Speaker
Description
In the last decade, many observations of bright quasars at $z > 5$, have revealed the existence of Supermassive Black Holes (SMBHs), giants of billion solar masses shining close to their Eddington limit. The mechanism of their
formation at these early epochs represents currently an open problem in galaxy evolution.
Several scenarios have been proposed to overcome this problem, such as the Super-Eddington accretion onto stellar Black Hole seeds, with typical masses of ?$100M_{\odot}$?, or the existence of more massive seeds, such as the Direct Collapse Black Holes with masses picked around $10^5 M_{\odot}$?. Intermediate mass black holes forming from the runaway collapse into dense stellar cluster, with mass of $\sim 10^3M_{\odot} $, actually represent another potential solution.
Following the early growth and coalescence of BH seeds in cosmological simulations, I will discuss the formation sites of these seeds and their
relative contribution to the formation of the central Black Hole mass. The resulting theoretical predictions constrain the detectability of gravitational wave signals produced by binary BH seeds mergers with future third generation gravitational telescopes, such as the Einstein telescope and the Laser Interferometer Space Antenna (LISA).
