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The evolution of the galactic morphological types in clusters

By Giovanni Fasano, Bianca M. Poggianti, Warrick J. Couch, Daniela Bettoni and Per Kjærgaard

Abstract

The morphological types of galaxies in nine clusters in the redshift range 0.1 < ∼ z < ∼ 0.25 are derived from very good seeing images taken at the NOT and the La Silla–Danish telescopes, with all galaxies at MV < −20 and within the central ∼1 Mpc 2 area being classified. With the purpose of investigating the evolution of the fraction of different morphological types with redshift, we compare our results with the morphological content of nine distant clusters studied by the MORPHS group (Dressler et al. 1997), five clusters observed with HST-WFPC2 at redshift z = 0.2 − 0.3 (Couch et al.1998), and Dressler’s (1980) large sample of nearby clusters. After having checked the reliability of our morphological classification both in an absolute sense and relative to the MORPHS scheme (Smail et al.1997), we analyze the relative occurrence of elliptical, S0 and spiral galaxies as a function of the cluster properties and redshift. We find a large intrinsic scatter in the S0/E ratio, mostly related to the cluster morphology. In particular, in our cluster sample, clusters with a high concentration of ellipticals display a low S0/E rati

Year: 2000
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