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Evolution of red-sequence cluster galaxies from redshift 0.8 to 0.4: ages, metallicities, and morphologies

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. https://resolver.caltech.edu/CaltechAUTHORS:20090910-133413787

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Abstract

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.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/200811355DOIArticle
http://www.aanda.org/index.php?option=article&access=doi&doi=10.1051/0004-6361/200811355PublisherArticle
ORCID:
AuthorORCID
Poggianti, B. M.0000-0001-8751-8360
Desai, V.0000-0002-1340-0543
Rudnick, G.0000-0001-5851-1856
Zaritsky, D.0000-0002-5177-727X
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.
Group:Infrared Processing and Analysis Center (IPAC)
Funders:
Funding AgencyGrant Number
Marie Curie FellowshipUNSPECIFIED
Dasnish National Research FoundationUNSPECIFIED
Subject Keywords:galaxies: evolution; galaxies elliptical and lenticular, cD; galaxies: clusters: general; galaxies: stellar content; galaxies: high-redshift; galaxies: abundances
Issue or Number:1
Record Number:CaltechAUTHORS:20090910-133413787
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20090910-133413787
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.
ID Code:15734
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:15 Sep 2009 15:44
Last Modified:28 Oct 2019 17:15

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