A rapid channel for the collisional formation and gravitational wave driven mergers of supermassive black hole seeds at high redshift

Motivated by JWST observations of dense, clumpy and clustered high redshift star formation, we simulate the hierarchical assembly of nine $M_{\mathrm{c}\mathrm{l}}={10}^6{M}_{\odot }$ star clusters using the BIFROST N-body code. Our low metallicity models ($0.01Z_{\odot }$) with post-Newtonian equations of motion for black holes include evolving populations of single, binary and triple stars. Massive stars grow by stellar collisions and collapse into intermediate mass black holes (IMBHs) up to $M_{\bullet }\sim 6200M_{\odot }$, stellar multiplicity boosting the IMBH masses by a factor of $2$–$3$. The IMBHs tidally disrupt (TDE) $\sim 50$ stars in $10$ Myr with peak TDE rates up to $\mathrm{\Gamma }\sim 5\times {10}^{-5}$ yr${}^{-1}$ per cluster. These IMBHs are natural seeds for supermassive black holes (SMBHs) and the hierarchical assembly frequently leads to $>2$ SMBH seeds per cluster and their rapid mergers ($t<10$ Myr). We propose that a gravitational wave (GW) driven merger of IMBHs with $1000M_{\odot }\lesssim M_{\bullet }\lesssim 10000M_{\odot }$ with comparable masses is a characteristic GW fingerprint of SMBH seed formation at redshifts $z>10$, and IMBH formation in similar environments at lower redshifts. Massive star clusters provide a unique environment for the early Universe GW studies for the next-generation GW observatories including the Einstein Telescope and the Laser Interferometer Space Antenna.