# Are all fast radio bursts repeating sources?

## TL;DR

This study uses Monte-Carlo simulations to explore whether all fast radio bursts (FRBs) are repeating sources, analyzing different models of repetition and energy distribution, and comparing results with observational data.

## Contribution

It introduces a comprehensive simulation framework for repeating FRBs considering various energy and wait-time distributions, and constrains their population characteristics based on observational limits.

## Key findings

- Cannot rule out a single FRB population with current data.
- FRBs 171020 and 010724 likely do not repeat like FRB 121102.
- Energy distribution slope constrained to -2.0 < γ < -1.0.

## Abstract

We present Monte-Carlo simulations of a cosmological population of repeating fast radio burst (FRB) sources whose comoving density follows the cosmic star formation rate history. We assume a power-law model for the intrinsic energy distribution for each repeating FRB source located at a randomly chosen position in the sky and simulate their dispersion measures (DMs) and propagation effects along the chosen lines-of-sight to various telescopes. In one scenario, an exponential distribution for the intrinsic wait times between pulses is chosen, and in a second scenario we model the observed pulse arrival times to follow a Weibull distribution. For both models we determine whether the FRB source would be deemed a repeater based on the telescope sensitivity and time spent on follow-up observations. We are unable to rule out the existence of a single FRB population based on comparisons of our simulations with the longest FRB follow-up observations performed. We however rule out the possibility of FRBs 171020 and 010724 repeating with the same rate statistics as FRB 121102 and also constrain the slope of a power-law fit to the FRB energy distribution to be $-2.0 < \gamma <-1.0$. All-sky simulations of repeating FRB sources imply that the detection of singular events correspond to the bright tail-end of the adopted energy distribution due to the combination of the increase in volume probed with distance, and the position of the burst in the telescope beam.