  The detection of gravitational waves (GWs) generated by merging black holes
has recently opened up a new observational window into the Universe. The mass
of the black holes in the first and third LIGO detections, ($36-29 \,
\mathrm{M_{\odot}}$ and $32-19 \, \mathrm{M_{\odot}}$), suggests
low-metallicity stars as their most likely progenitors. Based on
high-resolution N-body simulations, coupled with state-of-the-art metal
enrichment models, we find that the remnants of Pop III stars are
preferentially located within the cores of galaxies. The probability of a GW
signal 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 $\sim
5\%$ outside the core. The predicted merger rates inside bulges is $\sim 60
\times \beta_{III} \, \mathrm{Gpc^{-3} \, yr^{-1}}$ ($\beta_{III}$ is the Pop
III binarity fraction). To match the $90\%$ credible range of LIGO merger
rates, we obtain: $0.03 < \beta_{III} < 0.88$. Future advances in GW
observatories and the discovery of possible electromagnetic counterparts could
allow the localization of such sources within their host galaxies. The
preferential concentration of GW events within the bulge of galaxies would then
provide an indirect proof for the existence of Pop III stars.
