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Two neutron star (NS)-black hole (BH) binaries, GW200105 and GW200115 foundin the LIGO/Virgo O3b run have smaller BH mass of 6--9\,$M_{\odot}$ which isconsistent with Population I and II origin. Our population synthesissimulations using $10^6$ Population I and II binaries with appropriate initialparameters show consistent binary mass, event rate, and no detection of radiopulsar (PSR) and BH binaries in our galaxy so far. Especially, we foundpossible progenitors of GW200105 and GW200115 which were formed at redshift$z=0.15$ and $z=1.6$ with binary mass of $(34M_{\odot},\, 9.2M_{\odot})$ and$(23.7M_{\odot},\, 10.6M_{\odot})$, respectively. The final masses of thesebinaries are $(6.85M_{\odot},\,2.14M_{\odot})$ and$(6.04M_{\odot},\,1.31M_{\odot})$ which look like$(9.0_{-1.7}^{+1.7}M_{\odot},\, 1.91_{-0.24}^{+0.33}M_{\odot})$ of GW200105 and$(5.9_{-2.5}^{+2.0}M_{\odot},\,1.44_{-0.29}^{+0.85}M_{\odot})$ of GW200115,respectively. We also estimate that 2.68-19.7 PSR-BH binaries in our galaxywill be observed by SKA. The existence of NS-BHs in our galaxy can be confirmedin future SKA era. Using the GW observation of NS-BH mergers and the radioobservation of PSR-BHs in future, we can get more severe constraints on theNS-BH formation process.

Constraints on Population I/II neutron star-black hole binary formation by gravitational wave and radio observations