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We perform population synthesis simulations for Population III (Pop III)coalescing binary neutron stars (NS-NSs), neutron star - black hole binaries(NS-BHs), and binary black holes (BH-BHs) which merge within the age of theuniverse. We found that the typical mass of Pop III BH-BHs is $\sim 30\\rm{M}_{\odot}$ so that the inspiral chirp signal of gravitational waves can bedetected up to z=0.28 by KAGRA, Adv. LIGO, Adv. Virgo and GEO network. Oursimulations suggest that the detection rate of the coalescing Pop III BH-BHs is$140 (68) \cdot ({\rm SFR}_{\rm p}/10^{-2.5} \rm{M}_{\odot} {\rm yr}^{-1} {\rmMpc}^{-3}) \cdot {\rm Err}_{\rm sys} ~{\rm events} ~{\rm yr}^{-1}$ for the flat(Salpeter) initial mass function (IMF), respectively, where $\rm SFR_p$ and$\rm Err_{sys}$ are the peak value of the Pop III star formation rate and thepossible systematic errors due to the assumptions in Pop III populationsynthesis, respectively. $\rm Err_{sys}=1$ correspond to conventionalparameters for Pop I stars. From the observation of the chirp signal of thecoalescing Pop III BH-BHs, we can determine both the mass and the redshift ofthe binary for the cosmological parameters determined by Planck satellite. Oursimulations suggest that the cumulative redshift distribution of the coalescingPop III BH-BHs depends almost only on the cosmological parameters. We might beable to confirm the existence of Pop III massive stars of mass $\sim 30~\rmM_{\odot}$ by the detections of gravitational waves if the merger rate of thePop III massive BH-BHs dominates that of Pop I BH-BHs.

Possible Indirect Confirmation of the Existence of Pop III Massive Stars by Gravitational Wave