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This page lists all entries on GRB240125A in GRBweb

Summary IPN GCN 35630 GCN 35637 GCN 35639 GCN 35645 GCN 35699

Summary table
Variable	Value	Source
T0	9:35:03.601 UTC	GCN_circulars,Konus-Wind Det
ra	131.5292°	IPN
decl	66.8500°	IPN
pos_error	2.46e+01°	IPN
GBM_located	False
mjd	60334.3993472338	GCN_circulars,Konus-Wind Det

IPN table
GRB_name	GRB240125A
ra	131.5292°
decl	66.8500°
pos_error	2.46e+01°

GCN 35630 table
GRB_name	GRB240125A
GCN_number	35630
Detection_method	CALET
Circular_text	TITLE: GCN CIRCULAR NUMBER: 35630 SUBJECT: GRB 240125A (short): Glowbug gamma-ray detection DATE: 24/01/25 18:08:11 GMT FROM: C.C. Cheung at Naval Research Lab GRB 240125A (short): Glowbug gamma-ray detection C.C. Cheung, M. Kerr, J.E. Grove, R. Woolf (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report: The Glowbug gamma-ray telescope [1,2], operating on the International Space Station, reports the detection of the short GRB 240125A, which was also detected by CALET/CGBM (Trigger 1390210300). Using an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2024-01-25 09:34:59.200 with a duration of 1.28 s and a total significance of about 51.2 sigma. The light curve comprises a triple-peaked structure. Using a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a photon index dN/dE~E^x of x=0.8 and a cutoff energy ("Epeak") of 705 keV. The modeled 10-10000 keV fluence is 3.2e-06 erg/cm^2. The best-fit localization is RA, Decl. (J2000, deg) = 153.4, 48.7 with a radius of 9.3 deg (95% confidence), with a highly uncertain systematic uncertainty. The analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS. Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Program’s STP-H9 to the ISS. The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2/3 sky) over a wide energy band of 50 keV to >2 MeV. [1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959 [2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O [3] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006 Distribution Statement A: Approved for public release. Distribution is unlimited.

GCN 35637 table
GRB_name	GRB240125A
GCN_number	35637
Detection_method	AstroSat CZTI
Circular_text	TITLE: GCN CIRCULAR NUMBER: 35637 SUBJECT: GRB 240125A: AstroSat CZTI detection of a short burst DATE: 24/01/26 08:30:34 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 short-duration GRB 240125A which was also detected by Glowbug (C.C. Cheung, GCN Circ. 35630). The source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve peaks at 2024-01-25 09:35:00.35 UTC. The measured peak count rate associated with the burst is 287 (+139, -40) counts/s above the background in the combined data of three quadrants (out of four), with a total of 208 (+50, -50) counts. The local mean background count rate was 263 (+7, -10) counts/s. Using cumulative rates, we measure a T90 of 1.4 (+0.11, -0.47) s. The source was also detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve peaks at 2024-01-23 09:34:58.75UTC. The measured peak count rate associated with the burst is 532 (+74, -81) counts/s above the background in the combined data of all quadrants, with a total of 1132 (+156, -172) counts. The local mean background count rate was 1587 (+5, -6) counts/s. Due to the intrinsic 1 s binning of veto data, we cannot reliably estimate a T90 from it. 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=grb

GCN 35639 table
GRB_name	GRB240125A
GCN_number	35639
Detection_method	CALET
Circular_text	TITLE: GCN CIRCULAR NUMBER: 35639 SUBJECT: GRB 240125A: CALET Gamma-Ray Burst Monitor detection DATE: 24/01/27 00:35:22 GMT FROM: Yuta Kawakubo at Louisiana State University P. S. Marrocchesi (U of Siena), A. Yoshida, T. Sakamoto, S. Sugita (AGU), Y. Kawakubo (LSU), 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 short GRB 240125A (Glowbug gamma-ray detection: Cheung et al., GCN Circ. 35630; AstroSat CZTI detection: Joshi et al., GCN Circ. 35637) triggered the CALET Gamma-ray Burst Monitor (CGBM) at 09:34:58.79 UTC on 25 January 2024 (http://cgbm.calet.jp/cgbm_trigger/flight/1390210300/). The burst signal was seen by all CGBM detectors. The burst light curve shows a triple-peaked structure that starts at T+0.50 sec, peaks at T+1.02 sec, and ends at T+1.65 sec. The T90 and T50 durations measured by the SGM data are 1.10 +/- 0.05 sec and 0.65 +/- 0.11 sec (40-1000 keV), respectively. The ground-processed light curve is available at http://cgbm.calet.jp/cgbm_trigger/ground/1390210300/index.html The CALET data used in this analysis are provided by the Waseda CALET Operation Center located at Waseda University.

GCN 35645 table
GRB_name	GRB240125A
GCN_number	35645
Detection_method	CALET
Circular_text	TITLE: GCN CIRCULAR NUMBER: 35645 SUBJECT: GRB 240125A: GRBAlpha detection DATE: 24/01/28 17:29:33 GMT FROM: Marianna Dafčíková at Masaryk University <500025@mail.muni.cz> M. Dafcikova, J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner (Masaryk U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), N. Husarikova, F. Munz , M. Topinka, M. Kolar, L. Szakszonova, J.-P. Breuer, F. Hroch (Masaryk U.), T. Urbanec, M. Kasal, A. Povalac (Brno U. of Technology), J. Hudec, J. Kapus, M. Frajt (Spacemanic s.r.o), R. Laszlo, M. Koleda (Needronix s.r.o), M. Smelko, P. Hanak, P. Lipovsky (Technical U. of Kosice), G. Galgoczi (Wigner Research Center/Eotvos U.), Y. Uchida, H. Poon, H. Matake (Hiroshima U.), N. Uchida (ISAS/JAXA), T. Bozoki (Eotvos U.), G. Dalya (Eotvos U.), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), G. Friss (Eotvos U.), Y. Fukazawa, K. Hirose (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), K. Kapas (Eotvos U.), L. L. Kiss (Konkoly Observatory), T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), J. Takatsy (Eotvos U.), K. Torigoe (Hiroshima U.), N. Kogiso, M. Yoneyama (Osaka Metropolitan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration. The short-duration GRB 240125A (Glowbug detection: GCN 35630; AstroSat detection: GCN 35637; CALET/CGBM detection: GCN 35639; Konus/Wind trigger at 2024-01-25 09:35:03.601 UT) was observed by the GRBAlpha 1U CubeSat (Pal et al. 2023, A&A, 677, 40; arXiv:2302.10048). The subthreshold detection was confirmed at the peak time 2024-01-25 09:35:00 UTC. The T90 duration measured by GRBAlpha is 1 s and the overall significance during T90 reaches 4.4 sigma. The light curve obtained by GRBAlpha is available here: https://grbalpha.konkoly.hu/static/share/GRB240125A_GCN.pdf All GRBAlpha detections are listed at: https://monoceros.physics.muni.cz/hea/GRBAlpha/ GRBAlpha, launched on 2021 March 22, is a demonstration mission for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). The detector of GRBAlpha consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~50 keV to ~1000 keV. To increase the duty cycle and the downlink rate, the upgrade of the on-board data acquisition software stack is in progress. The ground segment is also supported by the radio amateur community and it takes advantage of the SatNOGS network for increased data downlink volume.

GCN 35699 table
GRB_name	GRB240125A
GCN_number	35699
Detection_method	Konus-Wind Det
t_trigger	9:35:03.601 UTC
Circular_text	TITLE: GCN CIRCULAR NUMBER: 35699 SUBJECT: Konus-Wind detection of GRB 240125A DATE: 24/02/07 14:51:18 GMT FROM: Dmitry Svinkin at Ioffe Institute A. Ridnaia, D. Frederiks, A. Lysenko, D. Svinkin, A. Tsvetkova, M. Ulanov, and T. Cline, on behalf of the Konus-Wind team, report: The short-duration GRB 240125A (Glowbug gamma-ray detection: Cheung et al., GCN 35630; AstroSat CZTI detection: Joshi et al., GCN 35637; CALET CGBM detection: Marrocchesi et al., GCN 35639; GRBAlpha detection: Dafcikova et al., GCN 35645; IPN triangulation: Kozyrev et al., GCN 35652) triggered Konus-Wind at T0=34503.601 s UT (09:35:03.601). The burst light curve shows a multipeaked structure which starts at ~T0-0.5 s and has a total duration of ~1.0 s. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB240125_T34503/ As observed by Konus-Wind, the burst had a fluence of 4.79(-1.52,+5.06)x10^-6 erg/cm2, and a 16-ms peak flux, measured from T0-0.220 s, of 1.13(-0.57,+1.27)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range). Since the main fraction of the burst emission was detected before the trigger, the spectral analysis was performed using the KW 3-channel light curve data. Modelling the KW 3-channel time-integrated spectrum (measured from T0-0.512 s to T0+0.448 s) by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep), yields alpha = 0.01(-0.59,+1.53) and Ep = 982(-418,+1876) keV. All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.