Gamma-ray Burst 240125A

(All information courtesy of the instrument teams.)

Previous IAU Circulars

none

Results of Observations

GCN Circular #35630
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: =20 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). =20 Using an adaptive window with a resolution of 32-ms, the burst onset is det= ermined 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-peak= ed structure. =20 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/d= E~E^x of x=3D0.8 and a cutoff energy ("Epeak") of 705 keV. The modeled 10-= 10000 keV fluence is 3.2e-06 erg/cm^2. =20 The best-fit localization is RA, Decl. (J2000, deg) =3D 153.4, 48.7 with a = radius of 9.3 deg (95% confidence), with a highly uncertain systematic unce= rtainty. =20 The analysis results presented here are preliminary and use a response func= tion that lacks a detailed characterization of the surrounding passive stru= cture of the ISS. =20 Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost ga= mma-ray transient telescopes developed, built, and operated by the U.S. Nav= al 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=E2=80=99s 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 Circular #35637
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 Circular #35639
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 Circular #35645
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. Sza= kszonova, J.-P. Breuer, F. Hroch (Masaryk U.), T. Urbanec, M. Kasal, A. Po= valac (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. Lipovs= ky (Technical U. of Kosice), G. Galgoczi (Wigner Research Center/Eotvos U.)= , Y. Uchida, H. Poon, H. Matake (Hiroshima U.), N. Uchida (ISAS/JAXA), T. B= ozoki (Eotvos U.), G. Dalya (Eotvos U.), T. Enoto (Kyoto U.), Zs. Frei (Eot= vos U.), G. Friss (Eotvos U.), Y. Fukazawa, K. Hirose (Hiroshima U.), S. Hi= sadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), K. Kapas (Eotvos U.), L. L. Ki= ss (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 dete= ction: GCN 35637; CALET/CGBM detection: GCN 35639; Konus/Wind trigger at 20= 24-01-25 09:35:03.601 UT) was observed by the GRBAlpha 1U CubeSat (Pal et a= l. 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 signif= icance during T90 reaches 4.4 sigma.
The light curve obtained by GRBAlpha is available here: https://grbalpha.ko= nkoly.hu/static/share/GRB240125A_GCN.pdf
All GRBAlpha detections are listed at: https://monoceros.physics.muni.cz/he= a/GRBAlpha/=20 GRBAlpha, launched on 2021 March 22, is a demonstration mission for a futur= e CubeSat constellation (Werner et al. Proc. SPIE 2018). The detector of GR= BAlpha consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM ar= ray, covering the energy range from ~50 keV to ~1000 keV. To increase the d= uty cycle and the downlink rate, the upgrade of the on-board data acquisiti= on software stack is in progress. The ground segment is also supported by t= he radio amateur community and it takes advantage of the SatNOGS network fo= r increased data downlink volume.
GCN Circular #35652
A.S. Kozyrev, D.V. Golovin, M.L. Litvak, I.G. Mitrofanov, and A.B. Sanin on behalf of the HEND/Mars Odyssey team,
D. Svinkin, D. Frederiks, A. Lysenko, A. Ridnaia, and T. Cline on behalf of the Konus-Wind team,
G. Waratkar (IITB), J.Joshi (IUCAA), A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka University/IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) on behalf of the Astrosat-CZTI team,
S. Barthelmy, J. Cummings, H. Krimm, D. Palmer, and A. Tohuvavohu on behalf of the Swift-BAT team,
and
W. Boynton, C. Fellows, K. Harshman, H. Enos, R. Starr, and A.S. Gardner on on behalf of the GRS-Odyssey GRB team, report:
The short-duration GRB 240125A (Glowbug 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) was detected by Glowbug, Astrosat (CZTI) Konus-Wind, GRBAlpha, CALET (CGBM) and Mars-Odyssey (HEND) at about 34499 s UT (09:34:59).
We have triangulated it to a preliminary, 3 sigma error box whose coordinates are:
```
 -------------------------------
  RA(2000), deg   Dec(2000), deg
 -------------------------------
 Center:
  131.528          +66.846
 Corners:
  147.975          +59.476
  147.882          +59.456
   92.799          +68.770
   93.211          +68.871
 --------------------------------
```
The error box area is 1.85 sq. deg and its maximum dimension is 24.6 deg (the minimum one is 3.3 arcmin). The Sun distance was 132 deg.
This localization may be improved.
A triangulation map and HEALPix FITS file are posted at http://www.ioffe.ru/LEA/GRBs/GRB240125_T34503/IPN
The Konus-Wind time history and spectrum will be given in a forthcoming GCN Circular.
GCN Circular #35699
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.

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Jochen Greiner, last update: 07-Feb-2024 [Disclaimer]