GRB250106A

This page lists all entries on GRB250106A in GRBweb

Summary IPN Swift GCN 38826 GCN 38828 GCN 38830 GCN 38834 GCN 38838

Summary table
Variable Value Source
T0 2:29:19.972 UTC Swift
ra 117.2383° Swift
decl 63.8124° Swift
pos_error 3.88e-04° Swift
redshift 0.0150 Swift
GBM_located False
mjd 60681.10370337963 Swift
IPN table
GRB_name GRB250106A
ra 117.1500°
decl 63.7667°
pos_error 1.47e-01°
Swift table
GRB_name GRB250106A
t_trigger 2:29:19.972 UTC
ra 117.2383°
decl 63.8124°
pos_error 3.88e-04°
redshift 0.0150
GCN 38826 table
GRB_name GRB250106A
GCN_number 38826
Detection_method Other
ra 117.1520°
decl 63.7700°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38826 SUBJECT: GRB 250106A: SVOM detection of a long burst DATE: 25/01/06 03:58:22 GMT FROM: SVOM_group D.-H. ZHAO, C. WU, W.-J. XIE (NAOC, CAS), D. Turpin (CEA), S. Guillot (IRAP), D. Götz (CEA), C-W. Wang (IHEP) report on behalf of the SVOM team. The SVOM/ECLAIRs telescope triggered and located the long duration GRB 250106A (sb25010601) starting at 2025-01-06T02:29:19.972 UTC (Tb). 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 8 alerts were received. The best detection is obtained by IMT with a signal-to-noise ratio of 8.94 in the 8-50 keV energy band over a time window of 20.48 s starting at Tb. The localization of the best Alert is RA, Dec = 117.152, 63.770 (J2000), which is RA(J2000) = 07h 48m 36.480s Dec(J2000)= +63d 46' 12.000' The uncertainty on this position is 8.84 arcminutes at 90% C.L., to which we recommend adding 2 arcminutes of systematic uncertainty in quadrature. The light curve shows one broad peak in 5-120 keV in ECLAIRs with a preliminary T90 duration of 93.64 s. The SVOM/GRM light curve can be found here: https://www.bursthub.cn//admin/static/svgrb250106A.png SVOM slewed automatically on this burst. The information about MXT and VT observations will be reported later. 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. The SVOM point of contact for this burst is: Donghua ZHAO(zhaodh@bao.ac.cn)
GCN 38828 table
GRB_name GRB250106A
GCN_number 38828
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38828 SUBJECT: GRB 250106A: Swift ToO observations DATE: 25/01/06 08:03:23 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 250106A. Automated analysis of the XRT data will be presented online at https://www.swift.ac.uk/ToO_GRBs/00021753 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 38830 table
GRB_name GRB250106A
GCN_number 38830
Detection_method Swift-XRT Other
ra 117.2387°
decl 63.8123°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38830 SUBJECT: GRB 250106A: Swift-XRT observations DATE: 25/01/06 14:45:52 GMT FROM: Phil Evans at U of Leicester J.P. Osborne (U. Leicester), P. D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), E. Ambrosi (INAF-IASFPA) , M. A. Williams (PSU), S. Dichiara (PSU), J.A. Kennea (PSU), K.L. Page (U. Leicester), A.P. Beardmore (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 250106A (Zhao et al., GCN Circ. 38826), collecting 2.9 ks of Photon Counting (PC) mode data between T0+19.9 ks and T0+27.1 ks. Four uncatalogued X-ray sources have been detected, however none of them is above the RASS limit or shows definitive signs of fading. However, Source 2 was reported by Qiu et al. (GCN Circ. 38829) to be consistent with the position of a SVOM/VT optical candiate. Details of the Swift-XRT sources are given below: Source 1: RA (J2000): 117.2387 = 07:48:57.28 Dec (J2000): +63.8123 = +63:48:44.3 Error: 3.0 arcsec (radius, 90% conf. [Enhanced position]) Count-rate: 0.0209 +/- 0.0032 ct s^-1 Distance: 205 arcsec from SVOM/ECLAIRs position. Flux: (5.99 +/- 0.91)e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV) Source 2: RA (J2000): 117.3686 = 07:49:28.47 Dec (J2000): +63.7079 = +63:42:28.6 Error: 5.9 arcsec (radius, 90% conf.) Count-rate: (5.7 [+2.1, -1.7])e-3 ct s^-1 Distance: 411 arcsec from SVOM/ECLAIRs position. Flux: (4.1 [+1.5, -1.2])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV) Source 3: RA (J2000): 116.9049 = 07:47:37.18 Dec (J2000): +63.9115 = +63:54:41.5 Error: 6.5 arcsec (radius, 90% conf. [Enhanced position]) Count-rate: (4.5 [+1.9, -1.5])e-3 ct s^-1 Distance: 642 arcsec from SVOM/ECLAIRs position. Flux: (3.1 [+1.3, -1.0])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV) Source 4: RA (J2000): 117.2096 = 07:48:50.31 Dec (J2000): +63.8218 = +63:49:18.4 Error: 7.1 arcsec (radius, 90% conf.) Count-rate: (2.4 [+1.4, -1.0])e-3 ct s^-1 Distance: 207 arcsec from SVOM/ECLAIRs position. Flux: (7.3 [+4.2, -3.1])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV) 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/00021753. This circular is an official product of the Swift-XRT team.
GCN 38834 table
GRB_name GRB250106A
GCN_number 38834
Detection_method Optical
ra 117.3710°
decl 63.7082°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38834 SUBJECT: GRB 250106A: NOT optical observations DATE: 25/01/07 01:47:52 GMT FROM: Daniele B. Malesani at IMAPP / Radboud University L. Izzo (INAF/OACn and DARK/NBI), D. B. Malesani (DAWN/NBI and Radboud Univ.), D. Xu (NAOC), Z.P. Zhu (NAOC), X. Liu (NAOC), T. Pursimo (NOT), report on behalf of a larger collaboration: We observed the field of GRB 250106A (Zhao et al., GCN 38826) using the Nordic Optical Telescope (NOT) equipped with the ALFOSC camera, using the SDSS z filter. The instrument was rotated in order to include XRT sources #1 and #2 (Osborne et al., GCN 38830), as well as the candidate SVOM/VT optical afterglow (which is consistent with the position of XRT source #2; Qiu et al., GCN 38829). The observation mid time was 2025 Jan 6.982 UT (10.13 hr after the SVOM trigger), and the exposure time was 2000 s. No source is detected within the localization circle of XRT source #1, down to a limiting magnitude z > 23.3 (AB). Two sources are detected within the localization circle of XRT source #2. Source A (coincident with the SVOM/VT optical candidate): RA = 07:49:29.04 Dec = +63:42:29.4 mag z = 22.23 +- 0.10 AB Source B: RA = 07:49:27.99 Dec = +63:42:31.5 mag z = 19.90 +- 0.02 AB At the locations of both sources, objects are visible in the Legacy Survey, for which we measure AB magnitudes z = 22.24 +- 0.11 and z = 19.84 +- 0.02 for sources A and B, respectively. Our measured values are thus fully consistent with those in the archival images. Source B is also detected by Gaia, which provides a QSO classification. This opens the question whether object B could be responsible for the X-ray emission detected by Swift/XRT. Source A could be the host galaxy of GRB 250106A, though we note that its archival r-band magnitude (r = 23) is only marginally fainter than the SVOM/VT magnitude (R = 22.5 +- 0.3 mag; Qiu et al., GCN 38829). We encourage further observations with both SVOM/VT and Swift/XRT in order to establish variability of both the optical and X-ray sources.
GCN 38838 table
GRB_name GRB250106A
GCN_number 38838
Detection_method Optical
ra 117.2372°
decl 63.8132°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38838 SUBJECT: GRB 250106A: SVOM/VT 2nd optical deep observation DATE: 25/01/07 09:31:41 GMT FROM: SVOM_group SVOM/VT commissioning team: Y. L. Qiu, H. L. Li, C. Wu, D. H. Zhao, L. P. Xin, 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, Z. H. Yao (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 TOO observations of GRB 250106A (Zhao et al., GCN 38826) at 8.88 hr after the trigger. The observations were carried out in VT_B (400nm-650nm) and VT_R (650nm-1000nm) channel simultaneously. The candidate reported by Qiu et al. (GCN 38829) were detected in both of stacked images of VT_B and VT_R. The brightness are, channel (t-T0)_mid(hr) exptime mag(AB) VT_B 13.25 149x100s 23.5 +/-0.2 VT_R 13.26 142x100s 22.4 +/-0.1 No definite fading was found compared to brightness reported (Qiu et al., GCN 38829). This observation is consistent with the result (Izzo et al. GCN 38834). Thus, this source is not a good candidate for the burst. A new source with a low S/N with a magnitude of VT_R~24.0 mag was tentatively detected near the errorbox of XRT source #1 (Osborne et al. GCN 38830), with a distance of 4.0 arcseconds from the XRT source #1. Its position is RA=117.2372, DEC=63.8132 deg, which is equivalent to: RA (J2000) : 07:48:56.93 Dec (J2000): +63:48:47.5 with an uncertainty of 0.5 arcsec. 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.