Direct collapse to supermassive black hole seeds: the critical conditions for suppression of H2 cooling

Observations of high-redshift quasars imply the presence of supermassive black holes (SMBHs) already at z similar to 7.5. An appealing and promising pathway to their formation is the direct collapse scenario of a primordial gas in atomic-cooling haloes at z similar to 10-20, when the H-2 formation is inhibited by a strong background radiation field, whose intensity exceeds a critical value, J(crit). To estimate J(crit), typically, studies have assumed idealized spectra, with a fixed ratio of H-2 photodissociation rate k(H2) to the H- photodetachment rate k(H)(-). This assumption, however, could be too narrow in scope as the nature of the background radiation field is not known precisely. In this work we argue that the critical condition for suppressing the H-2 cooling in the collapsing gas could be described in a more general way by a combination of k(H2) and k(H-) parameters, without any additional assumptions about the shape of the underlying radiation spectrum. By performing a series of cosmological zoom-in simulations covering a wide range of relevant k(H2), and kH(-) parameters, we examine the gas flow by following evolution of basic parameters of the accretion flow. We test under what conditions the gas evolution is dominated by H-2 and/or atomic cooling. We confirm the existence of a critical curve in the k(H2)-k(H)- plane and provide an analytical fit to it. This curve depends on the conditions in the direct collapse, and reveals domains where the atomic cooling dominates over the molecular cooling. Furthermore, we have considered the effect of H-2 self-shielding on the critical curve, by adopting three methods for the effective column density approximation in H-2. We find that the estimate of the characteristic length scale for shielding can be improved by using lambda(Jeans25), which is 0.25 times that of the local Jeans length, which is consistent with previous one-zone modelling.