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We performed Population III (Pop III) binary evolution by using populationsynthesis simulations for seven different models. We found that Pop IIIbinaries tend to be binary black holes (BBHs) with chirp mass $M_{\rm chirp}\sim 30~M_{\odot}$ and they can merge at present day due to long merger time.The merger rate densities of Pop III BBHs at $z=0$ ranges 3.34--21.2 $\rm/yr/Gpc^3$ which is consistent with the aLIGO/aVIRGO result of 9.7--101 $\rm/yr/Gpc^3$. These Pop III binaries might contribute to some part of the massiveBBH gravitational wave (GW) sources detected by aLIGO/aVIRGO. We alsocalculated the redshift dependence of Pop III BBH mergers. We found that PopIII low spin BBHs tend to merge at low redshift, while Pop III high spin BBHsdo at high redshift, which can be confirmed by future GW detectors such as ET,CE, and DECIGO. These detectors can also check the redshift dependence of BBHmerger rate and spin distribution. Our results show that except for one model,the mean effective spin $\left\langle \chi_{\rm eff} \right\rangle$ at $z=0$ranges $0.02$--$0.3$ while at $z=10$ it does $0.16$--$0.64$. Therefore, massivestellar-mass BBH detection by GWs will be a key for the stellar evolution studyin the early universe.

Chirp Mass and Spin of Binary Black Holes from First Star Remnants