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

[vsnet-grb-info 36568] GRB 241209D: CALET Gamma-Ray Burst Monitor detection
by GCN Circulars 14 Dec '24

14 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38569 SUBJECT: GRB 241209D: CALET Gamma-Ray Burst Monitor detection DATE: 24/12/14 09:21:25 GMT FROM: Yuta Kawakubo at Aoyama Gakuin University <kawakubo(a)phys.aoyama.ac.jp> 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, T. Tamura (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 241209D (Fermi GBM Final Real-time Localization: Fermi GBM team, GCN Circ 38488; Swift detection of a burst: Parsotan et al., GCN Circ 38489; Fermi GBM Observation: Malacaria et al., GCN Circ 38507; AstroSat CZTI detection: Tembhurnikar et al., GCN Circ 38518; Konus-Wind detection: Ridnaia et al., GCN Circ 38526) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 10:59:46.760 UTC on 9 December 2024 (https://cgbm.calet.jp/cgbm_trigger/flight/1417777157/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 single pulse that starts at T-4.0 sec, peaks at T+0.6 sec, and ends at T+6.7 sec. The T90 and T50 durations measured by the SGM data are 9.2 +/- 0.7 sec and 4.6 +/- 0.4 sec (40-1000 keV), respectively. The ground-processed light curve is available at https://cgbm.calet.jp/cgbm_trigger/ground/1417777157/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at Waseda University. View this GCN Circular online at https://gcn.nasa.gov/circulars/38569. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36567] GRB 241209B: SVOM/VT optical continuous fading
by GCN Circulars 14 Dec '24

14 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38568 SUBJECT: GRB 241209B: SVOM/VT optical continuous fading DATE: 24/12/14 06:11:47 GMT FROM: Chao Wu at NAOC <cwu(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, D. H. Zhao (NAOC), J. Zhang, L. J. Dan, G. Y. Zou, C. J. Wang, Y. F. Du, C. Huang (XIOPM), H. Zhou (PMO), C. Plasse (CEA) 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: SVOM/VT revisited GRB 241209B（Xie et al., GCN 38478）since 2024-12-10T15:07:15 UT with a total exposure time of 8750 seconds. The optical counterpart (Qiu et al. GCN 38516) was continuously fading, reaching a magnitude of 23.70 +/-0.30 in VT_R. Nothing was seen down to limiting magnitude of 23.80 (3 sigma) in simultaneous channel VT_B. 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/38568. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36566] EP trigger ID 01709128824 is not a real source
by GCN Circulars 14 Dec '24

14 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38567 SUBJECT: EP trigger ID 01709128824 is not a real source DATE: 24/12/14 06:00:09 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> D.-F. Hu (PMO, CAS), X.-Y. Zhou (PRIC), R.-Z. Li (YNAO, CAS), S.-X. Wen, H.-W. Pan (NAO, CAS) report on behalf of the Einstein Probe team: WXT trigger ID: 01709128824 is not a real source. It is a trigger caused by the arm of the point spread function of a bright known source on the detector image. 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/38567. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36565] GRB 241213A: SVOM/VT optical candidate
by GCN Circulars 14 Dec '24

14 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38566 SUBJECT: GRB 241213A: SVOM/VT optical candidate DATE: 24/12/14 04:24:28 GMT FROM: SVOM_group <svomgroup(a)bao.ac.cn> SVOM/VT commissioning team: Y. L. Qiu, H. L. Li (NAOC), Y. Wang (PMO), R.-Z. Li (YNAO), 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, D. H. Zhao (NAOC), J. Zhang, L. J. Dan, G. Y. Zou, C. J. Wang, Y. F. Du, C. Huang (XIOPM) 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 SVOM/VT conducted follow-up observations of the Swift-triggered GRB 241213A (Gupta et al., GCN 38547) in VT_B (400nm-650nm) and VT_R (650nm-1000nm) channel simultaneously, from 10.636 hours to 15.7 hours after the burst. With the X band downlinked data, an uncatalogued optical source was detected within the errorbox of XRT (Osborne et al., GCN 38552) in VT_R stacked image, compared to the PanSTARRS catalog. The brightness of the source was estimated to be 23.8 ± 0.3 mag in AB magnitude in VT_R image at the mid time of 13.6 hours post the burst, with a total exposure time of 135*50 seconds. The source can not be detected in VT_B stacked image with 3 sigma upper limit of ~24.0 mag in AB magnitude. The source is located at RA, Dec = 116.17031, 35.27805, which is equivalent to: RA (J2000) : 07:44:40.87 Dec (J2000): +35:16:40.99 with an uncertainty of 0.5 arcsec. We proposed that this source is the candidate for the gamma-ray burst. Further follow-ups with SVOM/VT are scheduled to confirm the nature of the source. More deep follow-ups are encouraged. 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/38566. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36564] GRB 241213B: Tiled Swift observations
by GCN Circulars 14 Dec '24

14 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38565 SUBJECT: GRB 241213B: Tiled Swift observations DATE: 24/12/14 03:58:22 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 series of observations, tiled on the sky, of the MAXI GRB 241213B. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00130 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. The probability of finding serendipitous sources, unrelated to the MAXI event is high: 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/38565. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36563] GRB 241213A: Swift/UVOT Upper Limits
by GCN Circulars 13 Dec '24

13 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38564 SUBJECT: GRB 241213A: Swift/UVOT Upper Limits DATE: 24/12/13 22:54:19 GMT FROM: Sam Shilling at Lancaster University <shilling.sam(a)gmail.com> S.P.R. Shilling (Lancaster) and R. Gupta (NASA GSFC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 241213A 106 s after the BAT trigger (Gupta et al., GCN Circ. 38547). No optical afterglow consistent with the enhanced XRT position (Osborne et al., GCN Circ. 38552) is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 106 256 147 >20.6 u_FC 318 568 246 >19.8 white 106 945 259 >20.7 v 648 4786 236 >19.2 b 573 766 39 >19.0 u 318 742 265 >19.9 w1 698 5045 67 >18.7 m2 673 4991 216 >19.5 w2 624 4581 236 >19.5 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.060 in the direction of the burst (Schlegel et al. 1998). View this GCN Circular online at https://gcn.nasa.gov/circulars/38564. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36562] GRB 241213B: CALET Gamma-Ray Burst Monitor detection
by GCN Circulars 13 Dec '24

13 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38563 SUBJECT: GRB 241213B: CALET Gamma-Ray Burst Monitor detection DATE: 24/12/13 16:50:42 GMT FROM: Yuta Kawakubo at Aoyama Gakuin University <kawakubo(a)phys.aoyama.ac.jp> P. S. Marrocchesi (U of Siena), 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, T. Tamura (Kanagawa U), N. Cannady (GSFC/UMBC), M. L. Cherry (LSU), S. Ricciarini (U of Florence), and the CALET collaboration: The GRB 241213B (MAXI/GSC detection: Negoro et al., GCN Circ. 38555) was detected in the ground analysis of the CALET Gamma-ray Burst Monitor (CGBM) data around 12:56:30 on 13 December 2024 (referenced to the MAXI detection: GCN Circ. 38555). (https://cgbm.calet.jp/cgbm_trigger/flight/1418129753/index.html). The burst signal was seen by all CGBM detectors. The burst light curve shows a single pulse that starts at T+1.8 sec, peaks at T+2.4 sec, and ends at T+4.5 sec. The T90 and T50 durations measured by the SGM data are 2.4 +/- 0.5 sec and 1.2 +/- 0.4 sec (7-100 keV), respectively. The ground-processed light curve is available at https://cgbm.calet.jp/cgbm_trigger/ground/1418129753/ The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at Waseda University. View this GCN Circular online at https://gcn.nasa.gov/circulars/38563. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36561] GRB 241213A: Swift-XRT refined Analysis
by GCN Circulars 13 Dec '24

13 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38562 SUBJECT: GRB 241213A: Swift-XRT refined Analysis DATE: 24/12/13 16:21:52 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-XRT team: We have analysed 4.5 ks of XRT data for GRB 241213A, from 106 s to 33.0 ks after the BAT trigger. The data comprise 275 s in Windowed Timing (WT) mode 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=0.59 (+0.07, -0.08), followed by a break at T+680 s to an alpha of 1.20 (+0.16, -0.06). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.89 (+/-0.10). The best-fitting absorption column is 3.3 (+0.5, -0.4) x 10^21 cm^-2, in excess of the Galactic value of 6.7 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.85 (+/-0.14) and a best-fitting absorption column of 3.9 (+0.8, -0.7) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.3 x 10^-11 (6.2 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 3.9 (+0.8, -0.7) x 10^21 cm^-2 Galactic foreground: 6.7 x 10^20 cm^-2 Excess significance: 7.4 sigma Photon index: 1.85 (+/-0.14) If the light curve continues to decay with a power-law decay index of 1.20, the count rate at T+24 hours will be 0.014 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.9 x 10^-13 (8.5 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/01274039. This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/38562. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36560] GRB 241212A: Fermi GBM detection
by GCN Circulars 13 Dec '24

13 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38561 SUBJECT: GRB 241212A: Fermi GBM detection DATE: 24/12/13 15:43:11 GMT FROM: Joe Mangan at IJCLab <joseph.mangan(a)ijclab.in2p3.fr> 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/" View this GCN Circular online at https://gcn.nasa.gov/circulars/38561. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 36559] EP241208a: NOT optical upper limits
by GCN Circulars 13 Dec '24

13 Dec '24

TITLE: GCN CIRCULAR NUMBER: 38560 SUBJECT: EP241208a: NOT optical upper limits DATE: 24/12/13 15:33:41 GMT FROM: Dong Xu at NAOC/CAS <dxu(a)nao.cas.cn> X. Liu, J. An, S.Q. Jiang, S.Y. Fu, Z.P. Zhu, D. Xu (NAOC), J.P.U. Fynbo (DAWN/NBI), A.H. de la Fuente, A.G. Theil (NOT) report: We observed the field of EP241208a detected by EP-WXT (Wang et al., GCN 38477) and SVOM/ECLAIRs (Atteia et al., GCN 38557) using the 2.56-m Nordic Optical Telescope (NOT) equipped with the ALFOSC camera. Observations started at 02:48:15.84 UT on 2024-12-09, i.e., ~ 10.20 hrs after the EP-WXT trigger, and 5 x 200 s Sloan r- and z- band images were obtained, respectively. No new optical source is found within the ~ 10 arcsec EP-FXT error circle (Wang et al., GCN 38513) after performing image differencing using the DESI Legacy Survey as template, down to the following 3-sigma limits: Filter Tmid-T0 (hr) UL (AB) ------------------------------------------- r 10.35 >23.2 z 10.67 >21.7 calibrated with nearby Pan-STARRS stars and not corrected for Galactic extinction. View this GCN Circular online at https://gcn.nasa.gov/circulars/38560. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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