The peak flux of GRB 221009A measured with GRBAlpha
The result's identifiers
Result code in 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>
Alternative codes found
RIV/00216224:14310/23:00131591
Result on the web
<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>
Alternative languages
Result language
angličtina
Original language name
The peak flux of GRB 221009A measured with GRBAlpha
Original language 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 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
Czech name
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Czech description
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Classification
Type
J<sub>imp</sub> - Article in a specialist periodical, which is included in the Web of Science database
CEP classification
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OECD FORD branch
10308 - Astronomy (including astrophysics,space science)
Result continuities
Project
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Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace
Others
Publication year
2023
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů
Data specific for result type
Name of the periodical
ASTRONOMY & ASTROPHYSICS
ISSN
0004-6361
e-ISSN
1432-0746
Volume of the periodical
677
Issue of the periodical within the volume
neuvedeno
Country of publishing house
FR - FRANCE
Number of pages
7
Pages from-to
1-7
UT code for WoS article
001073813400004
EID of the result in the Scopus database
2-s2.0-85170829752