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We propose a new mechanism for the growth of supermassive black hole (BH)seeds in the star-forming progenitors of local early-type galaxies (ETGs) at$z\gtrsim 1$. This envisages the migration and merging of stellar compactremnants (neutron stars and stellar-mass BHs) via gaseous dynamical frictiontoward the central high-density regions of such galaxies. We show that, underreasonable assumptions and initial conditions, the process can build up centralBH masses of order $10^4-10^6\, M_\odot$ within some $10^7$ yr, so effectivelyproviding heavy seeds before standard disk (Eddington-like) accretion takesover to become the dominant process for further BH growth. Remarkably, such amechanism may provide an explanation, alternative to super-Eddington accretionrates, for the buildup of billion solar masses BHs in quasar hosts at $z\gtrsim7$, when the age of the Universe $\lesssim 0.8$ Gyr constitutes a demandingconstraint; moreover, in more common ETG progenitors at redshift $z\sim 2-6$ itcan concur with disk accretion to build such large BH masses even at moderateEddington ratios $\lesssim 0.3$ within the short star-formation duration$\lesssim$ Gyr of these systems. Finally, we investigate the perspectives todetect the merger events between the migrating stellar remnants and theaccumulating central supermassive BH via gravitational wave emission withfuture ground and space-based detectors such as the Einstein Telescope (ET) andthe Laser Interferometer Space Antenna (LISA).

astrophysical journal/the astrophysical journal

Growth of Supermassive Black Hole Seeds in ETG Star-Forming Progenitors:  Multiple Merging of Stellar Compact Remnants via Gaseous Dynamical Friction  and Gravitational Wave Emission