Abstract

Nuclear Star Clusters (NSCs) and/or Supermassive Black Holes (SMBHs) are observed in the center of galaxies. Although each object is found in different regimes, it is possible to find both of them coexisting in galaxies with stellar masses ∼1010M⊙. In this work we present an implementation of a NSC model in {\sc Galacticus}, a semi-analytic code designed for simulating galaxy formation and evolution. Our focus is exploring the role of NSCs during the formation of SMBHs. We assume an in situ star formation scenario in the gas accumulated in the center of the galaxy. Moreover, we introduce a collapse model for NSCs, where they ultimately collapse into a BH seed upon reaching a critical mass for which collisions between stars become relevant within the cluster. This critical mass is reached when the collisional timescale is shorted than the age of the system. By exploring this collapse scenario, we aim to shed light on its potential implications for the resulting population of SMBHs. Our investigation delves into how this collapse scenario can impact the overall SMBH, as wel as the intricate connections between NSCs, galaxies, and SMBHs. This research provides insights into the formation and evolution of NSCs and their impact on the galactic and black hole environments. We find the formation of BH seeds with masses in the range 103−105.5M⊙.