On the association of GW190425 with its potential electromagnetic counterpart FRB 20190425A

Abstract

Recent work by Moroianu et al. (2022) has suggested that the binary neutron star (BNS) merger GW190425 might have a potential fast radio burst (FRB) counterpart association, FRB 20190425A, at the 2.8$σ$ level of confidence with a likely host galaxy association, namely UGC10667. The authors argue that the observations are consistent with a long-lived hypermassive neutron star (HMNS) that formed promptly after the BNS merger and was stable for approximately 2.5 hours before promptly collapsing into a black hole. Recently, Bhardwaj et al. (2023) conclusively associated FRB 20190425A with UGC10667, potentially providing a direct host galaxy candidate for GW190425. In this work, we examine the multi-messenger association based on the space-time localization overlaps between GW190425 and the FRB host galaxy UGC10667 and find that the odds for a coincident association are $\mathcal{O}(5)$. We validate this estimate by using a Gaussian Process (GP) density estimator. Assuming that the association is indeed real, we then perform Bayesian parameter estimation on GW190425 assuming that the BNS event took place in UGC10667. We find that the viewing angle of GW190425 excludes an on-axis system at $p(θ_v>30^o)\approx99.99$\%, highly favouring an off-axis system similar to GRB 170817A. We also find a slightly higher source frame total mass for the binary, namely, $m_{\rm{total}} = 3.42^{+0.34}_{-0.11} M_{\odot}$, leading to an increase on the probability of prompt collapse into a black hole and therefore disfavors the long-lived HMNS formation scenario. Given our findings, we conclude that the association between GW190425 and FRB 20190425A is disfavoured by current state-of-the-art gravitational-wave analyses.