Metallicity estimates for A-, F-, and G-type stars from the Edinburgh-Cape blue object survey

Details Metallicity estimates for A-, F-, and G-type stars from the Edinburgh-Cape blue object survey Metallicity estimates for A-, F-, and G-type stars from the Edinburgh-Cape blue object survey

2000-11-27

arxiv.org/abs/astro-ph/0011491v1

Mon.Not.Roy.Astron.Soc. 320 (2001) 451

Astronomy and Astrophysics

Astrophysics

Includes 10 figures, 6 tables, to be published in the Monthly Notices of the Royal Astronomical Society

Scientific paper

10.1046/j.1365-8711.2001.03952.x

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.

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