Magnesium, silicon, and iron abundances and the cluster metallicity scale

Details Magnesium, silicon, and iron abundances and the cluster metallicity scale Magnesium, silicon, and iron abundances and the cluster metallicity scale

Dec 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984apj...287l..85g&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 287, Dec. 15, 1984, p. L85-L89.

Astronomy and Astrophysics

Astrophysics

34

Abundance, Globular Clusters, High Dispersion Spectrographs, Metallicity, Stellar Spectrophotometry, Iron, Magnesium, Silicon

Scientific paper

Abundances have been determined for a number of giant stars in open and globular clusters on the basis of broadband Washington photometry, and high-resolution echelle spectroscopy. The photometric observations were made with the CTIO 91-nm and 1.5 m reflectors, and the KPNO 1.3 m reflector during 44 consecutive nights between May 1980 and September 1982. The spectrographic observations were carried out between 1981 and January 1982, with the KNO KPNO 4-m echelle spectrograph. The spectral resolution was approximately 0.3 A and the wavelength coverage was from 5500 to 7000 A. The classical metal-rich globular clusters NGC 6352, M69, and M71 are found to have Fe/H values of less than -1. The metal-poor open clusters NGC 2141, 2158, 2506, and Melotte 66 have Fe/H values ranging from -0.5 to -1.2. Mg and Si were significantly enhanced relative to Fe in many of the clusters, and a much better correlation is found between the color of the cluster giant branch and the mean (Mg + Si + Fe) abundance than with the Fe abundance alone. The data for the cluster abundances are presented in a table.

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