The Fast Radio Burst Dispersion Measure Distribution

TL;DR

This study models the dispersion measure distribution of fast radio bursts detected by ASKAP and Parkes, revealing insights into their population characteristics and evolution, with implications for understanding their origins and the intergalactic medium.

Contribution

It introduces a joint modeling approach for FRB DM distributions from different telescopes, constraining population parameters and evolution models with observational data.

Findings

Best-fit spectral index $eta$ around 2.2

Power-law index $eta$ near 2.0 for energy distribution

No evidence of rapid evolution beyond star formation rate

Abstract

We compare the dispersion measure (DM) statistics of FRBs detected by the ASKAP and Parkes radio telescopes. We jointly model their DM distributions, exploiting the fact that the telescopes have different survey fluence limits but likely sample the same underlying population. After accounting for the effects of instrumental temporal and spectral resolution of each sample, we find that a fit between the modelled and observed DM distribution, using identical population parameters, provides a good fit to both distributions. Assuming a one-to-one mapping between DM and redshift for an homogeneous intergalactic medium (IGM), we determine the best-fit parameters of the population spectral index, $\hat{\alpha}$, and the power-law index of the burst energy distribution, $\hat{\gamma}$, for different redshift evolutionary models. Whilst the overall best-fit model yields $\hat{\alpha}=2.2_{-1.0}^{+0.7}$ and $\hat{\gamma}=2.0_{-0.1}^{+0.3}$, for a strong redshift evolutionary model, when we admit the further constraint of $\alpha=1.5$ we favour the best fit $\hat{\gamma}=1.5 \pm 0.2$ and the case of no redshift evolution. Moreover, we find no evidence that the FRB population evolves faster than linearly with respect to the star formation rate over the DM (redshift) range for the sampled population.