-ray Telescope (FXT) on board the Einstein Probe (EP). The observation started at 2024-11-26 03:08:45 (UTC), about 26 hours after the GW event, with an exposure of ~ 11 ks. Within the 5-arcmin error circle of Swift/BAT (50% containment; DeLaunay et al., GCN 38308), one X-ray source is detected by both modules of the EP-FXT, at an averaged position at R.A. = 58.1097 deg, DEC = 69.6392 deg (J2000), with an uncertainty of 10 arcsec (radius, 90% C.L. statistical and systematic). The average 0.5-10 keV spectrum can be fitted with an absorbed power law with a photon index of 0.43 (+0.76/-0.74) (with a column density fixed at the Galactic value of 3.4 x 10^21 cm^-2). The derived average unabsorbed 0.5-10 keV flux is 1.17 (+1.18/-0.63) x 10^(-13) erg/s/cm^2. The uncertainties are at the 90% confidence level for the above parameters. The location of this source is consistent with S241125n_X3, an uncatalogued X-ray source detected by Swift/XRT (Page et al., GCN 38324). Outside the 5-arcmin error circle of the Swift/BAT source position, EP-FXT detected several other X-ray sources, some of which are consistent with the sources reported by Swift/XRT (Page et al., GCN 38324). We list the sources within the 10-arcmin radius in the followed two tables for FXT-A and FXT-B, respectively, with the seperations from the BAT source given. The observed 0.5-10 keV flux given in the tables is a rough estimate assuming the same spectral paramters as quoted before, and is not corrected for absorption. | FXT-A source | R.A. (deg, J2000) | DEC (deg, J2000) | Sep. (arcmin) | Flux (erg/s/cm^2) | | EPF_J035226.4+693824*| 58.1096 | 69.6383 | 3.11 | 1.05 x 10^(-13) | | EPF_J035109.4+693830*| 57.7917 | 69.6411 | 6.64 | 1.52 x 10^(-13) | | EPF_J035330.7+693812 | 58.3826 | 69.6391 | 7.00 | 1.64 x 10^(-13) | | EPF_J035104.0+693411 | 57.7667 | 69.5698 | 9.68 | 2.34 x 10^(-13) | | EPF_J035318.9+693257*| 58.3287 | 69.5492 | 9.88 | 1.28 x 10^(-13) | | EPF_J035113.2+694926*| 57.8023 | 69.8230 | 9.88 | 5.84 x 10^(-13) | | FXT-A source | R.A. (deg, J2000) | DEC (deg, J2000) | Sep. (arcmin) | Flux (erg/s/cm^2) | | EPF_J035226.4+693824*| 58.1098 | 69.6401 | 3.00 | 1.87 x 10^(-13) | | EPF_J035109.4+693830*| 57.7891 | 69.6418 | 6.68 | 2.45 x 10^(-13) | | EPF_J035330.7+693812 | 58.3779 | 69.6368 | 6.98 | 1.52 x 10^(-13) | | EPF_J035044.0+694519 | 57.6832 | 69.7554 | 9.14 | 2.45 x 10^(-13) | | EPF_J035113.2+694926*| 57.8051 | 69.8238 | 9.89 | 7.71 x 10^(-13) | | EPF_J035028.2+694407 | 57.6174 | 69.7353 | 10.00 | 1.17 x 10^(-13) | * sources also detected by Swift/XRT (Page et al., GCN 38324) Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with onboard 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/38345. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

1 0

[vsnet-grb-info 36336] EP241126a: Optical Upper limits with Kinder observations
by GCN Circulars 27 Nov '24

27 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38344 SUBJECT: EP241126a: Optical Upper limits with Kinder observations DATE: 24/11/27 13:42:19 GMT FROM: Amar Aryan at National Central University, Institute of Astronomy (NCUIA) <amararyan941(a)gmail.com> C.-H. Lai, A. Aryan, T.-W. Chen, Y. J. Yang, C.-S. Lin (all NCU), A. K. H. Kong (NTHU), J. Gillanders (Oxford), S. J. Smartt (Oxford/QUB), A. Sankar. K, Y.-C. Pan, C.-C. Ngeow, M.-H. Lee, H.-C. Lin, W.-J. Hou, H.-Y. Hsiao, J.-K. Guo (all NCU), S. Yang, Z. N. Wang, L. L. Fan, G. H. Sun (all HNAS), H.-W. Lin (UMich), H. F. Stevance, S. Srivastav, L. Rhodes (all Oxford), M. Nicholl, M. Fulton, T. Moore, K. W. Smith, C. Angus, A. Aamer (all QUB), A. Schultz and M. Huber (both IfA, Hawaii) report: We observed the field of the fast X-ray transient EP241126a (Hu et al., GCN 38335, Fu et al., GCN 38337; Li et al., GCN 38338; Zheng et al., GCN 38339) using the 1m LOT at the Lulin Observatory in Taiwan as part of the Kinder collaboration (Chen & Yang et al., 2024 arXiv:2406.09270). The first LOT epoch of observations started at 11:53 UTC on 27th November 2024 (MJD 60641.495), 16.23 hr after the EP-WXT trigger. We utilize the astroalign (Beroiz et al., 2020, A&C, 32, 100384) and astropy (Astropy Collaboration et al., 2022, ApJ, 935, 167) packages to align and stack the individual frames. In our combined frame, we do not detect the optical counterpart proposed by Fu et al. (GCN 38337). The optical counterpart seems to have faded beyond our detection limit. Moreover, we utilize the Python-based package AutoPhOT (Brennan & Fraser, 2022, A&A, 667, A62) to perform PSF photometry on our stacked frames. The details of the observations and measured 3-sigma limits (in the AB system) are as follows: ------------------------------------------------------------------------------------------------------ Telescope | Filter | MJD (start) | t-t0 (hr) | Exposure (s) | Magnitude | avg. Seeing | med. Airmass LOT | r | 60641.495 | 16.23 | 300 * 6 | > 22.5 | 1".37 | 1.10 The presented magnitude was calibrated using the field stars from the Pan-STARRS1 catalog and was not corrected for the expected Galactic foreground extinction corresponding to a reddening of A_r = 0.38 mag in the direction of the transient (Schlafly & Finkbeiner 2011). View this GCN Circular online at https://gcn.nasa.gov/circulars/38344. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

1 0

[vsnet-grb-info 36335] SVOM/GRM observation of GRB 241126B or a short burst from magnetar
by GCN Circulars 27 Nov '24

27 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38343 SUBJECT: SVOM/GRM observation of GRB 241126B or a short burst from magnetar DATE: 24/11/27 12:23:43 GMT FROM: zhengchao_astro(a)foxmail.com SVOM/GRM team: Chao Zheng, Shao-Lin Xiong, Shi-Jie Zheng, Chen-Wei Wang, Yong-Wei Dong, Jiang-Tao Liu, Jian-Chao Sun, Yue Huang, Jiang He, Min Gao, Hao-Xuan Guo, Lu Li, Yong-Ye Li, Hong-Wei Liu, Xin Liu, Hao-Li Shi, Li-Ming Song, You-Li Tuo, Wen-Long Zhang, Wen-Jun Tan, Hao-Xi Wang, Jin Wang, Jin-Zhou Wang, Ping Wang, Rui-Jie Wang, Yu-Xi Wang, Bo-Bing Wu, Jian-Ying Ye, Yi-Tao Yin, Wen-Hui Yu, Fan Zhang, Li Zhang, Peng Zhang, Shuang-Nan Zhang, Yan-Qiu Zhang, Yan-Ting Zhang, Shu-Min Zhao, Xiao-Yun Zhao (IHEP), Maria-Grazia Bernardini (LUPM/INAF-OAB), Laurent Bouchet (IRAP), David Corre (CEA), Tais Maiolino (LUPM), Frédéric Piron (LUPM), Stéphane Schanne (CEA), Jingwei Wang (IAP), JeanLuc Attéia (IRAP) SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (IHEP), Stéphane Basa (LAM), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Frédéric Daigne (IAP), Jin-Song Deng (NAOC), Olivier Godet (IRAP), Andrea Goldwurm (APC), Diego Götz (CEA), Xu-Hui Han (NAOC), Cyril Lachaud (APC), En-Wei Liang (GXU), Yu-Lei Qiu (NAOC), Susanna Vergani (Obs.Paris), Jing Wang (NAOC), Chao Wu (NAOC), Li-Ping Xin (NAOC), Shao-Lin Xiong (IHEP), Bing Zhang (UNLV) report on behalf of the SVOM team: During the commissioning phase, SVOM/GRM was triggered (trigger reference: sb24112602) in-flight by a short burst at 2024-11-26T17:58:15.000 UT (T0). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of multiple pulses with a duration of about 0.09 s. No significant signal could be observed above 70 keV (deposit energy) from the multiple energy band light curves. The SVOM/GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb241126B.png We tentatively name this burst as GRB 241126B, as we note that there is a similar short burst detected by GECAM-B (C. Zheng et al., GCN 38326) and SVOM/GRM (C. Zheng et al., GCN 38327) around 2024-11-26T05:12:17, which was suggested to probably originate from SGR 1830-0645 based on the localization provided by GECAM-B (C. Zheng et al., GCN 38326). Considering the observed features (short duration, soft spectrum, location) of GRB 241126B, and the short time interval between these two bursts, we suggest that GRB 241126B is also likely from SGR 1830-0645. The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), the 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: Chao Zheng (IHEP)(zhengchao97(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/38343. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

1 0

[vsnet-grb-info 36334] GRB 241126A: SVOM/GRM observation
by GCN Circulars 27 Nov '24

27 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38342 SUBJECT: GRB 241126A: SVOM/GRM observation DATE: 24/11/27 11:48:37 GMT FROM: zhengchao_astro(a)foxmail.com SVOM/GRM team: Chao Zheng, Chen-Wei Wang, Shi-Jie Zheng, Yong-Wei Dong, Jiang-Tao Liu, Jian-Chao Sun, Yue Huang, Jiang He, Min Gao, Hao-Xuan Guo, Lu Li, Yong-Ye Li, Hong-Wei Liu, Xin Liu, Hao-Li Shi, Li-Ming Song, You-Li Tuo, Wen-Long Zhang, Wen-Jun Tan, Hao-Xi Wang, Jin Wang, Jin-Zhou Wang, Ping Wang, Rui-Jie Wang, Yu-Xi Wang, Bo-Bing Wu, Shao-Lin Xiong, Jian-Ying Ye, Yi-Tao Yin, Wen-Hui Yu, Fan Zhang, Li Zhang, Peng Zhang, Shuang-Nan Zhang, Yan-Qiu Zhang, Yan-Ting Zhang, Shu-Min Zhao, Xiao-Yun Zhao (IHEP), Maria-Grazia Bernardini (LUPM/INAF-OAB), Laurent Bouchet (IRAP), David Corre (CEA), Tais Maiolino (LUPM), Frédéric Piron (LUPM), Stéphane Schanne (CEA), Jingwei Wang (IAP), JeanLuc Attéia (IRAP) SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (IHEP), Stéphane Basa (LAM), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Frédéric Daigne (IAP), Jin-Song Deng (NAOC), Olivier Godet (IRAP), Andrea Goldwurm (APC), Diego Götz (CEA), Xu-Hui Han (NAOC), Cyril Lachaud (APC), En-Wei Liang (GXU), Yu-Lei Qiu (NAOC), Susanna Vergani (Obs.Paris), Jing Wang (NAOC), Chao Wu (NAOC), Li-Ping Xin (NAOC), Shao-Lin Xiong (IHEP), Bing Zhang (UNLV) report on behalf of the SVOM team: During the commissioning phase, SVOM/GRM was triggered in-flight by GRB 241126A (SVOM trigger reference: sb24112601) at 2024-11-26T05:04:16.000 UT (T0). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of multiple pulses with a duration of about 60 seconds. The SVOM/GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb241126A.png ECLAIRs was not in operation at the time of the burst. 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: Chao Zheng (IHEP)(zhengchao97(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/38342. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

1 0

[vsnet-grb-info 36333] IPN triangulation of GRB 241114B
by GCN Circulars 27 Nov '24

27 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38341 SUBJECT: IPN triangulation of GRB 241114B DATE: 24/11/27 10:20:05 GMT FROM: Dmitry Svinkin at Ioffe Institute <svinkin(a)mail.ioffe.ru> D. Svinkin, D. Frederiks, A. Lysenko, A. Ridnaia, and T. Cline on behalf of the Konus-Wind team, E. Bozzo and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, C. Wang, S. Xiong, S. Zheng and Y. Zhang, on behalf of the Insight-HXMT team, S. Barthelmy, J. Cummings, H. Krimm, D. Palmer, and A. Tohuvavohu on behalf of the Swift-BAT team, E. Burns on behalf of the IPN, and B. Grefenstette on behalf of the NuSTAR team, report: The long-duration GRB 241114B (Insight-HXMT-HE detection: Wang et al., GCN 38284) was detected by Konus-Wind, INTEGRAL (SPI-ACS), Swift (BAT), NuSTAR (AC), and Insight-HXMT (HE) at about 39904 s UT (11:05:04). The burst was outside the coded field of view of the BAT. We have triangulated it to a preliminary, 3 sigma error box whose coordinates are: --------------------------------------------- RA(2000), deg Dec(2000), deg --------------------------------------------- Center: 304.514 (20h 18m 03s) -10.028 (-10d 01' 40") Corners: 302.298 (20h 09m 12s) -7.588 ( -7d 35' 17") 303.748 (20h 15m 00s) -7.242 ( -7d 14' 31") 306.603 (20h 26m 25s) -12.501 (-12d 30' 04") 305.164 (20h 20m 39s) -12.843 (-12d 50' 34") --------------------------------------------- The error box area is 8.4 sq. deg, and its maximum dimension is 6.5 deg (the minimum one is 1.4 deg). The Sun distance was 70 deg. This localization may be improved. A triangulation map and HEALPix FITS file are posted at http://www.ioffe.ru/LEA/GRBs/GRB241114_T39903/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/38341. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

1 0

2025

2024

2023

2022

2021

vsnet-grb-info November 2024