  The Edinburgh-Cape Blue Object Survey is an ongoing project to identify and
analyse a large sample of hot stars selected initially on the basis of
photographic colours (down to a magnitude limit B~18.0) over the entire
high-Galactic-latitude southern sky, then studied with broadband UBV photometry
and medium-resolution spectroscopy. Due to unavoidable errors in the initial
candidate selection, stars that are likely metal-deficient dwarfs and giants of
the halo and thick-disk populations are inadvertently included, yet are of
interest in their own right. In this paper we discuss a total of 206 candidate
metal-deficient dwarfs, subgiants, giants, and horizontal-branch stars with
photoelectric colours redder than (B-V)o = 0.3, and with available
spectroscopy. Radial velocities, accurate to ~10-15 km/s, are presented for all
of these stars. Spectroscopic metallicity estimates for these stars are
obtained using a recently re-calibrated relation between Ca II K-line strength
and (B-V)o colour. The identification of metal-poor stars from this
colour-selection technique is remarkably efficient, and competitive with
previous survey methods. An additional sample of 186 EC stars with
photoelectric colours in the range -0.4 < (B-V)o < 0.3, comprised primarily of
field horizontal-branch stars and other, higher-gravity, A- and B-type stars,
is also analysed. Estimates of the physical parameters Teff, log g, and [Fe/H]
are obtained for cooler members of this subsample, and a number of candidate RR
Lyrae variables are identified.
