GRB250103B

This page lists all entries on GRB250103B in GRBweb

Summary IPN Swift GCN 38796 GCN 38797 GCN 38803 GCN 38805 GCN 38813 GCN 38822 GCN 38823 GCN 38832

Summary table
Variable Value Source
T0 15:44:17 UTC GCN_circulars,Swift Det
ra 54.6640° Swift
decl -33.7496° Swift
pos_error 2.46e-04° Swift
redshift 1.4160 IPN
GBM_located False
mjd 60678.655752314815 GCN_circulars,Swift Det
IPN table
GRB_name GRB250103B
ra 54.6500°
decl -33.7667°
pos_error 5.00e-02°
redshift 1.4160
Swift table
GRB_name GRB250103B
t_trigger 15:44:17 UTC
ra 54.6640°
decl -33.7496°
pos_error 2.46e-04°
GCN 38796 table
GRB_name GRB250103B
GCN_number 38796
Detection_method Swift Det
t_trigger 15:44:17 UTC
ra 54.6510°
decl -33.7720°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38796 SUBJECT: GRB 250103B: Swift detection of a burst DATE: 25/01/03 15:58:32 GMT FROM: P.A. Evans at U. Leicester R. A. J. Eyles-Ferris (U Leicester), S. Dichiara (PSU), P. A. Evans (U Leicester), R. Gupta (NASA GSFC), N. P. M. Kuin (UCL-MSSL), M. J. Moss (GSFC), K. L. Page (U Leicester), D. M. Palmer (LANL) and M. A. Williams (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 15:44:17 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 250103B (trigger=1278865). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 54.651, -33.772 which is RA(J2000) = 03h 38m 36s Dec(J2000) = -33d 46' 18" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a complex structure with a duration of about 30 sec. The peak count rate was ~600 counts/sec (15-350 keV), at ~3 sec after the trigger. The XRT began observing the field at 15:46:48.8 UT, 151.2 seconds after the BAT trigger. Using promptly downlinked data we find a fading, uncatalogued X-ray source with an enhanced position: RA, Dec 54.66403, -33.74965 which is equivalent to: RA(J2000) = 03h 38m 39.37s Dec(J2000) = -33d 44' 58.7" with an uncertainty of 1.9 arcseconds (radius, 90% containment). This location is 89 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 (9.99 x 10^19 cm^-2, Willingale et al. 2013), with an excess column of 4.1 (+3.96/-3.24) x 10^21 cm^-2 (90% confidence). UVOT took a finding chart exposure of 150 seconds with the White filter starting 155 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 none of the XRT error circle. 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 0.008. Burst Advocate for this burst is R. A. J. Eyles-Ferris (raje1 AT leicester.ac.uk). 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/)
GCN 38797 table
GRB_name GRB250103B
GCN_number 38797
Detection_method Swift Other
ra 54.6600°
decl -33.7690°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38797 SUBJECT: GRB 250103B: SVOM detection of a long burst DATE: 25/01/03 16:30:29 GMT FROM: SVOM_group T. Bouchet, D. Turpin (CEA), S. Guillot (IRAP), H. Goto (CEA), F. Daigne (IAP), L. Zhang (IHEP) report on behalf of the SVOM team: The SVOM/ECLAIRs telescope triggered (sb25010303) at 2025-01-03T15:44:04.223 UTC (Tb) and located the long duration GRB 250103B also detected by Swift (Eyles-Ferris et al. GCN 38796). 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 7 alerts were received. The best detection is obtained by IMT with a signal-to-noise ratio of 10.6 in the 5-8 keV energy band over a time window of 41 s starting at Tb. The localization of the best Alert is RA, Dec = 54.660, -33.769 (J2000). R.A. = 03:38:38.46 Dec = -33:46:09.67 The uncertainty on this position is 7.6 arcminutes at 90% C.L., which includes a systematic uncertainty of 2 arcminutes in quadrature. The light curve shows a main single episode in the GRM data with a preliminary T90 duration of about 25 s below 550 keV. Further analysis will be conducted once the X-band telemetry data of ECLAIRs and GRM are received. 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. The SVOM point of contact for this burst is: Tristan Bouchet (tristan.bouchet@cea.fr)
GCN 38803 table
GRB_name GRB250103B
GCN_number 38803
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38803 SUBJECT: Swift GRB 250103B: Global MASTER-Net observations report DATE: 25/01/03 18:51:27 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-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 Swift GRB 250103B ( R. A. J. Eyles-Ferris et al., GCN 38796) errorbox 10372 sec after notice time and 10451 sec after trigger time at 2025-01-03 18:38:29 UT, with upper limit up to 18.0 mag. Observations started at twilight. The observations began at zenith distance = 10 deg. The sun altitude is -9.9 deg. The galactic latitude b = -53 deg., longitude l = 234 deg. Real time updated cover map and OT discovered available here: https://master.sai.msu.ru/site/master2/observ.php?id=2732251 We obtain a following upper limits. Tmid-T0 | Site |Filt.| Expt. | Limit| Comment _________|_____________________|_____|_______|______|________ 10542 | MASTER-SAAO | C | 180 | 18.0 | Filter C is a clear (unfiltred) band. The observation and reduction will continue. The message may be cited.
GCN 38805 table
GRB_name GRB250103B
GCN_number 38805
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38805 SUBJECT: GRB 250103B: LCOGT Optical Upper Limit DATE: 25/01/03 19:44:52 GMT FROM: Robert Strausbaugh at Eastern Illinois University R. Strausbaugh (Eastern Illinois University), A. Cucchiara (NASA) report on behalf of a larger collaboration: We observed the Swift GRB 250103B field (Eyles-Ferris et al., GCN 38796) with the LCOGT 1-meter Sinistro instrument at the South African Astronomical Observatory site, on January 3, from 18:51 to 19:23 UT (corresponding to 4.12 to 4.65 hours after the GRB trigger time) with the Bessel I and R filters. We performed a series of 3x300s exposures in I-band and R-band. We do not detect a source within the XRT error region in either band. The following 5-sigma upper limits are calculated using the USNO-B1.0 catalog as reference: R > 23.0 I > 22.1 These magnitudes are not corrected for galactic extinction.
GCN 38813 table
GRB_name GRB250103B
GCN_number 38813
Detection_method Optical
ra 54.6637°
decl -33.7493°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38813 SUBJECT: GRB 250103B：SVOM/VT optical counterpart DATE: 25/01/04 02:54:27 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, Z. H. Yao (NAOC), J. Zhang, L. J. Dan, G. Y. Zou, C. J. Wang, Y. F. Du, C. Huang (XIOPM),T. Bouchet, D. Turpin (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: The SVOM/VT conducted a ToO follow-up observations for GRB 250103B triggered by both Swift(R. A. J. Eyles-Ferris, GCN 38796) and SVOM (T. Bouchet, GCN 38797) in VT_B (400nm-650nm) and VT_R (650nm-1000nm) channel simultaneously, from 2.467 hours to 7.573 hours after the burst. An uncatalogued fading source was clearly detected within the errorbox of XRT (R. A. J. Eyles-Ferris, GCN 38796) in both VT_B and VT_R stacked images, compared to DESI DR10 catalog. The brightness of the source was estimated to be VT_B=22.1+/-0.1 mag and VT_R=21.8+/-0.1 mag in AB magnitude at the mid time of 2.79 hours post the burst, with a total exposure time of 23*100 seconds. The source is located at RA, Dec = 54.66373, -33.74927 deg, which is equivalent to: RA (J2000) : 03:38:39.30 Dec (J2000): -33:44:57.4 with an uncertainty of 0.2 arcsec. We proposed that the source is the counterpart for the gamma-ray burst. More deep follow-ups are encouraged. The magnitudes give above are not corrected for the expected Galactic foreground extinction, corresponding to a reddening of E(B-V) = 0.0067 mag in the direction of the optical counterpart (Schlafly & Finkbeiner 2011). 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 38822 table
GRB_name GRB250103B
GCN_number 38822
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 38822 SUBJECT: GRB 250103B: LCO/1m optical afterglow candidate detection DATE: 25/01/04 15:54:30 GMT FROM: Damien Turpin at CEA-Saclay D. Turpin (CEA/Irfu), A. Saccardi (GEPI/Obs. de Paris, CEA/Irfu), S. Basa (UAR Pytheas, OHP, LAM), D. B. Malesani (DAWN/NBI and Radboud Univ.), J. T. Palmerio (CEA/Irfu, GEPI/Obs. de Paris), S. Vergani (GEPI/Obs. de Paris), E. Le Floc'h (CEA Paris-Saclay, DAp/AIM) on behalf of a larger collaboration. We observed the field of GRB 250103B detected by Swift (Eyles-Ferris et al. GCN 38796) and SVOM (Bouchet et al., GCN 38797) with the LCO 1.0m telescope at the Sutherland Observatory (SAAO) equipped with the Sinistro instrument. Our observation started at 2025-01-03T20:25:20.617 (T - TGRB ~ 4.68 hr) with 5 x 120s exposure using the sdss-r filter. We marginally detect the optical afterglow candidate seen by SVOM/VT (Qiu et al., GCN 38813) and VLT (Habeeb et al., GCN 38820) from the difference image analysis between our stacked image and the Legacy Survey DR10 template image. At the position reported by VLT, we derived the following magnitude r = 22.32 +/- 0.26 (at Tmid - T0 = 4.78 hr) calibrated with the SkyMapper DR4 catalog and not corrected from the galactic extinction E(B-V): 0.01. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 101004719.
GCN 38823 table
GRB_name GRB250103B
GCN_number 38823
Detection_method Swift-XRT Other
ra 54.6641°
decl -33.7495°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38823 SUBJECT: GRB 250103B: Swift-XRT refined Analysis DATE: 25/01/04 18:05:05 GMT FROM: Phil Evans at U of Leicester J.P. Osborne (U. Leicester), T. Sbarrato (INAF-OAB), P. D'Avanzo (INAF-OAB), M.G. Bernardini (INAF-OAB), D.N. Burrows (PSU), M. A. Williams (PSU), S. Dichiara (PSU), K.L. Page (U. Leicester) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 3.5 ks of XRT data for GRB 250103B, from 144 s to 44.7 ks after the BAT trigger. The data comprise 31 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The best available XRT position (using the promptly downlinked event data, the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue) is RA, Dec = 54.66413, -33.74945 which is equivalent to: RA (J2000): 03 38 39.39 Dec(J2000): -33 44 58.0 with an uncertainty of 1.9 arcsec (radius, 90% confidence). The light curve can be modelled with a power-law decay with a decay index of alpha=3.9 (+/-0.4). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 4.2 (+0.7, -0.5). The best-fitting absorption column is 6.3 (+6.6, -4.5) x 10^20 cm^-2, in excess of the Galactic value of 1.0 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 2.5 x 10^-11 (4.8 x 10^-11) erg cm^-2 count^-1. A summary of the WT-mode spectrum is thus: Total column: 6.3 (+6.6, -4.5) x 10^20 cm^-2 Galactic foreground: 1.0 x 10^20 cm^-2 Excess significance: 2.0 sigma Photon index: 4.2 (+0.7, -0.5) If the light curve continues to decay with a power-law decay index of 3.9, the count rate at T+24 hours will be 2.5 x 10^-10 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.3 x 10^-21 (1.2 x 10^-20) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01278865. This circular is an official product of the Swift-XRT team.
GCN 38832 table
GRB_name GRB250103B
GCN_number 38832
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 38832 SUBJECT: GRB 250103B: REM optical/NIR upper limits DATE: 25/01/06 15:59:56 GMT FROM: Matteo Ferro at INAF-OAB M. Ferro, R. Brivio, P. D’Avanzo, S. Covino, D. Fugazza (INAF-OAB) report on behalf of the REM team: We observed the field of GRB 250103B detected by Swift (Eyles-Ferris et al., GCN 38796), also detected by SVOM (Bouchet et al., GCN 38797) 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, K bands, starting on 2025 January 04 at 00:47:49 UT (i.e. 9.1 hours after the Swift trigger), and lasting for about 1 hour. From preliminary photometry we do not detect any optical or NIR counterpart at the optical afterglow position (Qiu et al., GCN 38813; Habeeb et al., GCN 38820; Turpin et al., GCN 38822) down to the following 3sigma magnitude upper limits: r > 20.4 (AB; calibrated against the SkyMapper catalogue) at a mid-time of t - t0 = 9.5 hr after the trigger, H > 17.3 (Vega; calibrated against the 2MASS catalogue) at a mid-time of t - t0 = 9.4 hr after the trigger.