Integrated Spectroscopy of Bulge Globular Clusters and Fields. II. Implications for stellar population models and elliptical galaxies

Details Integrated Spectroscopy of Bulge Globular Clusters and Fields. II. Implications for stellar population models and elliptical galaxies Integrated Spectroscopy of Bulge Globular Clusters and Fields. II. Implications for stellar population models and elliptical galaxies

2002-09-11

arxiv.org/abs/astro-ph/0209220v2

Astron.Astrophys. 400 (2003) 823-840

Astronomy and Astrophysics

Astrophysics

19 pages, 13 figures, Astronomy and Astrophysics in press. Only minor changes after the referee report

Scientific paper

10.1051/0004-6361:20021723

Synthetic Lick indices (e.g. Mg_2, Fe, etc.) of Simple Stellar Population (SSP) models are calibrated for the first time up to solar metallicity with a sample of Milky Way globular clusters (GCs) which includes the metal rich GCs of the Galactic bulge. This metallicity range is relevant to elliptical galaxies. It is shown that the Bulge GCs and integrated light follow the same correlation between Mg and Fe indices of elliptical galaxies, showing weaker Fe indices at given Mg indices with respect to models that assume solar-scaled abundances. This similarity is the robust empirical evidence for enhanced alpha/Fe ratios in the stellar populations of elliptical galaxies, since the globular clusters are independently known to be alpha-enhanced. The uniqueness of this alpha-overabundance solution is checked by exploring the whole range of model ingredients. We argue that the standard models reproduce the Mg-Fe correlation at low metallicities because the stellar templates used in the synthesis are the alpha-enhanced stars of the galactic Halo. These same models, however, fail to recover the Mg-Fe pattern of Bulge clusters and ellipticals at high metallicities because the high-metallicity templates are disk stars, which are not alpha-enhanced. The new SSP models by Thomas, Maraston & Bender (2002) which incorporate the dependence on alpha/Fe reproduce the Mg and Fe indices of GCs at all metallicities, with alpha/Fe=+0.3, which is in agreement with spectroscopic abundance determinations. The Balmer indices (Hbeta, Hdelta, Hgamma) are very well calibrated, provided the Horizontal Branch morphology is taken into account. In particular, we reproduce the Balmer lines of NGC 6388 and NGC 6441, which are metal-rich GCs with a tail of warm Horizontal Branch stars. {Abridged}

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