Luminosity–duration relations and luminosity functions of repeating and non-repeating fast radio bursts. Issue 2 (9th April 2020)

• Record Type: Journal Article
• Authors: Hashimoto, Tetsuya; Goto, Tomotsugu; Wang, Ting-Wen; Kim, Seong Jin; Ho, Simon C-C; On, Alvina Y L; Lu, Ting-Yi; Santos, Daryl Joe D
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 494:Issue 2(2020)
• Page Start: 2886
• Page End: 2904
• Publication Date: 2020-04-09
• Subjects: binaries: general -- stars: luminosity function, mass function -- stars: magnetars -- stars: magnetic field -- stars: neutron; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa895
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Fast radio bursts (FRBs) are mysterious radio bursts with a time-scale of approximately milliseconds. Two populations of FRB, namely repeating and non-repeating FRBs, are observationally identified. However, the differences between these two and their origins are still cloaked in mystery. Here we show the time-integrated luminosity–duration ( L ν – w int, rest ) relations and luminosity functions (LFs) of repeating and non-repeating FRBs in the FRB Catalogue project. These two populations are obviously separated in the L ν - w int, rest plane with distinct LFs, i.e. repeating FRBs have relatively fainter L ν and longer w int, rest with a much lower LF. In contrast with non-repeating FRBs, repeating FRBs do not show any clear correlation between L ν and w int, rest . These results suggest essentially different physical origins of the two. The faint ends of the LFs of repeating and non-repeating FRBs are higher than volumetric occurrence rates of neutron star (NS) mergers and accretion-induced collapse (AIC) of white dwarfs (WDs), and are consistent with those of soft gamma-ray repeaters (SGRs), Type Ia supernovae (SNe Ia), magnetars, and WD mergers. This indicates two possibilities: either (i) faint non-repeating FRBs originate in NS mergers or AIC and are actually repeating during the lifetime of the progenitor, or (ii) faint non-repeating FRBs originate in any of SGRs, SNe Ia, magnetars, and WD mergers. The bright ends of LFs of repeating and non-repeating FRBs are lower than any candidates of progenitors, suggesting that bright FRBs are produced from a very small fraction of the progenitors regardless of the repetition. Otherwise, they might originate in unknown progenitors.