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This paper presents theoretical star formation and chemical enrichmenthistories for the stellar halo of the Milky Way based on new chemodynamicalmodeling. The goal of this study is to assess the extent to which metal-poorstars in the halo reflect the star formation conditions that occurred in haloprogenitor galaxies at high redshift, before and during the epoch ofreionization. Simple prescriptions that translate dark-matter halo mass intobaryonic gas budgets and star formation histories yield models that resemblethe observed Milky Way halo in its total stellar mass, metallicitydistribution, and the luminosity function and chemical enrichment of dwarfsatellite galaxies. These model halos in turn allow an exploration of how thepopulations of interest for probing the epoch of reionization are distributedin physical and phase space, and of how they are related to lower-redshiftpopulations of the same metallicity. The fraction of stars dating from before aparticular time or redshift depends strongly on radius within the galaxy,reflecting the "inside-out" growth of cold-dark-matter halos, and onmetallicity, reflecting the general trend toward higher metallicity at latertimes. These results suggest that efforts to discover stars from z > 6 - 10should select for stars with [Fe/H] <~ -3 and favor stars on more tightly boundorbits in the stellar halo, where the majority are from z > 10 and 15 - 40% arefrom z > 15. The oldest, most metal-poor stars - those most likely to revealthe chemical abundances of the first stars - are most common in the very centerof the Galaxy's halo: they are in the bulge, but not of the bulge. These modelshave several implications for the larger project of constraining the propertiesof the first stars and galaxies using data from the local Universe.

astrophysical journal/the astrophysical journal

Chemical Evolution in Hierarchical Models of Cosmic Structure II: The  Formation of the Milky Way Stellar Halo and the Distribution of the Oldest  Stars