Metallicity estimates for A-, F-, and G-type stars from the Edinburgh-Cape Blue Object Survey

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 $B\sim 18.0)$ over the entire high-Galactic-latitude southern sky, and then studied with broad-band 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-disc 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 $(B-V)_0=0.3$, and with available spectroscopy. Radial velocities, accurate to ∼10–15 km s⁻¹, are presented for all of these stars. Spectroscopic metallicity estimates for these stars are obtained using a recently recalibrated relation between Ca ii K-line strength and $(B-V)_0$ 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 $-0.4\leq(B-V)_0\ \lt0.3$, composed 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.