Sánchez-Blázquez, P. and Jablonka, P. and Noll, S. and Poggianti, B. M. and Moustakas, J. and Milvang-Jensen, B. and Halliday, C. and Aragón-Salamanca, A. and Saglia, R. P. and Desai, V. and De Lucia, G. and Clowe, D. I. and Pelló, R. and Rudnick, G. and Simard, L. and White, S. D. M. and Zaritsky, D. (2009) Evolution of red-sequence cluster galaxies from redshift 0.8 to 0.4: ages, metallicities, and morphologies. Astronomy and Astrophysics, 499 (1). pp. 47-68. ISSN 0004-6361 http://resolver.caltech.edu/CaltechAUTHORS:20090910-133413787
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We present a comprehensive analysis of the stellar population properties and morphologies of red-sequence galaxies in 24 clusters and groups from z ~ 0.75 to z ~ 0.45. The dataset, consisting of 215 spectra drawn from the ESO Distant Cluster Survey, constitutes the largest spectroscopic sample at these redshifts for which such an analysis has been conducted. Analysis reveals that the evolution of the stellar population properties of red-sequence galaxies depend on their mass: while the properties of the most massive are well described by passive evolution and high-redshift formation, those of the less massive galaxies are consistent with a more extended star-formation history. We show that these scenarios reproduce the index-σ relations and the galaxy colours. The two main results of this work are: (1) the evolution of the line-strength indices for the red-sequence galaxies can be reproduced if 40% of the galaxies with σ < 175 km s^(−1) entered the red-sequence between z = 0.75 to z = 0.45, in agreement with the fraction derived in studies of the luminosity functions; and (2) the percentage of red-sequence galaxies exhibiting early-type morphologies (E and S0) decreases by 20% from z = 0.75 to z = 0.45. This can be understood if the red-sequence becomes more populated at later times with disc galaxies whose star formation has been quenched. We conclude that the processes quenching star formation do not necessarily produce a simultaneous morphological transformation of the galaxies entering the red-sequence.
|Additional Information:||© ESO 2009. Received 16 November 2008 / Accepted 14 February 2009. We thank the anonymous referee for useful suggestions that have improved the final presentation of the paper. PSB is supported by a Marie Curie Intra-European Fellowship within the 6th European Community Framework Programme. The Dark Cosmology Centre is funded by the Danish National Research Foundation.|
|Subject Keywords:||galaxies: evolution; galaxies elliptical and lenticular, cD; galaxies: clusters: general; galaxies: stellar content; galaxies: high-redshift; galaxies: abundances|
|Official Citation:||Evolution of red-sequence cluster galaxies from redshift 0.8 to 0.4: ages, metallicities, and morphologies P. Sánchez-Blázquez, P. Jablonka, S. Noll, B. M. Poggianti, J. Moustakas, B. Milvang-Jensen, C. Halliday, A. Aragón-Salamanca, R. P. Saglia, V. Desai, G. De Lucia, D. I. Clowe, R. Pelló, G. Rudnick, L. Simard, S. D. M. White and D. Zaritsky A&A 499 (1) 47-68 (2009) DOI: 10.1051/0004-6361/200811355|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Tony Diaz|
|Deposited On:||15 Sep 2009 15:44|
|Last Modified:||26 Dec 2012 11:21|
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