GRB luminosity function synthesized from Swift/BAT, Fermi/GBM and Konus-Wind data

We study the luminosity function of long gamma-ray 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 power-law 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 samples (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 $3\sigma$ error. The results obtained for the luminosity function from our data samples are consistent with those published in previous works.