paper

Evolutionary population synthesis: models, analysis of the ingredients and application to high-z galaxies

arXiv:astro-ph/0410207 · doi:10.1111/j.1365-2966.2005.09270.x

Abstract

Evolutionary population synthesis models for a wide range of metallicities, ages, star formation histories, and Horizontal Branch morphologies, including blue morphologies at high metallicity, are computed. The energetics of the post Main Sequence evolutionary phases are evaluated with the fuel consumption theorem. The impact on the models of the stellar evolutionary tracks is assessed. We find modest differences in synthetic broad-band colours as induced by the use of different tracks in our code (e.g. d(V-K) ~ 0.08 mag; d(B-V) ~ 0.03 mag). These differences are smaller than the scatter among other models in the literature, even when the latter adopt the same evolutionary tracks. The models are calibrated with globular cluster data from the Milky Way for old ages, and the Magellanic Clouds plus the merger remnant galaxy NGC 7252, for ages of ~ 0.1 - 2 Gyr, in a large wavelength range from U to K. Particular emphasis is put on the contribution from the Thermally-Pulsing Asymptotic Giant Branch phase. We show that this phase is crucial for the modelling of young stellar populations by the comparison with observed spectral energy distributions of Magellanic Clouds clusters, which are characterised by high fluxes both blueward and redward the V-band. We find that the combination of the near-IR spectral indices C2 and H2O can be used to determine the metallicity of ~ 1 Gyr stellar populations. We re-analyze the spectral energy distributions of some of the high-z galaxies (2.4 < z < 2.9) observed with the Spitzer Space Telescope by Yan et al. (2004). Their high rest-frame near-IR fluxes are reproduced very well with the models including Thermally-Pulsing Asymptotic Giant Branch stars for ages in the range 0.6-1.5 Gyr, suggesting formation redshifts around z ~ 3-6.

29 pages, 30 figures, MNRAS, in press. Very few minor revisions with respect to the submitted version. Improved Figures 2, 18, 19, 23 and 27. More models available at http://www-astro.physics.ox.ac.uk/~maraston/

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