Chemo-evolutionary Population Synthesis II. (Vazdekis+ 1997)

Details Chemo-evolutionary Population Synthesis II. (Vazdekis+ 1997) Chemo-evolutionary Population Synthesis II. (Vazdekis+ 1997)

Jul 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997ycat..21110203v&link_type=abstract

VizieR On-line Data Catalog: J/ApJS/111/203. Originally published in: 1997ApJS..111..203V

Other

Models: Evolutionary, Abundances

Scientific paper

We present the results of applying a new chemo-evolutionary stellar population model, developed in a previous paper, to new high-quality observational data of the nuclear regions of two representative elliptical galaxies and the bulge of the Sombrero galaxy. Here we fit in detail ~20 absorption lines and six optical and near-infrared colors, following two approaches: fitting a single-age, single-metallicity model and fitting our full chemical evolutionary model. We find that all the iron lines are weaker than the best-fitting models predict, indicating that the iron abundance is anomalous and deficient. We also find that the Ca I index at 4227 A is much lower than predicted by the models. We can obtain good fits for all the other lines and observed colors with models of old and metal-rich stellar populations and can show that the observed radial gradients are due to metallicity decreasing outward. We find that good fits are obtained both with fully evolutionary models and with single-age, single-metallicity models. This is due to the fact that in the evolutionary model more than 80% of the stars form within 1.5 Gyr after the formation of the galaxies. The fact that slightly better fits are obtained with evolutionary models indicates that these galaxies contain a small spread in metallicity. (3 data files).

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