Long and Short Fast Radio Bursts are Different from Repeating and Non-repeating Transients

TL;DR

This study analyzes 133 FRBs, revealing differences in properties between long and short, repeating and non-repeating bursts, with implications for their classification and detection at high redshifts.

Contribution

It systematically investigates observational properties of FRBs, introducing classifications based on duration and frequency, and explores their correlations and energy distributions.

Findings

Bimodal pulse width distribution at frequencies below 1 GHz.

Short FRBs at higher frequencies are generally shorter.

Long FRBs are more energetic than short FRBs.

Abstract

We collect 133 Fast Radio Bursts (FRBs), including 110 non-repeating and 23 repeating ones, and systematically investigate their observational properties. To check the frequency dependence of FRB classifications, we define our samples with a central frequency below/above 1GHz as subsample I/II. We find that there is a clear bimodal distribution of pulse width for the subsample I. And If we classify FRBs into short FRBs (\emph{s}FRBs) ($<$100 ms) and long FRBs (\emph{l}FRBs) ($>$100 ms) as done for short and long Gamma-Ray Bursts (GRBs), the \emph{s}FRBs at higher central frequency are commonly shorter than those at lower central frequency not only for non-repeating but also repeating \emph{s}FRBs. Secondly, we find that fluence and peak flux density are correlated with a power law relation of $F \varpropto S{^{\gamma}_{p,obs}}$ for both \emph{s}FRBs and \emph{l}FRBs whose distributions are obviously different. Thirdly, the \emph{l}FRBs with isotropic energies ranging from $10^{42}$ to $10^{44}$ erg are more energetic than the \emph{s}FRBs in the $F- DM_{EX}$ plane, indicating that they are two representative types. Finally, it is interestingly note that the peak flux density behaves an independence on the redshift when the distance of the FRBs becomes far enough, which is similar to the scenario of peak flux evolving with redshift in the field of GRBs. We predict that fainter FRBs at higher redshift of $z>2$ can be successfully detected by FAST and SKA in the near future.