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We obtain estimates of stellar atmospheric parameters for a previouslypublished sample of 1777 relatively bright (9 < B < 14) metal-poor candidatesfrom the Hamburg/ESO Survey. The original Frebel et al. analysis of these starswas only able to derive estimates of [Fe/H] and [C/Fe] for a subset of thesample, due to limitations in the methodology then available. A newspectroscopic analysis pipeline has been used to obtain estimates of Teff, logg, [Fe/H], and [C/Fe] for almost the entire dataset. This sample is very local- about 90% of the stars are located within 0.5 kpc of the Sun. We consider thechemodynamical properties of these stars in concert with a similarly localsample of stars from a recent analysis of the Bidelman & MacConnell'weak-metal' candidates by Beers et al. We use this combined sample to identifypossible members of the suggested halo stream of stars by Helmi et al. andChiba & Beers, as well as stars that may be associated with stripped debrisfrom the putative parent dwarf of the globular cluster Omega Centauri,suggested to exist by previous authors. We identify a clear increase in thecumulative frequency of carbon-enhanced metal-poor (CEMP) stars with decliningmetallicity, as well as an increase in the fraction of CEMP stars with distancefrom the Galactic plane, consistent with previous results. We also identify arelatively large number of CEMP stars with kinematics consistent with themetal-weak thick-disk population, with possible implications for its origin.

Bright Metal-Poor Stars from the Hamburg/ESO Survey. II. A Chemodynamical Analysis