The most probable host of CHIME FRB 190425A, associated with binary neutron star merger GW190425, and a late-time transient search. Issue 2 (9th December 2022)

• Record Type: Journal Article
• Authors: Panther, Fiona H; Anderson, Gemma E; Bhandari, Shivani; Goodwin, Adelle J; Hurley-Walker, Natasha; James, Clancy W; Kawka, Adela; Ai, Shunke; Kovalam, Manoj; Moroianu, Alexandra; Wen, Linqing; Zhang, Bing
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 519:Issue 2(2023)
• Page Start: 2235
• Page End: 2250
• Publication Date: 2022-12-09
• Subjects: galaxies: individual: UGC10667 -- fast radio bursts -- neutron star mergers; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stac3597
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: The identification and localization of fast radio bursts (FRBs) to their host galaxies have revealed important details about the progenitors of these mysterious, millisecond-long bursts of coherent radio emission. In this work, we study the most probable host galaxy of the apparently non-repeating CHIME/FRB event FRB 20190425A – a particularly high-luminosity, low-dispersion measure event that was demonstrated in a recent paper to be temporally and spatially coincident with the LIGO-Virgo-KAGRA binary neutron star merger GW190425, suggesting an astrophysical association ( p -value 0.0052). In this paper, we remain agnostic to this result, and we confirm UGC10667 as the most probable host galaxy of FRB 20190425A, demonstrating that the host galaxies of low-dispersion measure, one-off CHIME FRBs can be plausibly identified. We then perform multiwavelength observations to characterize the galaxy and search for any afterglow emission associated with the FRB and its putative GW counterpart. We find no radio or optical transient emission in our observations $2.5\, \mathrm{yr}$ post-burst. UGC10667 is a spiral galaxy at z ∼ 0.03, dominated by an old stellar population. We find no evidence of a large population of young stars, with nebular emission dominated by star formation at a rate of $1\!-\!2\, ~\mathrm{M_\odot \, yr^{-1}}$ . While we cannot rule out a young magnetar as the origin of FRB 20190425A, our observations are consistent with an origin in a long delay-time neutron star binary merger.