The Baade-Wesselink method and the distances to RR Lyrae Stars. VIII - Comparisons with other techniques and implications for globular cluster distances and ages

Details The Baade-Wesselink method and the distances to RR Lyrae Stars. VIII - Comparisons with other techniques and implications for globular cluster distances and ages The Baade-Wesselink method and the distances to RR Lyrae Stars. VIII - Comparisons with other techniques and implications for globular cluster distances and ages

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...386..663c&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 386, Feb. 20, 1992, p. 663-684. Research supported by SNFO and Danish Resea

Astronomy and Astrophysics

Astrophysics

263

Distance, Globular Clusters, Stellar Evolution, Stellar Oscillations, Variable Stars, Abundance, Horizontal Branch Stars, Main Sequence Stars, Metallicity, Red Giant Stars, Statistical Analysis

Scientific paper

All techniques that derive M(V) or M(bol) as a function of Fe/H for RR Lyrae variables are summarized. Recent results from main-sequence fitting are revised to account for metallicity-dependent errors in B - V from model isochrones; M(V)(RR) is found to vary as 0.12(Fe/H). The equilibrium temperature scale is redefined for RR Lyrae stars, and the period-shift analyses for RR Lyrae stars in globular clusters and in the field are readdressed. All methods agree that, within the errors, M(V)(RR) varies as 0.15(Fe/H) and M(bol)(RR) varies as 0.19(Fe/H). If O/Fe = 0.3, the Galaxy's age may be as high as 20 +/-3 Gyr, and the most metal-poor clusters are on average older than the more metal-rich ones. If O/Fe varies as -0.4(Fe/H), the Galaxy's age is about 14 +/-2 Gyr, and the cluster's ages do not correlate with metallicity. Regardless of the oxygen abundance, there is a significant range in ages among the intermediate-metallicity clusters.

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