The peak flux of GRB 221009A measured with GRBAlpha

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216305%3A26220%2F23%3APU149314" target="_blank" >RIV/00216305:26220/23:PU149314 - isvavai.cz</a>

Nalezeny alternativní kódy

RIV/00216224:14310/23:00131591

Výsledek na webu

<a href="https://www.aanda.org/articles/aa/pdf/2023/09/aa46128-23.pdf" target="_blank" >https://www.aanda.org/articles/aa/pdf/2023/09/aa46128-23.pdf</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1051/0004-6361/202346128" target="_blank" >10.1051/0004-6361/202346128</a>

Jazyk výsledku

angličtina

Název v původním jazyce

The peak flux of GRB 221009A measured with GRBAlpha

Popis výsledku v původním jazyce

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 a ffected 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 F-p (ph) = 1300+1200 200 ph cm (-2) s (-1), or F-p (erg) = 5:7+3:7 0:7 +/- 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+1:4 0:3 +/- 10 (-2) erg cm (-2), or S (bol) = 4:9+0:8 0:5 +/- 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 E-bol (iso) = 2:8+0:8 0:5 +/- 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 L-p (iso) = 3 :7+2:5 0:5 +/- 10(52) erg s (-1), and the bolometric peak isotropic-equivalent luminosity was L-p;bol (iso) = 8:4(+2:5) (1:5 Chi) 10(52) erg s 1 (4 s scale) in the 1 10 000 keV range (rest frame). The peak emitted energy is E (*) (p) = E-p(1 + z) = 1120 +/- 470 keV. Our measurement of Lp;bol iso 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 o

Název v anglickém jazyce

The peak flux of GRB 221009A measured with GRBAlpha

Popis výsledku anglicky

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 a ffected 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 F-p (ph) = 1300+1200 200 ph cm (-2) s (-1), or F-p (erg) = 5:7+3:7 0:7 +/- 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+1:4 0:3 +/- 10 (-2) erg cm (-2), or S (bol) = 4:9+0:8 0:5 +/- 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 E-bol (iso) = 2:8+0:8 0:5 +/- 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 L-p (iso) = 3 :7+2:5 0:5 +/- 10(52) erg s (-1), and the bolometric peak isotropic-equivalent luminosity was L-p;bol (iso) = 8:4(+2:5) (1:5 Chi) 10(52) erg s 1 (4 s scale) in the 1 10 000 keV range (rest frame). The peak emitted energy is E (*) (p) = E-p(1 + z) = 1120 +/- 470 keV. Our measurement of Lp;bol iso 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 o

Druh

J_imp - Článek v periodiku v databázi Web of Science

CEP obor

—

OECD FORD obor

10308 - Astronomy (including astrophysics,space science)

Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2023

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

Název periodika

ASTRONOMY & ASTROPHYSICS

ISSN

0004-6361

e-ISSN

1432-0746

Svazek periodika

677

Číslo periodika v rámci svazku

neuvedeno

Stát vydavatele periodika

FR - Francouzská republika

Počet stran výsledku

7

Strana od-do

1-7

Kód UT WoS článku

001073813400004

EID výsledku v databázi Scopus

2-s2.0-85170829752