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The detection of gravitational waves (GWs) generated by merging black holeshas recently opened up a new observational window into the Universe. The massof the black holes in the first and third LIGO detections, ($36-29 \,\mathrm{M_{\odot}}$ and $32-19 \, \mathrm{M_{\odot}}$), suggestslow-metallicity stars as their most likely progenitors. Based onhigh-resolution N-body simulations, coupled with state-of-the-art metalenrichment models, we find that the remnants of Pop III stars arepreferentially located within the cores of galaxies. The probability of a GWsignal to be generated by Pop III stars reaches $\sim 90\%$ at $\sim 0.5 \,\mathrm{kpc}$ from the galaxy center, compared to a benchmark value of $\sim5\%$ outside the core. The predicted merger rates inside bulges is $\sim 60\times \beta_{III} \, \mathrm{Gpc^{-3} \, yr^{-1}}$ ($\beta_{III}$ is the PopIII binarity fraction). To match the $90\%$ credible range of LIGO mergerrates, we obtain: $0.03 < \beta_{III} < 0.88$. Future advances in GWobservatories and the discovery of possible electromagnetic counterparts couldallow the localization of such sources within their host galaxies. Thepreferential concentration of GW events within the bulge of galaxies would thenprovide an indirect proof for the existence of Pop III stars.

Gravitational Wave Sources from Pop III Stars are Preferentially Located within the Cores of their Host Galaxies