Ages and Metallicities in Elliptical Galaxies from the H_beta, <Fe>, and Mg2 Diagnostics

Details Ages and Metallicities in Elliptical Galaxies from the H_beta, <Fe>, and Mg2 Diagnostics Ages and Metallicities in Elliptical Galaxies from the H_beta, <Fe>, and Mg2 Diagnostics

1997-10-22

arxiv.org/abs/astro-ph/9710246v3

Astronomy and Astrophysics

Astrophysics

15 pages, LaTeX file with 10 figures using l-aa-dipastro.sty. Will appear in A&A, Vol. 333

Scientific paper

Systematic variations in the line strength indices H_beta, Mg2, and are observed across elliptical galaxies and from one object to another. Furthermore arguments are given for an enhancement of Mg (\alfa in general) with respect to Fe toward the center of these galaxies. In this study we have investigated the ability of the H_beta, Mg2 and diagnostics to assess the metallicity, [Mg/Fe] ratios, and ages of elliptical galaxies. To this aim, first we derive basic calibrations for the variations dH_beta, dMg2 and d as a function of Dlog(t), Dlog(Z/Zo), and D[Mg/Fe]. Second, we analyze how the difference dH_beta, dMg2, and d between the external and central values translates into D[Mg/Fe], Dlog(Z/Zo), and Dlog(t). Third, we explore the variation from galaxy to galaxy of the nuclear values of H_beta, Mg2, and limited to a sub-sample of the Gonzales (1993) list. The differences dH_beta, dMg2, and d are converted into the differences Dlog(t), Dlog(Z/Zo), and D[Mg/Fe]. Various correlations among the age, metallicity, and enhancement variations are explored. In particular we thoroughly examine the relationship Dlog(t)-Mv. It is found that a sort of age limit is likely to exist in this plane, traced by galaxies with mild or no sign of rejuvenation. In these objects, the duration of the star forming activity is likely to have increased at decreasing galactic mass. The results are discussed in the context of current theories of galaxy formation and evolution. i.e. merger and isolation. Finally, the suggestion is advanced that models with time and space dependent IMF might be able to alleviate some of the difficulties encountered by the standard SN-driven galactic wind model.

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