Abundance ratios in the hot ISM of elliptical galaxies

Abstract

To constrain the recipes put forth to solve the theoretical Fe discrepancy in the hot interstellar medium of elliptical galaxies and at the same time explain the [alpha/Fe] ratios. In order to do so we use the latest theoretical nucleosynthetic yields, we incorporate the dust, we explore differing SNIa progenitor scenarios by means of a self-consistent chemical evolution model which reproduces the properties of the stellar populations in elliptical galaxies. Models with Fe-only dust and/or a lower effective SNIa rate achieve a better agreement with the observed Fe abundance. However, a suitable modification to the SNIa yield with respect to the standard W7 model is needed to fully match the abundance ratio pattern. The 2D explosion model C-DDT by Maeda et al. (2010) is a promising candidate for reproducing the [Fe/H] and the [alpha/Fe] ratios. (A&A format)

11 pages, 4 figures, to appear on A&A

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• Why do many early-type galaxies lack emission lines? I. Fossil clues
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• On the connection between galactic downsizing and the most fundamental galactic scaling relations
• Cosmic Star Formation: a simple model of the SFRD(z)
• The two regimes of the cosmic sSFR evolution are due to spheroids and discs
• An In-Depth Study of the Abundance Pattern in the Hot Interstellar Medium in NGC 4649
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