Issue |
A&A
Volume 680, December 2023
|
|
---|---|---|
Article Number | A45 | |
Number of page(s) | 29 | |
Section | Astrophysical processes | |
DOI | https://doi.org/10.1051/0004-6361/202347298 | |
Published online | 12 December 2023 |
The short gamma-ray burst population in a quasi-universal jet scenario⋆
1
INAF – Osservatorio Astronomico di Brera, Via Emilio Bianchi 46, 23807 Merate (LC), Italy
e-mail: om.salafia@inaf.it
2
INFN – sezione di Milano-Bicocca, Piazza della Scienza 3, 20126 Milano (MI), Italy
3
Department of Astrophysics/IMAPP, Radboud University, 6525 AJ Nijmegen, The Netherlands
4
School of Physics and Astronomy, Monash University, Clayton, Victoria 3800, Australia
5
ARC Center of Excellence for Gravitational Wave Discovery – OzGrav, Hawthorn, Australia
Received:
27
June
2023
Accepted:
7
September
2023
We present a model of the short gamma-ray burst (SGRB) population under a ‘quasi-universal jet’ scenario in which jets can differ somewhat in their on-axis peak prompt emission luminosity, Lc, but share a universal angular luminosity profile, ℓ(θv) = L(θv)/Lc, as a function of the viewing angle, θv. The model was fitted, through a Bayesian hierarchical approach inspired by gravitational wave (GW) population analyses, to three observed SGRB samples simultaneously: the Fermi/GBM sample of SGRBs with spectral information available in the catalogue (367 events); a flux-complete sample of 16 Swift/BAT SGRBs that are also detected by the GBM and have a measured redshift; and a sample of SGRBs with a binary neutron star (BNS) merger counterpart, which only includes GRB 170817A at present. Particular care was put into modelling selection effects. The resulting model, which reproduces the observations, favours a narrow jet ‘core’ with half-opening angle θc = 2.1−1.4+2.4 deg (uncertainties hereon refer to 90% credible intervals from our fiducial ‘full sample’ analysis) whose peak luminosity, as seen on-axis, is distributed as a power law, p(Lc) ∝ Lc−A with A = 3.2−0.4+0.7, above a minimum isotropic-equivalent luminosity, Lc⋆ = 5−2+11 × 1051 erg s−1. For viewing angles larger than θc, the luminosity profile scales as a single power law, l ∝ θv−αL with αL = 4.7−1.4+1.2, with no evidence of a break, despite the model allowing for it. While the model implies an intrinsic ‘Yonetoku’ correlation between L and the peak photon energy, Ep, of the spectral energy distribution, its slope is somewhat shallower, Ep ∝ L0.4 ± 0.2, than the apparent one, and the normalisation is offset towards larger Ep due to selection effects. The implied local rate density of SGRBs (regardless of the viewing angle) is between about one hundred up to several thousand events per cubic gigaparsec per year, in line with the BNS merger rate density inferred from GW observations. Based on the model, we predict 0.2 to 1.3 joint GW+SGRB detections per year by the advanced GW detector network and Fermi/GBM during the O4 observing run.
Key words: relativistic processes / gamma-ray burst: general / methods: statistical
The source code and posterior samples behind this work are publicly available at https://github.com/omsharansalafia/grbpop.
© The Authors 2023
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
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