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Larger sizes of massive quiescent early-type galaxies in clusters than in the field at 0.8 < z < 1.5

Delaye, L. and Huertas-Company, M. and Mei, S. and Lidman, C. and Licitra, R. and Newman, A. and Raichoor, A. and Shankar, F. and Barrientos, F. and Bernardi, M. and Cerulo, P. and Couch, W. and Demarco, R. and Muñoz, R. and Sánchez-Janssen, R. and Tanaka, M. (2014) Larger sizes of massive quiescent early-type galaxies in clusters than in the field at 0.8 < z < 1.5. Monthly Notices of the Royal Astronomical Society, 441 (1). pp. 203-223. ISSN 0035-8711. http://resolver.caltech.edu/CaltechAUTHORS:20140620-131059224

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Abstract

We analyse the mass–size relation of ∼400 quiescent massive ETGs (M_*/M_⊙ > 3 × 10^(10)) hosted by massive clusters (M_(200 ∼ 2–7) × 10^(14)M_⊙) at 0.8 < z < 1.5, compared to those found in the field at the same epoch. Size is parametrized using the mass-normalized B-band rest-frame size, γ=R_e/M^(0.57)_(11). We find that the γ distributions in both environments peak at the same position, but the distributions in clusters are more skewed towards larger sizes. This tail induces average sizes ∼30–40 per cent larger for cluster galaxies than for field galaxies of similar stellar mass, while the median sizes are statistically the same with a difference of ∼10 ± 10 per cent. Since this size difference is not observed in the local Universe, the evolution of average galaxy size at fixed stellar mass from z ∼ 1.5 for cluster galaxies is less steep at more than 3σ (∝(1 + z)^(−0.53 ± 0.04)) than the evolution of field galaxies (∝(1 + z)^(−0.92 ± 0.04)). The difference in evolution is not measured when the median values of γ are considered: ∝(1 + z)^(−0.84 ± 0.04) in the field versus ∝(1 + z)^(−0.71 ± 0.05) in clusters. In our sample, the tail of large galaxies is dominated by galaxies with 3 × 10^(10) < M_*/M_⊙ < 10^(11). At this low-mass end, the difference in the average size is better explained by the accretion of new galaxies that are quenched more efficiently in clusters and/or by different morphological mixing in the cluster and field environments. If part of the size evolution would be due to mergers, the difference that we see between cluster and field galaxies could be caused by higher merger rates in clusters at higher redshift, when galaxy velocities are lower.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/1307.0003arXivArticle
http://mnras.oxfordjournals.org/content/441/1/203.abstractPublisherArticle
http://dx.doi.org/10.1093/mnras/stu496DOIArticle
http://mnras.oxfordjournals.org/content/441/1/203/suppl/DC1Related ItemSupporting Information
Additional Information:© 2014 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. Accepted 2014 March 9. Received 2014 February 28; in original form 2013 May 2. The authors would like to thank G. Rousset for pointing out interesting suggestions and E. Daddi, V. Strazzulo, R. Gobat for stimulating discussions. RD gratefully acknowledges the support provided by the BASAL Center for Astrophysics and Associated Technologies (CATA), and by FONDECYT grant no. 1130528.
Group:COSMOS
Funders:
Funding AgencyGrant Number
BASAL Center for Astrophysics and Associated Technologies (CATA)UNSPECIFIED
FONDECYT1130528
Subject Keywords:galaxies: clusters: general galaxies: elliptical and lenticular galaxies: evolution
Record Number:CaltechAUTHORS:20140620-131059224
Persistent URL:http://resolver.caltech.edu/CaltechAUTHORS:20140620-131059224
Official Citation:L. Delaye, M. Huertas-Company, S. Mei, C. Lidman, R. Licitra, A. Newman, A. Raichoor, F. Shankar, F. Barrientos, M. Bernardi, P. Cerulo, W. Couch, R. Demarco, R. Muñoz, R. Sánchez-Janssen, and M. Tanaka Larger sizes of massive quiescent early-type galaxies in clusters than in the field at 0.8 < z < 1.5 MNRAS (June 11, 2014) Vol. 441 203-223 doi:10.1093/mnras/stu496
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:46400
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:20 Jun 2014 20:42
Last Modified:19 Nov 2015 00:54

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