The peak flux of GRB 221009A measured with GRBAlpha

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Authors	ŘÍPA Jakub TAKAHASHI Hiromitsu FUKAZAWA Yasushi WERNER Norbert MÜNZ Filip PÁL András OHNO Masanori DAFČÍKOVÁ Marianna MÉSZÁROS László CSÁK Balázs HUSÁRIKOVÁ Nikola KOLÁŘ Martin GALGÓCZI Gábor RIFFALD SOUZA BREUER Jean-Paul Bernhard HROCH Filip HUDEC Ján KAPUŠ Jakub FRAJT Marcel REZENOV Maksim LASZLO Robert KOLEDA Martin ŠMELKO Miroslav HANÁK Peter LIPOVSKÝ Pavol URBANEC Tomáš KASAL Miroslav POVALAČ Aleš UCHIDA Yuusuke POON Helen MATAKE Hiroto NAKAZAWA Kazuhiro UCHIDA Nagomi BOZÓKI Tamás DÁLYA Gergely ENOTO Teruaki FREI Zsolt FRISS Gergely ICHINOHE Yuto KAPÁS Kornél KISS László L. MIZUNO Tsunefumi ODAKA Hirokazu TAKÁTSY János TOPINKA Martin TORIGOE Kento
Year of publication	2023
Type	Article in Periodical
Magazine / Source	Astronomy & Astrophysics
MU Faculty or unit	Faculty of Science
Citation
Web	https://arxiv.org/abs/2302.10047 https://doi.org/10.1051/0004-6361/202346128
Doi	http://dx.doi.org/10.1051/0004-6361/202346128
Keywords	gamma-ray burst: individual: GRB 221009A
Description	Context. On 2022 October 9 the brightest gamma-ray burst (GRB) ever observed lit up the high-energy sky. It was detected by a multitude of instruments, attracting the close attention of the GRB community, and saturated many detectors. Aims. GRBAlpha, a nano-satellite with a form factor of a 1U CubeSat, detected this extraordinarily bright long-duration GRB, GRB 221009A, without saturation but affected by pile-up. We present light curves of the prompt emission in 13 energy bands, from 80 keV to 950 keV, and performed a spectral analysis to calculate the peak flux and peak isotropic-equivalent luminosity. Methods. Since the satellite’s attitude information is not available for the time of this GRB, more than 200 incident directions were probed in order to find the median luminosity and its systematic uncertainty. Results. We find that the peak flux in the 80 - 800 keV range (observer frame) was Fphp = 1300-200+1200 ph cm-2 s-1, or Fergp = 5.7-0.7+3.7 × 10-4 erg cm-2 s-1, and the fluence in the same energy range of the first GRB episode, which lasted 300 s and was observable by GRBAlpha, was S = 2.2-0.3+1.4 × 10-2 erg cm-2, or Sbol = 4.9-0.5+0.8 × 10-2 erg cm-2 for the extrapolated range of 0.9 - 8690 keV. We infer the isotropic-equivalent released energy of the first GRB episode to be Eisobol = 2.8-0.5+0.8 × 1054 erg in the 1 - 10 000 keV band (rest frame at z = 0.15). The peak isotropic-equivalent luminosity in the 92 - 920 keV range (rest frame) was Lisop = 3.7-0.5+2.5 × 1052 erg s-1, and the bolometric peak isotropic-equivalent luminosity was Lisop,bol = 8.4-1.5+2.5 × 1052 erg s-1 (4 s scale) in the 1 - 10 000 keV range (rest frame). The peak emitted energy is Ep* = Ep(1+z) = 1120 ± 470 keV. Our measurement of Lisop,bol is consistent with the Yonetoku relation. It is possible that, due to the spectral evolution of this GRB and the orientation of GRBAlpha at the peak time, the true values of peak flux, fluence, Liso, and Eiso are even higher.
Related projects:	MUNI Award in Science and Humanities 3 Integrated Activities for the High Energy Astrophysics Domain