Open AccessThe stellar populations of early‐type galaxies in the Fornax cluster
Author(s) -
Kuntschner Harald
Publication year - 2000
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1046/j.1365-8711.2000.03377.x
Subject(s) - physics , astrophysics , elliptical galaxy , metallicity , galaxy , stellar population , astronomy , velocity dispersion , lenticular galaxy , fornax cluster , surface brightness fluctuation , star formation
We have measured central line strengths for a magnitude‐limited sample of early‐type galaxies in the Fornax cluster, comprising 11 elliptical (E) and 11 lenticular (S0) galaxies, more luminous than M B =−17. When compared with single‐burst stellar population models we find that the centres of Fornax ellipticals follow a locus of fixed age and have metallicities varying roughly from half solar to twice solar. The centres of (lower luminosity) lenticular galaxies, however, exhibit a substantial spread to younger luminosity‐weighted ages, indicating a more extended star formation history. Galaxies with old stellar populations show tight scaling relations between metal‐line indices and the central velocity dispersion. Remarkably also, the Fe lines are well correlated with σ 0 . Our detailed analysis of the stellar populations suggests that these scaling relations are driven mostly by metallicity. Galaxies with a young stellar component do generally deviate from the main relation. In particular, the lower luminosity S0s show a large spread. Our conclusions are based on several age/metallicity diagnostic diagrams in the Lick/IDS system comprising established indices such as Mg 2 and H β as well as new and more sensitive indices such as H γ A and Fe3, a combination of three prominent Fe lines. The inferred difference in the age distribution between lenticular and elliptical galaxies is a robust conclusion, as the models generate consistent relative ages using different age and metallicity indicators, even though the absolute ages remain uncertain. The absolute age uncertainty is mainly caused by the effects of non‐solar abundance ratios which are not yet accounted for by the stellar population models. Furthermore, we find that elliptical galaxies and the bulge of one bright S0 are overabundant in magnesium, where the most luminous galaxies show the strongest overabundances. The stellar populations of young and faint S0s are consistent with solar abundance ratios or a weak Mg underabundance. Two of the faintest lenticular galaxies in our sample have blue continua and extremely strong Balmer‐line absorption, suggesting star formation <2 Gyr ago.