have used sink particles to allow the evolution of the gas to be followed beyond the formation of the first protostar consistently find evidence for more extensive fragmentation than is assumed in the conventional picture of Population III star formation (@cgk08 [@sgb10]; Clark et al., in prep.). If fragmentation is as common as these results suggest, and most Population III stars form in multiple systems rather than as single stars, then this has profound implications for the final masses of the stars, their production of ionizing photons and metals, the rate of high redshift gamma ray bursts, and many other issues.

It is therefore important to better understand the physical basis of fragmentation in these systems. To do this, we would ideally like to have a large sample of simulations, as basing our arguments on only one or two realizations of Population III star formation leaves one open to the possibility that these realizations may not be typical. Unfortunately, simulations starting from cosmological initial conditions and following collapse all the way to protostellar densities are computationally costly, making it difficult to explore a large region of parameter space. In these simulations, it is also difficult to be certain about which 