held constant and the chemical evolution is not followed. On the scales of interest in this study, gravitational forces from the dark matter are negligible compared to the self-gravity of the gas, and so for simplicity, we do not include dark matter in our models.

By re-scaling the mass and temperature of the cloud, we are then able to choose initial conditions that are gravitationally unstable, and which are similar to the initial conditions for the Pop. III.1 and Pop. III.2 star formation channels that occur in cosmological simulations. All of the simulations presented in this paper start with a maximum central cloud number density of $10^{5}$ cm$^{-3}$. The Pop.  III.1 simulations start with an initial temperature of 300K and contain 1000 of gas. For the Pop. III.2 simulations, we adopt an initial temperature of 75 K and examine two different initial masses. The first set of Pop. III.2 simulations contain 150 of gas, chosen such that they have the same ratio of thermal to gravitational energy as the Pop. III.1 simulations, roughly 0.15. As such, these Pop. III.2 simulations contain the same initial number of Jeans masses of gas as the Pop. III.1 simulations. For a uniform sphere, the 