GRB250114B

This page lists all entries on GRB250114B in GRBweb

Summary IPN GCN 38938 GCN 38941 GCN 38942 GCN 38947 GCN 38950 GCN 38952 GCN 38960

Summary table
Variable Value Source
T0 13:15:37 UTC GCN_circulars,INTEGRAL
ra 48.8667° IPN
decl -2.3167° IPN
pos_error 5.33e-02° IPN
GBM_located False
mjd 60689.552511574075 GCN_circulars,INTEGRAL
IPN table
GRB_name GRB250114B
ra 48.8667°
decl -2.3167°
pos_error 5.33e-02°
GCN 38938 table
GRB_name GRB250114B
GCN_number 38938
Detection_method INTEGRAL
t_trigger 13:15:37 UTC
ra 48.8765°
decl -2.3074°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38938 SUBJECT: GRB 250114B: a short GRB detected with INTEGRAL DATE: 25/01/14 14:08:18 GMT FROM: Diego Gotz at CEA D.Gotz (CEA, Saclay), S.Mereghetti (INAF, IASF-Milano), C.Ferrigno, E.Bozzo, V.Savchenko (ISDC, Versoix), L.Ducci (IAAT, Germany and ISDC, Versoix) and J.Borkowski (CAMK, Torun) report: a short gamma ray burst lasting about 1 s has been detected by IBAS in the IBIS/ISGRI data at 13:15:37 UT of 2025 January 14. The refined coordinates (J2000) are: R.A.= 48.8765 deg DEC.= -2.3074 deg with an uncertainty of 2.1 arcmin (90% c.l.). A plot of the light curve will be posted at http://ibas.iasf-milano.inaf.it/IBAS_Results.html
GCN 38941 table
GRB_name GRB250114B
GCN_number 38941
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 38941 SUBJECT: GRB 250114B: Swift ToO observations DATE: 25/01/14 16:26:10 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 INTEGRAL GRB 250114B. Automated analysis of the XRT data will be presented online at https://www.swift.ac.uk/ToO_GRBs/00021756 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 INTEGRAL 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 38942 table
GRB_name GRB250114B
GCN_number 38942
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 38942 SUBJECT: GRB 250114B : GIT optical upper limit DATE: 25/01/14 16:28:42 GMT FROM: V. Swain at IIT Bombay M. Goyal, A.P. Saikia, V. Swain, T. Mohan, V. Bhalerao (IITB), G.C. Anupama, S. Barway (IIA) and K. Angail (IAO) report on behalf of the GIT team: We observed the field of INTEGRAL GRB 250114B (Gotz et. al., GCN 38938) with 0.7m GROWTH-India Telescope (GIT) in r' filter. We started the observation at 2025-01-14 14:43:01 UT, i.e., 1.46 hours after the INTEGRAL trigger. We did not detect any new source in our stacked image within the uncertainty region reportedd in GCN 38938. The obtained upper limit is as follows: | MJD (mid) | Filter | Exposure (s) | Limiting Magnitude (AB) | | ----------------- |------- | ------------------ | -------------- | | 60689.62099 | r' | 3 x 300 | 20.3 | The measurement is calibrated against PanSTARRS DR1 (Chambers et al., 2016) and not corrected for Galactic extinction. The GROWTH India Telescope (GIT; Kumar et al. 2022) is a 70-cm telescope with a 0.7-degree field of view, set up by the Indian Institute of Astrophysics (IIA) and the Indian Institute of Technology Bombay (IITB) with funding from DST-SERB and IUSSTF. It is located at the Indian Astronomical Observatory (Hanle), operated by IIA. We acknowledge funding by the IITB alumni batch of 1994, which partially supports the operations of the telescope. Telescope technical details are available at https://sites.google.com/view/growthindia/.
GCN 38947 table
GRB_name GRB250114B
GCN_number 38947
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 38947 SUBJECT: GRB 250114B: OHP/T193 optical upper limit DATE: 25/01/14 22:47:18 GMT FROM: Benjamin Schneider at MIT B. Schneider (LAM), C. Adami (LAM/Pytheas/AMU), S. Basa (LAM/OHP/Pytheas/AMU), E. Le Floc'h (CEA), A. Saccardi (CEA), D. Turpin (CEA) report on behalf of a larger collaboration: We observed the field of the INTEGRAL GRB 250114B (Gotz et al., GCN 38938) with the T193cm telescope at the Observatoire de Haute-Provence (France) equipped with the MISTRAL spectro-imager. We obtained a total of 61 minutes (1x300s + 4x180s + 11x240s) in the i-band using the red MISTRAL setting from 2025-01-14T18:08 to 2025-01-14T19:29 (mid-time 5.6h after the trigger). In the stacked image, we do not detect any new source at the XRT #2 source position (Evans et al., GCN 38941) or within the INTEGRAL error circle (Gotz et. al., GCN 38938) down to the following 5-sigma limit: i > 20.88 mag (AB) The photometric calibration was performed using nearby stars from the PanSTARRS catalog. We acknowledge the excellent support from Observatoire de Haute-Provence, in particular Jean Balcaen, Orlagh Creevey and Flavien Kiefer.
GCN 38950 table
GRB_name GRB250114B
GCN_number 38950
Detection_method MITSuME
ra 48.8582°
decl -2.2936°
Circular_text TITLE: GCN CIRCULAR NUMBER: 38950 SUBJECT: GRB 250114B : MITSuME Akeno optical afterglow candidate detection DATE: 25/01/15 10:30:38 GMT FROM: Mahito Sasada at Tokyo Institute of Technology M. Sasada, I. Takahashi, H. Hagio, Y. Kubo, N. Higuchi, H. Seki, S. Joshima, Y. Yatsu and N. Kawai (Science Tokyo) report on behalf of the MITSuME collaboration: We observed the field of GRB 250114B (Gotz et al. GCN 38938; Evans et al. GCN 38941) with the optical three-color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50-cm telescope Akeno. The observation started at 2025-01-14 13:16:36.51 UT (60 seconds after the INTEGRAL trigger). We stacked the images with good conditions. Then we detected a point source in the Rc- and Ic-band images within the circle of INTEGRAL uncertainty area (Gotz et al. GCN 38938). The source position is R.A. = 48.8582 deg and Dec. = -2.2936 deg, which is consistent with the 2nd X-ray source position of R.A. = 48.8582 deg and Dec. = -2.2940 deg detected by XRT within 1 arcsec (Evans et al. GCN 38941; Williams et al. GCN 38949). Here we report upper limits of the observations, and magnitudes of the source as follows. T0+[sec] | MID-UT | T-EXP[sec] | 5-sigma limits and magnitudes ------------------------------------------------------------------------------------------------ 399 | 2025-01-14 13:22:16.31 | 480 | g'>18.0, Rc=18.1+/-0.1, Ic=17.6+/-0.1 2232 | 2025-01-14 13:52:49.03 | 2460 | g'>18.6, Rc=19.4+/-0.2, Ic=19.1+/-0.2 ------------------------------------------------------------------------------------------------ T0+ : Elapsed time after the trigger T-EXP: Total Exposure time We used the PS1 catalog for flux calibration. The catalog magnitudes in PS1 g, r and i bands were converted to our g', Rc and Ic band magnitudes following Tonry et al. (2012), Table 6. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ; https://github.com/MNiwano/Eclaire).
GCN 38952 table
GRB_name GRB250114B
GCN_number 38952
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 38952 SUBJECT: GRB 250114B: Liverpool Telescope optical upper limit DATE: 25/01/15 12:43:55 GMT FROM: Ben Gompertz at U of Birmingham B. P. Gompertz (U. Birmingham), Dimple (U. Birmingham), D. B. Malesani (DAWN/NBI and Radboud) and A. J. Levan (Radboud) report: We initiated follow-up observations of the INTEGRAL-detected GRB 250114B (Gotz et al., GCN 38938) with the IO:O camera on the 2m robotic Liverpool Telescope (LT). Observations began at 19:17:04 UT on 2025-01-14 and consisted of 5x120 s exposures in the SDSS r filter. We do not detect the candidate afterglow reported by MITSuME Akeno (Sasada et al., GCN 38950) nor any new source within the localisation region of XRT source 2 (Williams et al., GCN 38949) to a 3-sigma limiting magnitude of r(AB) > 21.17, at a mid-time of 6.24 hr after trigger. Observations were calibrated against nearby SDSS stars and are not corrected for foreground extinction. Our non-detection, and those reported by GIT (Goyal et al., GCN 38942) and OHP/T193 (Schneider et al., GCN 38947), support the rapid fading detected by MITSuME Akeno over a longer time baseline, indicating the source is likely the optical afterglow of GRB 250114B. In Legacy Survey images of the field there is no object directly underlying the afterglow position. The closest object is a galaxy with r = 24.4 and an offset of ~1.5 arcseconds. This galaxy has a probability of chance alignment of ~5% (cf. Bloom et al. 2002, ApJ, v123, p1111).
GCN 38960 table
GRB_name GRB250114B
GCN_number 38960
Detection_method INTEGRAL
Circular_text TITLE: GCN CIRCULAR NUMBER: 38960 SUBJECT: GRB 250114B: SVOM/VT upper limit DATE: 25/01/16 07:48:38 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, Y. N. Ma (NAOC), J. Zhang, L. J. Dan, G. Y. Zou, C. J. Wang, Y. F. Du, C. Huang (XIOPM), Diego Götz, Bertrand Cordier (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 observations of the INTEGRAL-detected GRB 250114B (Gotz et al., GCN 38938) . The observations were carried out in VT_B (400nm-650nm) and VT_R (650nm-1000nm) channel simultaneously. The afterglow reported (Williams et al., GCN 38949; Sasada et al., GCN 38950) was not detected either in VT_B or VT_R stacked images. The 3 sigma limits in AB magnitude were derived with VT_B= 23.9 mag with exposure time of 37*100 sec and VT_R= 23.6 mag with exposure time of 35*100 sec, at the mid time of about 24.0 hours after the burst. The non-detection is consistent with the reports (Goyal et al., GCN 38942; Schneider et al., GCN 38947; Gompertz et al., GCN 38952). The galaxy noticed (Gompertz et al., GCN 38952) was marginal detected in VT_R stacked image. 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.