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@article{2306578,
author = {Řípa, Jakub and Takahashi, Hiromitsu and Fukazawa, Yasushi and Werner, Norbert and Münz, Filip and Pál, András and Ohno, Masanori and Dafčíková, Marianna and Mészáros, László and Csák, Balázs and Husáriková, Nikola and Kolář, Martin and Galgóczi, Gábor and Riffald Souza Breuer, JeanandPaul Bernhard and Hroch, Filip and Hudec, Ján and Kapuš, Jakub and Frajt, Marcel and Rezenov, Maksim and Laszlo, Robert and Koleda, Martin and Šmelko, Miroslav and Hanák, Peter and Lipovský, Pavol and Urbanec, Tomáš and Kasal, Miroslav and Povalač, Aleš and Uchida, Yuusuke and Poon, Helen and Matake, Hiroto and Nakazawa, Kazuhiro and Uchida, Nagomi and Bozóki, Tamás and Dálya, Gergely and Enoto, Teruaki and Frei, Zsolt and Friss, Gergely and Ichinohe, Yuto and Kapás, Kornél and Kiss, László L. and Mizuno, Tsunefumi and Odaka, Hirokazu and Takátsy, János and Topinka, Martin and Torigoe, Kento},
article_number = {September},
doi = {http://dx.doi.org/10.1051/0004-6361/202346128},
keywords = {gamma-ray burst: individual: GRB 221009A},
language = {eng},
issn = {0004-6361},
journal = {Astronomy & Astrophysics},
title = {The peak flux of GRB 221009A measured with GRBAlpha},
url = {https://doi.org/10.1051/0004-6361/202346128},
volume = {677},
year = {2023}
}
TY - JOUR
ID - 2306578
AU - 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
PY - 2023
TI - The peak flux of GRB 221009A measured with GRBAlpha
JF - Astronomy & Astrophysics
VL - 677
IS - September
SP - 1-7
EP - 1-7
PB - EDP Sciences
SN - 00046361
KW - gamma-ray burst: individual: GRB 221009A
UR - https://doi.org/10.1051/0004-6361/202346128
N2 - 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.
ER -
ŘÍPA, Jakub, Hiromitsu TAKAHASHI, Yasushi FUKAZAWA, Norbert WERNER, Filip MÜNZ, András PÁL, Masanori OHNO, Marianna DAFČÍKOVÁ, László MÉSZÁROS, Balázs CSÁK, Nikola HUSÁRIKOVÁ, Martin KOLÁŘ, Gábor GALGÓCZI, Jean-Paul Bernhard RIFFALD SOUZA BREUER, Filip HROCH, Ján HUDEC, Jakub KAPUŠ, Marcel FRAJT, Maksim REZENOV, Robert LASZLO, Martin KOLEDA, Miroslav ŠMELKO, Peter HANÁK, Pavol LIPOVSKÝ, Tomáš URBANEC, Miroslav KASAL, Aleš POVALAČ, Yuusuke UCHIDA, Helen POON, Hiroto MATAKE, Kazuhiro NAKAZAWA, Nagomi UCHIDA, Tamás BOZÓKI, Gergely DÁLYA, Teruaki ENOTO, Zsolt FREI, Gergely FRISS, Yuto ICHINOHE, Kornél KAPÁS, László L. KISS, Tsunefumi MIZUNO, Hirokazu ODAKA, János TAKÁTSY, Martin TOPINKA a Kento TORIGOE. The peak flux of GRB 221009A measured with GRBAlpha. \textit{Astronomy \&{} Astrophysics}. EDP Sciences, 2023, roč.~677, September, s.~1-7. ISSN~0004-6361. Dostupné z: https://dx.doi.org/10.1051/0004-6361/202346128.
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