Quantitative Morphology of Galaxies in the Core of the Coma Cluster

Details Quantitative Morphology of Galaxies in the Core of the Coma Cluster Quantitative Morphology of Galaxies in the Core of the Coma Cluster

2003-10-19

arxiv.org/abs/astro-ph/0310527v1

Astrophys.J. 602 (2004) 664-677

Astronomy and Astrophysics

Astrophysics

34 pages, 12 figures, Accepted for publication in ApJ

Scientific paper

10.1086/381022

We present a quantitative morphological analysis of 187 galaxies in a region covering the central 0.28 square degrees of the Coma cluster. Structural parameters from the best-fitting Sersic r^{1/n} bulge plus, where appropriate, exponential disc model, are tabulated here. This sample is complete down to a magnitude of R=17 mag. By examining the Edwards et al. (2002) compilation of galaxy redshifts in the direction of Coma, we find that 163 of the 187 galaxies are Coma cluster members, and the rest are foreground and background objects. For the Coma cluster members, we have studied differences in the structural and kinematic properties between early- and late-type galaxies, and between the dwarf and giant galaxies. Analysis of the elliptical galaxies reveals correlations among the structural parameters similar to those previously found in the Virgo and Fornax clusters. Comparing the structural properties of the Coma cluster disc galaxies with disc galaxies in the field, we find evidence for an environmental dependence: the scale lengths of the disc galaxies in Coma are 30% smaller. A kinematical analysis shows marginal differences between the velocity distributions of ellipticals with Sersic index n<2 (dwarfs) and those with n>2 (giants); the dwarf galaxies having a greater (cluster) velocity dispersion. Finally, our analysis of all 421 background galaxies reveals a non-uniform distribution in redshift with contrasts in density ~3, characterized by a void extending from ~10,000 to ~20,000 km s^{-1}, and two dense and extended structures centred at ~20,000 and ~47,000 km s^{-1}.

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