Primordial black holes in cosmological simulations: growth prospects for supermassive black holes

It has long been suggested that a fraction of the dark matter in the Universe could exist in the form of primordial black holes (PBHs) that have existed since the radiation dominated era. Recent studies have suggested that these PBHs may be the progenitors to the population of high-redshift, supermassive black holes (SMBHs) observed since the launch of JWST. For the first time, we have included PBHs in cosmological simulations, to test whether PBHs can sink to the center of collapsing halos, locate dense gaseous regions experience significant growth. We tested PBH-to-DM mass ratios of \(f_{\rm PBH}\) = 10⁻⁴ and 10⁻³, with an initial PBH mass of 1000 \(M_\odot\), as inspired by recent observational constraints. We find that at \(f_{\rm PBH}\)=10⁻³, a number of PBHs were able to embed themselves in dense gas and grow to 10⁴-10⁵ M⊙ by z=20. These intermediate black holes (IMBHs) are possible progenitors to the highest redshift SMBH observations such as GNZ-11 (10⁶ \(M_\odot\) by z=10), outperforming light seed black hole (BH) growth seen in recent simulations without the need to invoke heavy seeding prescriptions. On the other hand, \(f_{\rm PBH}\)=10⁻⁴ resulted in no significant BH growth, emphasizing that the ability of PBHs to act as SMBH seeds is sensitive to the true value of fPBH in the Universe, and showing that the \(f_{\rm PBH}\)=10⁻⁴−10⁻³ boundary marks the threshold above which SMBH seeding via 1000 \(M_\odot\) PBHs becomes effective. This is the first step towards building a realistic PBH framework in cosmological simulations.