The first generation of stars: first steps towards chemical evolution of galaxies

Abstract

We argue that extreme metal-poor stars show a high dispersion in metallicity, because their abundances are the outcome of very few supernova events. Abundance anomalies should appear because of the discrete range of progenitor masses. There is a natural metallicity threshold of $Z/Z_{\odot }\sim 10^{-4}$ below which one would expect to find very few, if any, halo stars. Similar reasoning is applied to lower mass systems, such as metal-poor compact blue galaxies and Lyman alpha absorption line clouds seen towards high redshift quasars, where a somewhat higher threshold is inferred.

7 pages of plain TEX, no figures, to appear in Astrophysical Journal Letters

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• Absence of a Lower Limit on Omega_b in Inhomogeneous Primordial Nucleosynthesis

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