The Stellar IMF in Very Metal-Deficient Gas

In the context of the star formation through the fragmentation of an extremely metal-deficient protogalactic cloud, the gravitational collapse of filamentary gas clouds is explored with H$_2$ and HD chemistry. It is found by 1D hydrodynamical simulations that the cloud evolution is prescribed mainly by the initial density ($n_0$) and H$_2$ abundance ($x_{\rm H_2,0}$). In particular, it turns out that the evolution of low-density filaments ($n_0 \lesssim 10^5$ cm$^{-3}$) bifurcates at a critical H$_2$ abundance of $x_{\rm H_2,cr}\simeq 3\times 10^{-3}$, beyond which HD cooling overwhelms H$_2$ cooling. The numerical results indicate that the stellar IMF is likely to be double-peaked and deficient in sub-solar mass stars, where the high mass peak of the IMF is around $10M_\odot$ or $10^2M_\odot$, dependently on the initial density and H$_2$ abundance. If the gas in protogalactic clouds is photoionized by UV radiation or shock-heated, the H$_2$ abundance could exceed $x_{\rm H_2,cr}\simeq 3\times 10^{-3}$ by H$^-$ reactions. Then, the high mass peak would be $O(10) M_\odot$.

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