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Preprint typeset using LATEX style emulateapj v. 12/14/05 THE EVOLUTION OF SPIRAL, S0 AND ELLIPTICAL GALAXIES IN CLUSTERS

By Bianca M. Poggianti, Giovanni Fasano, Daniela Bettoni, Antonio Cava, A. Dressler, E. Vanzella, Warrick J. Couch, Jacopo Fritz, Per Kjaergaard, Mariano Moles and T. Valentinuzzi

Abstract

We quantify the evolution of the spiral, S0 and elliptical fractions in galaxy clusters as a function of cluster velocity dispersion (σ) and X-ray luminosity (LX) using a new database of 72 nearby clusters from the WIde-Field Nearby Galaxy-cluster Survey (WINGS) combined with literature data at z = 0.5 − 1.2. Most WINGS clusters have σ between 500 and 1100 kms −1, and LX between 0.2 and 5 × 10 44 erg/s. The S0 fraction in clusters is known to increase with time at the expense of the spiral population. We find that the spiral and S0 fractions have evolved more strongly in lower σ, less massive clusters. The proportion of ellipticals has remained unchanged in clusters with σ> 800kms −1, but has increased with time in less massive clusters. Our results demonstrate that morphological evolution since z = 1 is not confined to massive clusters, but is actually more pronounced in low mass clusters, and therefore must originate either from secular (intrinsic) evolution and/or from environmental mechanisms that act preferentially in low-mass environments, or both in low- and high-mass systems. We also find that the evolution of the spiral fraction perfectly mirrors the evolution of the fraction of star-forming galaxies. Interestingly, at low-z the spiral fraction anticorrelates, and the S0 and elliptical fractions weakly correlate, with LX. Conversely, no correlation is observed between morphologica

Year: 2009
OAI identifier: oai:CiteSeerX.psu:10.1.1.244.5309
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