Metal abundances in metal-poor globular clusters

Details Metal abundances in metal-poor globular clusters Metal abundances in metal-poor globular clusters

Feb 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...211...41g&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 211, no. 1, Feb. 1989, p. 41-55.

Astronomy and Astrophysics

Astrophysics

99

Abundance, Astronomical Spectroscopy, Globular Clusters, Metallicity, Astronomical Photometry, Line Spectra, Milky Way Galaxy, Radial Velocity, Spectral Line Width, Stellar Atmospheres

Scientific paper

The abundances of twelve elements (including O, Fe, Mg, and Si) were derived for stars in seven globular clusters, including NGC 1904, NGC 3201, NGC 4590, NGC 4833, NGC 6254, NGC 6397, and NGC 6656, using high-dispersion spectra obtained with the ESO's 3.6-m telescope. These data, added to the already available abundance data, constitute a data base of metal abundances for stars in a total of 17 globular clusters, some of which are metal-poor and some metal-rich. These metal abundances were found to correlate well with abundance indices obtained from integrated spectroscopy and photometry of clusters or from spectroscopy and photometry of individual stars. Present data indicate that the O-rich clusters have 'normal' abundances, following the general galactic enrichment scheme and reflecting the original abundance pattern, while O-poor clusters are in some way anomalous.

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