GRB 240125A
GCN Circular 35699
Subject
Konus-Wind detection of GRB 240125A
Date
2024-02-07T14:51:18Z (2 years ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
Via
legacy email
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.
GCN Circular 35652
Subject
IPN triangulation of GRB 240125A (short)
Date
2024-01-29T20:50:21Z (2 years ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
Via
legacy email
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 35645
Subject
GRB 240125A: GRBAlpha detection
Date
2024-01-28T17:29:33Z (2 years ago)
From
Marianna Dafčíková at Masaryk University <500025@mail.muni.cz>
Via
Web form
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 Circular 35639
Subject
GRB 240125A: CALET Gamma-Ray Burst Monitor detection
Date
2024-01-27T00:35:22Z (2 years ago)
From
Yuta Kawakubo at Louisiana State University <kawakubo1@lsu.edu>
Via
Web form
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 35637
Subject
GRB 240125A: AstroSat CZTI detection of a short burst
Date
2024-01-26T08:30:34Z (2 years ago)
From
Gaurav Waratkar at IIT Bombay <gauravwaratkar@iitb.ac.in>
Via
Web form
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 35630
Subject
GRB 240125A (short): Glowbug gamma-ray detection
Date
2024-01-25T18:08:11Z (2 years ago)
From
C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>
Via
Web form
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
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