2022MNRAS.515.5106W

Previous theoretical studies suggest that the Population III (Pop3) stars tend to form in extremely metal-poor gas clouds with approximately $10^5 \ \mathrm{M}_\odot$ embedded in mini dark matter haloes. Very massive stars can form via multiple collisions in Pop3 star clusters and eventually evolve to intermediate-mass black holes (IMBHs). In this work, we conduct star-by-star N-body simulations for modelling the long-term evolution of Pop3 star clusters. We find that if the mini dark matter haloes can survive today, these star clusters can avoid tidal disruption by the galactic environment and can efficiently produce IMBH-black hole (BH) mergers among a wide range of redshift from 0 to 20. The average gravitational wave event rate is estimated to be $0.1\!-\!0.8\ \mathrm{yr}^{-1} \,\mathrm{Gpc}^{-3}$, and approximately 40-80 per cent of the mergers occur at high redshift (z > 6). The characteristic strain shows that a part of low-redshift mergers can be detected by LISA, TianQin, and Taiji, whereas most mergers can be covered by DECIGO and advanced LIGO/Virgo/KAGRA. Mergers with pair-instability BHs have a rate of approximately 0.01-0.15 yr^–1 Gpc^–3, which can explain the GW190521-like events.