GRB luminosity function synthesized from Swift/BAT , Fermi/GBM and Konus-Wind data
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ORIGINAL ARTICLE
GRB luminosity function synthesized from Swift/BAT, Fermi/GBM and Konus-Wind data H. Zitouni1
· N. Guessoum2 · W.J. Azzam3 · Y. Benturki1
Received: 13 May 2020 / Accepted: 9 November 2020 / Published online: 17 November 2020 © Springer Nature B.V. 2020
Abstract We study the luminosity function of long gammaray bursts (LGRBs) using the peak flux obtained from three LGRB samples with known redshifts: (a) a sample of 251 LGRBs from the Swift/BAT satellite/instrument; (b) a sample of 37 LGRBs from the Fermi/GBM telescope; (c) a sample of 152 GRBs from the Konus-Wind instrument. For the Swift/BAT and Fermi/GBM samples, we use data available on the Swift Burst Analyser websites (http://www.swift.ac. uk/burst_analyser; (Evans at al. in Astron. Astrophys. 519: 102, 2010)) and (http://swift.gsfc.nasa.gov/archive/grb/ table/) and on the Fermi website (https://heasarc.gsfc.nasa. gov/W3Browse/fermi/fermigbrst.html; (Gruber et al. in Astrophys. J. Suppl. Ser. 211(1):12, 2014; von Kienlin et al. in Astrophys. J. Suppl. Ser. 211(1):13, 2014; Bhat et al. in Astrophys. J. Suppl. Ser. 223(2):28, 2016)) to calculate the luminosity at the peak of the flux by using a cut-off powerlaw spectrum (CPL). For the Konus-Wind sample, we use the Yonetoku correlation relationship (Yonetoku et al. in Publ. Astron. Soc. Jpn. 62:1495, 2010) to determine the isotropic luminosity from the energy at the peak of the flux measured in the source frame (Minaev and Pozanenko in Mon. Not. R. Astron. Soc. 492(2):1919, 2019). With these three sam-
B H. Zitouni
[email protected] N. Guessoum [email protected] W.J. Azzam [email protected]
1
PTEA Laboratory, Faculty of Science, Dr Yahia Fares University, Médéa, Algeria
2
Department of Physics, College of Arts & Sciences, American University of Sharjah, Sharjah, UAE
3
Department of Physics, College of Science, University of Bahrain, Sakheer, Bahrain
ples (totalling 439 GRBs), we use the Monte Carlo method to synthesize 10,000 “artificial” GRBs similar to each real GRB by considering that each physical quantity observed obeys a normal distribution, where the tabulated value and uncertainty represent the mean and the 3σ error. The results obtained for the luminosity function from our data samples are consistent with those published in previous works. Keywords Gamma-rays bursts · Luminosity function · Statistical methods
1 Introduction Gamma-ray bursts (GRBs) are extremely powerful explosions that involve either the death of massive stars or the merger of compact stellar objects. The equivalent isotropic energy of GRBs can exceed 1054 erg, and their nonthermal spectra peak between 10 and 104 keV (e.g. Atteia et al. (2017)). Their light curves display intense pulses that can last anywhere from less than a second to hundreds of seconds, they are often irregular and sometimes include multiple pulses. Although the radiation emitted by GRBs is believed to come out mainly through jets (with collisions inside), the precise formation mechanism behind these jets is not fully unders
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