3883 CN band strengths for 238 metal-poor halo giants - Evidence for chemical differences between globular-cluster and halo field giants

Details 3883 CN band strengths for 238 metal-poor halo giants - Evidence for chemical differences between globular-cluster and halo field giants 3883 CN band strengths for 238 metal-poor halo giants - Evidence for chemical differences between globular-cluster and halo field giants

Jul 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992pasp..104..523l&link_type=abstract

Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 104, no. 677, July 1992, p. 523-532. Research supported

Astronomy and Astrophysics

Astronomy

45

Cn Emission, Giant Stars, Globular Clusters, Spectral Bands, Stellar Composition, Abundance, Galactic Structure, Metallicity, Stellar Evolution

Scientific paper

Cyanogen band strengths m(CN) for 238 metal-poor giants in the halo field and in 13 globular clusters are tabulated. The distribution of m (CN) in field giants of intermediate metallicity is compared with that of giants of similar evolutionary state in M79, M3, and M13. The field star population is dominated by weak-CN stars. M79 has mostly giants with CN bands of intermediate strength, M3 has relatively few giants with strong CN bands, and M 13 is dominated by strong-CN giants. These results add evidence in support of the notion that halo field stars and stars of most globular clusters differ chemically even at equivalent [Fe/H]. In the spectra of giant stars in the very metal-poor clusters M 15 and M92, CN bands tend to disappear, and become noticeable only in stars having exceptionally large nitrogen abundances.

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