than previously thought. This prompts the need for a large, high-resolution study of the formation of dark matter minihalos that is capable of resolving the turbulent flows in the gas at the moment when the baryons become self-gravitating. This would help to determine the applicability of our results to primordial star formation'
author:
- 'Paul C. Clark$^1$, Simon C.O. Glover$^1$, Ralf S. Klessen$^{1, 2}$ & Volker Bromm$^3$'
title: Gravitational fragmentation in turbulent primordial gas and the initial mass function of Population III stars
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Introduction {#sec:intro}
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Over the course of the last decade, work by a number of groups has led to the development of a widely accepted picture for the formation of the first stars, the so-called Population III (or Pop. III) stars. In this picture, the very first stars (Population III.1 in the nomenclature of @tm08 and @omha2008) form within small dark matter halos that have total masses $M \sim 10^{6} \: {\rm M_{\odot}}$, virial temperatures of around a thousand K, and that are assembled at redshifts $z \sim 25$–30 or above [@bl04; @g05; @byhm09]. Gas falling into one of these small dark matter halos is shock-heated to a temperature close to the virial temperature of the 