paper

Stellar populations, neutral hydrogen and ionised gas in field early-type galaxies

arXiv:0712.2852 · doi:10.1051/0004-6361:20078954

Abstract

We present a study of the stellar populations of a sample of 39 local, field early-type galaxies whose HI properties are known from interferometric data. Our aim is to understand whether stellar age and chemical composition depend on the HI content of galaxies. As a by-product of our analysis, we also study their ionised gas content and how it relates to the neutral hydrogen gas. Stellar populations and ionised gas are studied from optical long-slit spectra. We determine stellar age, metallicity and alpha-to-iron ratio by analysing a set of Lick/IDS line-strength indices measured from the spectra after modelling and subtracting the ionised-gas emission. We do not find any trend in the stellar populations parameters with M(HI). However, we do find that, at stellar velocity dispersion below 230 km/s, 2/3 of the galaxies with less than 100 million solar masses of HI are centrally rejuvenated, while none of the HI-richer systems are. Furthermore, none of the more massive (velocity-dispersion>230 km/s) objects are centrally rejuvenated independently on their HI mass. Concerning the ionised gas, we detect emission in 60% of the sample. This is generally extended and always carachterised by LINER-like emission-line ratios at any radius. We find that a large HI mass is necessary (but not sufficient) for a galaxy to host bright ionised-gas emission. A plausible interpretation of our results is that gas-rich mergers play a significant role in E/S0 formation, especially at lower mass. Within this picture, HI-poor, centrally-rejuvenated objects could form in mergers where gas angular-momentum removal (and therefore inflow) is efficient; HI-rich galaxies with no significant age gradients (but possibly uniformly young) could be formed in interactions characterised by high-angular momentum gas.

arXiv commentAccepted for publication in Astronomy & Astrophysics, 17 pages, 10 figures, 5 tables, 1 appendix

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