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Title:
Kinematic Properties and Stellar Populations of Faint Early-Type Galaxies. II. Line-Strength Measurements of Central Coma Galaxies
Authors:
Matković, A.; Guzmán, R.; Sánchez-Blázquez, P.; Gorgas, J.; Cardiel, N.; Gruel, N.
Affiliation:
AA(Astronomy Department, University of Florida, P.O. Box 112055, Gainesville, FL 32611, USA ), AB(Astronomy Department, University of Florida, P.O. Box 112055, Gainesville, FL 32611, USA ), AC(Centre for Astrophysics, University of Central Lancashire, PR1 2HE, Preston, UK ), AD(Departamento de Astrofísica, Facultad de Físicas, Universidad Complutense de Madrid, Ciudad Universitaria, 28040 Madrid, Spain), AE(Departamento de Astrofísica, Facultad de Físicas, Universidad Complutense de Madrid, Ciudad Universitaria, 28040 Madrid, Spain), AF(Astronomy Department, University of Florida, P.O. Box 112055, Gainesville, FL 32611, USA )
Publication:
The Astrophysical Journal, Volume 691, Issue 2, pp. 1862-1878 (2009). (ApJ Homepage)
Publication Date:
02/2009
Origin:
IOP
ApJ Keywords:
galaxies: abundances, galaxies: clusters: individual: Coma, galaxies: dwarf, galaxies: elliptical and lenticular, cD
DOI:
10.1088/0004-637X/691/2/1862
Bibliographic Code:
2009ApJ...691.1862M

Abstract

We present line-strength measurements for 74 early-type galaxies in the core of the Coma cluster reaching down to velocity dispersions, σ, of 30 km s-1. The index-σ relations for our sample, including galaxies with σ < 100 km s-1 (low-σ), differ in shape depending on which index is used. We note two types of relations for the metallic indices: one showing a break in the slope around ~100 km s-1 and another group with strong linear relations between an index and log σ. We find no connection between the behavior of index-σ relations with either α- or Fe-peak elements. However, we find indications that the relations are tighter for indices which do not depend on the microturbulent velocities of stellar atmospheres. We confirm previous results that low-σ galaxies including dE/dS0s are on average younger, less metal rich, and have lower [α/Fe] in comparison with E/S0s. Our data show that these trends derived for high-σ galaxies extend down to dE/dS0s. This is a factor of ~2 lower in σ than previously published work. We confirm that the observed anticorrelation between age and metallicity for high-σ galaxies is consistent with the effects of correlated errors. Low-σ galaxies also show a similar relation between age and metallicity as a result of correlated errors. However, they are offset from this relationship so that, on average, they are less metal rich and younger than their high-σ counterparts.
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