GRB241104A

This page lists all entries on GRB241104A in GRBweb

Summary Fermi GBM IPN GCN 38075 GCN 38076 GCN 38078 GCN 38081 GCN 38082 GCN 38083 GCN 38086 GCN 38089 GCN 38090 GCN 38093 GCN 38094 GCN 38096 GCN 38129

Summary table
Variable Value Source
GRB_name_Fermi GRB241104771
T0 18:30:11.905 UTC Fermi_GBM
ra 32.5500° IPN
decl 31.5500° IPN
pos_error 4.33e-02° IPN
T90 10.496 s Fermi_GBM
T90_error 0.724 s Fermi_GBM
T90_start 18:30:11.905 UTC Fermi_GBM
fluence 3.61e-06 erg/cm² Fermi_GBM
fluence_error 2.68e-08 erg/cm² Fermi_GBM
T100 10.496 s
GBM_located False
mjd 60618.770971122685 Fermi_GBM
Fermi GBM table
GRB_name_Fermi GRB241104771
trigger_name bn241104771
ra 32.5742°
decl 31.5550°
pos_error 3.27e+00°
datum 2024-11-04
t_trigger 18:30:15.425 UTC
T90 10.496 s
T90_error 0.724 s
T90_start 18:30:11.905 UTC
fluence 3.61e-06 erg/cm²
fluence_error 2.68e-08 erg/cm²
flux_1024 6.95e+00 erg/cm²/s
flux_1024_error 2.54e-01 erg/cm²/s
flux_1024_time 2.56e+00 erg/cm²/s
flux_64 9.57e+00 erg/cm²/s
flux_64_error 1.10e+00 erg/cm²/s
IPN table
GRB_name GRB241104A
ra 32.5500°
decl 31.5500°
pos_error 4.33e-02°
GCN 38075 table
GRB_name GRB241104A
GCN_number 38075
Detection_method Fermi GBM final loc
t_trigger 18:30:15 UTC
ra 32.4000°
decl 31.8000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38075 SUBJECT: GRB 241104A: Fermi GBM Final Real-time Localization DATE: 24/11/04 18:40:50 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 18:30:15 UT on 4 Nov 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241104A (trigger 752437820.424838 / 241104771). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 32.4, Dec = 31.8 (J2000 degrees, equivalent to J2000 02h 09m, 31d 48'), with a statistical uncertainty of 2.8 degrees. The angle from the Fermi LAT boresight is 62.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241104771/quicklook/glg_skymap_all_bn241104771.png The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241104771/quicklook/glg_healpix_all_bn241104771.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241104771/quicklook/glg_lc_medres34_bn241104771.gif
GCN 38076 table
GRB_name GRB241104A
GCN_number 38076
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38076 SUBJECT: Fermi GRB 241104A: Global MASTER-Net observations report DATE: 24/11/04 19:30:37 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs 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 241104A ( Fermi GBM team, GCN 38075) errorbox 35 sec after notice time and 57 sec after trigger time at 2024-11-04 18:31:12 UT, with upper limit up to 20.1 mag. The observations began at zenith distance = 34 deg. The sun altitude is -49.2 deg. The galactic latitude b = -28 deg., longitude l = 142 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2659245 We obtain a following upper limits. Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment _________|_____________________|_____________________|____________________________________|_____|_______|_______|________ 62 | 2024-11-04 18:31:12 | MASTER-Tunka | (02h 03m 04.48s , +29d 10m 35.6s) | C | 10 | 17.8 | 77 | 2024-11-04 18:31:12 | MASTER-Tunka | (02h 03m 04.48s , +29d 10m 35.6s) | C | 40 | 18.8 | Coadd 75 | 2024-11-04 18:31:25 | MASTER-Tunka | (02h 03m 04.48s , +29d 10m 35.8s) | C | 10 | 17.9 | 94 | 2024-11-04 18:31:39 | MASTER-Tunka | (02h 03m 04.47s , +29d 10m 35.9s) | C | 20 | 18.5 | 117 | 2024-11-04 18:32:02 | MASTER-Tunka | (02h 03m 04.45s , +29d 10m 36.7s) | C | 20 | 18.5 | 153 | 2024-11-04 18:32:33 | MASTER-Tunka | (02h 03m 36.52s , +31d 21m 04.2s) | C | 30 | 18.7 | 188 | 2024-11-04 18:32:33 | MASTER-Tunka | (02h 03m 36.52s , +31d 21m 04.2s) | C | 100 | 19.7 | Coadd 187 | 2024-11-04 18:33:07 | MASTER-Tunka | (02h 03m 36.49s , +31d 21m 05.1s) | C | 30 | 18.8 | 225 | 2024-11-04 18:33:40 | MASTER-Tunka | (02h 03m 36.47s , +31d 21m 06.0s) | C | 40 | 18.8 | 274 | 2024-11-04 18:34:23 | MASTER-Tunka | (02h 03m 36.41s , +31d 21m 07.0s) | C | 50 | 19.1 | 332 | 2024-11-04 18:35:17 | MASTER-Tunka | (02h 03m 36.35s , +31d 21m 08.4s) | C | 60 | 19.2 | 644 | 2024-11-04 18:39:59 | MASTER-Tunka | (02h 09m 20.45s , +31d 47m 01.4s) | C | 120 | 19.4 | 799 | 2024-11-04 18:39:59 | MASTER-Tunka | (02h 09m 20.45s , +31d 47m 01.4s) | C | 430 | 20.1 | Coadd 777 | 2024-11-04 18:42:02 | MASTER-Tunka | (02h 09m 20.33s , +31d 47m 04.1s) | C | 140 | 19.5 | 935 | 2024-11-04 18:44:25 | MASTER-Tunka | (02h 09m 20.15s , +31d 47m 07.5s) | C | 170 | 19.4 | 1114 | 2024-11-04 18:47:19 | MASTER-Tunka | (02h 09m 19.95s , +31d 47m 11.2s) | C | 180 | 19.4 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 38078 table
GRB_name GRB241104A
GCN_number 38078
Detection_method Fermi GBM Other
ra 32.5520°
decl 31.5540°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38078 SUBJECT: GRB 241104A : Detection and localization by SVOM/ECLAIRs DATE: 24/11/05 09:21:16 GMT FROM: Stéphane Schanne at CEA Paris-Saclay/IRFU SVOM/ECLAIRs Commissioning Team: Stéphane Schanne, Nicolas Dagoneau, Hervé Le Provost, Frédéric Chateau (CEA), Jean-Luc Atteia, Laurent Bouchet, Sebastien Guillot, Juliette Alaux, Hui Yang (IRAP), Tais Maiolino (LUPM), Wenjin Xie, Donghua Zhao (NAOC), Alexis Coleiro (APC), 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 detected and localized the bright long duration GRB 241104A at 2024-11-04T18:30:15 UTC (Tb), previously detected by Fermi (Fermi GBM team, GCN circular 38075), and by SVOM/GRM (SVOM reference: sb24110402). The onboard trigger was not in operations, the following information was obtained by reprocessing the data on ground in the flight trigger algorithms. The burst was detected by the Count-Rate Trigger (CRT) and Image Trigger (IMT) which produced 21 Alert messages. The best Alert was obtained by CRT in the 8-120 keV energy band with a signal-to-noise ratio of 55.5 in a time window of 10.24 s starting at Tb. The event location is RA, Dec = 32.552, 31.554 (J2000). The statistical uncertainty on this position is 1.6 arcminutes to which we recommend adding 2 arcminutes of systematic uncertainty in quadrature. SVOM did not slew to the burst since automated slewing was not enabled. 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: s.schanne AT cea.fr.
GCN 38081 table
GRB_name GRB241104A
GCN_number 38081
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38081 SUBJECT: EP241104a: EP detection of GRB 241104A X-ray emission DATE: 24/11/05 13:00:44 GMT FROM: EP Team at NAOC/CAS H. Zhou (PMO, CAS), R.-Z. Li (YNAO, CAS), Q. C. Liu (TSU), H. Q. Cheng, Z. X. Ling (NAO,CAS) report on behalf of the Einstein Probe team: We report on the detection of an X-ray transient, designated EP241104a, by the Wide-field X-ray Telescope (WXT) on board the Einstein Probe (EP) mission. The WXT position of EP241104a is R.A.= 32.574 deg, DEC = 31.555 deg (J2000) with an uncertainty of 2.7 arcmin (radius, 90% C.L. statistical and systematic). The lightcurve of the transient observed by the WXT lasts around 400 seconds and has a peak flux of ~5.0 x 10^-10 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 1.3(-0.7, +0.8) and a fixed absorbing column density value of 7.8 x 10^20 cm^-2. The derived average unabsorbed 0.5-4 keV flux is 2.0(-1.1, +1.0) x 10^-10 erg/s/cm^2. The uncertainties are at the 90% confidence level for the above parameters. EP241104a is spatially and temporally consistent with GRB 241104A (Fermi GBM Team, GCN 38075; Vladimir et al., GCN 38076; Stéphane et al., GCN 38078). The EP-WXT detection is about 4 minutes after the Fermi-GBM trigger (2024-11-04T18:30:15). Before the detection, the WXT observation was interrupted by the Earth obscuration for about 1.5 ks which covered the Fermi GBM trigger time. EP-FXT follow-up observation has been arranged. 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).
GCN 38082 table
GRB_name GRB241104A
GCN_number 38082
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38082 SUBJECT: GRB 241104A: SVOM/GRM observation DATE: 24/11/05 13:19:34 GMT FROM: zhangjinpeng@ihep.ac.cn SVOM/GRM team: Jin-Peng Zhang, 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, 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 241104A at 2024-11-04T18:30:14 UT (T0), which was also observed by Fermi/GBM (Fermi GBM Team, GCN 38075) and SVOM/ECLAIRs (GCN 38078). 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 11.9 +0.3/-0.3 s. The GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb241104A.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: Jin-Peng Zhang (IHEP)(zhangjinpeng@ihep.ac.cn)
GCN 38083 table
GRB_name GRB241104A
GCN_number 38083
Detection_method Fermi GBM Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38083 SUBJECT: GRB 241104A: COLIBRÍ Upper Limits on the Optical Counterpart DATE: 24/11/05 13:37:47 GMT FROM: Alan Watson at UNAM Alan M. Watson (UNAM), Francis Fortin (IRAP), Stéphane Basa (UAR Pytheas), William H. Lee (UNAM), S. Antier (OCA), D. Akl (AUS), Jean-Luc Atteia (IRAP), Nathaniel R. Butler (ASU), Damien Dornic (CPPM), J.-G. Ducoin (CPPM), Simona Lombardo (LAM), Francesco Magnani (CPPM), and Margarita Pereyra (UNAM) SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (IHEP), Stéphane Basa (LAM), Jean-Luc Atteia (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: We imaged the field of GRB 241104A detected by Fermi/GBM, SVOM/GRM, SVOM/ECLAIRs, and EP/WXT (Fermi GBM Team, GCN Circ. 38075; Schanne et al., GCN Circ. 38078; SVOM/GRM Team, GCN Circ. 38082; Zhou et al., GCN Circ. 38081) during the commissioning of the COLIBRÍ (SVOM/F-GFT) telescope at the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir in Mexico. We observed with the engineering test camera in a red filter that approximates SDSS r. The data were reduced using custom software and then analysed and calibrated against the PS1 catalog using the STDWeb service (Karpov et al. 2022). In 960 seconds of exposure from 2024-11-05 12:12 to 12:32 UTC (17.70 to 18.03 hours after the trigger), at high airmass, we detect no sources in the ECLAIRs localization region other than those previously identified in the PS1 or GAIA DR3 catalogs to a 5-sigma limiting AB magnitude of: r > 20.8 We warmly thank the COLIBRÍ engineering team and the staff of the Observatorio Astronómico Nacional on the Sierra de San Pedro Mártir.
GCN 38086 table
GRB_name GRB241104A
GCN_number 38086
Detection_method Optical
ra 32.5558°
decl 31.5852°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38086 SUBJECT: GRB 241104A: SVOM/VT optical candidate DATE: 24/11/05 18:38:03 GMT FROM: Liping Xin at NAOC, SVOM 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). 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: VT started to observe the field of GRB 241104A (Fermi GBM Team, GCN #38075; Schanne et al., GCN #38078; Zhou et al., GCN #38081; Zhang et al., GCN #38082) in ToO mode from 2024-11-05T13:51:35 UT, about 19.4 hours after the burst. The VT conducted observations in VT_B band (400-650nm) and VT_R band (650-1000nm) simutaneously. An uncatalogued source was found in VT_R band stacked image with a total exposure time of 900s ranging from 13:51:35 to 14:08:15 UT, after compared to the DESI DR10 catalog. The coordinates are R.A.= 02:10:13.392, DEC.= +31:35:06.60, Error = 0.5 arcseconds, J2000. The magnitude was VT_R=21.6+/-0.1 mag and VT_B>23.0 mag (3 sigma). We proposed that it is likely the optical afterglow 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.
GCN 38089 table
GRB_name GRB241104A
GCN_number 38089
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 38089 SUBJECT: GRB 241104A: NOT optical non-detection DATE: 24/11/05 21:36:21 GMT FROM: Daniele B. Malesani at IMAPP / Radboud University D. B. Malesani (DAWN/NBI and Radboud Univ.), A. Martin-Carrillo (UCD), D. Xu (NAOC), M. Turkki (NOT) report on behalf of a larger collaboration: We observed the candidate optical counterpart (Qiu et al., GCN 38086) of GRB 241104A (Fermi GBM team, GCN 38075; Schanne et al., GCN 38078; Zhang et al., GCN 38082), using the Nordic Optical Telescope (NOT) equipped with the ALFOSC imager. Observations were carried out in the SDSS r, i, and z filters. No object is detected at the location of the candidate counterpart, down to the following 3-sigma limiting magnitudes: r > 24.0 AB 2024 Nov 5.859 UT (1.088 days after the trigger) i > 23.7 AB 2024 Nov 5.871 UT (1.100 days after the trigger) z > 22.2 AB 2024 Nov 5.847 UT (1.077 days after the trigger) Calibration was performed against nearby Pan-STARRS sources.
GCN 38090 table
GRB_name GRB241104A
GCN_number 38090
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38090 SUBJECT: GRB 241104A: Swift ToO observations DATE: 24/11/05 23:40:27 GMT FROM: Phil Evans at U of Leicester P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a ToO observation of the Fermi/GBM GRB 241104A. Automated analysis of the XRT data will be presented online at https://www.swift.ac.uk/ToO_GRBs/00021727 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 Fermi/GBM 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.
GCN 38093 table
GRB_name GRB241104A
GCN_number 38093
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38093 SUBJECT: GRB 241104A: The SVOM/VT candidate in GCN circular 38086 is not an astrophysical source DATE: 24/11/06 05:57:04 GMT FROM: Liping Xin at NAOC, SVOM 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). 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: After further analysis of all data acquired via the X-band downlink, the candidate was reported by VT commission team in the previous report(Qiu et al., GCN #38086), is a defect on the detector in VT_R band image,that is detectable in other fields, as well as in the new dark master images. A more detailed analysis is still in progress. 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.
GCN 38094 table
GRB_name GRB241104A
GCN_number 38094
Detection_method Fermi GBM Det
t_trigger 18:30:15.420 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 38094 SUBJECT: GRB241104A: Fermi GBM Observation DATE: 24/11/06 07:33:06 GMT FROM: Rushikesh Digambar Sonawane PHD231014 at IISER, TVM S. Rushikesh (IISER, TVM), U. Pathak (IITB), O. Mukherjee (USRA), S. Bala (USRA) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 18:30:15.42 UT on 04 November 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB241104A (trigger 752437820/241104771) which was also detected by EP/WXT (Zhou et al. 2024, GCN 38081), SVOM/VT (Qiu et al. 2024, GCN 38086) and SVOM/ECLAIRs (Schanne et al. 2024, GCN 38078). The Fermi GBM on-ground location is consistent with the EP/WXT position. The angle from the Fermi LAT boresight is 62 degrees. The GBM light curve consist of single pulse with multiple peaks with a duration (T90) of about 10.5 s (50-300 keV). The time-averaged spectrum from T0-7.6 to T0+11.8 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.69 +/- 0.08 and the cutoff energy, parameterized as Epeak, is 74 +/- 2 keV. The event fluence (10-1000 keV) in this time interval is (3.4 +/- 0.8)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+2.6 s in the 10-1000 keV band is 6.9 +/- 0.3 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 68 +/- 3 keV, alpha = -0.6 +/- 0.1 and beta = -3.0 +/- 0.3. 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/"
GCN 38096 table
GRB_name GRB241104A
GCN_number 38096
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38096 SUBJECT: GRB 241104A: Swift-XRT observations DATE: 24/11/06 08:51:15 GMT FROM: Phil Evans at U of Leicester S. Dichiara (PSU), J.A. Kennea (PSU), D.N. Burrows (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), M. Capalbi (INAF-IASFPA), M. Perri (SSDC & INAF-OAR), V. D'Elia (SSDC & INAF-OAR) and P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Swift-XRT has performed follow-up observations of the Fermi/GBM-detected burst GRB 241104A, using the localisation by SVOM/ECLAIRs (Schanne et al., GCN 38078), collecting 2.9 ks of Photon Counting (PC) mode data between T0+98.0 ks and T0+105.0 ks. No X-ray sources have been detected consistent with being within 256 arcsec of the SVOM/ECLAIRs position. The 3-sigma upper limit in the field is 0.005 ct s^-1, corresponding to a 0.3-10 keV observed flux of 2.1e-13 erg cm^-2 s^-1 (assuming a typical GRB spectrum). Three uncatalogued sources were detected too far from the GRB position to be likely afterglow candidates. These sources are also inconsistent with the X-ray localisation by EP/WXT (Zhou et al., GCN 38081). 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/00021727. This circular is an official product of the Swift-XRT team.
GCN 38129 table
GRB_name GRB241104A
GCN_number 38129
Detection_method CALET
Circular_text TITLE: GCN CIRCULAR NUMBER: 38129 SUBJECT: GRB 241104A: CALET Gamma-Ray Burst Monitor detection DATE: 24/11/08 15:27:54 GMT FROM: Yuta Kawakubo at Aoyama Gakuin University T. Tamura (Kanagawa U), A. Yoshida, T. Sakamoto, S. Sugita, Y. Kawakubo (AGU), K. Yamaoka (Nagoya U), S. Nakahira (JAXA), Y. Asaoka (ICRR), S. Torii, Y. Akaike, K. Kobayashi (Waseda U), Y. Shimizu (Kanagawa U), N. Cannady (GSFC/UMBC), M. L. Cherry (LSU), S. Ricciarini (U of Florence), P. S. Marrocchesi (U of Siena), and the CALET collaboration: The long GRB 241104A (Fermi GBM Final Real-time Localization: Fermi GBM team, GCN Circ. 38075; Detection and localization by SVOM/ECLAIRs: Schanne et al., GCN Circ. 38078; EP detection of GRB 241104A X-ray emission: Zhou et al., GCN Circ. 38081; SVOM/GRM observation: Zhang et al., GCN Circ. 38082) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 18:30:15.957 UTC on 04 November 2024 (https://cgbm.calet.jp/cgbm_trigger/flight/1414780091/index.html). The burst signal was seen by only the SGM detector. Because of a problem with the ground alert processing script, the GCN notice was not distributed automatically for this event. The burst light curve shows a multi-peaked structure that starts at T-0.6 sec, peaks at T+2.6 sec, and ends at T+5.1 sec. The T90 and T50 durations measured by the SGM data are 5.0 +/- 0.4 sec and 3.3 +/- 0.5 sec (40-1000 keV), respectively. The ground-processed light curve is available at https://cgbm.calet.jp/cgbm_trigger/ground/1414780091/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at Waseda University.