Metal Abundances and Mixing in Metal-Rich Globular Clusters with Blue Horizontal Branches

Details Metal Abundances and Mixing in Metal-Rich Globular Clusters with Blue Horizontal Branches Metal Abundances and Mixing in Metal-Rich Globular Clusters with Blue Horizontal Branches

Feb 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001noao.prop..236s&link_type=abstract

NOAO Proposal ID #2001A-0236

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Scientific paper

High metallicity globular clusters almost always have stubby red horizontal branches. NGC 6388 and NGC 6441 are apparent exceptions to this rule. They are believed to be as metal-rich as the canonical metal- rich globular 47 Tuc, but very unexpectedly they exhibit blue as well as red horizontal branch populations. Explanations for this phenomenon run the gamut from deep mixing in stars on the red giant giant branch to the hypothesis that stars in NGC 6388 and NGC 6441 have a range in [Fe/H], similar to that of the so-far unique globular cluster ω Cen. We propose to obtain low resolution blue-green spectra of RR Lyrae stars, type II Cepheids, and red giants in NGC 6388 to test whether deep mixing or a spread in metallicity is responsible for the unusual horizontal branch morphology of that cluster. If the latter explanation is correct, then the RR Lyrae stars and Cepheids should be much more metal- poor than the cluster as a whole, while the the red giants would show a range in metallicity from metal-rich to metal-poor. If, on the other hand, deep mixing is the correct explanation, we should be able to identify its signature in the relative abundances of chemical elements in the stars.

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