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We explore the effect of an early population of intermediate‐mass stars in the 2–8 M  ⊙   range on the cosmic chemical evolution. We discuss the implications of this population as it pertains to several cosmological and astrophysical observables. For example, some very metal poor Galactic stars show large enhancements of carbon, typical of the C‐rich ejecta of intermediate‐mass stars; moreover, halo star carbon and oxygen abundances show wide scatter, which imply a wide range of star formation and nucleosynthetic histories contributed to the first generations of stars. Also, recent analyses of the   4 He  abundance in metal‐poor extragalactic H  ii  regions suggest an elevated abundance   Y  p ≃ 0.256  by mass, higher than the predicted result from the big bang nucleosynthesis, assuming the baryon density determined by the  WMAP ,   Y  p = 0.249 . Although there are large uncertainties in the observational determination of   4 He , this offset may suggest a prompt initial enrichment of   4 He  in early metal‐poor structures. We also discuss the effect of intermediate‐mass stars on the global cosmic evolution, the reionization of the Universe, the density of white dwarfs, as well as Type II supernovae (SN II) and SN Ia rates at high redshift. We also comment on the early astration of D and   7 Li . We conclude that if intermediate‐mass stars are to be associated with Population III stars, their relevance is limited (primarily from observed abundance patterns) to low‐mass structures involving a limited fraction of the total baryon content of the Universe.

Cosmic chemical evolution with an early population of intermediate‐mass stars