Black hole--neutron star and binary neutron star mergers from Population III and II stars

Population III (Pop. III) stars are expected to be massive and to undergo minimal mass loss due to their lack of metals, making them ideal progenitors of black holes and neutron stars. Here, we investigate the formation and properties of binary neutron star (BNS) and black hole--neutron star (BHNS) mergers originating from Pop. III stars, and compare them to their metal-enriched Population II (Pop. II) counterparts, focusing on their merger rate densities (MRDs), primary masses, and delay times. We find that, despite the high merger efficiency of Pop. III BNSs and BHNSs, their low star formation rate results in a MRD at least one order of magnitude lower than that of Pop. II stars. The MRD of Pop. III BNSs peaks at redshift z∼15, attaining a value mathcal R ̊m BNS (z∼15) ∼ 15,̊m Gpc^ yr^ while the MRD of Pop. III BHNSs is maximum at z∼13, reaching a value of mathcal R ̊m BHNS (z∼13) ∼ 2,̊m Gpc^ yr^ . Finally, we observe that the black hole masses of Pop. III BHNS mergers have a nearly flat distribution, with a peak at ∼20 and extending up to ∼50 Black holes in Pop. II BHNS mergers instead show a peak at łesssim15 We consider these predictions in light of recent gravitational-wave observations in the local Universe, finding that a Pop. III origin is preferred relative to Pop. II for some events.