The Stellar Population Histories of Local Early-Type Galaxies. I. Population Parameters

Details The Stellar Population Histories of Local Early-Type Galaxies. I. Population Parameters The Stellar Population Histories of Local Early-Type Galaxies. I. Population Parameters

2000-01-06

arxiv.org/abs/astro-ph/0001072v1

Astron.J.119:1645-1676,2000

Astronomy and Astrophysics

Astrophysics

Accepted to the Astronomical Journal, April 2000. 35 pages, 15 figures. Uses emulateapj.sty

Scientific paper

10.1086/301299

We present single stellar population (SSP) equivalent ages, metallicities, and abundance ratios for local elliptical galaxies derived from Hbeta, Mgb, and absorption line strengths. We use an extension of the Worthey (1994) stellar population models that incorporates non-solar line-strength "response functions" by Tripicco & Bell (1995), allowing us to correct the models for the enhancements of Mg and other alpha-like elements relative to the Fe-peak elements. SSP-equivalent ages of local ellipticals from Gonzalez (1993) are found to vary widely, 1.5 < t < 18 Gyr, while metallicities [Z/H] and enhancement ratios [E/Fe] are strongly peaked around <[Z/H]>=+0.26 and <[E/Fe]>=+0.20 (in an aperture of radius Re/8). The enhancement ratios are milder than previous estimates, owing to the application of non-solar abundance corrections to both Mgb and for the first time. Gradients in stellar populations within galaxies are found to be mild, with SSP-equivalent age decreasing by 25%, metallicity decreasing by <[Z/H]>=0.20 dex, and [E/Fe] remaining nearly constant out to an aperture of radius Re/2 for nearly all systems. Our ages have an overall zeropoint uncertainty of at least 25% due to uncertainties in the stellar evolution prescription, the oxygen abundance, the effect of non-solar abundances on the isochrones, and other unknowns. However, the relative age rankings of stellar populations should be largely unaffected by these errors. In particular, the large spread in ages appears to be real and cannot be explained by contamination of Hbeta by blue stragglers or hot horizontal branch stars, or by fill-in of Hbeta by emission. Correlations between these derived SSP-equivalent parameters and other galaxy observables will be discussed in future papers. (Abridged)

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