SIMBAD references

New spectroscopic observations are presented for a sample of thirty-one blue horizontal branch (BHB) star candidates that are sufficiently nearby to have reliable proper motions. Comments are given on a further twenty-five stars that have previously been suggested as BHB star candidates but which were not included in our sample. Moderately high-resolution spectra (λ/Δλ≃15000) of twenty five of our program stars were taken with the coude feed spectrograph at Kitt Peak. Twelve of the program stars were also observed with the CAT spectrograph at ESO. Six of these program stars were observed from both hemispheres. IUE low-resolution spectra are available for most of our candidates and were used, in addition to other methods, in the determination of their T_eff and reddening. A compilation of the visual photometry for these stars (including new photometry obtained at Kitt Peak) is also given. Abundances were obtained from these spectra using models computed by Castelli with an updated version of the ATLAS9 code (Kurucz, 1993, ATLAS9, CD-ROM No. 13). All thirty one candidates are halo stars. Of these, twenty eight are classified as BHB stars because: (o) [(1)]they lie close to the ZAHB (in a similar position to the BHB stars in globular clusters) in the T_eff versus logg plot. For all but one of these stars, far-UV data were available which were consistent with other data (Stroemgren photometry, energy distributions, Hγ profiles) for deriving T_eff and logg. (o) [(2)]they have a distribution of vsini (≤40km/s) that is similar to that found for the BHB in globular clusters. Peterson et al. (1995ApJ...453..214P) and Cohen & McCarthy (1997AJ....113.1353C) have shown that the BHB stars in the globular clusters M13 and M92 have a higher vsini (≤ 40km/s) than those in M3 and NGC 288 (≤20km/s). The mean deprojected rotational velocity (<v>) was calculated for both the two globular clusters and the nearby BHB star samples. A comparison of these suggests that both globular cluster vsini types are present in our nearby sample. No obvious trend is seen between vsini and either (B-V)₀ or [Fe/H]. (o) [(3)]they have -0.99≥[Fe/H]≥-2.95 (mean [Fe/H] -1.67; dispersion 0.42dex), which is similar to that found for field halo RR Lyrae and red HB stars. These local halo field stars appear (on average) to be more metal-poor than the halo globular clusters. The local sample of red giant stars given by Chiba & Yoshii (1998AJ....115..168C) contains a greater fraction of metal-poor stars than either our halo samples or the halo globular clusters. The stars in our sample that have a T_eff that exceeds about 8500K show the HeI (λ 4471) line with a strength that corresponds to the solar helium abundance. (o) [(4)]they show a similar enhancement of the α-elements (<[Mg/Fe]≥+0.43±0.04 and also <[Ti/Fe]≥+0.44±0.02) to that found for other halo field stars of similar metallicity.