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[vsnet-grb-info 36252] GRB 241117A: SVOM/GRM observation of a short burst with extended emission
by GCN Circulars 18 Nov '24

18 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38266 SUBJECT: GRB 241117A: SVOM/GRM observation of a short burst with extended emission DATE: 24/11/18 03:09:57 GMT FROM: Chenwei Wang at IHEP <cwwang(a)ihep.ac.cn> SVOM/GRM team: 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, Chao Zheng (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, the SVOM/GRM was triggered in-flight by GRB 241117A (SVOM trigger reference: sb24111701) at 2024-11-17T03:00:43.3 UT (T0) , which was also observed by Fermi/GBM (Fermi GBM Team, GCN 38258) The real-time alert data and light curves of SVOM/GRM were downlinked to the ground through the VHF system with low latency. With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that the main emission of this burst consists of multiple pulses with a duration of about 3.2 s, which is followed by a long soft extended emission lasting longer than 70 s. The GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb241117A.png This burst is located at about 72 degrees from the SVOM optical axis, and outside the ECLAIRs field of view. 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 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/38266. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36251] GRB 241117A: Fermi GBM Detection
by GCN Circulars 17 Nov '24

17 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38265 SUBJECT: GRB 241117A: Fermi GBM Detection DATE: 24/11/17 20:47:14 GMT FROM: Lorenzo Scotton at UAH <lscottongcn(a)outlook.com> L. Scotton (UAH) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 03:00:43.23 UT on 17 November 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241117A (trigger 753505248/241117125). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 2.04, Dec = 16.33 (J2000 degrees, equivalent to J2000 0h 8m, +16d 19'), with a statistical uncertainty of 1.74 degrees. (radius, 1-sigma containment, statistical only; there is additionally a systematic error which we have characterized as a mixture of two Gaussians, one with a radius of 1.8 degrees (52% contribution) and one with a radius of 4.1 degrees (47% contribution) [A. Goldstein et al. 2020, ApJ, 895, 1]). The angle from the Fermi LAT boresight is 58 degrees. The GBM light curve consists of a single emission episode with a duration (T90) of about 8.9 s (50-300 keV). The time-averaged spectrum from T0-0.3 to T0+9.86 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.46 +/- 0.07 and the cutoff energy, parameterized as Epeak, is 724 +/- 62 keV. The event fluence (10-1000 keV) in this time interval is (9.7 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+0.58 s in the 10-1000 keV band is 13.2 +/- 0.3 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak = 708 +/- 68 keV, alpha = -0.45 +/- 0.07 and beta = -3.16 +/- 0.98. 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/38265. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36250] Fermi GRB 241117B: Global MASTER-Net observations report
by GCN Circulars 17 Nov '24

17 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38264 SUBJECT: Fermi GRB 241117B: Global MASTER-Net observations report DATE: 24/11/17 20:31:10 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, 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. 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-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 241117B ( Fermi GBM team, GCN 38263) errorbox 109 sec after notice time and 141 sec after trigger time at 2024-11-17 20:19:17 UT, with upper limit up to 17.5 mag. The observations began at zenith distance = 78 deg. The sun altitude is -30.8 deg. The galactic latitude b = -21 deg., longitude l = 76 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2673826 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 157 | 2024-11-17 20:19:17 | MASTER-SAAO | (21h 31m 20.93s , +22d 14m 37.0s) | C | 30 | 17.0 | 192 | 2024-11-17 20:19:17 | MASTER-SAAO | (21h 31m 20.93s , +22d 14m 37.0s) | C | 100 | 17.5 | Coadd 206 | 2024-11-17 20:20:06 | MASTER-SAAO | (21h 31m 21.63s , +22d 14m 38.4s) | C | 30 | 16.9 | 260 | 2024-11-17 20:20:56 | MASTER-SAAO | (21h 31m 22.48s , +22d 14m 39.7s) | C | 40 | 16.9 | 329 | 2024-11-17 20:21:55 | MASTER-SAAO | (21h 31m 23.55s , +22d 14m 42.0s) | C | 60 | 16.8 | 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/38264. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36249] GRB 241117B: Fermi GBM Final Real-time Localization
by GCN Circulars 17 Nov '24

17 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38263 SUBJECT: GRB 241117B: Fermi GBM Final Real-time Localization DATE: 24/11/17 20:27:34 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 20:16:55 UT on 17 Nov 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241117B (trigger 753567420.985494 / 241117845). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 323.5, Dec = 23.5 (J2000 degrees, equivalent to J2000 21h 33m, 23d 30'), with a statistical uncertainty of 1.7 degrees. The angle from the Fermi LAT boresight is 65.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241117845/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241117845/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241117845/… View this GCN Circular online at https://gcn.nasa.gov/circulars/38263. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36248] IceCube-Cascade 241116A: Upper limits from a search for additional neutrino events in IceCube
by GCN Circulars 17 Nov '24

17 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38262 SUBJECT: IceCube-Cascade 241116A: Upper limits from a search for additional neutrino events in IceCube DATE: 24/11/17 19:08:01 GMT FROM: Jessie Thwaites at IceCube/U Wisc-Madison <thwaites(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 241116A (https://gcn.gsfc.nasa.gov/notices_amon_icecube_cascade/140090_5847360.amon) in a time range of 1000 seconds centered on the alert event time (2024-11-16 14:23:58.900 UTC to 2024-11-16 14:40:38.900 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 241116A.The IceCube sensitivity to neutrino point sources with an E^-2.5 spectrum (E^2 dN/dE at 1 TeV) within the locations spanned by the 90% spatial containment region of IceCube-Cascade 241116A ranges from 1.9e+01 to 2.4e+01 GeV cm^-2 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 5e+04 GeV and 4e+06 GeV. A subsequent search was performed including 2 days of data centered on the alert event time (2024-11-15 14:32:18.900 UTC to 2024-11-17 14:32:18.900 UTC). In this case, we report a p-value of 0.45, consistent with no significant excess of track events. The IceCube sensitivity to neutrino point sources with an E^-2.5 spectrum (E^2 dN/dE at 1 TeV) within the locations spanned by the 90% spatial containment region of IceCube-Cascade 241116A ranges from 1.9e+01 to 2.7e+01 GeV cm^-2 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/38262. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36247] LIGO/Virgo/KAGRA S241116cq: Updated Sky localization
by GCN Circulars 17 Nov '24

17 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38261 SUBJECT: LIGO/Virgo/KAGRA S241116cq: Updated Sky localization DATE: 24/11/17 08:28:18 GMT FROM: jgolomb(a)caltech.edu The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We have conducted further analysis of the LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) data around the time of the compact binary merger (CBC) candidate S241116cq (GCN Circular 38255). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.offline0.multiorder.fits,0, distributed via GCN Notice, is available for retrieval from the GraceDB event page: https://gracedb.ligo.org/superevents/S241116cq For the Bilby.offline0.multiorder.fits,0 sky map, the 90% credible region is 2292 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 5600 +/- 2218 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/. [1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. PRD 108, 123040 (2023) doi:10.1103/PhysRevD.108.123040 View this GCN Circular online at https://gcn.nasa.gov/circulars/38261. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36246] GRB 241115B: Swift/BAT-GUANO localization skymap of a long burst
by GCN Circulars 17 Nov '24

17 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38260 SUBJECT: GRB 241115B: Swift/BAT-GUANO localization skymap of a long burst DATE: 24/11/17 03:54:42 GMT FROM: Samuele Ronchini at PSU <sjs8171(a)psu.edu> Samuele Ronchini (PSU), James DeLaunay (PSU), Aaron Tohuvavohu (Caltech), Gayathri Raman (PSU), Jamie A. Kennea (PSU), Tyler Parsotan (NASA GSFC) report: Swift/BAT did not localize GRB 241115B onboard (T0: 2024-11-15T18:07:25.97 UTC, Fermi GCN 38241) The Fermi notice, distributed in near real-time, triggered the Swift Mission Operations Center operated Gamma-ray Urgent Archiver for Novel Opportunities (GUANO; Tohuvavohu et al. 2020, ApJ, 900, 1). Upon trigger by this notice, GUANO sent a command to the Swift Burst Alert Telescope (BAT) to save 200 seconds of BAT event-mode data from [-50,+150] seconds around the time of the burst. All the requested event mode data was delivered to the ground. The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu 2022, ApJ, 941, 169), performed on the temporal window [T0-20 s, T0+20 s], detects the burst with a sqrt(TS) of 15.25 in a 2.048 s analysis time bin, starting at T0 + 12.8001 s. Using the NITRATES analysis, parameter estimation was performed to obtain the localization of this burst in the form of a HEALPIX Multi-Order Coverage (MOC) skymap. This localization accounts for both statistical and systematic errors. More details in the creation and calibration of these maps will soon be published (DeLaunay et al. 2024. in prep) The 90% credible area is 12371 deg2 and the 50% credible area is 3770 deg2. The integrated probability inside the coded field of view is <1%. The NITRATES skymap is consistent with the Fermi localization reported in the final position notice. The combined Fermi/GBM+NITRATES 90% credible area is 286 deg2 and the 50% credible area is 82 deg2. A plot of the probability skymap can be viewed here: [skymap_plot](https://guano.swift.psu.edu/trigger_report?id=753386880/#:~:te… The probability skymap file can be downloaded from the link here [skymap_fits_file](https://guano.swift.psu.edu/files/753386880/0_n_PROBMAP) Instructions on how to read and manipulate this map can be found here: https://guano.swift.psu.edu/documentation More details about this burst can be found on the trigger report page here: https://guano.swift.psu.edu/trigger_report?id=753386880 GUANO is a fully autonomous, extremely low latency, spacecraft commanding pipeline designed for targeted recovery of BAT event mode data around the times of compelling astrophysical events to enable more sensitive GRB searches. A live reporting of Swift/BAT event data recovered by GUANO can be found at: https://www.swift.psu.edu/guano/ View this GCN Circular online at https://gcn.nasa.gov/circulars/38260. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36245] Fermi GRB 241117A: Global MASTER-Net observations report
by GCN Circulars 17 Nov '24

17 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38259 SUBJECT: Fermi GRB 241117A: Global MASTER-Net observations report DATE: 24/11/17 03:15:26 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, 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. 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-OAFA robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 241117A ( Fermi GBM team, GCN 38258) errorbox 113 sec after notice time and 156 sec after trigger time at 2024-11-17 03:03:20 UT, with upper limit up to 19.5 mag. The observations began at zenith distance = 55 deg. The sun altitude is -36.8 deg. The galactic latitude b = -45 deg., longitude l = 109 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2672996 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 162 | 2024-11-17 03:03:20 | MASTER-OAFA | (00h 20m 31.03s , +16d 32m 14.8s) | C | 10 | 16.9 | 187 | 2024-11-17 03:03:20 | MASTER-OAFA | (00h 20m 31.02s , +16d 32m 14.7s) | C | 60 | 18.0 | Coadd 172 | 2024-11-17 03:03:20 | MASTER-OAFA | (00h 11m 05.86s , +16d 08m 16.7s) | C | 30 | 18.6 | 217 | 2024-11-17 03:03:20 | MASTER-OAFA | (00h 11m 05.86s , +16d 08m 16.7s) | C | 120 | 19.5 | Coadd 203 | 2024-11-17 03:03:56 | MASTER-OAFA | (00h 20m 31.02s , +16d 32m 16.3s) | C | 20 | 17.3 | 214 | 2024-11-17 03:03:56 | MASTER-OAFA | (00h 11m 05.84s , +16d 08m 17.6s) | C | 40 | 18.8 | 254 | 2024-11-17 03:04:42 | MASTER-OAFA | (00h 20m 30.98s , +16d 32m 18.3s) | C | 30 | 17.5 | 265 | 2024-11-17 03:04:42 | MASTER-OAFA | (00h 11m 05.80s , +16d 08m 18.4s) | C | 50 | 18.8 | 315 | 2024-11-17 03:05:38 | MASTER-OAFA | (00h 20m 30.94s , +16d 32m 20.4s) | C | 40 | 17.8 | 375 | 2024-11-17 03:05:38 | MASTER-OAFA | (00h 20m 30.94s , +16d 32m 20.4s) | C | 160 | 18.5 | Coadd 326 | 2024-11-17 03:05:38 | MASTER-OAFA | (00h 11m 05.80s , +16d 08m 19.5s) | C | 60 | 18.9 | 386 | 2024-11-17 03:06:44 | MASTER-OAFA | (00h 20m 30.93s , +16d 32m 22.4s) | C | 50 | 17.8 | 397 | 2024-11-17 03:06:44 | MASTER-OAFA | (00h 11m 05.76s , +16d 08m 20.9s) | C | 70 | 19.0 | 473 | 2024-11-17 03:08:01 | MASTER-OAFA | (00h 20m 30.89s , +16d 32m 24.5s) | C | 70 | 17.9 | 483 | 2024-11-17 03:08:01 | MASTER-OAFA | (00h 11m 05.72s , +16d 08m 22.0s) | C | 90 | 19.0 | 579 | 2024-11-17 03:09:37 | MASTER-OAFA | (00h 20m 30.85s , +16d 32m 26.6s) | C | 90 | 18.0 | 590 | 2024-11-17 03:09:37 | MASTER-OAFA | (00h 11m 05.68s , +16d 08m 23.7s) | C | 110 | 19.1 | 679 | 2024-11-17 03:11:40 | MASTER-OAFA | (00h 08m 08.45s , +16d 24m 27.9s) | C | 43.3333 | 18.7 | 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/38259. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36244] GRB 241117A: Fermi GBM Final Real-time Localization
by GCN Circulars 17 Nov '24

17 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38258 SUBJECT: GRB 241117A: Fermi GBM Final Real-time Localization DATE: 24/11/17 03:11:11 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 03:00:43 UT on 17 Nov 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241117A (trigger 753505248.23077 / 241117125). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 2.0, Dec = 16.3 (J2000 degrees, equivalent to J2000 00h 08m, 16d 18'), with a statistical uncertainty of 1.7 degrees. The angle from the Fermi LAT boresight is 58.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241117125/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241117125/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241117125/… View this GCN Circular online at https://gcn.nasa.gov/circulars/38258. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36243] GRB 241115C: Fermi GBM Observation
by GCN Circulars 16 Nov '24

16 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38257 SUBJECT: GRB 241115C: Fermi GBM Observation DATE: 24/11/16 21:50:57 GMT FROM: Lorenzo Scotton at UAH <lscottongcn(a)outlook.com> L. Scotton (UAH), S. Dalessi (UAH) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 04:35:33.96 UT on 15 November 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241115C (trigger 753338138/241115191). which was also detected by Swift/BAT-GUANO (S. Ronchini et al. 2024, GCN 38245). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 257.26, Dec = 16.20 (J2000 degrees, equivalent to J2000 17h 9m, +16d 11'), with a statistical uncertainty of 4.91 degrees. The Fermi GBM on-ground location is consistent with the Swift/BAT-NITRATES position. The angle from the Fermi LAT boresight is 66 degrees. The GBM light curve consists of a single emission episode with a duration (T90) of about 5.1 s (50-300 keV). The time-averaged spectrum from T0-1.0 to T0+7.0 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -1.77 +/- 0.08 and the cutoff energy, parameterized as Epeak, is 53 +/- 7 keV. The event fluence (10-1000 keV) in this time interval is (2.1 +/- 0.1)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+0.32 s in the 10-1000 keV band is 9.9 +/- 0.4 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak = 51 +/- 7 keV, alpha = -1.72 +/- 0.11 and beta = -2.61 +/- 0.49. 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/38257. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36242] GRB 241115A: Swift-XRT afterglow detection
by GCN Circulars 16 Nov '24

16 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38256 SUBJECT: GRB 241115A: Swift-XRT afterglow detection DATE: 24/11/16 21:27:36 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> R. Brivio (INAF-OAB), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAR), D.N. Burrows (PSU), M. A. Williams (PSU), S. Dichiara (PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester) and P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the Swift-BAT-detected burst GRB 241115A, collecting 11.3 ks of Photon Counting (PC) mode data between T0+92 s and T0+102.8 ks. An uncatalogued X-ray source is detected consistent with being within 296 arcsec of the Swift-BAT position and is above the RASS 3-sigma upper limit at this position and fading with >3-sigma significance, and is therefore likely the GRB afterglow. Using 2620 s of PC mode data and 5 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 = 86.77097, -0.67462 which is equivalent to: RA (J2000): 05h 47m 05.03s Dec(J2000): -00d 40' 28.6" with an uncertainty of 2.2 arcsec (radius, 90% confidence). This position is 50 arcsec from the Swift-BAT position. The light curve can be modelled with a power-law decay with a decay index of alpha=1.13 (+/-0.07). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.0 (+/-0.4). The best-fitting absorption column is 1.7 (+0.6, -0.5) x 10^22 cm^-2, in excess of the Galactic value of 3.3 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 5.9 x 10^-11 (1.2 x 10^-10) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.7 (+0.6, -0.5) x 10^22 cm^-2 Galactic foreground: 3.3 x 10^21 cm^-2 Excess significance: 4.5 sigma Photon index: 2.0 (+/-0.4) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01267921. The results of the full analysis of the XRT observations are available at https://www.swift.ac.uk/ToO_GRBs/01267921. This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/38256. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36241] LIGO/Virgo/KAGRA S241116cq: Identification of a GW compact binary merger candidate
by GCN Circulars 16 Nov '24

16 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38255 SUBJECT: LIGO/Virgo/KAGRA S241116cq: Identification of a GW compact binary merger candidate DATE: 24/11/16 15:55:06 GMT FROM: joan-rene.merou(a)ligo.org The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We identified the compact binary merger candidate S241116cq during real-time processing of data from LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) at 2024-11-16 15:17:53.684 UTC (GPS time: 1415805491.684). The candidate was found by the cWB BBH [1], GstLAL [2], MBTA [3], and PyCBC Live [4] analysis pipelines. S241116cq is an event of interest because its false alarm rate, as estimated by the online analysis, is 7e-09 Hz, or about one in 4 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S241116cq The classification of the GW signal, in order of descending probability, is BBH (>99%), Terrestrial (<1%), BNS (<1%), or NSBH (<1%). Assuming the candidate is astrophysical in origin, the probability that the lighter compact object is consistent with a neutron star mass (HasNS) is <1%. [5] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [5] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%. Two sky maps are available at this time and can be retrieved from the GraceDB event page: * bayestar.multiorder.fits,0, an initial localization generated by BAYESTAR [6], distributed via GCN notice about 30 seconds after the candidate event time. * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [6], distributed via GCN notice about 5 minutes after the candidate event time. The preferred sky map at this time is bayestar.multiorder.fits,1. For the bayestar.multiorder.fits,1 sky map, the 90% credible region is 2222 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 4374 +/- 1228 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/. [1] T. Mishra et al. PRD 105, 083018 (2022) doi:10.1103/PhysRevD.105.083018 [2] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. (2023) arXiv:2305.05625 [3] Aubin et al. CQG 38, 095004 (2021) doi:10.1088/1361-6382/abe913 [4] Dal Canton et al. ApJ 923, 254 (2021) doi:10.3847/1538-4357/ac2f9a [5] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe [6] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013 View this GCN Circular online at https://gcn.nasa.gov/circulars/38255. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36240] EP241115a/GRB 241115D: Optical upper limits with Kinder observations
by GCN Circulars 16 Nov '24

16 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38254 SUBJECT: EP241115a/GRB 241115D: Optical upper limits with Kinder observations DATE: 24/11/16 15:29:35 GMT FROM: Janet Chen at National Central University <janetstars(a)gmail.com> L. L. Fan (HNAS), A. Aryan, T.-W. Chen, H.-Y. Hsiao (all NCU), A. K. H. Kong (NTHU), J. Gillanders (Oxford), S. J. Smartt (Oxford/QUB), Y. J. Yang, A. Sankar. K, Y.-C. Pan, C.-C. Ngeow, M.-H. Lee, H.-C. Lin, C.-H. Lai, W.-J. Hou, C.-S. Lin, J.-K. Guo (all NCU), S. Yang, Z. N. Wang, 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 EP241115a/GRB 241115D (Hu et al., GCN 38239; Dai et al., GCN 38251; Lipunov et al., GCN 38242; SVOM/GRM team + SVOM JSWG, GCN 38250) using the 40cm SLT and 1m LOT at Lulin Observatory in Taiwan as part of the Kinder collaboration (Chen & Yang et al., 2024arXiv240609270C). We utilized 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. We do not find any new and uncataloged optical source in the stacked frames within the 4.3-arcsecond error circle of the Swift-XRT localization (Dai et al., GCN 38251). Moreover, we utilized the Python-based package AutoPhOT (Brennan & Fraser, 2022, A&A, 667, A62) to perform the PSF photometry on our stacked frames. The details of the observations and measured 3-sigma upper limit (in the AB system) are as follows: -------------------------------------------------------------------------------------------- The first SLT epoch of observations started at 12:26 UTC on the 16th of November 2024 (MJD = 60630.518), 1.28d after the EP WXT trigger. Telescope | Filter | MJD (start) | t-t0 (d) | Exposure (s) | Magnitude | avg. Seeing | med. Airmass SLT | r | 60630.518 | 1.28 | 300 * 6 | > 20.5 | 2".45 | 1.36 -------------------------------------------------------------------------------------------- The first LOT epoch of observations started at 13:06 UTC on the 16th of November 2024 (MJD = 60630.546), 1.30d after the EP WXT trigger. Telescope | Filter | MJD (start) | t-t0 (d) | Exposure (s) | Magnitude | avg. Seeing | med. Airmass LOT | r | 60630.546 | 1.30 | 300 * 6 | > 21.7 | 1".44 | 1.33 The presented magnitudes are calibrated using the field stars from the Pan-STARRS1 catalog and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E(B-V) = 0.02 mag in the direction of the transient (Schlafly & Finkbeiner 2011). View this GCN Circular online at https://gcn.nasa.gov/circulars/38254. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36239] GRB 241115A: Mephisto upper limits
by GCN Circulars 16 Nov '24

16 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38253 SUBJECT: GRB 241115A: Mephisto upper limits DATE: 24/11/16 14:26:24 GMT FROM: Brajesh Kumar at SWIFAR, YNU <brajesh(a)ynu.edu.cn> Guowang Du, Brajesh Kumar, Weikang Lin, Yehao Cheng, Yaosong Yu, Yu Pan, Xingzhu Zou, Xinlei Chen, Jinghua Zhang, Yuanpei Yang, Yuan Fang, Xiangkun Liu, Xiaowei Liu (SWIFAR, YNU) report on behalf of the Mephisto Team: The field of GRB 241115A (Williams et al., GCN 38235)was observed with the 1.6m Multi-channel Photometric Survey Telescope (Mephisto) of Yunnan University located at Lijiang Observatory starting from 15:54:07 UT 2024-11-15 (~2.6 hr after the trigger). Multiple frames with 180s and 50s exposures in uvgr bands were taken. No new source is detected in our stacked images, consistent to Lipunov et al., (GCN 38237) and Strausbaugh & Cucchiara (GCN 38246). The 3-sigma upper limits are listed below. Start_Time(UT) Band Exp(s) Lim-mag(AB) 2024-11-15T15:54:07 u 180*3 >20.35 2024-11-15T16:04:30 v 180*3 >20.65 2024-11-15T15:54:07 g 50*9 >21.06 2024-11-15T16:04:31 r 50*9 >21.38 -------------------------------------------------------------------------- Mephisto (Multi-channel Photometric Survey Telescope) is a 1.6m wide-field multi-channel telescope, the first of its type in the world, capable of imaging the same field of view in three optical bands simultaneously. It provides real-time, high-quality colors of stellar objects. The on-site telescope assemblage and commissioning were carried out in September 2022. The first light in all three channels was achieved on 2023 December 21. -------------------------------------------------------------------------- View this GCN Circular online at https://gcn.nasa.gov/circulars/38253. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36238] GRB 241113B: Mephisto upper limits
by GCN Circulars 16 Nov '24

16 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38252 SUBJECT: GRB 241113B: Mephisto upper limits DATE: 24/11/16 14:23:37 GMT FROM: Brajesh Kumar at SWIFAR, YNU <brajesh(a)ynu.edu.cn> Guowang Du, Brajesh Kumar, Weikang Lin, Yaosong Yu, Yehao Cheng, Yu Pan, Xinlei Chen, Xingzhu Zou, Jinghua Zhang, Yuanpei Yang, Yuan Fang (all SWIFAR, YNU), Xuhui Han, Pinpin Zhang, Liping Xin, Chao Wu (all NAOC), Xiangkun Liu, Xiaowei Liu (all SWIFAR, YNU) report on behalf of the Mephisto Team: The field of GRB 241113B (SVOM/ECLAIRs, Dagoneau et al., GCN 38196; SVOM/GRM, Liu et al., GCN 38212; EP/WXT, Liu et al., GCN 38214) was observed with the 1.6m Multi-channel Photometric Survey Telescope (Mephisto) of Yunnan University located at Lijiang Observatory starting from 16:17:01 UT 2024-11-13 (~4.9 hr after the trigger). Six simultaneous frames in vrz bands were taken with 300s each exposure. The optical afterglow candidate reported by Zheng et al. (GCN 38232) is not visible in our stacked images. The 3-sigma upper limits are below. Start_Time(UT) Band Exp(s) Lim-mag(AB) 2024-11-13T16:17:01 v 300*6 >22.18 2024-11-13T16:17:01 r 300*6 >22.79 2024-11-13T16:17:01 z 300*6 >21.07 -------------------------------------------------------------------------- Mephisto (Multi-channel Photometric Survey Telescope) is a 1.6m wide-field multi-channel telescope, the first of its type in the world, capable of imaging the same field of view in three optical bands simultaneously. It provides real-time, high-quality colors of stellar objects. The on-site telescope assemblage and commissioning were carried out in September 2022. The first light in all three channels was achieved on 2023 December 21. -------------------------------------------------------------------------- View this GCN Circular online at https://gcn.nasa.gov/circulars/38252. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36237] EP241115a/GRB 241115D: Swift/XRT follow-up observation
by GCN Circulars 16 Nov '24

16 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38251 SUBJECT: EP241115a/GRB 241115D: Swift/XRT follow-up observation DATE: 24/11/16 12:07:06 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> C. Y. Dai (NJU),M. Q. Huang, Z. Y. Liu (USTC), Y. J. Zhang (THU), C. X. Zhang (HUST), J. W. Hu, Y. Liu (NAO, CAS) on behalf of the Einstein Probe team Following up on the new X-ray transient EP241115a detected by the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) mission (Hu et al., GCN 38239), which was associated with the GRB 241115D (Wang et al., GCN 38250), we performed a target of opportunity observation with Swift about 24 hours later. The Swift XRT observation began at 2024-11-16 at 06:00:03 (UTC) with an exposure time of 1448 seconds in the Photon Counting mode. An uncatalogued X-ray source was detected at R.A. = 19.4188 deg, DEC = -17.9596 deg (J2000) with an uncertainty of about 4.3 arcsec (radius, 90% C.L. statistical and systematic) and a signal-to-noise (S/N) ratio of 6.98, which is consistent with the position of the WXT transient within the uncertainties. We suggest that this XRT source is most likely associated with EP241115a. The average XRT spectrum can be fitted with an absorbed power law with a photon index of 1.50(+/-0.38) (with a column density fixed at the Galactic one of 1.6 x 10^20 cm^-2). The derived average unabsorbed 0.3-10 keV flux is 2.1(+0.9/-0.5) x 10^(-12) erg/s/cm^2. The uncertainties are at the 90% confidence level for the above parameters. We thank the Neil Gehrels Swift Observatory team for making the X-ray observation possible. View this GCN Circular online at https://gcn.nasa.gov/circulars/38251. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36236] GRB 241115D / EP 241115a: SVOM/GRM observation
by GCN Circulars 16 Nov '24

16 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38250 SUBJECT: GRB 241115D / EP 241115a: SVOM/GRM observation DATE: 24/11/16 09:46:30 GMT FROM: Chenwei Wang at IHEP <cwwang(a)ihep.ac.cn> SVOM/GRM team: 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, Chao Zheng (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, the SVOM/GRM was triggered in-flight by GRB 241115D / EP 241115a at 2024-11-15T05:45:36 UT (T0). The time and localization are in consistent with EP241115a (J. W. Hu et al., GCN 38239). The real-time alert data and light curves of SVOM/GRM were downlinked to the ground through the VHF system with low latency. 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 T90 of 45 +3/-4 s. The GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb241115D.png This burst is located at about 60 degrees from the SVOM optical axis, and outside the ECLAIRs field of view. At the time of the burst, ECLAIRs was not collecting data. 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 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/38250. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36235] The EP-WXT trigger 01709120856 is likely a flaring star
by GCN Circulars 16 Nov '24

16 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38249 SUBJECT: The EP-WXT trigger 01709120856 is likely a flaring star DATE: 24/11/16 08:39:07 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> Q. Y. Wu, D. H. Zhao (NAO, CAS), C. Y. Dai (NJU), Y. C. Fu (BNU), C. X. Zhang (HUST), Y. Liu (NAO,CAS) report on behalf of the Einstein Probe team: The EP-WXT trigger on 2024-11-16T07:42:57.649 (UTC), with the GCN Notice ID 01709120856, is likely a stellar flare associated with a double or multiple star system BPS CS 31060-0015. The estimated flux of the flare is around 8 x 10^-11 erg/s/cm^2 in 0.5-4 keV, corresponding to a X-ray luminosity of around 3 x 10^30 erg/s, which is a typical value for a M-type dwarf. 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/38249. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36234] EP241113a: Swift XRT weak detection
by GCN Circulars 16 Nov '24

16 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38248 SUBJECT: EP241113a: Swift XRT weak detection DATE: 24/11/16 03:29:12 GMT FROM: P.G. Jonker at Radboud University <p.jonker(a)astro.ru.nl> P.G. Jonker (Radboud Univ.), D. Malesani (DAWN/NBI and Radboud Univ.) and A. Levan (Radboud Univ. & Warwick Univ.) report on behalf of a larger collaboration: We observed the field of EP241113a (Liu et al., GCN 38221) with Swift/XRT starting on 2024-11-15 at 21:10:03 (UTC) for ~3325 seconds. We detect a faint X-ray source at an astrometrically corrected position RA, Dec = 131.9998, 52.3819 (=08 47 59.95, +52 22 55.0) with an error radius of 14.2′′ (90% confidence) using the XRT UK build products website (Goad et al. 2007, A&A, 476, 1401; Evans et al. 2009, MNRAS, 397, 1177). This position is consistent with that of the Einstein Probe Follow-up X-ray Telescope position (Liu et al., GCN 38221). This position is also consistent with the object reported by Rossi et al. (GCN 38233), but also with the galaxy 2MASX J08480182+5222544 with a measured spectroscopic redshift of z=0.115. An approximate X-ray flux of 1E-13 erg cm^-2 s^-1 (0.3-10 keV) was derived using a powerlaw with an index fixed to 2 and Galactic absorption fixed to 3E20 cm^-2 using C-stat. View this GCN Circular online at https://gcn.nasa.gov/circulars/38248. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36233] GRB 241115A: Fermi GBM Observation
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38247 SUBJECT: GRB 241115A: Fermi GBM Observation DATE: 24/11/15 23:08:01 GMT FROM: Cuán de Barra at UCD <cuan.debarra(a)ucdconnect.ie> C. de Barra (University College Dublin), M. Dafčíková (Masaryk U.), and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 13:18:24.73 UT on 15 November 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241115A (trigger 753369509/241115554). which was also detected by Swift BAT (M. A. Williams et al. 2024, GCN 38235). The Fermi GBM on-ground location is consistent with the Swift BAT position. The angle from the Fermi LAT boresight is 46 degrees. The GBM light curve consists of a single emission episode with a duration (T90) of about 3.1 s (50-300 keV). The time-averaged spectrum from T0-3.4 to T0+5.8 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.7 +/- 0.1 and the cutoff energy, parameterized as Epeak, is 90 +/- 7 keV. The event fluence (10-1000 keV) in this time interval is (1.57 +/- 0.08)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+0.32 s in the 10-1000 keV band is 7.7 +/- 0.3 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 80 +/- 9 keV, alpha = -0.6 +/- 0.2 and beta = -2.7 +/- 0.4. 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/38247. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36232] GRB 241115A: LCOGT Optical Upper Limits
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38246 SUBJECT: GRB 241115A: LCOGT Optical Upper Limits DATE: 24/11/15 22:53:03 GMT FROM: Robert Strausbaugh at Eastern Illinois University <rstrausbaugh(a)eiu.edu> R. Strausbaugh (Eastern Illinois University), A. Cucchiara (NASA) report on behalf of a larger collaboration: We observed the Swift GRB 241115A field (Williams et al., GCN 38235) with the LCOGT 1-meter Sinistro instrument at the South African Astronomical Observatory site, on November 15, from 21:52 to 22:24 UT (corresponding to 8.57 to 9.10 hours after the GRB trigger time) with the sdss r and i filters. We performed a series of 3x300s exposures in i- and r-bands. We do not detect a source within the Swift XRT error region in either band. The following 5-sigma upper limits are calculated using the PanSTARRS catalog as reference: r > 21.5 i > 21.2 These magnitudes are not corrected for galactic extinction. View this GCN Circular online at https://gcn.nasa.gov/circulars/38246. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36231] GRB 241115C: Swift/BAT-GUANO localization skymap of a burst
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38245 SUBJECT: GRB 241115C: Swift/BAT-GUANO localization skymap of a burst DATE: 24/11/15 20:45:18 GMT FROM: Samuele Ronchini at PSU <sjs8171(a)psu.edu> Samuele Ronchini (PSU), James DeLaunay (PSU), Aaron Tohuvavohu (Caltech), Gayathri Raman (PSU), Jamie A. Kennea (PSU), Tyler Parsotan (NASA GSFC) report: Swift/BAT did not localize GRB 241115C onboard (T0: 2024-11-15T04:35:33.96 UTC, Fermi trig 753338138) The Fermi notice, distributed in near real-time, triggered the Swift Mission Operations Center operated Gamma-ray Urgent Archiver for Novel Opportunities (GUANO; Tohuvavohu et al. 2020, ApJ, 900, 1). Upon trigger by this notice, GUANO sent a command to the Swift Burst Alert Telescope (BAT) to save 200 seconds of BAT event-mode data from [-50,+150] seconds around the time of the burst. All the requested event mode data was delivered to the ground. The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu 2022, ApJ, 941, 169), performed on the temporal window [T0-20 s, T0+20 s], detects the burst with a sqrt(TS) of 14.65 in a 2.048 s analysis time bin, starting at T0 - 0.5119 s. Using the NITRATES analysis, parameter estimation was performed to obtain the localization of this burst in the form of a HEALPIX Multi-Order Coverage (MOC) skymap. This localization accounts for both statistical and systematic errors. More details in the creation and calibration of these maps will soon be published (DeLaunay et al. 2024. in prep) The 90% credible area is 2,129 deg2 and the 50% credible area is 416 deg2. The integrated probability inside the coded field of view is 1%. The NITRATES skymap is consistent with the Fermi localization reported in the final position notice. The combined Fermi/GBM+NITRATES 90% credible area is 245 deg2 and the 50% credible area is 63 deg2. A plot of the probability skymap can be viewed here: [skymap_plot](https://guano.swift.psu.edu/trigger_report?id=753338168/#:~:te… The probability skymap file can be downloaded from the link here [skymap_fits_file](https://guano.swift.psu.edu/files/753338168/0_n_PROBMAP) Instructions on how to read and manipulate this map can be found here: https://guano.swift.psu.edu/documentation More details about this burst can be found on the trigger report page here: https://guano.swift.psu.edu/trigger_report?id=753338168 GUANO is a fully autonomous, extremely low latency, spacecraft commanding pipeline designed for targeted recovery of BAT event mode data around the times of compelling astrophysical events to enable more sensitive GRB searches. A live reporting of Swift/BAT event data recovered by GUANO can be found at: https://www.swift.psu.edu/guano/ View this GCN Circular online at https://gcn.nasa.gov/circulars/38245. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36230] GRB 241115C: Swift/BAT-GUANO localization skymap of a burst
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38245 SUBJECT: GRB 241115C: Swift/BAT-GUANO localization skymap of a burst DATE: 24/11/15 20:45:18 GMT FROM: Samuele Ronchini at PSU <sjs8171(a)psu.edu> Samuele Ronchini (PSU), James DeLaunay (PSU), Aaron Tohuvavohu (Caltech), Gayathri Raman (PSU), Jamie A. Kennea (PSU), Tyler Parsotan (NASA GSFC) report: Swift/BAT did not localize GRB 241115C onboard (T0: 2024-11-15T04:35:33.96 UTC, Fermi trig 753338138) The Fermi notice, distributed in near real-time, triggered the Swift Mission Operations Center operated Gamma-ray Urgent Archiver for Novel Opportunities (GUANO; Tohuvavohu et al. 2020, ApJ, 900, 1). Upon trigger by this notice, GUANO sent a command to the Swift Burst Alert Telescope (BAT) to save 200 seconds of BAT event-mode data from [-50,+150] seconds around the time of the burst. All the requested event mode data was delivered to the ground. The BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu 2022, ApJ, 941, 169), performed on the temporal window [T0-20 s, T0+20 s], detects the burst with a sqrt(TS) of 14.65 in a 2.048 s analysis time bin, starting at T0 - 0.5119 s. Using the NITRATES analysis, parameter estimation was performed to obtain the localization of this burst in the form of a HEALPIX Multi-Order Coverage (MOC) skymap. This localization accounts for both statistical and systematic errors. More details in the creation and calibration of these maps will soon be published (DeLaunay et al. 2024. in prep) The 90% credible area is 2,129 deg2 and the 50% credible area is 416 deg2. The integrated probability inside the coded field of view is 1%. The NITRATES skymap is consistent with the Fermi localization reported in the final position notice. The combined Fermi/GBM+NITRATES 90% credible area is 245 deg2 and the 50% credible area is 63 deg2. A plot of the probability skymap can be viewed here: [skymap_plot](https://guano.swift.psu.edu/trigger_report?id=753338168/#:~:te… The probability skymap file can be downloaded from the link here [skymap_fits_file](https://guano.swift.psu.edu/files/753338168/0_n_PROBMAP) Instructions on how to read and manipulate this map can be found here: https://guano.swift.psu.edu/documentation More details about this burst can be found on the trigger report page here: https://guano.swift.psu.edu/trigger_report?id=753338168 GUANO is a fully autonomous, extremely low latency, spacecraft commanding pipeline designed for targeted recovery of BAT event mode data around the times of compelling astrophysical events to enable more sensitive GRB searches. A live reporting of Swift/BAT event data recovered by GUANO can be found at: https://www.swift.psu.edu/guano/ View this GCN Circular online at https://gcn.nasa.gov/circulars/38245. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36229] Fermi GRB 241115B: Global MASTER-Net observations report
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38244 SUBJECT: Fermi GRB 241115B: Global MASTER-Net observations report DATE: 24/11/15 20:00:52 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, 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. 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-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 241115B ( Fermi GBM team, GCN 38241) errorbox 5337 sec after notice time and 5370 sec after trigger time at 2024-11-15 19:36:56 UT, with upper limit up to 16.8 mag. The observations began at zenith distance = 77 deg. The sun altitude is -25.5 deg. The galactic latitude b = -15 deg., longitude l = 137 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2671334 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 5400 | 2024-11-15 19:36:56 | MASTER-SAAO | (01h 09m 37.94s , +44d 33m 45.2s) | C | 60 | 16.6 | 6289 | 2024-11-15 19:51:44 | MASTER-SAAO | (01h 09m 58.65s , +44d 32m 52.9s) | C | 60 | 16.8 | 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/38244. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36228] LIGO/Virgo/KAGRA S241114bi: Updated Sky localization and EM Bright Classification
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38243 SUBJECT: LIGO/Virgo/KAGRA S241114bi: Updated Sky localization and EM Bright Classification DATE: 24/11/15 19:53:57 GMT FROM: Charlie Hoy at University of Portsmouth <charlie.hoy(a)port.ac.uk> The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We have conducted further analysis of the LIGO Livingston Observatory (L1) and Virgo Observatory (V1) data around the time of the compact binary merger (CBC) candidate S241114bi (GCN Circular 38228). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.offline0.multiorder.fits,0, distributed via GCN Notice, is available for retrieval from the GraceDB event page: https://gracedb.ligo.org/superevents/S241114bi Based on posterior support from parameter estimation [1], under the assumption that the candidate S241114bi is astrophysical in origin, the probability that at least one of the compact objects is consistent with a neutron star mass (HasNS) is <1%. [2] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [2] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is 2%. For the Bilby.offline0.multiorder.fits,0 sky map, the 90% credible region is 10127 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 752 +/- 195 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/. [1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. PRD 108, 123040 (2023) doi:10.1103/PhysRevD.108.123040 [2] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe View this GCN Circular online at https://gcn.nasa.gov/circulars/38243. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36227] LIGO/Virgo/KAGRA S241114bi: Updated Sky localization and EM Bright Classification
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38243 SUBJECT: LIGO/Virgo/KAGRA S241114bi: Updated Sky localization and EM Bright Classification DATE: 24/11/15 19:53:57 GMT FROM: Charlie Hoy at University of Portsmouth <charlie.hoy(a)port.ac.uk> The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We have conducted further analysis of the LIGO Livingston Observatory (L1) and Virgo Observatory (V1) data around the time of the compact binary merger (CBC) candidate S241114bi (GCN Circular 38228). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.offline0.multiorder.fits,0, distributed via GCN Notice, is available for retrieval from the GraceDB event page: https://gracedb.ligo.org/superevents/S241114bi Based on posterior support from parameter estimation [1], under the assumption that the candidate S241114bi is astrophysical in origin, the probability that at least one of the compact objects is consistent with a neutron star mass (HasNS) is <1%. [2] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [2] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is 2%. For the Bilby.offline0.multiorder.fits,0 sky map, the 90% credible region is 10127 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 752 +/- 195 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/. [1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. PRD 108, 123040 (2023) doi:10.1103/PhysRevD.108.123040 [2] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe View this GCN Circular online at https://gcn.nasa.gov/circulars/38243. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36226] EP241115a: Global MASTER-Net observations report
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38242 SUBJECT: EP241115a: Global MASTER-Net observations report DATE: 24/11/15 18:36:32 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, 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. 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-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) was pointed to the EP241115a ( EP Team et al., GCN 38239) errorbox 8625 sec after notice time and 45587 sec after trigger time at 2024-11-15 18:27:07 UT, with upper limit up to 18.6 mag. Observations started at twilight. The observations began at zenith distance = 28 deg. The sun altitude is -14.1 deg. The galactic latitude b = -78 deg., longitude l = 159 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2671161 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 45617 | 2024-11-15 18:27:07 | MASTER-SAAO | (01h 16m 06.64s , -18d 19m 58.1s) | C | 60 | 18.6 | 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/38242. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36225] GRB 241115B: Fermi GBM Final Real-time Localization
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38241 SUBJECT: GRB 241115B: Fermi GBM Final Real-time Localization DATE: 24/11/15 18:18:08 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 18:07:25 UT on 15 Nov 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241115B (trigger 753386850.967696 / 241115755). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 31.8, Dec = 45.0 (J2000 degrees, equivalent to J2000 02h 07m, 45d 00'), with a statistical uncertainty of 9.2 degrees. The angle from the Fermi LAT boresight is 97.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241115755/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241115755/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241115755/… View this GCN Circular online at https://gcn.nasa.gov/circulars/38241. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36224] GRB 241115B: Fermi GBM Final Real-time Localization
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38241 SUBJECT: GRB 241115B: Fermi GBM Final Real-time Localization DATE: 24/11/15 18:18:08 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 18:07:25 UT on 15 Nov 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241115B (trigger 753386850.967696 / 241115755). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 31.8, Dec = 45.0 (J2000 degrees, equivalent to J2000 02h 07m, 45d 00'), with a statistical uncertainty of 9.2 degrees. The angle from the Fermi LAT boresight is 97.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241115755/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241115755/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241115755/… View this GCN Circular online at https://gcn.nasa.gov/circulars/38241. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36223] LIGO/Virgo/KAGRA S241113p: Updated Sky localization
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38240 SUBJECT: LIGO/Virgo/KAGRA S241113p: Updated Sky localization DATE: 24/11/15 17:12:21 GMT FROM: Charlie Hoy at University of Portsmouth <charlie.hoy(a)port.ac.uk> The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We have conducted further analysis of the LIGO Livingston Observatory (L1) and Virgo Observatory (V1) data around the time of the compact binary merger (CBC) candidate S241113p (GCN Circular 38204). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.multiorder.fits,0, distributed via GCN Notice, is available for retrieval from the GraceDB event page: https://gracedb.ligo.org/superevents/S241113p For the Bilby.multiorder.fits,0 sky map, the 90% credible region is 11825 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1321 +/- 400 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/. [1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. PRD 108, 123040 (2023) doi:10.1103/PhysRevD.108.123040 View this GCN Circular online at https://gcn.nasa.gov/circulars/38240. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36222] EP241115a: EP detection of a fast X-ray transient
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38239 SUBJECT: EP241115a: EP detection of a fast X-ray transient DATE: 24/11/15 16:02:42 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> J. W. Hu (NAO, CAS), M. Q. Huang, Z. Y. Liu (USTC), C. Y. Dai (NJU), Y. J. Zhang (THU), C. X. Zhang (HUST), Y. Liu (NAO, CAS) on behalf of the Einstein Probe team We report on the detection of a fast X-ray transient, designated EP241115a, by the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) mission. The transient was detected at 2024-11-15 05:47:20 (UTC) and lasted for around 500 seconds. The WXT position of EP241115a is R.A.= 19.416 deg, DEC = -17.954 deg (J2000) with an uncertainty of 2.6 arcmin (radius, 90% C.L. statistical and systematic). It has a peak flux of ~1 x 10^-9 erg/s/cm^2 in the 0.5-4 keV band. The average 0.5-4 keV spectrum can be fitted with an absorbed power law with a photon index of 0.56(+0.54/-0.51) (with a column density fixed at the Galactic one of 1.6 x 10^20 cm^-2). The derived average unabsorbed 0.5-4 keV flux is 1.42(+0.6/-0.4) x 10^(-10) erg/s/cm^2. The uncertainties are at the 90% confidence level for the above parameters. No previously known bright X-ray sources are found within the error circle around the source position. Further follow-up observations are encouraged to identify the nature of this X-ray transient. 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/38239. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36221] EP241115a: EP detection of a fast X-ray transient
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38239 SUBJECT: EP241115a: EP detection of a fast X-ray transient DATE: 24/11/15 16:02:42 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> J. W. Hu (NAO, CAS), M. Q. Huang, Z. Y. Liu (USTC), C. Y. Dai (NJU), Y. J. Zhang (THU), C. X. Zhang (HUST), Y. Liu (NAO, CAS) on behalf of the Einstein Probe team We report on the detection of a fast X-ray transient, designated EP241115a, by the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) mission. The transient was detected at 2024-11-15 05:47:20 (UTC) and lasted for around 500 seconds. The WXT position of EP241115a is R.A.= 19.416 deg, DEC = -17.954 deg (J2000) with an uncertainty of 2.6 arcmin (radius, 90% C.L. statistical and systematic). It has a peak flux of ~1 x 10^-9 erg/s/cm^2 in the 0.5-4 keV band. The average 0.5-4 keV spectrum can be fitted with an absorbed power law with a photon index of 0.56(+0.54/-0.51) (with a column density fixed at the Galactic one of 1.6 x 10^20 cm^-2). The derived average unabsorbed 0.5-4 keV flux is 1.42(+0.6/-0.4) x 10^(-10) erg/s/cm^2. The uncertainties are at the 90% confidence level for the above parameters. No previously known bright X-ray sources are found within the error circle around the source position. Further follow-up observations are encouraged to identify the nature of this X-ray transient. 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/38239. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36220] EP241113a: No Detection in Fermi-GBM Observations
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38238 SUBJECT: EP241113a: No Detection in Fermi-GBM Observations DATE: 24/11/15 15:28:34 GMT FROM: P.G. Jonker at Radboud University <p.jonker(a)astro.ru.nl> E. Burns (LSU), M. E. Ravasio (Radboud Univ.) and P.G. Jonker (Radboud Univ.) report on behalf of the Fermi-GBM Team: Fermi-GBM had full spatial and temporal coverage of the EP WXT signal of EP241113a (Liu et al., GCN 38211). There was no Fermi-GBM onboard trigger around the EP-WXT trigger time T0=2024-11-13T19:12:53 UTC, nor at the earlier starting time of the transient (as reported in the EP-WXT GCN 38211, 2024-11-13T19:09:19 UTC). An automated, blind search for a short gamma-ray burst below the onboard triggering threshold in Fermi-GBM also identified no counterpart candidates. The GBM targeted search, the most sensitive, coherent search for GRB-like signals, was run from 50 s before the EP trigger time until 500 s after both reported times, seeking signals between 64 ms and 32.768 s in duration. A candidate was found, but its localization is not consistent with the EP transient and appears to be a soft Galactic source. No signal consistent both temporally and spatially is identified, as confirmed by visual inspection of the data. View this GCN Circular online at https://gcn.nasa.gov/circulars/38238. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36219] Swift GRB 241115A: Global MASTER-Net observations report
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38237 SUBJECT: Swift GRB 241115A: Global MASTER-Net observations report DATE: 24/11/15 15:02:19 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, 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. 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-Tunka robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Applied Physics Institute, Irkutsk State University) was pointed to the Swift GRB 241115A ( M. A. Williams et al., GCN 38235) errorbox 2802 sec after notice time and 2828 sec after trigger time at 2024-11-15 14:05:33 UT, with upper limit up to 16.4 mag. The observations began at zenith distance = 83 deg. The sun altitude is -44.1 deg. The galactic latitude b = -14 deg., longitude l = 206 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2671057 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 2831 | MASTER-Tunka | C | 5 | 14.0 | 2871 | MASTER-Tunka | C | 5 | 13.8 | 2888 | MASTER-Tunka | C | 5 | 13.9 | 3335 | MASTER-Tunka | C | 1 | 13.7 | 3348 | MASTER-Tunka | C | 1 | 13.3 | 5552 | MASTER-Tunka | C | 60 | 16.4 | Coadd 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/38237. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36218] Fermi GRB 241115A: Global MASTER-Net observations report
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38236 SUBJECT: Fermi GRB 241115A: Global MASTER-Net observations report DATE: 24/11/15 14:45:31 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, 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. 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-Tunka robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB 241115A ( Fermi GBM team, GCN 38234) errorbox 2796 sec after notice time and 2828 sec after trigger time at 2024-11-15 14:05:33 UT, with upper limit up to 14.0 mag. The observations began at zenith distance = 83 deg. The sun altitude is -44.1 deg. The galactic latitude b = -14 deg., longitude l = 203 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2671089 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 2832 | 2024-11-15 14:05:33 | MASTER-Tunka | (05h 47m 14.08s , -00d 46m 37.1s) | C | 5 | 14.0 | 2871 | 2024-11-15 14:06:12 | MASTER-Tunka | (05h 47m 14.46s , -00d 48m 32.9s) | C | 5 | 13.8 | 2888 | 2024-11-15 14:06:30 | MASTER-Tunka | (05h 47m 20.52s , -00d 48m 31.2s) | C | 5 | 13.9 | 3335 | 2024-11-15 14:13:59 | MASTER-Tunka | (05h 47m 20.28s , -00d 46m 37.9s) | C | 1 | 13.7 | 3348 | 2024-11-15 14:14:12 | MASTER-Tunka | (05h 47m 14.99s , -00d 47m 15.0s) | C | 1 | 13.3 | 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/38236. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36217] GRB 241115A: Swift detection of a burst
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38235 SUBJECT: GRB 241115A: Swift detection of a burst DATE: 24/11/15 13:36:51 GMT FROM: K.L. Page at U Leicester <klp5(a)leicester.ac.uk> M. A. Williams (PSU), J. J. DeLaunay (PSU), S. Dichiara (PSU), R. Gupta (NASA GSFC), K. L. Page (U Leicester) and D. M. Palmer (LANL) report on behalf of the Neil Gehrels Swift Observatory Team: At 13:18:25 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 241115A (trigger=1267921). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 86.765, -0.662 which is RA(J2000) = 05h 47m 04s Dec(J2000) = -00d 39' 44" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single-peaked structure with a duration of about 5 sec. The peak count rate was ~7600 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began observing the field at 13:20:14.5 UT, 109.5 seconds after the BAT trigger. Using promptly downlinked data we find a fading, uncatalogued X-ray source located at RA, Dec 86.77049, -0.67381 which is equivalent to: RA(J2000) = 05h 47m 04.92s Dec(J2000) = -00d 40' 25.7" with an uncertainty of 3.5 arcseconds (radius, 90% containment). This location is 46 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received; the latest position is available at https://www.swift.ac.uk/sper. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density in excess of the Galactic value (3.32 x 10^21 cm^-2, Willingale et al. 2013), with an excess column of 9.4 (+6.11/-4.63) x 10^21 cm^-2 (90% confidence). UVOT took a finding chart exposure of 150 seconds with the White filter starting 113 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag. The 8'x8' region for the list of sources generated on-board covers 100% of the XRT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 1.028. Burst Advocate for this burst is M. A. Williams (mjw6837 AT psu.edu). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/) View this GCN Circular online at https://gcn.nasa.gov/circulars/38235. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36216] GRB 241115A: Fermi GBM Final Real-time Localization
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38234 SUBJECT: GRB 241115A: Fermi GBM Final Real-time Localization DATE: 24/11/15 13:28:56 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 13:18:24 UT on 15 Nov 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241115A (trigger 753369509.732778 / 241115554). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 85.2, Dec = 2.7 (J2000 degrees, equivalent to J2000 05h 40m, 2d 42'), with a statistical uncertainty of 6.0 degrees. The angle from the Fermi LAT boresight is 43.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241115554/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241115554/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241115554/… View this GCN Circular online at https://gcn.nasa.gov/circulars/38234. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36215] EP 241113a: LBT possible optical counterpart
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38233 SUBJECT: EP 241113a: LBT possible optical counterpart DATE: 24/11/15 10:38:26 GMT FROM: Andrea Rossi at INAF <andrea.rossi(a)inaf.it> A. Rossi (INAF/OAS), A.J. Levan (Radboud Univ.), D. B. Malesani (DAWN/NBI and Radboud Univ.), P.G. Jonker (Radboud Univ.), J. Rastinejad (Northwestern), E. Maiorano (INAF/OAS), report on behalf of a larger collaboration: We observed the field of EP 241113a (Liu et al., GCN 38211) with the LBC camera mounted on LBT (Mt. Graham, AZ, USA) in the r' band (22 min of exposure time) with approximate midtime 07:45:00 UT on 2024-11-15, or 1.52 days after the burst. Observations were performed under an average seeing of ~1.5". We detect a very faint source within the EP/WXT error circle, which is not present in Legacy Survey r-band images, and is located at coordinates (J2000): RA = 08:47:59.39 Dec = +52:22:54.7 We measure a preliminary AB magnitude of r' = 23.35 +- 0.15, calibrated against Pan-STARRS field stars, and not corrected for the foreground Galactic extinction. We note that the candidate afterglow is offset ~20” from the galaxy 2MASX J08480182+5222544 with a measured spectroscopic redshift of z=0.115. This corresponds to ~40 kpc in projection and the probability of chance alignment is approximately 3%. We acknowledge excellent support from the LBTO and LBT-INAF staff, particularly A. Becker and D. G. Huerta. View this GCN Circular online at https://gcn.nasa.gov/circulars/38233. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36213] GRB 241113B: KAIT Optical Afterglow Candidate
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38232 SUBJECT: GRB 241113B: KAIT Optical Afterglow Candidate DATE: 24/11/15 08:40:03 GMT FROM: Weikang Zheng at UC Berkeley <weikang(a)berkeley.edu> WeiKang Zheng and Alexei V. Filippenko (UCB), 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 KAIT GRB team: The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at Lick Observatory, automatically responded to GRB 241113B (SVOM/ECLAIRs, Dagoneau et al., GCN 38196; SVOM/GRM, Liu et al., GCN 38212; EP/WXT, Liu et al., GCN 38214) starting at 11:24:48 UT, 103s after ECLAIRs trigger. Observations were performed in 3x3 tiling mode and lasted for about 2 hours, a set of clear (roughly R) filter images were obtained. We detected a bright uncataloged optical afterglow candidate at J2000 position of (error ~0.5"): RA: 07:20:57.72 Dec: +46:47:12.3 Its brightness decayed from 16.7 mag at ~250s to 20.5 mag (Vega) at ~1.37 hours, we therefor suggest this to be the optical afterglow of GRB 241113B. ~ View this GCN Circular online at https://gcn.nasa.gov/circulars/38232. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36214] GRB 241113B: KAIT Optical Afterglow Candidate
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38232 SUBJECT: GRB 241113B: KAIT Optical Afterglow Candidate DATE: 24/11/15 08:40:03 GMT FROM: Weikang Zheng at UC Berkeley <weikang(a)berkeley.edu> WeiKang Zheng and Alexei V. Filippenko (UCB), 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 KAIT GRB team: The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at Lick Observatory, automatically responded to GRB 241113B (SVOM/ECLAIRs, Dagoneau et al., GCN 38196; SVOM/GRM, Liu et al., GCN 38212; EP/WXT, Liu et al., GCN 38214) starting at 11:24:48 UT, 103s after ECLAIRs trigger. Observations were performed in 3x3 tiling mode and lasted for about 2 hours, a set of clear (roughly R) filter images were obtained. We detected a bright uncataloged optical afterglow candidate at J2000 position of (error ~0.5"): RA: 07:20:57.72 Dec: +46:47:12.3 Its brightness decayed from 16.7 mag at ~250s to 20.5 mag (Vega) at ~1.37 hours, we therefor suggest this to be the optical afterglow of GRB 241113B. ~ View this GCN Circular online at https://gcn.nasa.gov/circulars/38232. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36212] LIGO/Virgo/KAGRA S241114bi: Upper limits from Fermi-GBM Observations
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38231 SUBJECT: LIGO/Virgo/KAGRA S241114bi: Upper limits from Fermi-GBM Observations DATE: 24/11/15 05:13:30 GMT FROM: Sarah Dalessi at UAH <sd0104(a)uah.edu> S. Dalessi (UAH) reports on behalf of the Fermi-GBM Team: For S241114bi (GCN 38228) and using the initial bayestar skymap, Fermi-GBM was observing 59.4% of the localization probability at event time. There was no Fermi-GBM onboard trigger around the event time of the LIGO/Virgo/KAGRA (LVK) detection of GW trigger S241114bi. An automated, blind search for short gamma-ray bursts below the onboard triggering threshold in Fermi-GBM also identified no counterpart candidates. The GBM targeted search, the most sensitive, coherent search for GRB-like signals, was run from +/-30 s around merger time, and also identified no counterpart candidates. Part of the LVK localization region is behind the Earth for Fermi, located at an RA=63.3, Dec=4.0 with a radius of 68.0 degrees. We therefore set upper limits on impulsive gamma-ray emission for the GW localization region visible to Fermi at merger time. Using the representative soft, normal, and hard GRB-like templates described in arXiv:1612.02395, we set the following 3 sigma flux upper limits over 10-1000 keV, weighted by GW localization probability (in units of 10^-7 erg/s/cm^2): Timescale Soft Normal Hard ------------------------------------ 0.128 s: 1.2 2.0 3.7 1.024 s: 0.42 0.66 1.2 8.192 s: 0.13 0.18 0.22 Assuming the median luminosity distance of 781.7 Mpc from the GW detection, we estimate the following intrinsic luminosity upper limits over the 1 keV-10 MeV energy range (in units of 10^50 erg/s): Timescale Soft Normal Hard ------------------------------------ 0.128s: 0.14 0.21 0.63 1.024s: 0.047 0.068 0.20 8.192s: 0.015 0.019 0.038 View this GCN Circular online at https://gcn.nasa.gov/circulars/38231. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36211] LIGO/Virgo/KAGRA S241114bi: Coverage and upper limits from MAXI/GSC observations
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38230 SUBJECT: LIGO/Virgo/KAGRA S241114bi: Coverage and upper limits from MAXI/GSC observations DATE: 24/11/15 04:41:09 GMT FROM: Yuta Kawakubo at Aoyama Gakuin University <kawakubo(a)phys.aoyama.ac.jp> K. Takagi, H. Negoro, M. Nakajima (Nihon U.), N. Kawai, T. Mihara, (RIKEN), S. Sugita, M. Serino, Y. Kawakubo, H. Hiramatsu, H. Nishikawa, Y. Kondo (AGU) report on behalf of the MAXI team: We examined MAXI/GSC all-sky X-ray images (2-20 keV) after compact binary merger candidate S241114bi at 2024-11-14 23:52:58.148 UTC (#38228). At the trigger time of S241114bi, the high-voltage of MAXI/GSC was off, and it was turned on at T0+792 sec (+13.2 min). The first one-orbit (92 min) scan observation with GSC after the event covered 94% of the 90% credible region of the bayestar skymap from 00:06:11 to 01:13:09 UTC (T0+793 to T0+4811 sec). No significant new source was found in the region in the one-orbit scan observation. A typical 1-sigma averaged upper limit obtained in one scan observation is 20 mCrab at 2-20 keV. If you require information about X-ray flux by MAXI/GSC at specific coordinates, please contact the submitter of this circular by email. View this GCN Circular online at https://gcn.nasa.gov/circulars/38230. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36210] GRB 241113A: Swift-BAT refined analysis
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38229 SUBJECT: GRB 241113A: Swift-BAT refined analysis DATE: 24/11/15 03:13:37 GMT FROM: Takanori Sakamoto at AGU <tsakamoto(a)phys.aoyama.ac.jp> C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), R. Gupta (GSFC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), C. B. Markwardt (GSFC), M. J. Moss (GSFC), D. M. Palmer (LANL), T. Parsotan (GSFC), D. Sadaula (GSFC/UMBC), T. Sakamoto (AGU), M. H. Siegel (PSU) (i.e. the Swift-BAT team): Using the data set from T-239 to T+329 sec from the recent telemetry downlink, we report further analysis of BAT GRB 241113A (trigger #1267501) (Siegel, et al., GCN Circ. 38194). The BAT ground-calculated position is RA, Dec = 16.578, -22.658 deg which is RA(J2000) = 01h 06m 18.7s Dec(J2000) = -22d 39' 27.8" with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment). The partial coding was 93%. The mask-weighted light curve shows a single-pulse structure that starts at T0, peaks at T+0.5 sec, and ends at T+2 sec. There is a hint of the emission between T+35 sec and T+80 sec. T90 (15-350 keV) is 1.7 +- 0.4 sec (estimated error including systematics). The time-averaged spectrum from T+0.01 to T+2.06 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.76 +- 0.23. The fluence in the 15-150 keV band is 1.3 +- 0.2 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T-0.00 sec in the 15-150 keV band is 1.4 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at https://swift.gsfc.nasa.gov/results/batgrbcat/BAT_refined_circular/1267501 View this GCN Circular online at https://gcn.nasa.gov/circulars/38229. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36209] GRB 241113A: Swift-BAT refined analysis
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38229 SUBJECT: GRB 241113A: Swift-BAT refined analysis DATE: 24/11/15 03:13:37 GMT FROM: Takanori Sakamoto at AGU <tsakamoto(a)phys.aoyama.ac.jp> C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC), R. Gupta (GSFC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), C. B. Markwardt (GSFC), M. J. Moss (GSFC), D. M. Palmer (LANL), T. Parsotan (GSFC), D. Sadaula (GSFC/UMBC), T. Sakamoto (AGU), M. H. Siegel (PSU) (i.e. the Swift-BAT team): Using the data set from T-239 to T+329 sec from the recent telemetry downlink, we report further analysis of BAT GRB 241113A (trigger #1267501) (Siegel, et al., GCN Circ. 38194). The BAT ground-calculated position is RA, Dec = 16.578, -22.658 deg which is RA(J2000) = 01h 06m 18.7s Dec(J2000) = -22d 39' 27.8" with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment). The partial coding was 93%. The mask-weighted light curve shows a single-pulse structure that starts at T0, peaks at T+0.5 sec, and ends at T+2 sec. There is a hint of the emission between T+35 sec and T+80 sec. T90 (15-350 keV) is 1.7 +- 0.4 sec (estimated error including systematics). The time-averaged spectrum from T+0.01 to T+2.06 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.76 +- 0.23. The fluence in the 15-150 keV band is 1.3 +- 0.2 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T-0.00 sec in the 15-150 keV band is 1.4 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at https://swift.gsfc.nasa.gov/results/batgrbcat/BAT_refined_circular/1267501 View this GCN Circular online at https://gcn.nasa.gov/circulars/38229. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36208] LIGO/Virgo/KAGRA S241114bi: Identification of a GW compact binary merger candidate
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38228 SUBJECT: LIGO/Virgo/KAGRA S241114bi: Identification of a GW compact binary merger candidate DATE: 24/11/15 00:25:28 GMT FROM: Jade Powell at LIGO Scientific Collaboration <jade.powell(a)ligo.org> The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We identified the compact binary merger candidate S241114bi during real-time processing of data from LIGO Livingston Observatory (L1) and Virgo Observatory (V1) at 2024-11-14 23:52:58.148 UTC (GPS time: 1415663596.148). The candidate was found by the GstLAL [1] analysis pipeline. S241114bi is an event of interest because its false alarm rate, as estimated by the online analysis, is 1.8e-13 Hz, or about one in 1e5 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S241114bi After parameter estimation by RapidPE-RIFT [2], the classification of the GW signal, in order of descending probability, is BBH (91%), NSBH (9%), Terrestrial (<1%), or BNS (<1%). Assuming the candidate is astrophysical in origin, the probability that the lighter compact object is consistent with a neutron star mass (HasNS) is <1%. [3] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [3] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is 6%. Two sky maps are available at this time and can be retrieved from the GraceDB event page: * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [4], distributed via GCN notice about 27 seconds after the candidate event time. * bayestar.multiorder.fits,2, an initial localization generated by BAYESTAR [4], distributed via GCN notice about 5 minutes after the candidate event time. The preferred sky map at this time is bayestar.multiorder.fits,2. For the bayestar.multiorder.fits,2 sky map, the 90% credible region is 9934 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 782 +/- 219 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/. [1] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. (2023) arXiv:2305.05625 [2] Rose et al. (2022) arXiv:2201.05263 and Pankow et al. PRD 92, 023002 (2015) doi:10.1103/PhysRevD.92.023002 [3] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe [4] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013 View this GCN Circular online at https://gcn.nasa.gov/circulars/38228. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36207] GRB 241113A: PRIME near-infrared upper limits
by GCN Circulars 15 Nov '24

15 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38227 SUBJECT: GRB 241113A: PRIME near-infrared upper limits DATE: 24/11/15 00:00:26 GMT FROM: Joe Durbak at UMD <gcn.joedurbak(a)gmail.com> J. Durbak (UMD), O. Guiffreda (UMD), A. S. Kutyrev (NASA/GSFC), E. Troja (U Rome), S. B. Cenko (NASA/GSFC) Following the Swift BAT detection (GCN 38194), we observed the transient field in J and H filters with PRIME ~13 hours after Swift BAT detection. At the counterpart positions reported by Swift XRT and UVOT and (GCN 38194, GCN 38198), LCOGT (GCN 38197), LCO (GCN 38201) and KAIT (GCN 38216), we detect no uncatalogued sources in J-band. Using nearby VISTA Hemispherical Survey (VHS) stars for preliminary calibration we derive a limiting magnitude of <20.4 AB. We also detect no uncatalogued sources in H-band. Using nearby 2MASS stars for preliminary calibration we derive a limiting magnitude of <20.6 AB. Neither of these results are corrected for Galactic extinction. 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). We thank the Osaka University 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/38227. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36206] Fermi GRB 241114A: Global MASTER-Net observations report
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38226 SUBJECT: Fermi GRB 241114A: Global MASTER-Net observations report DATE: 24/11/14 23:45:58 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, 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. 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-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 241114A ( Fermi GBM team, GCN 38224) errorbox 1540 sec after notice time and 1575 sec after trigger time at 2024-11-14 23:28:10 UT, with upper limit up to 16.5 mag. The observations began at zenith distance = 72 deg. The sun altitude is -37.2 deg. The galactic latitude b = -46 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=2670389 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 1605 | 2024-11-14 23:28:10 | MASTER-SAAO | (00h 03m 31.91s , +04d 46m 20.6s) | C | 60 | 16.4 | 1938 | 2024-11-14 23:33:42 | MASTER-SAAO | (00h 03m 18.06s , -02d 48m 23.5s) | C | 60 | 16.5 | 2222 | 2024-11-14 23:38:27 | MASTER-SAAO | (00h 04m 00.96s , +08d 35m 22.4s) | C | 60 | 15.7 | 2302 | 2024-11-14 23:39:46 | MASTER-SAAO | (00h 03m 44.90s , +04d 48m 38.5s) | C | 60 | 16.5 | 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/38226. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36205] EP241113a: Global MASTER-Net observations report
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38225 SUBJECT: EP241113a: Global MASTER-Net observations report DATE: 24/11/14 23:18:29 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, 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. 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-Tunka robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Applied Physics Institute, Irkutsk State University) was pointed to the EP241113a ( EP Team et al., GCN 38211) errorbox 30873 sec after notice time and 63871 sec after trigger time at 2024-11-14 12:57:24 UT, with upper limit up to 15.2 mag. The observations began at zenith distance = 71 deg. The sun altitude is -33.9 deg. MASTER-Kislovodsk robotic telescope located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) was pointed to the EP241113a errorbox 62177 sec after notice time and 1 days 8776 sec after trigger time at 2024-11-14 21:39:09 UT, with upper limit up to 15.3 mag. The observations began at zenith distance = 46 deg. The sun altitude is -63.7 deg. The galactic latitude b = 39 deg., longitude l = 166 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2669629 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 63901 | 2024-11-14 12:57:24 | MASTER-Tunka | (08h 47m 28.22s , +52d 20m 09.3s) | C | 60 | 15.3 | Coadd 64205 | 2024-11-14 13:02:28 | MASTER-Tunka | (08h 47m 25.95s , +52d 21m 42.1s) | C | 60 | 14.6 | Coadd 64422 | 2024-11-14 13:06:04 | MASTER-Tunka | (08h 47m 26.36s , +52d 19m 37.9s) | C | 60 | 14.5 | Coadd 64632 | 2024-11-14 13:09:35 | MASTER-Tunka | (08h 47m 30.22s , +52d 19m 47.5s) | C | 60 | 14.7 | Coadd 64998 | 2024-11-14 13:15:41 | MASTER-Tunka | (08h 47m 27.35s , +52d 21m 30.0s) | C | 60 | 14.0 | Coadd 65244 | 2024-11-14 13:19:47 | MASTER-Tunka | (08h 47m 29.00s , +52d 19m 25.6s) | C | 60 | 14.7 | Coadd 65497 | 2024-11-14 13:24:00 | MASTER-Tunka | (08h 47m 32.84s , +52d 19m 41.7s) | C | 60 | 15.2 | Coadd 65860 | 2024-11-14 13:30:02 | MASTER-Tunka | (08h 47m 31.41s , +52d 21m 17.9s) | C | 60 | 13.6 | Coadd 66303 | 2024-11-14 13:37:25 | MASTER-Tunka | (08h 47m 35.63s , +52d 19m 41.6s) | C | 60 | 13.1 | Coadd 95206 | 2024-11-14 21:39:09 | MASTER-Kislovodsk | (08h 46m 45.12s , +52d 31m 54.4s) | C | 60 | 15.1 | 95685 | 2024-11-14 21:47:08 | MASTER-Kislovodsk | (08h 46m 40.57s , +52d 32m 18.9s) | C | 60 | 15.3 | 95965 | 2024-11-14 21:51:48 | MASTER-Kislovodsk | (08h 46m 45.53s , +52d 30m 29.5s) | C | 60 | 14.6 | 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/38225. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36204] GRB 241114A: Fermi GBM Final Real-time Localization
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38224 SUBJECT: GRB 241114A: Fermi GBM Final Real-time Localization DATE: 24/11/14 23:12:38 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 SHORT GRB At 23:01:54 UT on 14 Nov 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241114A (trigger 753318119.98625 / 241114960). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 13.5, Dec = 16.4 (J2000 degrees, equivalent to J2000 00h 54m, 16d 23'), with a statistical uncertainty of 33.7 degrees. The angle from the Fermi LAT boresight is 54.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241114960/… The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241114960/… The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241114960/… View this GCN Circular online at https://gcn.nasa.gov/circulars/38224. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36203] GRB 241113B: J-band upper limit from WINTER
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38223 SUBJECT: GRB 241113B: J-band upper limit from WINTER DATE: 24/11/14 21:18:47 GMT FROM: Benjamin Schneider at MIT <bschn(a)mit.edu> Benjamin Schneider (MIT), Geoffrey Mo (MIT), Tomas Ahumada (Caltech), Viraj Karambelkar (Caltech), Robert Stein (UMD), Nathan Lourie (MIT), Danielle Frostig (CFA), Robert Simcoe (MIT), and Mansi Kasliwal (Caltech) report: We observed the field of the GRB 241113B (Dagoneau et al, GCN 38196; Liu et al., GCN 38212; Liu et al., GCN 38214) in the near-infrared J-band with the Palomar 1-m telescope, equipped with the 1-square degree WINTER camera (Lourie et al. 2020, Frostig et al. 2024). Our observations began at 2024-11-13T12:14:04.71 UTC (51 mins after the GRB trigger) and consisted of 30x120s exposures. The images were processed using the WINTER data reduction pipeline (https://github.com/winter-telescope/mirar, https://doi.org/10.5281/zenodo.10888436), with image subtraction performed relative to J-band images from the UKIRT Hemisphere survey (Dye et al., 2017). Our observations covered the entire SVOM/ECLAIRs statistical error circle. In the stacked and subtracted images, we do not detect any new source down to a 5-sigma depth of J ~ 19.1 mag (AB). WINTER (Wide-field INfrared Transient ExploreR) is a partnership between MIT and Caltech, housed at Palomar Observatory, and funded by NSF MRI, NSF AAG, the David and Lucile Packard Foundation, and the MIT Kavli Institute for Astrophysics and Space Research. View this GCN Circular online at https://gcn.nasa.gov/circulars/38223. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36202] GRB 241113A: J-band observations with WINTER
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38222 SUBJECT: GRB 241113A: J-band observations with WINTER DATE: 24/11/14 19:18:17 GMT FROM: Geoffrey Mo at MIT <gmo(a)mit.edu> Geoffrey Mo (MIT), Tomas Ahumada (Caltech), Benjamin Schneider (MIT), Viraj Karambelkar (Caltech), Danielle Frostig (CfA), Robert Stein (UMD), Nathan Lourie (MIT), Robert Simcoe (MIT), and Mansi Kasliwal (Caltech) report: We observed the field of GRB 241113A (Siegel et al., GCN 38194; Beardmore et al., GCN 38209) in the near-infrared J-band with the Palomar 1-m telescope, equipped with the 1-square degree WINTER camera (Lourie et al. 2020, Frostig et al. 2024). Observations were triggered automatically and began at 2024-11-14T02:40:03 UTC (~18.9 hours after the GRB), consisting of 15 x 120 s exposures. The images were processed using the WINTER data reduction pipeline (https://github.com/winter-telescope/mirar, https://doi.org/10.5281/zenodo.13352565). We do not detect a source at the optical and enhanced Swift/XRT counterpart location (Siegel et al., GCN 38194; Francile et al., GCN 38195; Huertas Ferrer et al., GCN 38197; Goad et al., GCN 38198; Izzo et al., GCN 38201; Ferro et al., GCN 38206; Breeveld et al., GCN 38207; Zheng et al., GCN 38216; Du et al., GCN 38217). We obtain the following 5-sigma upper limit: J ~ 18.3 mag (AB). WINTER (Wide-field INfrared Transient ExploreR) is a partnership between MIT and Caltech, housed at Palomar Observatory, and funded by NSF MRI, NSF AAG, the David and Lucile Packard Foundation, and the MIT Kavli Institute for Astrophysics and Space Research. View this GCN Circular online at https://gcn.nasa.gov/circulars/38222. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36201] EP241113a : J-band observations with WINTER
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38221 SUBJECT: EP241113a : J-band observations with WINTER DATE: 24/11/14 18:57:48 GMT FROM: Tomas Ahumada Mena at Caltech <tahumada(a)caltech.edu> Tomas Ahumada (Caltech), Geoffrey Mo (MIT), Benjamin Schneider (MIT), Viraj Karambelkar (Caltech), Danielle Frostig (CfA), Robert Stein (UMD), Nathan Lourie (MIT), Robert Simcoe (MIT), and Mansi Kasliwal (Caltech) report: We observed the field of the EP-WXT and EP-FXT X-ray transient EP241113a (Liu et al., GCN 38211) in the near-infrared J-band with the Palomar 1-m telescope, equipped with the 1 square degree WINTER camera (Lourie et al. 2020, Frostig et al. 2024). Observations began at 2024-11-14T11:44:10.899 UTC (~16.5 hrs after the X-ray transient) and consisted of 30 x 120 s exposures. The images were processed using the WINTER data reduction pipeline (https://github.com/winter-telescope/mirar, https://doi.org/10.5281/zenodo.13352565). No source is detected in the FXT error region (Liu et al., GCN 38211), setting a 5-sigma upper limit of 18.5 mag (AB) in the J band. WINTER (Wide-field INfrared Transient ExploreR) is a partnership between MIT and Caltech, housed at Palomar Observatory, and funded by NSF MRI, NSF AAG, the David and Lucile Packard Foundation, and the MIT Kavli Institute for Astrophysics and Space Research. View this GCN Circular online at https://gcn.nasa.gov/circulars/38221. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36200] GRB 241030A: LCO optical observation
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38220 SUBJECT: GRB 241030A: LCO optical observation DATE: 24/11/14 16:40:32 GMT FROM: ankur ghosh at CAPP, University of Johannesburg <ghosh.ankur1994(a)gmail.com> Ankur Ghosh, Soebur Razzaque (CAPP, University of Johannesburg), Alexander Moskvitin, Yulia Sotnikova (SAO RAS) on behalf of a larger collaboration. We observed the field of the GRB 241030A (Klingler et al., GCN 37956; Beardmore et al., GCN 37962; Wang et al., GCN 37972; Pillera et al., GCN 37979; Ridnaia et al., GCN 37982; Ambrosi et al., GCN 37988; Wu et al., GCN 37997) using B, R filters of the 1-meter Sinistro telescope and V filter of the 0.4-m SCICAM QHY600 at the Las Cumbres Observatory Global Telescope (LCOGT) node located at Teide Observatory, Tenerife, SPAIN. The 1-m Sinistro telescope is equipped with a 4K x 4K CCD (FOV: 26 x 26 arcmin, scale: 0.39 arcsec/pixel) and the 0.4 m SCICAM QHY600 is equipped with 9576 x 6388 pixel CCD (FOV: 1.9 x 1.2 degrees, scale: 0.74 arcsec/pixel). Observations began on October 30 2024, starting from 14.21 to 14.41 hours after the GRB trigger. We clearly detect the optical transient (OT) reported by GCNs (Klingler et al., GCN 37956; Watson et al., GCN 37957; Fernández-Rodríguez et al., GCN 37958; Zheng et al., GCN 37959; An et al., GCN 37960; Higuchi et al., GCN 37963; Qiu et al., GCN 37965; Lin et al., GCN 37966; Wu et al., GCN 37970; Breeveld & Klingler, GCN 37974; Méndez-Lapido et al., GCN 37993, Moskvitin & Goranskij, GCN 38016; Busmann et al., GCN 38019; Schneider et al., GCN 38021; Li et al., GCN 38027; Masi, GCN 38031, Yan et al., GCN 38035, Pankov et al., GCN 38105, Reguitti et al., GCN 38105) in our stacked images. Our detection is well consistent with the observation reported at the similar epoch by Moskvitin & Goranskij, GCN 38016. Date UTstart-end t-T0 (hours) Exp (sec) Filter Magnitude 2024-10-30 19:55:20--20:05:50 14.21 2 x 300 B B = 19.52 +/- 0.14 2024-10-30 19:48:10--20:08:18 14.17 2 x 600 V V = 19.51 +/- 0.14 2024-10-30 20:07:31--20:17:59 14.41 2 x 300 R R = 19.10 +/- 0.04 The field was calibrated against nearby SDSS stars, with magnitudes converted using Lupton (2005) equations, and has not been corrected for Galactic extinction. View this GCN Circular online at https://gcn.nasa.gov/circulars/38220. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36199] GRB 241113B: Swift-XRT observations
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38219 SUBJECT: GRB 241113B: Swift-XRT observations DATE: 24/11/14 16:03:31 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), C. Salvaggio (INAF-OAB), M. Ferro (INAF-OAB), R. Brivio (INAF-OAB), S. Dichiara (PSU), J.A. Kennea (PSU), D.N. Burrows (PSU) and P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the SVOM/ECLAIRs-detected burst GRB 241113B, collecting 1.5 ks of Photon Counting (PC) mode data between T0+10.3 ks and T0+16.1 ks. No X-ray sources have been detected consistent with being within 572 arcsec of the SVOM/ECLAIRs position. The 3-sigma upper limit in the field ranges from ~0.006 to ~0.007 ct s^-1, corresponding to a 0.3-10 keV observed flux of 2.4e-13 to 2.8e-13 erg cm^-2 s^-1 (assuming a typical GRB spectrum). 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/ToO_GRBs/00021731. This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/38219. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36198] IceCube-241113A: Upper limits from a search for additional neutrino events in IceCube
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38218 SUBJECT: IceCube-241113A: Upper limits from a search for additional neutrino events in IceCube DATE: 24/11/14 15:47:55 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-241113A (https://gcn.nasa.gov/circulars/38200) in a time range of 1000 seconds centered on the alert event time (2024-11-13 00:14:00.680 UTC to 2024-11-13 00:30:40.680 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-241113A. The IceCube sensitivity to neutrino point sources with an E^-2.5 spectrum (E^2 dN/dE at 1 TeV) within the locations spanned by the 90% spatial containment region of IceCube-241113A is 1.3e-01 GeV cm^-2 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 1e+05 GeV. A subsequent search was performed including 2 days of data centered on the alert event time (2024-11-12 00:22:20.680 UTC to 2024-11-14 00:22:20.680 UTC). In this case, we report a p-value of 1.00, consistent with no significant excess of track events. The IceCube sensitivity to neutrino point sources with an E^-2.5 spectrum (E^2 dN/dE at 1 TeV) within the locations spanned by the 90% spatial containment region of IceCube-241113A is 1.5e-01 GeV cm^-2 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/38218. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36197] GRB 241113A: 1.6m Mephisto and 50cm array optical upper limits
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38217 SUBJECT: GRB 241113A: 1.6m Mephisto and 50cm array optical upper limits DATE: 24/11/14 15:11:38 GMT FROM: Brajesh Kumar at SWIFAR, YNU <brajesh(a)ynu.edu.cn> Guowang Du, Brajesh Kumar, Weikang Lin, Yaosong Yu, Yehao Cheng, Yu Pan, Xinlei Chen, Xingzhu Zou, Jinghua Zhang, Yuanpei Yang, Yuan Fang, Xiangkun Liu, Xiaowei Liu (SWIFAR, YNU) report on behalf of the Mephisto Team: The field of GRB 241113A detected by Swift (Siegel et al., GCN 38194) was observed with the 1.6m Multi-channel Photometric Survey Telescope (Mephisto) and 50cm array facilities of Yunnan University located at Lijiang Observatory. The observations were initiated after ~4.3 hr with 50cm array and Mephisto telescopes starting from 12:03:04 and 12:08:46 UT on 2024-11-13. Multiple frames (uvgriz and gr bands with Mephisto and 50 cm array) with different exposure time were obtained. The images were suffered with high background due to proximity of the moon. The optical afterglow (Siegel et al., GCN 38194; Francile et al., GCN 38195; Ferrer et al., GCN 38197; Izzo et al., GCN 38201; Ferro et al., GCN 38206; Breeveld et al., GCN 38207; Zheng et al., GCN 38216) was not detected in the stacked images and the 3-sigma upper limits are below. 50CM array Start_Time(UT) Band Exp(s) Lim-mag(AB) 2024-11-13T12:03:05 g 120*2 >19.39 2024-11-13T12:03:04 r 120*2 >19.40 Mephisto Start_Time(UT) Band Exp(s) Lim-mag(AB) 2024-11-13T12:08:46 u 180*4 >20.97 2024-11-13T12:26:51 v 180*2|300*2 >21.34 2024-11-13T12:08:46 g 50*12 >21.41 2024-11-13T12:26:51 r 50*6|300*2 >21.82 2024-11-13T12:08:46 i 79*8 >20.79 2024-11-13T12:26:51 z 79*4|294*2 >20.22 -------------------------------------------------------------------------- Mephisto (Multi-channel Photometric Survey Telescope) is a 1.6m wide-field multi-channel telescope, the first of its type in the world, capable of imaging the same field of view in three optical bands simultaneously. It provides real-time, high-quality colors of stellar objects. The on-site telescope assemblage and commissioning were carried out in September 2022. The first light in all three channels was achieved on 2023 December 21. The 50cm array consists of two 50cm telescopes for wide-field surveys and also serves as the supporting facility for monitoring the Mephisto detected targets. -------------------------------------------------------------------------- View this GCN Circular online at https://gcn.nasa.gov/circulars/38217. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36196] GRB 241113A: 1.6m Mephisto and 50cm array optical upper limits
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38217 SUBJECT: GRB 241113A: 1.6m Mephisto and 50cm array optical upper limits DATE: 24/11/14 15:11:38 GMT FROM: Brajesh Kumar at SWIFAR, YNU <brajesh(a)ynu.edu.cn> Guowang Du, Brajesh Kumar, Weikang Lin, Yaosong Yu, Yehao Cheng, Yu Pan, Xinlei Chen, Xingzhu Zou, Jinghua Zhang, Yuanpei Yang, Yuan Fang, Xiangkun Liu, Xiaowei Liu (SWIFAR, YNU) report on behalf of the Mephisto Team: The field of GRB 241113A detected by Swift (Siegel et al., GCN 38194) was observed with the 1.6m Multi-channel Photometric Survey Telescope (Mephisto) and 50cm array facilities of Yunnan University located at Lijiang Observatory. The observations were initiated after ~4.3 hr with 50cm array and Mephisto telescopes starting from 12:03:04 and 12:08:46 UT on 2024-11-13. Multiple frames (uvgriz and gr bands with Mephisto and 50 cm array) with different exposure time were obtained. The images were suffered with high background due to proximity of the moon. The optical afterglow (Siegel et al., GCN 38194; Francile et al., GCN 38195; Ferrer et al., GCN 38197; Izzo et al., GCN 38201; Ferro et al., GCN 38206; Breeveld et al., GCN 38207; Zheng et al., GCN 38216) was not detected in the stacked images and the 3-sigma upper limits are below. 50CM array Start_Time(UT) Band Exp(s) Lim-mag(AB) 2024-11-13T12:03:05 g 120*2 >19.39 2024-11-13T12:03:04 r 120*2 >19.40 Mephisto Start_Time(UT) Band Exp(s) Lim-mag(AB) 2024-11-13T12:08:46 u 180*4 >20.97 2024-11-13T12:26:51 v 180*2|300*2 >21.34 2024-11-13T12:08:46 g 50*12 >21.41 2024-11-13T12:26:51 r 50*6|300*2 >21.82 2024-11-13T12:08:46 i 79*8 >20.79 2024-11-13T12:26:51 z 79*4|294*2 >20.22 -------------------------------------------------------------------------- Mephisto (Multi-channel Photometric Survey Telescope) is a 1.6m wide-field multi-channel telescope, the first of its type in the world, capable of imaging the same field of view in three optical bands simultaneously. It provides real-time, high-quality colors of stellar objects. The on-site telescope assemblage and commissioning were carried out in September 2022. The first light in all three channels was achieved on 2023 December 21. The 50cm array consists of two 50cm telescopes for wide-field surveys and also serves as the supporting facility for monitoring the Mephisto detected targets. -------------------------------------------------------------------------- View this GCN Circular online at https://gcn.nasa.gov/circulars/38217. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36195] GRB 241113A: KAIT optical observations
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38216 SUBJECT: GRB 241113A: KAIT optical observations DATE: 24/11/14 09:14:38 GMT FROM: Weikang Zheng at UC Berkeley <weikang(a)berkeley.edu> WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on behalf of the KAIT GRB team: The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at Lick Observatory, responded to GRB 241113A detected by Swift (Siegel et al., GCN 38194) starting at 08:03:11 UT, 898s after the bust under cloudy conditions. Observations were performed in the clear (roughly R) filter, and a set of 20s, 40s and 60s exposure images were obtained. The optical afterglow (Siegel et al., GCN 38194; Francile et al., GCN 38195; Ferrer et al., GCN 38197; Izzo et al., GCN 38201; Ferro et al., GCN 38206; Breeveld et al., GCN 38207) was barely detected in individual image due to cloudy weather. However, the optical afterglow was detected in the coadd images. We measure the following magnitude calibrated to PS1 catalog: tmid-t0(s) exp mag err 961 5x20s 17.9 +/- 0.2 1119 5x20s 18.1 +/- 0.2 1419 9x40s 18.5 +/- 0.3 2293 16x60s 19.0 +/- 0.3 View this GCN Circular online at https://gcn.nasa.gov/circulars/38216. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36194] EP241113b: Global MASTER-Net observations report
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38215 SUBJECT: EP241113b: Global MASTER-Net observations report DATE: 24/11/14 09:09:23 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, 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. 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) was pointed to the EP241113b ( EP Team et al., GCN 38214) errorbox 35232 sec after trigger time at 2024-11-13 21:10:02 UT, with upper limit up to 18.0 mag. The observations began at zenith distance = 40 deg. The sun altitude is -65.0 deg. MASTER-Tunka robotic telescope located in Russia (Applied Physics Institute, Irkutsk State University) was pointed to the EP241113b errorbox 35748 sec after trigger time at 2024-11-13 21:18:38 UT, with upper limit up to 20.8 mag. The observations began at zenith distance = 6 deg. The sun altitude is -28.5 deg. The galactic latitude b = 25 deg., longitude l = 171 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2669806 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 35262 | 2024-11-13 21:10:02 | MASTER-Kislovodsk | (07h 19m 25.31s , +46d 57m 34.8s) | C | 60 | 17.3 | 35322 | 2024-11-13 21:10:02 | MASTER-Kislovodsk | (07h 19m 25.31s , +46d 57m 34.8s) | C | 180 | 18.0 | Coadd 35554 | 2024-11-13 21:14:54 | MASTER-Kislovodsk | (07h 19m 28.89s , +46d 59m 28.3s) | C | 60 | 17.3 | 35636 | 2024-11-13 21:16:15 | MASTER-Kislovodsk | (07h 19m 28.71s , +46d 58m 01.3s) | C | 60 | 17.2 | 35718 | 2024-11-13 21:17:38 | MASTER-Kislovodsk | (07h 19m 30.58s , +46d 59m 35.6s) | C | 60 | 17.3 | 35778 | 2024-11-13 21:17:38 | MASTER-Kislovodsk | (07h 19m 30.58s , +46d 59m 35.7s) | C | 180 | 17.9 | Coadd 35778 | 2024-11-13 21:18:38 | MASTER-Tunka | (07h 20m 37.94s , +46d 54m 47.8s) | C | 60 | 18.5 | 35838 | 2024-11-13 21:18:38 | MASTER-Tunka | (07h 20m 37.95s , +46d 54m 47.9s) | C | 180 | 19.3 | Coadd 36378 | 2024-11-13 21:18:38 | MASTER-Tunka | (07h 20m 37.94s , +46d 54m 47.8s) | C | 1260 | 20.6 | Coadd 35800 | 2024-11-13 21:19:00 | MASTER-Kislovodsk | (07h 19m 25.38s , +46d 58m 45.1s) | C | 60 | 17.2 | 35854 | 2024-11-13 21:19:53 | MASTER-Tunka | (07h 20m 31.76s , +46d 53m 50.6s) | C | 60 | 18.5 | 35881 | 2024-11-13 21:20:21 | MASTER-Kislovodsk | (07h 19m 24.23s , +46d 59m 43.9s) | C | 60 | 17.3 | 35926 | 2024-11-13 21:21:05 | MASTER-Tunka | (07h 20m 39.09s , +46d 54m 14.9s) | C | 60 | 18.4 | 36001 | 2024-11-13 21:22:20 | MASTER-Tunka | (07h 20m 35.07s , +46d 55m 53.4s) | C | 60 | 18.5 | 36061 | 2024-11-13 21:22:20 | MASTER-Tunka | (07h 20m 35.07s , +46d 55m 53.4s) | C | 180 | 19.4 | Coadd 36072 | 2024-11-13 21:23:32 | MASTER-Tunka | (07h 20m 35.00s , +46d 54m 17.8s) | C | 60 | 18.4 | 36146 | 2024-11-13 21:24:46 | MASTER-Tunka | (07h 20m 38.35s , +46d 55m 52.1s) | C | 60 | 18.6 | 36223 | 2024-11-13 21:26:03 | MASTER-Tunka | (07h 20m 31.31s , +46d 55m 04.5s) | C | 60 | 18.6 | 36283 | 2024-11-13 21:26:03 | MASTER-Tunka | (07h 20m 31.30s , +46d 55m 04.4s) | C | 180 | 19.4 | Coadd 36296 | 2024-11-13 21:27:16 | MASTER-Tunka | (07h 20m 31.90s , +46d 56m 07.3s) | C | 60 | 18.5 | 36367 | 2024-11-13 21:27:56 | MASTER-Kislovodsk | (07h 19m 26.72s , +46d 59m 40.3s) | C | 120 | 17.3 | 36380 | 2024-11-13 21:28:40 | MASTER-Tunka | (07h 20m 38.02s , +46d 55m 10.0s) | C | 60 | 18.6 | 36509 | 2024-11-13 21:30:18 | MASTER-Kislovodsk | (07h 19m 27.33s , +46d 58m 31.5s) | C | 120 | 17.3 | 36862 | 2024-11-13 21:36:11 | MASTER-Kislovodsk | (07h 19m 22.82s , +46d 59m 19.5s) | C | 120 | 16.8 | 37004 | 2024-11-13 21:38:33 | MASTER-Kislovodsk | (07h 19m 24.47s , +47d 00m 18.7s) | C | 120 | 16.8 | 38196 | 2024-11-13 21:58:56 | MASTER-Tunka | (07h 20m 34.59s , +46d 56m 15.4s) | C | 60 | 19.6 | 38256 | 2024-11-13 21:58:56 | MASTER-Tunka | (07h 20m 34.60s , +46d 56m 15.5s) | C | 180 | 20.2 | Coadd 38466 | 2024-11-13 21:58:56 | MASTER-Tunka | (07h 20m 34.59s , +46d 56m 15.5s) | C | 600 | 20.8 | Coadd 38270 | 2024-11-13 22:00:09 | MASTER-Tunka | (07h 20m 28.15s , +46d 55m 17.7s) | C | 60 | 19.6 | 38348 | 2024-11-13 22:01:27 | MASTER-Tunka | (07h 20m 35.52s , +46d 55m 42.3s) | C | 60 | 19.5 | 38420 | 2024-11-13 22:02:40 | MASTER-Tunka | (07h 20m 31.85s , +46d 57m 17.0s) | C | 60 | 19.6 | 38480 | 2024-11-13 22:02:40 | MASTER-Tunka | (07h 20m 31.85s , +46d 57m 17.0s) | C | 180 | 20.1 | Coadd 38492 | 2024-11-13 22:03:52 | MASTER-Tunka | (07h 20m 31.77s , +46d 55m 25.9s) | C | 60 | 19.4 | 38564 | 2024-11-13 22:05:04 | MASTER-Tunka | (07h 20m 34.94s , +46d 56m 58.6s) | C | 60 | 19.4 | 38636 | 2024-11-13 22:06:16 | MASTER-Tunka | (07h 20m 28.92s , +46d 56m 29.0s) | C | 60 | 19.5 | 38696 | 2024-11-13 22:06:16 | MASTER-Tunka | (07h 20m 28.92s , +46d 56m 29.0s) | C | 180 | 20.2 | Coadd 38708 | 2024-11-13 22:07:28 | MASTER-Tunka | (07h 20m 28.35s , +46d 57m 31.3s) | C | 60 | 19.6 | 38782 | 2024-11-13 22:08:42 | MASTER-Tunka | (07h 20m 34.36s , +46d 56m 33.4s) | C | 60 | 19.6 | 38854 | 2024-11-13 22:09:54 | MASTER-Tunka | (07h 20m 28.04s , +46d 55m 35.5s) | C | 60 | 19.7 | 38914 | 2024-11-13 22:09:54 | MASTER-Tunka | (07h 20m 28.04s , +46d 55m 35.4s) | C | 180 | 20.3 | Coadd 38927 | 2024-11-13 22:11:06 | MASTER-Tunka | (07h 20m 34.43s , +46d 55m 40.2s) | C | 60 | 19.6 | 39000 | 2024-11-13 22:12:20 | MASTER-Tunka | (07h 20m 31.08s , +46d 57m 32.7s) | C | 60 | 19.8 | 39105 | 2024-11-13 22:13:35 | MASTER-Tunka | (07h 20m 30.97s , +46d 55m 53.0s) | C | 120 | 19.9 | 39225 | 2024-11-13 22:13:35 | MASTER-Tunka | (07h 20m 30.97s , +46d 55m 53.0s) | C | 360 | 20.5 | Coadd 39240 | 2024-11-13 22:15:49 | MASTER-Tunka | (07h 20m 32.98s , +46d 57m 37.2s) | C | 120 | 19.9 | 39371 | 2024-11-13 22:18:01 | MASTER-Tunka | (07h 20m 27.32s , +46d 56m 51.7s) | C | 120 | 19.9 | 39426 | 2024-11-13 22:18:56 | MASTER-Kislovodsk | (07h 17m 59.03s , +47d 11m 09.6s) | C | 120 | 16.2 | 39546 | 2024-11-13 22:18:56 | MASTER-Kislovodsk | (07h 17m 58.99s , +47d 11m 09.6s) | C | 360 | 16.4 | Coadd 39505 | 2024-11-13 22:20:14 | MASTER-Tunka | (07h 20m 27.95s , +46d 57m 56.0s) | C | 120 | 19.8 | 39625 | 2024-11-13 22:20:14 | MASTER-Tunka | (07h 20m 27.95s , +46d 57m 56.0s) | C | 360 | 20.4 | Coadd 39568 | 2024-11-13 22:21:17 | MASTER-Kislovodsk | (07h 17m 57.57s , +47d 12m 27.8s) | C | 120 | 16.3 | 39636 | 2024-11-13 22:22:25 | MASTER-Tunka | (07h 20m 32.35s , +46d 56m 60.0s) | C | 120 | 19.8 | 39709 | 2024-11-13 22:23:38 | MASTER-Kislovodsk | (07h 17m 57.13s , +47d 11m 11.1s) | C | 120 | 16.3 | 39768 | 2024-11-13 22:24:37 | MASTER-Tunka | (07h 20m 26.74s , +46d 56m 04.0s) | C | 120 | 19.9 | 40060 | 2024-11-13 22:29:30 | MASTER-Kislovodsk | (07h 17m 53.72s , +47d 12m 05.5s) | C | 120 | 16.6 | 40180 | 2024-11-13 22:29:30 | MASTER-Kislovodsk | (07h 17m 53.72s , +47d 12m 05.6s) | C | 360 | 17.5 | Coadd 40202 | 2024-11-13 22:31:51 | MASTER-Kislovodsk | (07h 17m 52.16s , +47d 13m 05.1s) | C | 120 | 17.0 | 40344 | 2024-11-13 22:34:14 | MASTER-Kislovodsk | (07h 17m 58.71s , +47d 12m 06.8s) | C | 120 | 16.9 | 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/38215. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36193] EP241113b/GRB 241113B: EP detection of GRB 241113B
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38214 SUBJECT: EP241113b/GRB 241113B: EP detection of GRB 241113B DATE: 24/11/14 09:01:38 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> Z. Y. Liu, M. Q. Huang (USTC), C. Y. Dai (NJU), X. P. Xu, M. H. Zhang, W. Yuan (NAO, CAS) report on behalf of the Einstein Probe team: We report on the detection of an X-ray transient, designated EP241113b, by the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) mission. The WXT position of EP241113b is R.A.= 110.233 deg, DEC = 46.800 deg (J2000) with an uncertainty of 2.5 arcmin (radius, 90% C.L. statistical and systematic). The lightcurve of the transient observed by the WXT lasts around 100 seconds. The 0.5-4.0 keV spectrum can be fitted using an absorbed power law with a photon index of 1.5 +/- 0.7, and a column density of 2.7 (+/- 1.8) ×10^(21) cm^-2. The derived average flux is estimated to be around 1.5 (+/- 0.4 ) ×10^(-9) erg/s/cm^2 in 0.5-4.0 keV. EP241113b is spatially and temporally consistent with GRB 241113B (GCN 38196; GCN 38212). The burst started at 2024-11-13T11:22:50 (UTC), which is about 15 seconds before the SVOM/ECLAIRs trigger time (2024-11-13T11:23:05). 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/38214. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36192] Fermi-LAT gamma-ray observations of IceCube-241113A
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38213 SUBJECT: Fermi-LAT gamma-ray observations of IceCube-241113A DATE: 24/11/14 08:48:22 GMT FROM: Leo Pfeiffer at University of Würzburg <pfeiffer.leo(a)gmail.com> L. Pfeiffer (Univ. of Wuerzburg), S. Buson (DESY, Univ. of Wuerzburg), C. Bartolini (INFN Bari), S. Garrappa (Weizmann Institute of Science) and J. Sinapius (DESY) and P. M. Veres (Ruhr University Bochum) on behalf of the Fermi-LAT collaboration: We report an analysis of observations of the vicinity of the high-energy IC-241113A neutrino event (GCN 38200) with all-sky survey data from the Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope. The IceCube event was detected on 2024-11-13 00:22:20.68 UTC (T0) with J2000 position RA = 196.17 (+0.60, -0.60) deg, Decl. = 8.57 (+0.77, -0.83) deg 90% PSF containment. No cataloged gamma-ray sources are found within the 90% IC-241113A localization error (Fourth Fermi-LAT catalog, 4FGL-DR4, The Fermi-LAT collaboration 2023, arXiv:2307.12546). We searched for the existence of intermediate (days to years) timescale emission from a new gamma-ray transient source. Preliminary analysis indicates no significant (>5sigma) new excess emission (> 100 MeV) within the IC-241113A 90% confidence localization. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IceCube best-fit position, the >100 MeV flux upper limit (95% confidence) is <4.75e-10 ph cm^-2 s^-1 for ~16-years (2008-08-04 / T0), <1.03e-08(<5.19e-08) ph cm^-2 s^-1 for a 1-month (1-day) integration time before T0. Since Fermi normally operates in an all-sky scanning mode, regular monitoring of this source will continue. For this source, the Fermi-LAT contact person is L. Pfeiffer (leonard.pfeiffer at stud-mail.uni-wuerzburg.de). The Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden. View this GCN Circular online at https://gcn.nasa.gov/circulars/38213. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36191] GRB 241113B: SVOM/GRM observation
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38212 SUBJECT: GRB 241113B: SVOM/GRM observation DATE: 24/11/14 07:15:06 GMT FROM: zhengchao_astro(a)foxmail.com SVOM/GRM team: Jia-Cong Liu, 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, Yue Wang, 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, Jin-Peng Zhang, Chao Zheng (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, the SVOM/GRM was triggered by GRB 241113B(SVOM trigger reference: sb24111301) at 2024-11-13T11:23:05 UT (T0), which was also triggered by SVOM/ECLAIRs (Dagoneau et al, GCN 38196). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of one pulse, with a T90 of 11.7 +1.9/-3.0 s (15-550 keV). This burst is located at about 23.8 degrees from the SVOM optical axis. The GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb241113B.png 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 point of contact for this burst is: Jia-Cong Liu (IHEP)(liujiacong(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/38212. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36190] EP241113a: EP on-board trigger and autonomous follow-up observation
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38211 SUBJECT: EP241113a: EP on-board trigger and autonomous follow-up observation DATE: 24/11/14 04:21:43 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> Z. Y. Liu, M. Q. Huang (USTC), C. Y. Dai (NJU), X. P. Xu, M. H. Zhang, W. Yuan (NAO, CAS) report on behalf of the Einstein Probe team: We report on the detection of an X-ray transient detected by EP-WXT, EP241113a, which triggered the on-board processing unit (trigger ID: 01709120178) at 2024-11-13T19:12:53 (UTC). The telemetry data show that the flare started at 2024-11-13T19:09:19 (UTC) . The 0.5-4 keV spectrum can be fitted using an absorbed power law with a photon index of 1.3 +/- 0.2 (with column density fixed to the Galactic value of 2.6e20 cm^-2). The derived average flux is estimated to be around 5.57 (+1.26/-0.76 ) ×10^(-10) erg/s/cm2 in 0.5-4 keV. An autonomous observation on the X-ray transient was performed by the EP-FXT about 2 minutes later, which detected an uncatalogued X-ray source at R.A. = 131.9964 deg, DEC = 52.3815 deg (J2000) with an uncertainty of about 10 arcsecs (radius, 90% C.L. statistical and systematic), consistent with the position of the WXT transient within the uncertainties. During the 5000-second exposure, a significant decline is observed in the light curve. We fit an absorbed power law model to the 0.5-10 keV spectra with N_H fixed at the Galactic value. The average flux is 2.5 (+0.3/-0.2)×10^(-11) erg/s/cm^2, and the photon index is 2.40+/-0.17. Further follow-up observations are encouraged to identify the nature of this X-ray transient. 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/38211. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36189] LIGO/Virgo/KAGRA S241114y: Identification of a GW compact binary merger candidate
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38210 SUBJECT: LIGO/Virgo/KAGRA S241114y: Identification of a GW compact binary merger candidate DATE: 24/11/14 03:26:50 GMT FROM: Jade Powell at LIGO Scientific Collaboration <jade.powell(a)ligo.org> The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We identified the compact binary merger candidate S241114y during real-time processing of data from LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) at 2024-11-14 02:47:11.780 UTC (GPS time: 1415587649.780). The candidate was found by the cWB [1], cWB BBH [2], GstLAL [3], MBTA [4], and SPIIR [5] analysis pipelines. S241114y is an event of interest because its false alarm rate, as estimated by the online analysis, is 9.1e-14 Hz, or about one in 1e6 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S241114y After parameter estimation by RapidPE-RIFT [6], the classification of the GW signal, in order of descending probability, is BBH (>99%), Terrestrial (<1%), NSBH (<1%), or BNS (<1%). Assuming the candidate is astrophysical in origin, the probability that the lighter compact object is consistent with a neutron star mass (HasNS) is <1%. [7] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [7] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%. Two sky maps are available at this time and can be retrieved from the GraceDB event page: * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [8], distributed via GCN notice about 34 seconds after the candidate event time. * bayestar.multiorder.fits,2, an initial localization generated by BAYESTAR [8], distributed via GCN notice about 5 minutes after the candidate event time. The preferred sky map at this time is bayestar.multiorder.fits,2. For the bayestar.multiorder.fits,2 sky map, the 90% credible region is 538 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 3539 +/- 992 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/. [1] Klimenko et al. PRD 93, 042004 (2016) doi:10.1103/PhysRevD.93.042004 [2] T. Mishra et al. PRD 105, 083018 (2022) doi:10.1103/PhysRevD.105.083018 [3] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. (2023) arXiv:2305.05625 [4] Aubin et al. CQG 38, 095004 (2021) doi:10.1088/1361-6382/abe913 [5] Chu et al. PRD 105, 024023 (2022) doi:10.1103/PhysRevD.105.024023 [6] Rose et al. (2022) arXiv:2201.05263 and Pankow et al. PRD 92, 023002 (2015) doi:10.1103/PhysRevD.92.023002 [7] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe [8] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013 View this GCN Circular online at https://gcn.nasa.gov/circulars/38210. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36188] GRB 241113A: Swift-XRT refined Analysis
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38209 SUBJECT: GRB 241113A: Swift-XRT refined Analysis DATE: 24/11/14 00:29:13 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> A.P. Beardmore (U. Leicester), M. Ferro (INAF-OAB), R. Brivio (INAF-OAB), A. D'Ai (INAF-IASFPA), J.A. Kennea (PSU), D.N. Burrows (PSU), M. A. Williams (PSU), J.P. Osborne (U. Leicester) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 7.7 ks of XRT data for GRB 241113A, from 60 s to 34.4 ks after the BAT trigger. The data comprise 75 s in Windowed Timing (WT) mode (the first 10 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The light curve can be modelled with an initial power-law decay with an index of alpha=1.90 (+/-0.24), followed by a break at T+165 s to an alpha of 0.92 (+0.04, -0.05). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.32 (+0.33, -0.30). The best-fitting absorption column is 2.2 (+1.1, -0.9) x 10^21 cm^-2, in excess of the Galactic value of 2.0 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 (5.1 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 2.2 (+1.1, -0.9) x 10^21 cm^-2 Galactic foreground: 2.0 x 10^20 cm^-2 Excess significance: 3.7 sigma Photon index: 2.32 (+0.33, -0.30) If the light curve continues to decay with a power-law decay index of 0.92, the count rate at T+24 hours will be 8.0 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.5 x 10^-13 (4.1 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01267501. This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/38209. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36187] EP241107a: SOAR upper limits
by GCN Circulars 14 Nov '24

14 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38208 SUBJECT: EP241107a: SOAR upper limits DATE: 24/11/14 00:19:31 GMT FROM: James Freeburn at Swinburne University of Technology <jamesfreeburn54(a)gmail.com> J. Freeburn (Swinburne/OzGrav), I. Andreoni (UNC), J. Carney (UNC) We observed the optical counterpart to EP241107a (Zhou et al., GCN 38112) with the Goodman High Throughput Spectrograph mounted on the SOAR telescope in imaging mode (Prop. ID: SOAR2024B-021). We took two 300s exposures each in g, r and i-band between 2024-11-11T03:05:18 and 2024-11-11T03:38:26 UTC corresponding to ~3.5 days after the initial trigger. Our observations do not reveal the optical counterpart associated with EP241107a (Odeh et al., GCN 38115; SVOM/C-GFT team, GCN 38116; Lipunov et al., GCN 38117; Mohan et al., GCN 38118; Busmann et al., GCN 38120; Adami et al., GCN 38122; Quirola-Vasquez et al., GCN 38126; Li et al., 38127; Odeh et al., GCN 38128; Kong et al., GCN 38131; Zheng et al., GCN 38136; Pankov et al, GCN 38147). With photometric calibration using the Pan-STARRS1 catalogue, we provide the following AB magnitude upper limits: g > 22.4 r > 22.9 i > 22.7 View this GCN Circular online at https://gcn.nasa.gov/circulars/38208. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36186] GRB 241113A: Swift/UVOT Detection
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38207 SUBJECT: GRB 241113A: Swift/UVOT Detection DATE: 24/11/13 22:12:55 GMT FROM: Alice Breeveld at MSSL-UCL <a.breeveld(a)ucl.ac.uk> A. A. Breeveld (UCL-MSSL) and M. H. Siegel (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT began observations of the field of GRB 241113A 61 s after the BAT trigger (Siegel et al., GCN Circ. 38194) with a short settling exposure in v, and a longer finding chart exposure in the white filter. A fading source consistent with the XRT position (Goad et al., GCN Circ. 38198) and also detected by Francile et al. (GCN Circ. 38195), Huertas Ferrer et al. (GCN Circ. 38197), Izzo et al. (GCN Circ. 38201) and Ferro et al. (GCN Circ. 38206) is detected in the initial UVOT exposures. Preliminary detections and 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag v 61 72 11 14.87 ± 0.07 white 82 183 100 15.90 ± 0.03 b 5359 5559 197 20.18 ± 0.36 u 5154 5354 197 19.80 ± 0.33 uvw1 4949 5149 197 >19.61 uvw2 4335 5970 393 >20.12 uvm2 4744 4944 197 >19.46 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.030 in the direction of the burst (Schlegel et al. 1998). View this GCN Circular online at https://gcn.nasa.gov/circulars/38207. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36185] GRB 241113A: REM detection of the optical/NIR afterglow
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38206 SUBJECT: GRB 241113A: REM detection of the optical/NIR afterglow DATE: 24/11/13 19:34:00 GMT FROM: Matteo Ferro at INAF-OAB <matteo.ferro(a)inaf.it> M. Ferro, Y.-D. Hu, S. Covino, R. Brivio, P. D’Avanzo, D. Fugazza (INAF-OAB), L. Izzo (INAF-OACn and DARK/NBI), and A. Melandri (INAF-OAR) report on behalf of the REM team: We observed the field of GRB 241113A (Siegel et al., GCN #38194; Goad et al., GCN #38198) with the REM 60cm robotic telescope located at the ESO observatory of La Silla (Chile). The observations were carried in the g, r, i, z, J, H and K bands, starting on 2024 Nov 13 at 08:03:10 UT (i.e. about 15 minutes after the Swift trigger) and lasted for about 1.75 hours. The optical afterglow is detected in the r band at a position coincident with that reported by Swift-UVOT (Siegel et al., GCN #38194) and other optical observations (Francile et al., GCN #38195, Huertas Ferrer et al., GCN #38197; Izzo et al., GCN #38201). The NIR afterglow is detected in the H band at a position consistent with the optical counterpart. From preliminary photometry, we derive the following magnitudes: r = 18.7 +/- 0.3 (AB; calibrated against the Pan-STARRS catalogue) at a mid-time of ~ 37 minutes after the trigger, H = 15.5 +/- 0.2 (Vega; calibrated against the 2MASS catalogue) at a mid-time of ~ 26 minutes after the trigger. View this GCN Circular online at https://gcn.nasa.gov/circulars/38206. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36184] Konus-Wind detection of GRB 241107A (short/hard)
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38205 SUBJECT: Konus-Wind detection of GRB 241107A (short/hard) DATE: 24/11/13 17:52:12 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 short GRB 241107A (SVOM/GRM detection: Wang et al., GCN 38125; INTEGRAL/IBIS/PICsIT detection: Rodi et al., GCN 38164; IPN triangulation: Kozyrev et al., GCN 38165; INTEGRAL IBIS localization: Mereghetti et al., GCN 38172; Swift/BAT candidate arcminute localization: DeLaunay et al.: GCN 38177) triggered Konus-Wind (KW) at T0=84602.493 s UT (23:30:02.493). The burst light curve starts with a bright, multi-peaked emission pulse with a duration of ~0.028 s, which is followed by a weaker, decaying emission. The total duration of the burst is ~0.160 s. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB241107_T84602/ As observed by Konus-Wind, the burst had a total fluence of 1.43(-0.33, +0.13)x10^-6 erg/cm^2 and a 16-ms peak energy flux, measured from T0-0.096 s, of 3.6 (-1.2, +0.2)x10^-5 erg/cm^2/s (both in the 20 keV - 10 MeV energy range). Since the bulk of the burst emission was detected before the trigger, the spectral analysis was performed using the KW 3-channel light curve data. The time-averaged spectrum of the burst (measured from T0-0.048 s to T0+0.080 s) is best fit by a blackbody (BB) function with kT(BB) = 193 (-18, +20) keV. This spectrum can be also described by a power law with exponential cutoff (CPL) model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with a hard photon index alpha = 1.32(-1.09,+2.7) and Ep = 760(-91,+390) keV. The spectrum of the initial pulse alone (measured from T0-0.112 s to T0-0.080 s) is best described by a blackbody function with kT(BB) = 251 (-31, +38) keV. The fluence in this pulse is 1.15(-0.38, +0.06)x10^-6 erg/cm^2, or ~80% of the total fluence. 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/38205. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36183] LIGO/Virgo/KAGRA S241113p: Identification of a GW compact binary merger candidate
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38204 SUBJECT: LIGO/Virgo/KAGRA S241113p: Identification of a GW compact binary merger candidate DATE: 24/11/13 17:08:35 GMT FROM: joan-rene.merou(a)ligo.org The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We identified the compact binary merger candidate S241113p during real-time processing of data from LIGO Livingston Observatory (L1) and Virgo Observatory (V1) at 2024-11-13 16:35:07.498 UTC (GPS time: 1415550925.498). The candidate was found by the GstLAL [1] analysis pipeline. S241113p is an event of interest because its false alarm rate, as estimated by the online analysis, is 1.5e-14 Hz, or about one in 1e6 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S241113p The classification of the GW signal, in order of descending probability, is BBH (>99%), Terrestrial (<1%), NSBH (<1%), or BNS (<1%). Assuming the candidate is astrophysical in origin, the probability that the lighter compact object is consistent with a neutron star mass (HasNS) is <1%. [2] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [2] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%. Two sky maps are available at this time and can be retrieved from the GraceDB event page: * bayestar.multiorder.fits,0, an initial localization generated by BAYESTAR [3], distributed via GCN notice about 27 seconds after the candidate event time. * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [3], distributed via GCN notice about 5 minutes after the candidate event time. The preferred sky map at this time is bayestar.multiorder.fits,1. For the bayestar.multiorder.fits,1 sky map, the 90% credible region is 11072 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1400 +/- 402 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/. [1] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. (2023) arXiv:2305.05625 [2] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe [3] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013 View this GCN Circular online at https://gcn.nasa.gov/circulars/38204. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36182] LIGO/Virgo/KAGRA S241113p: Identification of a GW compact binary merger candidate
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38204 SUBJECT: LIGO/Virgo/KAGRA S241113p: Identification of a GW compact binary merger candidate DATE: 24/11/13 17:08:35 GMT FROM: joan-rene.merou(a)ligo.org The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We identified the compact binary merger candidate S241113p during real-time processing of data from LIGO Livingston Observatory (L1) and Virgo Observatory (V1) at 2024-11-13 16:35:07.498 UTC (GPS time: 1415550925.498). The candidate was found by the GstLAL [1] analysis pipeline. S241113p is an event of interest because its false alarm rate, as estimated by the online analysis, is 1.5e-14 Hz, or about one in 1e6 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S241113p The classification of the GW signal, in order of descending probability, is BBH (>99%), Terrestrial (<1%), NSBH (<1%), or BNS (<1%). Assuming the candidate is astrophysical in origin, the probability that the lighter compact object is consistent with a neutron star mass (HasNS) is <1%. [2] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [2] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%. Two sky maps are available at this time and can be retrieved from the GraceDB event page: * bayestar.multiorder.fits,0, an initial localization generated by BAYESTAR [3], distributed via GCN notice about 27 seconds after the candidate event time. * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [3], distributed via GCN notice about 5 minutes after the candidate event time. The preferred sky map at this time is bayestar.multiorder.fits,1. For the bayestar.multiorder.fits,1 sky map, the 90% credible region is 11072 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1400 +/- 402 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/. [1] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. (2023) arXiv:2305.05625 [2] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe [3] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013 View this GCN Circular online at https://gcn.nasa.gov/circulars/38204. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36181] IceCube-241113A - IceCube observation of a high-energy neutrino candidate track-like event
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38200 SUBJECT: IceCube-241113A - IceCube observation of a high-energy neutrino candidate track-like event DATE: 24/11/13 14:38:33 GMT FROM: A. Zegarelli at Ruhr University Bochum <azegarelli(a)icecube.wisc.edu> The IceCube Collaboration (http://icecube.wisc.edu/) reports: On 2024-11-13 00:22:20.68 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. The average astrophysical neutrino purity for Gold alerts is 30%. This alert has an estimated false alarm rate of 3.8708 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/140078_30891383.amon), more sophisticated reconstruction algorithms have been applied offline, with the direction refined to: Date: 2024-11-13 Time: 00:22:20.68 UT RA: 196.17 (+0.60, -0.60 deg 90% PSF containment) J2000 Dec: 8.57 (+0.77, -0.83 deg 90% PSF containment) J2000 We encourage follow-up by ground and space-based instruments to help identify a possible astrophysical source for the candidate neutrino. No Fermi 4FGL or 3FHL catalog sources are in the 90% uncertainty region. 4FGL J1301.6+0834 (4FGL catalog source) at RA = 195.41 deg and Dec = 8.57 deg is the closest known source, located just outside the 90% uncertainty region (0.75 deg away from the best-fit position). 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/38200. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36180] Fermi Gamma-ray Burst Monitor trigger 753166198/241113201 is not a GRB
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38203 SUBJECT: Fermi Gamma-ray Burst Monitor trigger 753166198/241113201 is not a GRB DATE: 24/11/13 16:43:20 GMT FROM: Matt Godwin <msg0028(a)uah.edu> Matt Godwin (UAH) reports on behalf of the Fermi Gamma-ray Burst Monitor Team: "The Fermi Gamma-ray Burst Monitor (GBM) trigger 753166198/241113201 at 04:49:53.31 UT on 13 November 2024, tentatively classified as a GRB, is in fact not due to a GRB. This trigger is likely due to Local Particles. View this GCN Circular online at https://gcn.nasa.gov/circulars/38203. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36179] GRB 241113B: Swift ToO observations
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38202 SUBJECT: GRB 241113B: Swift ToO observations DATE: 24/11/13 14:50:26 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a ToO observation of the SVOM/ECLAIRs GRB 241113B. Automated analysis of the XRT data will be presented online at https://www.swift.ac.uk/ToO_GRBs/00021731 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. These are not necessarily related to the SVOM/ECLAIRs event. Any X-ray source considered to be a probable afterglow candidate will be reported via a GCN Circular after manual consideration. Details of the XRT automated analysis methods are detailed in Evans et al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8). This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/38202. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36178] GRB 241113A: LCO optical observations
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38201 SUBJECT: GRB 241113A: LCO optical observations DATE: 24/11/13 14:49:32 GMT FROM: luca.izzo(a)inaf.it L. Izzo (INAF-OACn and DARK/NBI), A. Martin-Carrillo (UCD), and D. B. Malesani (DAWN/NBI and Radboud Univ.) report: We observed the field of GRB 241113A (Siegel et al., GCN #38194) with the Sinistro instrument mounted on the 1-m telescope of the LCO network, located at Siding Spring, Australia. Observations started on 2024 November 13 at 09:55 UT (2.17 hr after the GRB trigger). We obtained a series of 3x180 s images in the SDSS-r filter, and of 5x120 s in the PS1-z filter. Poor telescope tracking affects individual frames, significantly disrupting the point spread function (PSF) in the stacked images. Nevertheless, in the stacked z-band image, we detect a faint source consistent with the position of the optical source reported by Swift-UVOT (Siegel et al., GCN #38194) and by other optical facilities (Francile et al., GCN #38195, Huertas Ferrer et al., GCN #38197). We measure a preliminary magnitude of z = 19.9 +/- 0.3 mag (AB), calibrated against nearby stars from the Pan-STARRS catalog. We did not detect any source at the same position in the r-band stacked image, up to a limit of ~ 20.1 mag. This project has received funding from the European Union's Horizon 2020 research and innovation program under grant agreement No 101004719. View this GCN Circular online at https://gcn.nasa.gov/circulars/38201. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36177] IceCube-241113A - IceCube observation of a high-energy neutrino candidate track-like event
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38200 SUBJECT: IceCube-241113A - IceCube observation of a high-energy neutrino candidate track-like event DATE: 24/11/13 14:38:33 GMT FROM: A. Zegarelli at Ruhr University Bochum <azegarelli(a)icecube.wisc.edu> The IceCube Collaboration (http://icecube.wisc.edu/) reports: On 2024-11-13 00:22:20.68 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. The average astrophysical neutrino purity for Gold alerts is 30%. This alert has an estimated false alarm rate of 3.8708 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/140078_30891383.amon), more sophisticated reconstruction algorithms have been applied offline, with the direction refined to: Date: 2024-11-13 Time: 00:22:20.68 UT RA: 196.17 (+0.60, -0.60 deg 90% PSF containment) J2000 Dec: 8.57 (+0.77, -0.83 deg 90% PSF containment) J2000 We encourage follow-up by ground and space-based instruments to help identify a possible astrophysical source for the candidate neutrino. 4FGL J1301.6+0834 (4FGL catalog source) at RA = 195.41 deg and Dec = 8.57 deg is located within the 90% uncertainty region (0.49 deg away from the best-fit position). Additionally, inside the uncertainty region, there is the IceCube neutrino event IC110907A (gold alert, with a 51% probability of being astrophysical) from the IceCat catalog [R. Abbasi et al 2023 ApJS 269 25], located at RA = 196.08 deg, Dec = 9.40 deg (0.83 deg away from the best-fit position of IC241113A here announced, and 1.06 deg away from 4FGL J1301.6+0834). 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/38200. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36176] GRB 241112B: GMG Optical Upper Limit
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38199 SUBJECT: GRB 241112B: GMG Optical Upper Limit DATE: 24/11/13 14:02:50 GMT FROM: wangbaiting(a)ynao.ac.cn B.-T. Wang, R.-Z. Li, F.-F. Song, J. Mao, H.-C. Feng and J.-M. Bai (YNAO, CAS) report: We observed the field of GRB 241112B (SVOM/ECLAIRs team, GCN 38173; Evans, GCN 38174; Kumar et. al, GCN 38175; Du et. al, GCN 38176; SVOM/VT team, GCN 38179; SVOM/GRM team, GCN 38180; Turpin et. al, GCN 38181; Osborne et. al, GCN 38182; Du et. al, GCN 38183; Pankov et.al, GCN 38184) with the GMG-2.4m telescope at the Lijiang Observatory. The observation began at 2024-11-12T16:42:20, about 5.75 hours after the trigger. No new uncataloged optical counterpart was detected within the SVOM/VT error circle (GCN 38179). It should be noted that due to the proximity and brightness of the Moon on the observational night, the optical signal from the GRB 241112B may have been affectd by the moonlight. The preliminary photometry is as follows: ----------------------------------------------------------------------------- UT EXP(s) filter mag ----------------------------------------------------------------------------- 2024-11-12T16:42:20 600 sdss-r >21.4 ----------------------------------------------------------------------------- The magnitudes were calibrated using nearby stars of Pan-STARRS DR1 field and without corrections for Galactic extinction. We acknowledge the staff at the Lijiang Observatory for conducting the observation. View this GCN Circular online at https://gcn.nasa.gov/circulars/38199. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36175] GRB 241113A: Enhanced Swift-XRT position
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38198 SUBJECT: GRB 241113A: Enhanced Swift-XRT position DATE: 24/11/13 13:40:01 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team. Using 1534 s of XRT Photon Counting mode data and 3 UVOT images for GRB 241113A, we find an astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 16.56522, -22.67165 which is equivalent to: RA (J2000): 01h 06m 15.65s Dec (J2000): -22d 40' 17.9" with an uncertainty of 2.3 arcsec (radius, 90% confidence). This position may be improved as more data are received. The latest position can be viewed at http://www.swift.ac.uk/xrt_positions. Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular was automatically generated, and is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/38198. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36174] GRB241113A: LCOGT (40-cm) optical counterpart detection
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38197 SUBJECT: GRB241113A: LCOGT (40-cm) optical counterpart detection DATE: 24/11/13 12:46:49 GMT FROM: Ismael Perez-Fournon at Instituto de Astrofisica de Canarias <ipf(a)iac.es> A. Huertas Ferrer, B. Armas-Chinea, F. Dobrindt, P. Escudero-Coca, G. Fernández-Rodríguez, Á. García Lozano, C. Méndez-Lapido, I. Ortega-Casas, M. Torreiro Martínez, G. Villa (all ULL), S.R. Berlanas (IAC and ULL), and I. Pérez-Fournon (IAC and ULL) We report on optical follow-up observations of GRB 241113A detected by Swift BAT, XRT, and UVOT (Siegel et al.; GCN circular 38194). We observed the field of GRB 2411113A with one of the two Las Cumbres Observatory Global telescope network (LCOGT) Planewave Delta Rho 350 telescopes and QHY600 CMOS cameras located at the LCOGT node at Haleakala Observatory (Maui, Hawaii, USA) in the SDSS i' filter, in a single exposure of 600 sec. We detect a faint optical counterpart at a position consistent with the Swift UVOT detection (Siegel et al.; GCN circular 38194) with magnitude of i' = 19.48 +/- 0.35 starting at 2024-11-13 09:02:49 UT (about 1.24 hours after the Swift trigger) calibrated against the PanSTARRS DR2 catalog and without corrections for Galactic extinction. This optical counterpart has also been detected by MASTER (Francile et al.; GCN 38195). These results are based on observations made with the Las Cumbres Observatory’s education network telescopes that were upgraded through generous support from the Gordon and Betty Moore Foundation, as part of a course on Astrophysical Techniques of the Master in Astrophysics of the Universidad de La Laguna, Tenerife, Spain (LCOGT observing programme IAC2024B-010, ULL-ASTRO-MASTER). View this GCN Circular online at https://gcn.nasa.gov/circulars/38197. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36173] GRB 241113B : detection of a long GRB by SVOM/ECLAIRs
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38196 SUBJECT: GRB 241113B : detection of a long GRB by SVOM/ECLAIRs DATE: 24/11/13 11:49:49 GMT FROM: Stéphane Schanne at CEA Paris-Saclay/IRFU <s.schanne(a)cea.fr> SVOM/ECLAIRs Commissioning Team: Nicolas Dagoneau, Stéphane Schanne, Frédéric Chateau, Hervé Le Provost (CEA), Jean-Luc Atteia, Laurent Bouchet, Marius Brunet, Sebastien Guillot, Juliette Alaux, Hui Yang (IRAP), Wenjin Xie, Donghua Zhao (NAOC), Alexis Coleiro (APC), Tais Maiolino (LUPM), Karine Mercier, Marie-Claire Charmeau, Stefano Crepaldi (CNES) SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (IHEP), Stéphane Basa (LAM), Olivier Godet (IRAP), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Frédéric Daigne (IAP), Jin-Song Deng (NAOC), 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), Bing Zhang (UNLV) Report on behalf of the SVOM team: During the commissioning phase, the SVOM/ECLAIRs telescope triggered and located the long duration GRB 241113B (sb24111301) at 2024-11-13T11:23:05 UT (Tb) which was also detected by SVOM/GRM. The following trigger information was received on the ground with low-latency by the SVOM VHF Alert Network. The burst was detected by both the on-board Count-Rate Trigger (CRT) and Image Trigger (IMT) and 20 alerts were received. The best detection is obtained by CRT with a signal-to-noise ratio of 22.4 in the 8-50 keV energy band over a time window of 20.48 s starting at Tb. The light curve shows a single peak. The localization of the best Alert is RA, Dec = 110.230, 46.804 (J2000). The statistical uncertainty on this position is 3.8 arcminutes, to which we recommend adding 2 arcminutes of systematic uncertainty in quadrature. SVOM did not slew on this burst. The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA), French Space Agency (CNES), and the Chinese Academy of Sciences (CAS), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. ECLAIRs was developed jointly by APC, CEA, CNES, and IRAP. The SVOM point of contact for this burst is: stephane.schanne AT cea.fr View this GCN Circular online at https://gcn.nasa.gov/circulars/38196. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36171] GRB 241113A: MASTER010615.66-224018.2 optical counterpart detection
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38195 SUBJECT: GRB 241113A: MASTER010615.66-224018.2 optical counterpart detection DATE: 24/11/13 08:39:27 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> C.Francile, F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA), V.Lipunov, I.Panchenko, A.Kuznetsov, K.Zhirkov, E.Gorbovskoy, N.Tiurina, D.Vlasenko, A.Chasovnikov, V.Topolev, P.Balanutsa, G.Antipov, A.Sankovich,M.Gulyaev, Ya.Kechin, V.Senik (Lomonosov MSU), A.Sosnovskij (CrAO RAS), O.Gress, N.Budnev(ISU), D.Buckley (SAAO), R.Rebolo (The Instituto de Astrofisica de Canarias), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity) 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 Global robotic net (http://observ.pereplet.ru Lipunov et al.,2010,Advances in Astronomy,2010,30L) started observation of Swift GRB 241113A (GCN 28194) at MASTER-OAFA (Lipunov et al. GCN 38193, cover map https://master.sai.msu.ru/site/master2/observ.php?id=2668531 ) There is MASTER010615.66-224018.2 inside Swift error-box (GCN 38194) with mOT~18.2 at 2024-11-13 08:02:50 observation and reduction will be continued View this GCN Circular online at https://gcn.nasa.gov/circulars/38195. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36172] GRB 241113A: MASTER010615.66-224018.2 optical counterpart detection
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38195 SUBJECT: GRB 241113A: MASTER010615.66-224018.2 optical counterpart detection DATE: 24/11/13 08:39:27 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> C.Francile, F. Podesta, R.Podesta, E. Gonzalez (Observatorio Astronomico Felix Aguilar (OAFA), V.Lipunov, I.Panchenko, A.Kuznetsov, K.Zhirkov, E.Gorbovskoy, N.Tiurina, D.Vlasenko, A.Chasovnikov, V.Topolev, P.Balanutsa, G.Antipov, A.Sankovich,M.Gulyaev, Ya.Kechin, V.Senik (Lomonosov MSU), A.Sosnovskij (CrAO RAS), O.Gress, N.Budnev(ISU), D.Buckley (SAAO), R.Rebolo (The Instituto de Astrofisica de Canarias), A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory), A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity) 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 Global robotic net (http://observ.pereplet.ru Lipunov et al.,2010,Advances in Astronomy,2010,30L) started observation of Swift GRB 241113A (GCN 28194) at MASTER-OAFA (Lipunov et al. GCN 38193, cover map https://master.sai.msu.ru/site/master2/observ.php?id=2668531 ) There is MASTER010615.66-224018.2 inside Swift error-box (GCN 38194) with mOT~18.2 at 2024-11-13 08:02:50 observation and reduction will be continued View this GCN Circular online at https://gcn.nasa.gov/circulars/38195. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36170] GRB 241113A: Swift detection of a burst with an optical counterpart
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38194 SUBJECT: GRB 241113A: Swift detection of a burst with an optical counterpart DATE: 24/11/13 08:28:43 GMT FROM: K.L. Page at U Leicester <klp5(a)leicester.ac.uk> M. H. Siegel (PSU), J. J. DeLaunay (PSU), P. A. Evans (U Leicester), R. Gupta (NASA GSFC), K. L. Page (U Leicester) and T. Sakamoto (AGU) report on behalf of the Neil Gehrels Swift Observatory Team: At 07:48:13 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 241113A (trigger=1267501). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 16.576, -22.667 which is RA(J2000) = 01h 06m 18s Dec(J2000) = -22d 40' 00" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single-peaked structure with a duration of about 4 sec. The peak count rate was ~2000 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began observing the field at 07:49:31.0 UT, 77.2 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source located at RA, Dec 16.56509, -22.67118 which is equivalent to: RA(J2000) = 01h 06m 15.62s Dec(J2000) = -22d 40' 16.2" with an uncertainty of 4.6 arcseconds (radius, 90% containment). This location is 39 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received; the latest position is available at https://www.swift.ac.uk/sper. We cannot determine whether the source is fading at the present time. No spectrum from the promptly downlinked event data is yet available to determine the column density. UVOT took a finding chart exposure of 101 seconds with the White filter starting 81 seconds after the BAT trigger. An uncatalogued source is found inside the XRT error circle at RA, Dec = 16.56518, -22.67177 which is equivalent to: RA(J2000) = 01h 06m 15.64s Dec(J2000) = -22d 40' 18.4" with an estimated uncertainty of 0.7 arcseconds (radius, 90% containment). This source is 2.1" from the centre of the XRT error circle. The estimated magnitude of the source is 15.8. Burst Advocate for this burst is M. H. Siegel (siegel AT swift.psu.edu). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/) View this GCN Circular online at https://gcn.nasa.gov/circulars/38194. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36169] Swift GRB241113.33: Global MASTER-Net observations report
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38193 SUBJECT: Swift GRB241113.33: Global MASTER-Net observations report DATE: 24/11/13 08:10:43 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, 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. 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-OAFA robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Argentina (OAFA observatory of San Juan National University) was pointed to the Swift GRB241113.33 (trigger No 1267501,01h 06m 18.24s , -22d 40m 01.2s, R=0.05) errorbox 36 sec after notice time and 876 sec after trigger time at 2024-11-13 08:02:50 UT, with upper limit up to 19.1 mag. The observations began at zenith distance = 77 deg. The sun altitude is -17.2 deg. The galactic latitude b = -84 deg., longitude l = 164 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2668531 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 906 | MASTER-OAFA | C | 60 | 19.1 | 972 | MASTER-OAFA | C | 60 | 19.0 | 1038 | MASTER-OAFA | C | 60 | 18.9 | 1104 | MASTER-OAFA | C | 60 | 18.9 | 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/38193. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36167] SVOM/GRM detection of a short burst from SGR 1E1841-045
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38192 SUBJECT: SVOM/GRM detection of a short burst from SGR 1E1841-045 DATE: 24/11/13 07:53:50 GMT FROM: wenlongzhang2018(a)163.com SVOM/GRM team: Wen-Long Zhang, Wen-Jun Tan, 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, Chen-Wei Wang, 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, Chao Zheng (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, a short burst from SGR 1E 1841-045 was detected during the routine on-ground search of the SVOM/GRM data at 2024-11-09T21:25:04.200 UT (T0), which was also detected by INTEGRAL/IBAS (GCN #38148). The GRM light curve shows that this burst consists of a single pulse with a T90 ~ 0.1s. The position of SGR 1E1841-045 is located at about 109.3 degrees from the SVOM optical axis, and outside the ECLAIRs field of view. At the time of the event, ECLAIRs was not collecting data. 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 point of contact for this burst is: Wen-Long Zhang (IHEP)(zhangwl(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/38192. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36168] SVOM/GRM detection of a short burst from SGR 1E1841-045
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38192 SUBJECT: SVOM/GRM detection of a short burst from SGR 1E1841-045 DATE: 24/11/13 07:53:50 GMT FROM: wenlongzhang2018(a)163.com SVOM/GRM team: Wen-Long Zhang, Wen-Jun Tan, 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, Chen-Wei Wang, 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, Chao Zheng (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, a short burst from SGR 1E 1841-045 was detected during the routine on-ground search of the SVOM/GRM data at 2024-11-09T21:25:04.200 UT (T0), which was also detected by INTEGRAL/IBAS (GCN #38148). The GRM light curve shows that this burst consists of a single pulse with a T90 ~ 0.1s. The position of SGR 1E1841-045 is located at about 109.3 degrees from the SVOM optical axis, and outside the ECLAIRs field of view. At the time of the event, ECLAIRs was not collecting data. 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 point of contact for this burst is: Wen-Long Zhang (IHEP)(zhangwl(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/38192. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36166] Fermi trigger No 753166198: Global MASTER-Net observations report
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38191 SUBJECT: Fermi trigger No 753166198: Global MASTER-Net observations report DATE: 24/11/13 07:30:25 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, 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. 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-OAFA robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB241113.20 (trigger No 753166198,08h 40m 31.20s , -50d 26m 24.0s, R=1.03) errorbox 76 sec after notice time and 114 sec after trigger time at 2024-11-13 04:51:47 UT, with upper limit up to 19.4 mag. The observations began at zenith distance = 55 deg. The sun altitude is -40.4 deg. The galactic latitude b = -5 deg., longitude l = 269 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2668421 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 124 | 2024-11-13 04:51:47 | MASTER-OAFA | (08h 29m 12.42s , -50d 56m 16.3s) | C | 20 | 16.8 | 124 | 2024-11-13 04:51:47 | MASTER-OAFA | (08h 43m 25.45s , -50d 28m 44.2s) | C | 20 | 17.5 | 159 | 2024-11-13 04:52:27 | MASTER-OAFA | (08h 29m 12.45s , -50d 56m 14.0s) | C | 10 | 16.5 | 169 | 2024-11-13 04:52:27 | MASTER-OAFA | (08h 43m 25.42s , -50d 28m 42.5s) | C | 30 | 17.7 | 208 | 2024-11-13 04:53:11 | MASTER-OAFA | (08h 25m 56.98s , -50d 58m 56.9s) | C | 20 | 16.9 | 243 | 2024-11-13 04:53:11 | MASTER-OAFA | (08h 25m 56.97s , -50d 58m 57.1s) | C | 90 | 17.9 | Coadd 218 | 2024-11-13 04:53:11 | MASTER-OAFA | (08h 40m 10.90s , -50d 31m 26.5s) | C | 40 | 17.9 | 273 | 2024-11-13 04:53:11 | MASTER-OAFA | (08h 40m 10.90s , -50d 31m 26.5s) | C | 150 | 18.5 | Coadd 259 | 2024-11-13 04:53:57 | MASTER-OAFA | (08h 25m 56.91s , -50d 58m 54.2s) | C | 30 | 17.1 | 270 | 2024-11-13 04:53:58 | MASTER-OAFA | (08h 40m 10.84s , -50d 31m 24.7s) | C | 50 | 18.0 | 320 | 2024-11-13 04:54:53 | MASTER-OAFA | (08h 25m 56.84s , -50d 58m 51.0s) | C | 40 | 17.3 | 330 | 2024-11-13 04:54:53 | MASTER-OAFA | (08h 40m 10.81s , -50d 31m 22.4s) | C | 60 | 18.0 | 391 | 2024-11-13 04:55:59 | MASTER-OAFA | (08h 25m 56.71s , -50d 58m 47.7s) | C | 50 | 17.4 | 471 | 2024-11-13 04:55:59 | MASTER-OAFA | (08h 25m 56.72s , -50d 58m 47.8s) | C | 210 | 18.3 | Coadd 402 | 2024-11-13 04:55:59 | MASTER-OAFA | (08h 40m 10.70s , -50d 31m 20.0s) | C | 70 | 18.1 | 502 | 2024-11-13 04:55:59 | MASTER-OAFA | (08h 40m 10.70s , -50d 31m 20.1s) | C | 270 | 18.6 | Coadd 478 | 2024-11-13 04:57:15 | MASTER-OAFA | (08h 25m 56.56s , -50d 58m 44.1s) | C | 70 | 17.6 | 488 | 2024-11-13 04:57:16 | MASTER-OAFA | (08h 40m 10.60s , -50d 31m 17.2s) | C | 90 | 18.1 | 584 | 2024-11-13 04:58:52 | MASTER-OAFA | (08h 25m 56.37s , -50d 58m 39.9s) | C | 90 | 17.7 | 594 | 2024-11-13 04:58:52 | MASTER-OAFA | (08h 40m 10.46s , -50d 31m 13.6s) | C | 110 | 18.2 | 709 | 2024-11-13 05:00:48 | MASTER-OAFA | (08h 25m 56.14s , -50d 58m 35.2s) | C | 105 | 17.7 | 814 | 2024-11-13 05:00:48 | MASTER-OAFA | (08h 25m 56.14s , -50d 58m 35.2s) | C | 315 | 18.4 | Coadd 719 | 2024-11-13 05:00:49 | MASTER-OAFA | (08h 40m 10.30s , -50d 31m 09.6s) | C | 125 | 18.2 | 844 | 2024-11-13 05:00:49 | MASTER-OAFA | (08h 40m 10.30s , -50d 31m 09.5s) | C | 375 | 18.5 | Coadd 840 | 2024-11-13 05:02:59 | MASTER-OAFA | (08h 25m 55.90s , -50d 58m 30.6s) | C | 105 | 17.7 | 850 | 2024-11-13 05:03:00 | MASTER-OAFA | (08h 40m 10.13s , -50d 31m 05.3s) | C | 125 | 18.2 | 971 | 2024-11-13 05:05:10 | MASTER-OAFA | (08h 25m 55.65s , -50d 58m 26.0s) | C | 105 | 17.7 | 981 | 2024-11-13 05:05:11 | MASTER-OAFA | (08h 40m 09.94s , -50d 31m 01.1s) | C | 125 | 18.2 | 1104 | 2024-11-13 05:07:22 | MASTER-OAFA | (08h 25m 55.40s , -50d 58m 21.2s) | C | 110 | 17.8 | 1214 | 2024-11-13 05:07:22 | MASTER-OAFA | (08h 25m 55.40s , -50d 58m 21.2s) | C | 330 | 18.5 | Coadd 1114 | 2024-11-13 05:07:22 | MASTER-OAFA | (08h 40m 09.76s , -50d 30m 56.7s) | C | 130 | 18.2 | 1244 | 2024-11-13 05:07:22 | MASTER-OAFA | (08h 40m 09.76s , -50d 30m 56.7s) | C | 390 | 18.5 | Coadd 1240 | 2024-11-13 05:09:38 | MASTER-OAFA | (08h 25m 55.15s , -50d 58m 16.6s) | C | 110 | 17.8 | 1250 | 2024-11-13 05:09:38 | MASTER-OAFA | (08h 40m 09.58s , -50d 30m 52.4s) | C | 130 | 18.2 | 1376 | 2024-11-13 05:11:54 | MASTER-OAFA | (08h 25m 54.90s , -50d 58m 12.0s) | C | 110 | 17.8 | 1386 | 2024-11-13 05:11:54 | MASTER-OAFA | (08h 40m 09.42s , -50d 30m 47.8s) | C | 130 | 18.2 | 1512 | 2024-11-13 05:14:10 | MASTER-OAFA | (08h 25m 54.65s , -50d 58m 07.3s) | C | 110 | 17.9 | 1522 | 2024-11-13 05:14:10 | MASTER-OAFA | (08h 40m 09.22s , -50d 30m 43.5s) | C | 130 | 18.2 | 1648 | 2024-11-13 05:16:26 | MASTER-OAFA | (08h 25m 54.42s , -50d 58m 02.8s) | C | 110 | 17.8 | 1659 | 2024-11-13 05:16:27 | MASTER-OAFA | (08h 40m 09.07s , -50d 30m 39.1s) | C | 130 | 18.2 | 7911 | 2024-11-13 07:00:14 | MASTER-OAFA | (08h 38m 03.68s , -52d 01m 34.8s) | C | 180 | 19.1 | 8091 | 2024-11-13 07:00:14 | MASTER-OAFA | (08h 38m 03.68s , -52d 01m 34.8s) | C | 540 | 19.4 | Coadd 8112 | 2024-11-13 07:03:35 | MASTER-OAFA | (08h 38m 09.59s , -52d 01m 07.4s) | C | 180 | 19.1 | 8309 | 2024-11-13 07:06:51 | MASTER-OAFA | (08h 38m 06.18s , -51d 59m 31.4s) | C | 180 | 19.1 | 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/38191. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36165] LIGO/Virgo/KAGRA S241111bn: Updated Sky localization
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38190 SUBJECT: LIGO/Virgo/KAGRA S241111bn: Updated Sky localization DATE: 24/11/13 06:21:59 GMT FROM: jgolomb(a)caltech.edu The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We have conducted further analysis of the LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) data around the time of the compact binary merger (CBC) candidate S241111bn (GCN Circular 38166). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.offline0.multiorder.fits,0, distributed via GCN Notice, is available for retrieval from the GraceDB event page: https://gracedb.ligo.org/superevents/S241111bn For the Bilby.offline0.multiorder.fits,0 sky map, the 90% credible region is 424 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1393 +/- 412 Mpc (a posteriori mean +/- standard deviation). For further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/. [1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. PRD 108, 123040 (2023) doi:10.1103/PhysRevD.108.123040 View this GCN Circular online at https://gcn.nasa.gov/circulars/38190. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36164] GRB 241105A: ATCA Radio Upper Limits
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38189 SUBJECT: GRB 241105A: ATCA Radio Upper Limits DATE: 24/11/13 05:19:36 GMT FROM: Gemma Anderson at Curtin U <gemma.anderson(a)curtin.edu.au> G. E. Anderson (Curtin), S. Belkin (Monash), J. K. Leung (UofT/HUJI), A. J. van der Horst (GWU), L. Rhodes (TSI/McGill), A. Gulati (USyd), S. Chastain (UNM), B. Gompertz (Birmingham) on behalf of the ATCA PanRadio GRB collaboration We observed the likely short GRB 241105A (Fermi GBM Collaboration, GCN 38085) with the Australia Telescope Compact Array (ATCA) 4.8 days post-burst on 2024-11-10 (08:30-13:30 UT). No radio source was detected at the location of the optical counterpart (Julakanti et al. GCN 38088, Izzo et al., GCN 38097; SVOM/VT team, GCN 38099; Hu et al., GCN 38106; Siegel et al., GCN 38110; Dichiara et al., GCN 38111; Rastinejad et al., GCN 38113; Tsalapatas et al., GCN 38119) at 5.5 and 9 GHz, with 3-sigma upper limits of 54 and 39 microJy/beam, respectively. We thank the CSIRO Space and Astronomy staff for supporting these observations. We acknowledge the Gomeroi people as the traditional owners of the Observatory site. The Australia Telescope Compact Array is part of the Australia Telescope National Facility (https://ror.org/05qajvd42) which is funded by the Australian Government for operation as a National Facility managed by CSIRO. View this GCN Circular online at https://gcn.nasa.gov/circulars/38189. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36163] GRB 241112B: AbAO optical upper limit
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38188 SUBJECT: GRB 241112B: AbAO optical upper limit DATE: 24/11/13 03:21:14 GMT FROM: Alexei Pozanenko at IKI, Moscow <grb.alex(a)gmail.com> N. Pankov (HSE, IKI), A. Pozanenko (IKI), R. Ya. Inasaridze (AbAO) report on behalf of IKI-GRB-FuN: We observed the field of GRB 241112B (SVOM/ECLAIRs Commissioning Team & SVOM JSWG, GCN 38173; Evans, GCN 38174; Kumar et. al, GCN 38175; Du et. al, GCN 38176; SVOM/VT commissioning team & SVOM JSWG, GCN 38179; SVOM/GRM team & SVOM JSWG, GCN 38180; Turpin et. al, GCN 38181) with 70-cm AS-32 telescope of Abastumani observatory (AbAO). The observations began on 2024-11-12 at 15:03:45 UT. In total, the series of 101x60 s frames was taken in the R-filter using CCD-photometer FLI PL4240. We do not detect the optical afterglow (SVOM/VT commissioning team & SVOM JSWG, GCN 38179; Turpin et. al, GCN 38181). The preliminary photometry is as follows: Date UTstart Exptime t-T0 Filter OT Err UL (s) (mid, days) (3sigma) 2024-11-12 15:03:45 98*60 0.205139 R n/d n/d 19.6 The magnitudes were calibrated using nearby stars of USNO-B1.0 (R2 magnitudes). RA Dec R2 01:56:20.7 +09:09:01.4 14.86 01:56:40.2 +09:10:09.0 15.24 View this GCN Circular online at https://gcn.nasa.gov/circulars/38188. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36162] GRB 241107A: GROWTH-India telescope optical upper limit
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38187 SUBJECT: GRB 241107A: GROWTH-India telescope optical upper limit DATE: 24/11/13 02:31:29 GMT FROM: Varun Bhalerao at IIT Bombay <varunb(a)iitb.ac.in> T. Mohan, G. Waratkar, A.P. Saikia, V. Swain, R. Kumar, 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 the GRB 241107A (SVOM/GRM team, GCN 38125, Rodi et al., GCN 38164, IPN GCN 38165) with the 0.7m GROWTH-India Telescope (GIT). Once arcminute positions became available (Mereghetti et al., GCN 38172 and DeLaunay et al., GCN 38177), we started observations at 2024-11-12 20:10:35 UT, about 4.8 days after the trigger. We obtained multiple images of 360s each in r' and i' filters. We did not detect any new source in our stacked image around the coordinates given by INTEGRAL IBIS or Swift BAT. Below is the upper limit in the stacked images: --------------------------------------------------------------------------------- | MJD (mid) | Filter | Exposure (s) | Limiting Magnitude (AB) | | ----------- | ------ | ------------ | ----------------------- | | 60626.85364 | r' | 6x360 | 20.8 | | 60626.87984 | i' | 6x360 | 20.6 | --------------------------------------------------------------------------------- The magnitude is calibrated against PanSTARRS DR1 (Chambers et al., 2016) and not corrected for Galactic extinction. 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/38187. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36161] IceCube Alert 241113.02: Global MASTER-Net observations report
by GCN Circulars 13 Nov '24

13 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38186 SUBJECT: IceCube Alert 241113.02: Global MASTER-Net observations report DATE: 24/11/13 00:39:22 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, 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. 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) was pointed to the IceCube Alert 241113.02 (trigger No 30891383,13h 04m 46.32s , +08d 29m 27.6s, R=0.53) errorbox 477 sec after notice time and 554 sec after trigger time at 2024-11-13 00:31:35 UT, with upper limit up to 16.0 mag. The observations began at zenith distance = 86 deg. The sun altitude is -38.1 deg. The galactic latitude b = 71 deg., longitude l = 315 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2668204 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 609 | 2024-11-13 00:31:35 | MASTER-Kislovodsk | (13h 02m 49.00s , +08d 34m 58.8s) | P- | 110 | 16.0 | The observation and reduction will continue. The message may be cited. View this GCN Circular online at https://gcn.nasa.gov/circulars/38186. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36160] Fermi GRB 241112A: Global MASTER-Net observations report
by GCN Circulars 12 Nov '24

12 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38185 SUBJECT: Fermi GRB 241112A: Global MASTER-Net observations report DATE: 24/11/12 23:45:22 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru> V.Lipunov, E.Gorbovskoy, N.Tiurina, P.Balanutsa, , D.Vlasenko, I.Panchenko, A.Kuznetsov, G.Antipov, A.Sankovich, A.Sosnovskij, Yu.Tselik, M.Gulyaev, 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. 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-OAFA robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Argentina (OAFA observatory of San Juan National University) started inspect of the Fermi GRB 241112A ( Fermi GBM team, GCN 38170) errorbox 24193 sec after notice time and 24227 sec after trigger time at 2024-11-12 08:33:26 UT, with upper limit up to 15.4 mag. Observations started at twilight. The observations began at zenith distance = 35 deg. The sun altitude is -11.8 deg. MASTER-SAAO robotic telescope located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 241112A errorbox 76564 sec after notice time and 76598 sec after trigger time at 2024-11-12 23:06:17 UT, with upper limit up to 18.1 mag. The observations began at zenith distance = 79 deg. The sun altitude is -39.0 deg. The galactic latitude b = 44 deg., longitude l = 245 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2666595 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 24317 | 2024-11-12 08:33:26 | MASTER-OAFA | (09h 35m 01.12s , -12d 02m 29.4s) | C | 180 | 15.4 | 76628 | 2024-11-12 23:06:17 | MASTER-SAAO | (09h 35m 42.48s , -11d 59m 33.3s) | C | 60 | 17.7 | 77437 | 2024-11-12 23:19:46 | MASTER-SAAO | (09h 35m 39.66s , -11d 59m 47.3s) | C | 60 | 17.9 | 78242 | 2024-11-12 23:33:11 | MASTER-SAAO | (09h 35m 36.25s , -11d 58m 53.8s) | C | 60 | 18.1 | 78480 | 2024-11-12 23:37:09 | MASTER-SAAO | (09h 43m 03.10s , -11d 59m 31.4s) | C | 60 | 18.0 | 78559 | 2024-11-12 23:38:28 | MASTER-SAAO | (09h 51m 11.62s , -11d 58m 00.7s) | C | 60 | 17.8 | 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/38185. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36159] Fermi-GBM Sub-Threshold Detection of GRB 241112B
by GCN Circulars 12 Nov '24

12 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38184 SUBJECT: Fermi-GBM Sub-Threshold Detection of GRB 241112B DATE: 24/11/12 22:00:20 GMT FROM: Oliver J Roberts at USRA/NASA <oliver.roberts(a)nasa.gov> O.J. Roberts (USRA/NASA-MSFC) and E. Burns (LSU) reports on behalf of the Fermi-GBM Team: SVOM detected GRB 241112B on 2024-11-12 at 10:57:21 UTC (i.e., Schanne et al., GCN #38173). There was no Fermi-GBM onboard trigger around this event time. An automated, blind search for gamma-ray bursts below the onboard triggering threshold in Fermi-GBM identified no candidates. The GBM Targeted Search [1], the most sensitive, coherent search for GRB-like signals, identified an unambiguous transient starting around the SVOM trigger time most significantly on the 16.384 s timescale, with a LogLR = 21.10. The Fermi-MET of the start time of this transient is 753101846.0 s. Using the standard search protocol, the Targeted Search localization was found to be RA=25.7 deg., Dec.= 32.8 deg., and an error of 31 deg. (90 % confidence level, includes the systematic error), at a SNR of 7.4. Additionally, the GBM Targeted Search event was found with the highest significance using a "normal" spectrum (Band function with Epeak = 230 keV, alpha = -1.0, beta = -2.3) for a GRB. The Targeted Search data release product for this event can be found here: https://zenodo.org/uploads/https://zenodo.org/records/14110881 [1] Goldstein et al. 2019 arXiv:1903.12597 View this GCN Circular online at https://gcn.nasa.gov/circulars/38184. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36158] GRB 241112B: Optical afterglow detection confirmation in revisiting the Mephisto data
by GCN Circulars 12 Nov '24

12 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38183 SUBJECT: GRB 241112B: Optical afterglow detection confirmation in revisiting the Mephisto data DATE: 24/11/12 20:22:30 GMT FROM: Brajesh Kumar at SWIFAR, YNU <brajesh(a)ynu.edu.cn> Guowang Du (SWIFAR, YNU), Weikang Lin (SWIFAR, YNU), Brajesh Kumar (SWIFAR, YNU), Yaosong Yu (SWIFAR, YNU), Yehao Cheng (SWIFAR, YNU), Xinlei Chen (SWIFAR, YNU), Yu Pan (SWIFAR, YNU), Xingzhu Zou (SWIFAR, YNU), Jinghua Zhang (SWIFAR, YNU), Yuanpei Yang (SWIFAR, YNU), Yuan Fang (SWIFAR, YNU), Xuhui Han (NAOC), Pinpin Zhang (NAOC), Liping Xin (NAOC), Chao Wu (NAOC), Xiangkun Liu (SWIFAR, YNU), Xiaowei Liu (SWIFAR, YNU) report on behalf of the Mephisto Team: The 1.6m Multi-channel Photometric Survey Telescope (Mephisto) of Yunnan University located at Lijiang Observatory was triggered to observe GRB 241112B (sb24111201) detected by SVOM/ECLAIRs and SVOM/GRM (Yang et al., GCN 38173; Liu et al., GCN 38180). The observations were started at 11:46:00 (UT) on 2024-11-12 (~0.8 hr after SVOM trigger) and multiple images were obtained in uvgriz bands (as mentioned in Du et al., GCN 38176). Based on the precise localization of the optical afterglow counterpart of GRB 241112B provided by SVOM/VT (Qiu et al., GCN 38179) and other facilities (Turpin et al., GCN 38181; Osborne et al., GCN 38182), we revisited the Mephisto data and identified the optical counterpart at this reported location. Initially, we missed this source while manually searching within the SVOM/ECLAIRs localization region due to its proximity to a faint, extended source in the DESI DR10 image and the lack of template subtraction, which led to confusion in identifying new transient sources. Preliminary photometry of the optical afterglow of GRB 241112B (without template subtraction) in the griz bands and 3-sigma upper limits in the u and v bands are as follows: Obs-start time band Exp(s) Mag (AB) 2024/11/12 11:46:00 i 50*1 18.71 +/- 0.10 2024/11/12 11:46:00 g 50*1 19.49+/- 0.31 2024/11/12 11:56:31 r 79*1 19.36 +/- 0.25 2024/11/12 11:56:31 z 79*1 18.90+/- 0.26 2024/11/12 11:46:00 u 180*3 >21.21 2024/11/12 11:56:31 v 180*3 >21.50 -------------------------------------------------------------------------- Mephisto (Multi-channel Photometric Survey Telescope) is a 1.6m wide-field multi-channel telescope, the first of its type in the world, capable of imaging the same field of view in three optical bands simultaneously. It provides real-time, high-quality colors of stellar objects. The on-site telescope assemblage and commissioning were carried out in September 2022. The first light in all three channels was achieved on 2023 December 21. -------------------------------------------------------------------------- View this GCN Circular online at https://gcn.nasa.gov/circulars/38183. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36157] GRB 241112B: Swift-XRT afterglow detection
by GCN Circulars 12 Nov '24

12 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38182 SUBJECT: GRB 241112B: Swift-XRT afterglow detection DATE: 24/11/12 19:15:04 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore (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) and P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the SVOM/ECLAIRs-detected burst GRB 241112B, collecting 2.5 ks of Photon Counting (PC) mode data between T0+11.0 ks and T0+17.6 ks. Two uncatalogued X-ray sources are detected consistent with being within 414 arcsec of the SVOM/ECLAIRs position, of which one ("Source 1") is above the LSXPS 3-sigma upper limit at this position, and is therefore likely the GRB afterglow. The position of this source is RA, Dec=29.0386, +9.1080 which is equivalent to: RA (J2000): 01:56:9.26 Dec(J2000): +09:06:29.0 with an uncertainty of 4.1 arcsec (radius, 90% confidence). This position is 2.5 arcmin from the SVOM/ECLAIRs position. The source has a mean count rate of 2.1e-02 ct/sec; we cannot determine at the present time whether it is fading. A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.9 (+0.9, -0.5). The best-fitting absorption column is 9 (+30, -3) x 10^20 cm^-2, consistent with the Galactic value of 5.6 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 3.6 x 10^-11 (4.3 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 9 (+30, -3) x 10^20 cm^-2 Galactic foreground: 5.6 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 1.9 (+0.9, -0.5) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00021730. The results of the full analysis of the XRT observations are available at https://www.swift.ac.uk/ToO_GRBs/00021730. This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/38182. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36156] GRB 241112B: LCO optical detection of the SVOM/VT candidate
by GCN Circulars 12 Nov '24

12 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38181 SUBJECT: GRB 241112B: LCO optical detection of the SVOM/VT candidate DATE: 24/11/12 18:18:50 GMT FROM: Damien Turpin at CEA-Saclay <dturpin-astro(a)hotmail.com> D. Turpin (CEA/Irfu), A. Saccardi (CEA/Irfu, GEPI/Obs. de Paris), J. T. Palmerio (CEA/Irfu, GEPI/Obs. de Paris), S. Vergani (GEPI/Obs. de Paris), S. Basa (OSU Pytheas, LAM), E. LeFloc'h (CEA Paris-Saclay, DAp/AIM) on behalf of a larger collaboration. We observed the field of GRB 241112B, detected by SVOM/ECLAIRs (Yang et al., GCN 38173) with the LCO 0.4m telescope at the Haleakala Observatory and the 1m telescope equipped with the Sinistro instrument at Siding Spring Observatory. Our observation started at 2024-11-12T11:41:20.771 (T - TGRB ~ 44min) with a series of 5x120s (sdssr, 0.4m), 4x180s (sdssi, 0.4m) and 5x120s (sdssr, 1.0m) exposures. At the position of the optical afterglow candidate reported by SVOM/VT (Qiu et al., GCN 38179), we detect a faint optical source at the detection limit of our single exposure frames which does not appear in the USNOB1.0 and SDSS DR12 catalogs. Note that the faint red extended source present in the Legacy Survey DR10 catalog, mentioned by Qiu et al., GCN 38179, is about 3 arcsecond away from the position of the optical counterpart. From our first exposure, we derive the following magnitude r = 19.0 +/- 0.3 (AB) at T-TGRB = 45 min (mid time). This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 101004719 View this GCN Circular online at https://gcn.nasa.gov/circulars/38181. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36155] GRB 241112B: SVOM/GRM observation
by GCN Circulars 12 Nov '24

12 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38180 SUBJECT: GRB 241112B: SVOM/GRM observation DATE: 24/11/12 17:16:45 GMT FROM: zhengchao_astro(a)foxmail.com SVOM/GRM team: Jia-Cong Liu, 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, Yue Wang, 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, Jin-Peng Zhang, Chao Zheng (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, the SVOM/GRM detected GRB 241112B at 2024-11-12T10:57:21 UT (T0), which was also observed by SVOM/ECLAIRs (Yang et al, GCN 38173). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of one pulse, with a T90 of 7.0 +1.6/-0.8 s (15-550 keV). This pulse is followed by a much weaker and softer (<25 keV) pulse that is consistent with the ECLAIRs observation. This burst is located at about 22.3 degrees from the SVOM optical axis. The GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb241112B.png 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 point of contact for this burst is: Jia-Cong Liu (IHEP)(liujiacong(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/38180. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36154] GRB 241112B: SVOM/GRM observation
by GCN Circulars 12 Nov '24

12 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38180 SUBJECT: GRB 241112B: SVOM/GRM observation DATE: 24/11/12 17:16:45 GMT FROM: zhengchao_astro(a)foxmail.com SVOM/GRM team: Jia-Cong Liu, 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, Yue Wang, 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, Jin-Peng Zhang, Chao Zheng (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, the SVOM/GRM detected GRB 241112B at 2024-11-12T10:57:21 UT (T0), which was also observed by SVOM/ECLAIRs (Yang et al, GCN 38173). With the event-by-event data downloaded through the X-band ground station, the GRM light curve shows that this burst consists of one pulse, with a T90 of 7.0 +1.6/-0.8 s (15-550 keV). This pulse is followed by a much weaker and softer (<25 keV) pulse that is consistent with the ECLAIRs observation. This burst is located at about 22.3 degrees from the SVOM optical axis. The GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb241112B.png 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 point of contact for this burst is: Jia-Cong Liu (IHEP)(liujiacong(a)ihep.ac.cn) View this GCN Circular online at https://gcn.nasa.gov/circulars/38180. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36153] GRB 241112B: SVOM/VT afterglow detection
by GCN Circulars 12 Nov '24

12 Nov '24

TITLE: GCN CIRCULAR NUMBER: 38179 SUBJECT: GRB 241112B: SVOM/VT afterglow detection DATE: 24/11/12 16:52:30 GMT FROM: Liping Xin at NAOC, SVOM <xlp(a)nao.cas.cn> SVOM/VT commissioning team: Y. L. Qiu, H. L. Li, L. P. Xin, C. Wu, X. H. Han, J. Wang, W. J. Xie, H. B. Cai, Y. Xu, Y. J. Xiao, P. P. Zhang, J. S. Deng, L. Lan, X. M. Lu, R. S. Zhang, (NAOC), J. Zhang, L. J. Dan, G. Y. Zou, C. J. Wang, Y. F. Du, C. Huang (XIOPM), H. Zhou (PMO), C. W. Wang(IHEP), W. J. Tan(IHEP), R. C. Chen(NJU). 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: The GRB 241112B (Yang et al., GCN 38173) was observed by on-board VT after the automatic slew of the platform. The VT conducted observations in VT_B (400nm-650nm) and VT_R (650nm-1000nm) channel simultaneously. An uncatalogued source was detected in data processing results on-board in VT_B and VT_R band images within the errorbox of Eclairs (Yang et al., GCN 38173), and further confirmed with the data downlinked via X band. The source is located near a faint extended source in DESI Dr10 catalog, and its brightness was fading for 3.5 magnitudes in VT_B images in the initial 5.5 hours. The magnitude was VT_B=18.24 mag and VT_R=17.70 mag in AB magnitude at 2024-11-12T11:04:59 UT, about 7.6 min after the burst. The coordinates are R.A.= 01:56:09.270, DEC. = 09:06:27.91, Error = 0.1 arcseconds, J2000. We proposed that this source is the optical counterpart 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. 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/38179. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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