http://arxiv.org/abs/2005.08112
Binary neutron star (BNS) mergers are one of the proposed origins for both repeating and non-repeating fast radio bursts (FRBs), which associates FRBs with gravitational waves and short gamma-ray bursts (GRBs). In this work, we explore detectability of radio counterparts to an FRB by calculating the radio afterglow flux powered by the two components: a relativistic jet and a slower isotropic ejecta from a BNS merger. Detection probability of a radio afterglow for a FRB is calculated as a function of the source redshift, observing time, and flux sensitivity, assuming that FRBs are not strongly beamed. The model parameter distributions inferred from short GRB afterglows are adopted. We find that the detection probability for an FRB at $z=0.5$ is 3.7 and 4.1% for the jet and isotropic components, respectively, when observed at the timing of their peak flux ($\sim$10 days and 1 year) with a typical sensitivity of 10 $\mu$Jy. The probability increases to 10 and 14%, respectively, with $\sim$1 $\mu$Jy sensitivity achievable with future facilities (e.g. SKA). In particular for the repeating FRB 180916.J0158+65, we find a high chance of detection (60% at 10 $\mu$Jy sensitivity) for the isotropic component that would peak around $\sim$10 years after the merger, as a natural consequence of its close distance ($z=0.03$). Therefore a long term radio monitoring of persistent radio emission for this object is important. The detection probability is similar for the jet component, though the peak time ($\sim$200 days) has likely already passed for this FRB.
H. Lin and T. Totani
Tue, 19 May 20
41/92
Comments: 7 pages, 3 figures. Submitted to MNRAS
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