Bright Metal-Poor Stars from the Hamburg/ESO Survey. II. A
  Chemodynamical Analysis
  We obtain estimates of stellar atmospheric parameters for a previously
published sample of 1777 relatively bright (9 < B < 14) metal-poor candidates
from the Hamburg/ESO Survey. The original Frebel et al. analysis of these stars
was only able to derive estimates of [Fe/H] and [C/Fe] for a subset of the
sample, due to limitations in the methodology then available. A new
spectroscopic analysis pipeline has been used to obtain estimates of Teff, log
g, [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 the
chemodynamical properties of these stars in concert with a similarly local
sample of stars from a recent analysis of the Bidelman & MacConnell
'weak-metal' candidates by Beers et al. We use this combined sample to identify
possible members of the suggested halo stream of stars by Helmi et al. and
Chiba & Beers, as well as stars that may be associated with stripped debris
from the putative parent dwarf of the globular cluster Omega Centauri,
suggested to exist by previous authors. We identify a clear increase in the
cumulative frequency of carbon-enhanced metal-poor (CEMP) stars with declining
metallicity, as well as an increase in the fraction of CEMP stars with distance
from the Galactic plane, consistent with previous results. We also identify a
relatively large number of CEMP stars with kinematics consistent with the
metal-weak thick-disk population, with possible implications for its origin.
