Population modelling of FRBs from intrinsic properties
Abstract
We develop a formalism to estimate the intrinsic properties of FRBs from observations by assuming a fixed DM contribution from a MWlike host galaxy, pulse temporal broadening models for turbulent plasma and a flat FRB energy spectrum. We then perform Monte Carlo simulations to constrain the properties of the FRB source, its host galaxy and scattering in the intervening plasma from the current observations. The typical scatter broadening of the intrinsic pulse is found to be considerably small $\lesssim 10^{2}1\ {\rm ms}$ with the ISM contribution suppressed significantly relative to IGM. The intrinsic width for nonrepeating FRBs is broadened by a factor $\sim 23$ on average primarily due to dispersive smearing. The host galaxy DM contribution is likely to be smaller than the Galactic contribution and the FRB energy decreases significantly at high frequencies. We find that the FRB spatial density increases upto redshift $\sim 0.51.0$ and then drops significantly at larger distances. We obtain the energy distribution for FRB 121102 with repetition rate $\sim 0.10.3\ {\rm hr^{1}}$ and exponential energy cutoff that is significantly smaller compared to typical FRB energies. We find that the probability of observing none of the other FRBs to be repeating at Parkes is $\sim 0.81.0$ with the current followup data insufficient to suggest more than one class of FRB progenitors.
 Publication:

arXiv eprints
 Pub Date:
 February 2019
 arXiv:
 arXiv:1902.10225
 Bibcode:
 2019arXiv190210225B
 Keywords:

 Astrophysics  High Energy Astrophysical Phenomena
 EPrint:
 20 pages, 8 figures, 7 tables