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We study the influence of gas metallicity, turbulence, and non-equilibriumchemistry on the evolution of the two-phase interstellar medium (warm and coldatomic phases), and thereby constrain the initial conditions for star formationprevailing in turbulent gas. We perform high-resolution simulations in threedimensions, including a realistic non-equilibrium treatment of the ionizationstate of the gas, and examine both driven and decaying turbulence. This allowsus to explore variations in the metallicity Z. In this paper, we study solarmetallicity, Z=Z_sun, and low metallicity, Z=1d-3 Z_sun, gas. For driven,large-scale turbulence, we find that the influence of the metallicity on theamount of mass in the cold gas component is small. However, in decayingturbulent conditions this picture is much changed. While cold regions survivein the case of solar metallicity, they are quickly heated and dispersed inlow-metallicity gas. This result suggests that star formation can be suppressedin environments of low metallicity, unless a strong turbulent driver is actingon time scales shorter than a few turbulent crossing times. Inter alia thisfinding could explain the overall inefficient star formation as well as theburst-like mode of star formation found in metal-poor, gas-rich systems likedwarf galaxies.

The turbulent fragmentation of the interstellar medium: The impact of metallicity on global star formation