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A promising supermassive black hole seed formation channel is that of directcollapse from primordial gas clouds. We perform a suite of 3D hydrodynamicssimulations of an isolated turbulent gas cloud to investigate conditionsconducive to forming massive black hole seeds via direct collapse, probing theimpact of cloud metallicity, gas temperature floor and cooling physics on cloudfragmentation. We find there is no threshold in metallicity which produces asharp drop in fragmentation. When molecular cooling is not present, metallicityhas little effect on fragmentation. When molecular cooling is present,fragmentation is suppressed by at most $\sim 25\%$, with the greatestsuppression seen at metallicities below $2\%$ solar. A gas temperature floor$\sim 10^{4}$K produces the largest drop in fragmentation of any parameterchoice, reducing fragmentation by $\sim 60\%$. At metallicities below $2\%$solar or at temperatures $\sim 10^{3}$K we see a reduction in fragmentation$\sim 20-25 \%$. For a cloud of metallicity $2\%$ solar above and a temperaturebelow $10^3$K, the detailed choices of temperature floor, metallicity, andcooling physics have little impact on fragmentation.

The effects of metallicity and cooling physics on fragmentation: implications on direct-collapse black hole formation