An interpretation of the line-strength indices in old stellar populations using an evolutionary synthesis approach

Details An interpretation of the line-strength indices in old stellar populations using an evolutionary synthesis approach An interpretation of the line-strength indices in old stellar populations using an evolutionary synthesis approach

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...185...97a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 185, no. 1-2, Oct. 1987, p. 97-101.

Astronomy and Astrophysics

Astrophysics

9

Early Stars, Elliptical Galaxies, Galactic Clusters, Globular Clusters, H Beta Line, Stellar Spectrophotometry, Galactic Nuclei, Magnesium, Metallic Stars, Stellar Mass

Scientific paper

Evolutionary population synthesis models with different metallicities have been computed in order to interpret the observed Mg2 and Hβ, line-strength indices in old stellar populations. These models have been applied to three different cases, with the following results: (1) Galactic globular clusters do not exhibit a significant dispersion in age, and the metallicities of the computed models resemble those estimated for the clusters. The indices for the metal-poor globulars ([Fe/H] < -1) cannot be attained with these models due to the lack of low metallicity evolutionary tracks and stellar spectra libraries. (2) The line-strength gradients observed in the elliptical galaxy NGC 5813 are due, essentially, to intrinsic variations in metallicity, and they cannot be explained just from changes in the remaining parameters of the stellar population. (3) In order to synthesize the M32 indices it is necessary to introduce a star formation elapsed for a long time-scale, the star formation being still significant ≅5 Gyr ago.

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