The impact of α/Fe enhanced stellar evolutionary tracks on the ages of elliptical galaxies

We complement our study of=Fe enhanced stellar population models of Lick absorption indices (Thomas et al. 2003) by comparing two sets of=Fe enhanced models. In both models the impact on Lick indices due to=Fe enhancement is accounted for through a modification of the stellar absorption line-strengths using the response functions of Tripicco & Bell (1995). One set of models, however, uses solar-scaled, the other =Fe enhanced stellar evolutionary tracks. Since the =Fe enhanced tracks are hotter than the solar-scaled ones (Salasnich et al. 2000), the correspondent stellar population models have slightly weaker metallic indices (i.e. Mg b,hFei etc.) and stronger Balmer line indices (H) (Maraston et al. 2003). Here we explore quantitatively the impact of this eect on the=Fe ratios, metallicities and ages that are derived for elliptical galaxies. We find that the modest decrease of the metallic indices Mg b andhFei balance each other, such that fully consistent=Fe ratios are derived for stellar systems using =Fe enhanced models with either solar-scaled or =Fe enhanced stellar tracks. The decrease of the metallic indices and the increase of H conspire in a way that also consistent metallicities are obtained. The derived ages, instead, are significantly dierent. The inclusion of=Fe enhanced stellar tracks leads to the derivation of ages as high as30 Gyr for elliptical galaxies. For the same objects, ages not older than 15 Gyr are obtained, if =Fe enhanced models using solar-scaled tracks are adopted. This may indicate that current stellar evolutionary models overestimate the bluing of stellar evolutionary tracks due to=Fe enhanced chemical mixtures at super-solar metallicities.