First stars, very massive black holes and metals

Recent studies suggest that the initial mass function (IMF) of the first stars was likely to be extremely top-heavy, unlike what is observed at present. We propose a scenario to generate fragmentation to lower masses once the first massive stars have formed and derive constraints on the primordial IMF. We estimate the mass fraction of pair-unstable supernovae, shown to be the dominant sources of the first heavy elements. These metals enrich the gas up to about $10^{-5}$ solar metallicity, when a transition to efficient cooling-driven fragmentation occurs producing 1 solar mass clumps. We argue that the remaining fraction of the first stars ends up in 100 solar mass VMBHs (Very Massive Black Holes). We obtain constraints on the fraction of first stars that contribute to the initial metal enrichment and the transition redshift for primordial IMF away from a top-heavy one, by making various assumptions about the fate of these VMBHs at late times. We conclude with a discussion of several hitherto unexplored implications of a high-mass dominated star formation mode in the early Universe.