Key points are not available for this paper at this time.
We study the genesis and evolution of super-massive black hole (SMBH) seeds through different formation channels, from PopIII remnants to massive seeds, modeled within the L-Galaxies semi-analytic code. We run the model on the Millennium-II simulation (MR-II) merger trees, as their halo-mass resolution (Mₕ₈ₑ, ₑ₄ₒ~10⁷ Msun h^-1) allows to study in a cosmological volume (L₁₎ₗ=₁₀₀ ₌₂ ₇^-₁) ₓ₇₄ ₄ₕ₎₋ₔₓ₈₎₍ ₎₅ ₀ₓ₎₌₈₂-₂₎₎₋₈₍₆ ₇₀₋₎ₒ (ₓ_{ₕ₈ₑ>10⁴ K) where intermediate-mass and heavy seeds are expected to form. We track the formation of these seeds according to spatial variations of the chemical and radiative feedback of star formation. Not being able to resolve the first mini-halos (Tₕ₈ₑ~10³ K), we inherit evolved PopIII remnants in a sub-grid fashion, using the results of the GQd model. We also include the formation of heavy seeds in gas-rich massive mergers, who are very rare in the MR-II volume. The descendants of light seeds numerically prevail among our SMBHs population at all masses and z. Heavier seeds form in dense environments where close neighbors provide the required UV illumination. Overall, our model produces a z=0 SMBHs population whose statistical properties meet current constraints. We find that the BH occupation fraction highly depends on the seeding efficiency and that the scaling relation between BH and stellar mass, in the dwarf-mass regime, is flatter than in the high-mass range. Finally, a fraction of BHs hosted in local dwarf galaxies never grow since they form at z>6.
Spinoso et al. (Fri,) studied this question.