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We study the birth of supermassive black holes from the direct collapseprocess and characterize the sites where these black hole seeds form. In thepre-reionization epoch, molecular hydrogen (H$_2$) is an efficient coolant,causing gas to fragment and form Population III stars, but Lyman-Wernerradiation can suppress H$_2$ formation and allow gas to collapse directly intoa massive black hole. The critical flux required to inhibit H$_2$ formation,$J_{\rm crit}$, is hotly debated, largely due to the uncertainties in thesource radiation spectrum, H$_2$ self-shielding, and collisional dissociationrates. Here, we test the power of the direct collapse model in aself-consistent, time-dependant, non-uniform Lyman-Werner radiation field --the first time such has been done in a cosmological volume -- using an updatedversion of the SPH+N-body tree code Gasoline with H$_2$ non-equilibriumabundance tracking, H$_2$ cooling, and a modern SPH implementation. We vary$J_{\rm crit} $ from $30$ to $10^3$ in units of $J_{21}$ to study how thisparameter impacts the number of seed black holes and the type of galaxies whichhost them. We focus on black hole formation as a function of environment, halomass, metallicity, and proximity of the Lyman-Werner source. Massive black holeseeds form more abundantly with lower $J_{\rm crit}$ thresholds, but regardlessof $J_{\rm crit}$, these seeds typically form in halos that have recently begunstar formation. Our results do not confirm the proposed atomic cooling halopair scenario; rather black hole seeds predominantly form in low-metallicitypockets of halos which already host star formation.

Sowing black hole seeds: Direct collapse black hole formation with realistic Lyman-Werner radiation in cosmological simulations