GRB241212A

This page lists all entries on GRB241212A in GRBweb

Summary Fermi GBM IPN GCN 38540 GCN 38544 GCN 38545 GCN 38546 GCN 38559 GCN 38561 GCN 38579 GCN 38677

Summary table
Variable Value Source
GRB_name_Fermi GRB241212390
T0 9:21:48 UTC GCN_circulars,Fermi GBM final loc
ra 45.1208° IPN
decl 6.7000° IPN
pos_error 5.83e-02° IPN
T90 39.421 s Fermi_GBM
T90_error 4.222 s Fermi_GBM
T90_start 9:21:48.665 UTC Fermi_GBM
fluence 3.04e-06 erg/cm² Fermi_GBM
fluence_error 2.40e-08 erg/cm² Fermi_GBM
T100 40.086 s
GBM_located False
mjd 60656.39013888889 GCN_circulars,Fermi GBM final loc
Fermi GBM table
GRB_name_Fermi GRB241212390
trigger_name bn241212390
ra 44.3000°
decl 6.5500°
pos_error 3.70e+00°
datum 2024-12-12
t_trigger 9:21:48.661 UTC
T90 39.421 s
T90_error 4.222 s
T90_start 9:21:48.665 UTC
fluence 3.04e-06 erg/cm²
fluence_error 2.40e-08 erg/cm²
flux_1024 2.82e+00 erg/cm²/s
flux_1024_error 2.41e-01 erg/cm²/s
flux_1024_time 4.42e+00 erg/cm²/s
flux_64 4.41e+00 erg/cm²/s
flux_64_error 1.16e+00 erg/cm²/s
IPN table
GRB_name GRB241212A
ra 45.1208°
decl 6.7000°
pos_error 5.83e-02°
GCN 38540 table
GRB_name GRB241212A
GCN_number 38540
Detection_method Fermi GBM final loc
t_trigger 9:21:48 UTC
ra 44.3000°
decl 6.5000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38540 SUBJECT: GRB 241212A: Fermi GBM Final Real-time Localization DATE: 24/12/12 09:32:08 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 09:21:48 UT on 12 Dec 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241212A (trigger 755688113.6612 / 241212390). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 44.3, Dec = 6.5 (J2000 degrees, equivalent to J2000 02h 57m, 6d 30'), with a statistical uncertainty of 3.6 degrees. The angle from the Fermi LAT boresight is 40.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241212390/quicklook/glg_skymap_all_bn241212390.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/bn241212390/quicklook/glg_healpix_all_bn241212390.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn241212390/quicklook/glg_lc_medres34_bn241212390.gif
GCN 38544 table
GRB_name GRB241212A
GCN_number 38544
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 38544 SUBJECT: GRB 241212A: AstroSat CZTI detection DATE: 24/12/12 15:45:53 GMT FROM: Gaurav Waratkar at IIT Bombay J. Joshi (IUCAA), G. Waratkar (IITB), A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka University/IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration: Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al., 2021, JApA, 42, 73) showed the detection of a long-duration GRB 241212A which was also detected by Fermi/GBM (Fermi-GBM Team, GCN Circ. 38540), and SVOM/ECLAIRs (Li et al., GCN Circ. 38541). The source was clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve peaks at 2024-12-12 09:21:49.4 UTC. The measured peak count rate associated with the burst is 238 (+71, -38) counts/s above the background in the combined data of all quadrants, with a total of 1473 (+319, -369) counts. The local mean background count rate was 1331 (+6, -7) counts/s. We measure a T90 of 14 (+1, -6) s from the cumulative Veto light curve. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, URSC, IUCAA, SAC, and PRL. The Indian Space Research Organisation funded, managed, and facilitated the project. CZTI GRB detections are reported regularly on the payload site at: http://astrosat.iucaa.in/czti/?q=grbs
GCN 38545 table
GRB_name GRB241212A
GCN_number 38545
Detection_method Optical
ra 45.0803°
decl 6.7168°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38545 SUBJECT: GRB 241212A : SVOM/VT bright optical afterglow DATE: 24/12/12 20:40:17 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, J. Zhang, L. J. Dan, G. Y. Zou, C. J. Wang, Y. F. Du, C. Huang (XIOPM), H. Zhou (PMO), Li Zhang (IHEP) 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 241212A (Zhang et al., GCN 38541; Fermi GBM team et al., GCN 38540) was observed by on-board SVOM/VT after the automatic slew of the platform. The VT conducted observations in VT_B (400nm-650nm) and VT_R (650nm-1000nm) channel simultaneously. With the X band downlinked data, an uncatalogued optical source was detected in VT_B and VT_R band images within the errorbox in both Eclairs and MXT (Zhang et al., GCN 38541) compared to the Desi D10 catalog. The source is located at RA, Dec = 45.08033, 6.71682, which is equivalent to: RA (J2000) : 03:00:19.28 Dec (J2000): +06:43:00.56 with an uncertainty of 0.2 arcsec. Its brightness was fading for 1.1 magnitude in both of VT_B and VT_R images from 0.7 hours to 4.8 hours after the burst. The magnitude was VT_B = 20.60 mag and VT_R = 19.88 mag in AB magnitude,about 1.15 hr post the trigger. 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 38546 table
GRB_name GRB241212A
GCN_number 38546
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 38546 SUBJECT: GRB 241212A : SVOM/C-GFT optical upper limit at early phase DATE: 24/12/13 00:58:36 GMT FROM: Chao Wu at NAOC SVOM/C-GFT team: Zhe Kang (CHO), Chao WU (NAOC), Liping Xin(NAOC), Xuhui Han(NAOC), Pinpin Zhang (NAOC), Xiaomeng Lu (NAOC), Zhenwei Li (CHO), You Lv (CHO), Ruosong Zhang (NAOC), Yujie Xiao(NAOC) 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) We observed the field of GRB 241212A (Zhang et. al, GCN 38541; Fermi team GCN 38540;Joshi et al. GCN 38544) starting at 2024-12-12T09:22:45 UT, ~53 sec after the burst trigger with C-GFT. A series of g, r and i band images were obtained with exposure time of 10s. Due to bad observation condition(not good weather, low altitude and ~13.8 deg to the moon), the optical counterpart reported by Qiu et al. (GCN 38545) was not detected in the images. The upper limit at early phase are, (T-T0)_mid(sec) limiting_mag(3sigma) ------------------------------------- 58 15.80 91 16.80 The photometry was calibrated with nearby stars in ucac4. We thank the observation assistant Bowen Li and Chunlei Guo at Jilin observatory for their excellent support. Chinese Ground Follow-up Telescope of SVOM mission is located at Jilin, Changchun Observatory, National Astronomical Observatories, CAS. It has FOV of 1.28 deg x 1.28 deg with a 4k*4k CMOS detector mounted on the primary focus of 1.2-meter-aperure telescope.
GCN 38559 table
GRB_name GRB241212A
GCN_number 38559
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38559 SUBJECT: GRB 241212A: Swift ToO observations DATE: 24/12/13 15:26:28 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 SVOM/ECLAIRs GRB 241212A. Automated analysis of the XRT data will be presented online at https://www.swift.ac.uk/ToO_GRBs/00021740 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.
GCN 38561 table
GRB_name GRB241212A
GCN_number 38561
Detection_method Fermi GBM Det
t_trigger 9:21:48.660 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 38561 SUBJECT: GRB 241212A: Fermi GBM detection DATE: 24/12/13 15:43:11 GMT FROM: Joe Mangan at IJCLab J. Mangan (CNRS/IJCLab) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 09:21:48.66 UT on 12 December 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 241212A (trigger 755688113 / 241212390), which was also detected by, SVOM-GRM (Zhang Li et al. 2024, GCN 38541), and for which there is a possible optical counterpart (P.A. Evans et al. 2024, GCN 38559). The Fermi GBM Final Real-time Localization is reported in GCN 38540. The angle from the Fermi LAT boresight at the GBM trigger time is 40 degrees. The GBM light curve consists of a single emission with a duration (T90) of about 39 s (50-300 keV). The time-averaged spectrum from T0-0 s to T0+34 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -1.1 +/- 0.1 and the cutoff energy, parameterized as Epeak, is 304.8 +/- 59.1 keV. The event fluence (10-1000 keV) in this time interval is (5.8 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+4.4 s in the 10-1000 keV band is 2.8 +/- 0.2 ph/s/cm^2. 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 38579 table
GRB_name GRB241212A
GCN_number 38579
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38579 SUBJECT: GRB 241212A: Swift-XRT observations DATE: 24/12/16 06:42:41 GMT FROM: Phil Evans at U of Leicester M. Perri (SSDC & INAF-OAR), V. D'Elia (SSDC & INAF-OAR), B. Sbarufatti (INAF-OAB), 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 SVOM/ECLAIRs-detected burst GRB 241212A, collecting 2.3 ks of Photon Counting (PC) mode data between T0+257.0 ks and T0+297.7 ks. No X-ray sources have been detected within the estimated 3-sigma SVOM/ECLAIRs error region (118 arcsec). The 3-sigma upper limit in the field is 0.004 ct s^-1, corresponding to a 0.3-10 keV observed flux of 1.4e-13 erg cm^-2 s^-1 (assuming a typical GRB spectrum). An uncatalogued was detected, however this was too far from the GRB position to be the afterglow. 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/00021740. This circular is an official product of the Swift-XRT team.
GCN 38677 table
GRB_name GRB241212A
GCN_number 38677
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 38677 SUBJECT: GRB 241212A: VZLUSAT-2 detection DATE: 24/12/27 06:45:12 GMT FROM: Jakub Ripa J. Ripa, M. Dafcikova (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner (Masaryk U.), M. Ohno (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), H. Takahashi (Hiroshima U.), F. Munz , M. Topinka, F. Hroch, N. Husarikova, J.-P. Breuer (Masaryk U.), J. Hudec, J. Kapus, M. Frajt, M. Rezenov (Spacemanic s.r.o), R. Laszlo (Needronix), G. Galgoczi (Wigner Research Center/Eotvos U.), N. Uchida (ISAS/JAXA), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), Y. Fukazawa, K. Hirose, H. Matake (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), L. L. Kiss (Konkoly Observatory), T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), K. Torigoe (Hiroshima U.), P. Svoboda, V. Daniel, J. Dudas, M. Junas, J. Gromes (VZLU), I. Vertat (FEL ZCU) -- the VZLUSAT-2/GRB payload collaboration. The long-duration GRB 241212A (Fermi/GBM detection: GCN 38540; AstroSat/CZTI detection: GCN 38544; SVOM detection: GCN 38541; INTEGRAL/SPI-ACS peak detection at 2024-12-12 09:21:47 UT) was detected by the GRB detector on board of the VZLUSAT-2 3U CubeSat (https://www.vzlusat2.cz/en/). The data acquisition was performed by GRB detector unit no. 1. The detection was confirmed at the peak time 2024-12-12 09:21:48 UTC. The T90 duration measured by VZLUSAT-2 is 25 s and the significance during T90 reaches 7.1 sigma. The light curve obtained by VZLUSAT-2 is available here: https://vzlusat2.konkoly.hu/static/share/GRB241212A_GCN_VZLUSAT2.pdf All VZLUSAT-2 detections are listed at: https://monoceros.physics.muni.cz/hea/VZLUSAT-2/ The GRB detectors on VZLUSAT-2 are a demonstration payload for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). Two GRB modules of VZLUSAT-2 are placed in a perpendicular manner and each consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~30 keV to ~1000 keV. VZLUSAT-2 was launched on 2022 January 13 from Cape Canaveral.