The peak-flux of GRB 221009A measured with GRBAlpha
Creators: name: Ripa, Jakub
name: Takahashi, Hiromitsu
name: Fukazawa, Yasushi
name: Werner, Norbert
name: Munz, Filip
name: Pal, Andras
name: Ohno, Masanori
name: Dafcikova, Marianna
name: Meszaros, Laszlo
name: Csak, Balazs
name: Husarikova, Nikola
name: Kolar, Martin
name: Galgoczi, Gabor
name: Breuer, Jean-Paul
name: Hroch, Filip
name: Hudec, Jan
name: Kapus, Jakub
name: Frajt, Marcel
name: Rezenov, Maksim
name: Laszlo, Robert
name: Koleda, Martin
name: Smelko, Miroslav
name: Hanak, Peter
name: Lipovsky, Pavol
name: Urbanec, Tomas
name: Kasal, Miroslav
name: Povalac, Ales
name: Uchida, Yuusuke
name: Poon, Helen
name: Matake, Hiroto
name: Nakazawa, Kazuhiro
name: Uchida, Nagomi
name: Bozoki, Tamas
name: Dalya, Gergely
name: Enoto, Teruaki
name: Frei, Zsolt
name: Friss, Gergely
name: Ichinohe, Yuto
name: Kapas, Kornel
name: Kiss, Laszlo L.
name: Mizuno, Tsunefumi
name: Odaka, Hirokazu
name: Takatsy, Janos
name: Topinka, Martin
name: Torigoe, Kento
Publisher: name: arXiv
Year: 2023
Subjects: subject: High Energy Astrophysical Phenomena (astro-ph.HE)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: The brightest gamma-ray burst ever observed, long-duration GRB 221009A, was detected by GRBAlpha nano-satellite without saturation. We present light curves of the prompt emission in 13 energy bands, from 80 keV to 950 keV, and perform a spectral analysis to calculate the peak flux and peak isotropic-equivalent luminosity. 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. We found that the peak flux in the $80-800$ keV range (observer frame) was $F_{\rm{ph}}^{\rm{p}}=1300_{-200}^{+1200}$ ph cm$^{-2}$s$^{-1}$ or $F_{\rm{erg}}^{\rm{p}}=5.7_{-0.7}^{+3.7}\times10^{-4}$ erg cm$^{-2}$s$^{-1}$ and the fluence in the same energy range of the first GRB episode lasting 300 s, which was observable by GRBAlpha, was $S=2.2_{-0.3}^{+1.4}\times10^{-2}$ erg cm$^{-2}$ or $S^{\rm{bol}}=4.9_{-0.5}^{+0.8}\times10^{-2}$ erg cm$^{-2}$ for the extrapolated range of $0.9-8,690$ keV. We infer the isotropic-equivalent released energy of the first GRB episode to be $E_{\rm{iso}}^{\rm{bol}}=2.8_{-0.5}^{+0.8}\times10^{54}$ 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 $L_{\rm{iso}}^{\rm{p}}=3.7_{-0.5}^{+2.5}\times10^{52}$ erg s$^{-1}$ and the bolometric peak isotropic-equivalent luminosity was $L_{\rm{iso}}^{\rm{p,bol}}=8.4_{-1.5}^{+2.5}\times10^{52}$ erg s$^{-1}$ (4 s scale) in the $1-10,000$ keV range (rest frame). The peak emitted energy is $E_p^\ast=E_p(1+z)=1120\pm470$ keV. Our measurement of $L_{\rm{iso}}^{\rm{p,bol}}$ is consistent with the Yonetoku relation. It is possible that, due to the spectral evolution of this GRB and orientation of GRBAlpha at the peak time, the true values of peak flux, fluence, $L_{\rm{iso}}$, and $E_{\rm{iso}}$ are even higher. [abridged]
description: 7 pages, 7 figures, 1 table, accepted for publication in Astronomy &amp; Astrophysics