How an improved implementation of H2 self-shielding influences the formation of massive stars and black holes
Abstract
High-redshift quasars at z > 6 have masses up to ∼109 M⊙. One of the pathways to their formation includes direct collapse of gas, forming a supermassive star, precursor of the black hole seed. The conditions for direct collapse are more easily achievable in metal-free haloes, where atomic hydrogen cooling operates and molecular hydrogen (H2) formation is inhibited by a strong external (ultraviolet) UV flux. Above a certain value of UV flux (Jcrit), the gas in a halo collapses isothermally at ∼104 K and provides the conditions for supermassive star formation. However, H2 can self-shield, reducing the effect of photodissociation. So far, most numerical studies used the local Jeans length to calculate the column densities for self-shielding. We implement an improved method for the determination of column densities in 3D simulations and analyse its effect on the value of Jcrit. This new method captures the gas geometry and velocity field and enables us to properly determine the direction-dependent self-shielding factor of H2 against photodissociating radiation. We find a value of Jcrit that is a factor of 2 smaller than with the Jeans approach (∼2000 J21 versus ∼4000 J21). The main reason for this difference is the strong directional dependence of the H2 column density. With this lower value of Jcrit, the number of haloes exposed to a flux > Jcrit is larger by more than an order of magnitude compared to previous studies. This may translate into a similar enhancement in the predicted number density of black hole seeds.
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