Metallicity in galactic clusters from high signal-to-noise spectroscopy

Details Metallicity in galactic clusters from high signal-to-noise spectroscopy Metallicity in galactic clusters from high signal-to-noise spectroscopy

Jan 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989apj...336..798b&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 336, Jan. 15, 1989, p. 798-807.

Astronomy and Astrophysics

Astrophysics

129

Astronomical Spectroscopy, Metallicity, Milky Way Galaxy, Open Clusters, Signal To Noise Ratios, Abundance, Chemical Evolution, Dwarf Stars, F Stars, Nuclear Fusion, Star Distribution, Stellar Spectra

Scientific paper

High-quality spectroscopic data on selected F dwarfs in six Galactic clusters are used to determine global (Fe/H) values for the clusters. For the two youngest clusters, Pleiades and Alpha Per, the (Fe/H) values are solar: 0.017 + or - 0.055. The Hyades and Praesepe are slightly metal-enhanced at (Fe/H) = + 0.125 + or - 0.032, even though they are an order of magnitude older than the Pleiades. Coma and the UMa Group at the age of the Hyades are slightly metal-deficient with (Fe/H) = - 0.082 + or - 0.039. The lack of an age-metallicity relationship indicates that the enrichment and mixing in the Galactic disk have not been uniform on time scales less than a billion years.

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