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The fundamental plane of EDisCS galaxies: The effect of size evolution

Saglia, R. P. and Sánchez-Blázquez, P. and Bender, R. and Simard, L. and Desai, V. and Aragón-Salamanca, A. and Milvang-Jensen, B. and Halliday, C. and Jablonka, P. and Noll, S. and Poggianti, B. and Clowe, D. I. and De Lucia, G. and Pelló, R. and Rudnick, G. and Valentinuzzi, T. and White, S. D. M. and Zaritsky, D. (2010) The fundamental plane of EDisCS galaxies: The effect of size evolution. Astronomy and Astrophysics, 524 . Art. NO. A6. ISSN 0004-6361. https://resolver.caltech.edu/CaltechAUTHORS:20101220-114217618

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Abstract

We study the evolution of spectral early-type galaxies in clusters, groups, and the field up to redshift 0.9 using the ESO Distant Cluster Survey (EDisCS) dataset. We measure structural parameters (circularized half-luminosity radii R_e, surface brightness I_e, and velocity dispersions σ) for 154 cluster and 68 field galaxies. On average, we achieve precisions of 10% in R_e, 0.1 dex in log I_e, and 10% in σ. We sample ≈20% of cluster and ≈10% of field spectral early-type galaxies to an I band magnitude in a 1 arcsec radius aperture as faint as I_1 = 22. We study the evolution of the zero point of the fundamental plane (FP) and confirm results in the literature, but now also for the low cluster velocity dispersion regime. Taken at face value, the mass-to-light ratio varies as Δ log M/L_B = (-0.54 ± 0.01) z = (-1.61 ± 0.01) log (1+z) in clusters, independent of their velocity dispersion. The evolution is stronger (Δ log M/L_B = (-0.76 ± 0.01) z = (-2.27 ± 0.03) log (1+z)) for field galaxies. A somewhat milder evolution is derived if a correction for incompleteness is applied. A rotation in the FP with redshift is detected with low statistical significance. The α and β FP coefficients decrease with redshift, or, equivalently, the FP residuals correlate with galaxy mass and become progressively negative at low masses. The effect is visible at z ≥ 0.7 for cluster galaxies and at lower redshifts z ≥ 0.5 for field galaxies. We investigate the size evolution of our galaxy sample. In agreement with previous results, we find that the half-luminosity radius for a galaxy with a dynamical or stellar mass of 2 × 10^(11) M_☉ varies as (1+z)^(-1.0±0.3) for both cluster and field galaxies. At the same time, stellar velocity dispersions grow with redshift, as (1+z)^(0.59±0.10) at constant dynamical mass, and as (1+z)^(0.34±0.14) at constant stellar mass. The measured size evolution reduces to R_e ∝ (1+z)^(-0.5±0.2) and σ ∝ (1+z)^(0.41±0.08), at fixed dynamical masses, and Re ∝ (1+z)^(-0.68±0.4) and σ ∝ (1+z)^(0.19±0.10), at fixed stellar masses, when the progenitor bias (PB, galaxies that locally are of spectroscopic early-type, but are not very old, disappear progressively from the EDisCS high-redshift sample; often these galaxies happen to be large in size) is taken into account. Taken together, the variations in size and velocity dispersion imply that the luminosity evolution with redshift derived from the zero point of the FP is somewhat milder than that derived without taking these variations into account. When considering dynamical masses, the effects of size and velocity dispersion variations almost cancel out. For stellar masses, the luminosity evolution is reduced to LB (1+z)1.0 for cluster galaxies and L_B ∝ (1+z)^(1.67) for field galaxies. Using simple stellar population models to translate the observed luminosity evolution into a formation age, we find that massive (>10^(11) M_☉) cluster galaxies are old (with a formation redshift z_f > 1.5) and lower mass galaxies are 3–4 Gyr younger, in agreement with previous EDisCS results from color and line index analyses. This confirms the picture of a progressive build-up of the red sequence in clusters with time. Field galaxies follow the same trend, but are ≈1 Gyr younger at a given redshift and mass. Taking into account the size and velocity dispersion evolution quoted above pushes all formation ages upwards by 1 to 4 Gyr.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1051/0004-6361/201014703DOIArticle
http://www.aanda.org/articles/aa/abs/2010/16/aa14703-10/aa14703-10.htmlPublisherArticle
http://dx.doi.org/10.1051/0004-6361/201014703eDOICorrigendum
ORCID:
AuthorORCID
Desai, V.0000-0002-1340-0543
Poggianti, B.0000-0001-8751-8360
Rudnick, G.0000-0001-5851-1856
Zaritsky, D.0000-0002-5177-727X
Additional Information:© 2010 ESO. Received 1 April 2010; Accepted 2 September 2010; Published online 19 November 2010. Based on observations collected at the European Southern Observatory, Paranal and La Silla, Chile, as part of the ESO LP 166.A-0162. This work was supported by the Sonderforschungsbereich 375 of the German Research Foundation. The Dark Cosmology Centre is funded by the Danish National Research Foundation. GDL acknowledges financial support from the European Research Council under the European Community’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement n. 202781. The anonymous referee report helped us improve the presentation of the results.
Funders:
Funding AgencyGrant Number
Deutsche Forschungsgemeinschaft (DFG)SFB 375
Danish National Research FoundationUNSPECIFIED
European Research Council (ERC)202781
Subject Keywords:galaxies: elliptical and lenticular, cD; galaxies: evolution; galaxies: formation; galaxies: fundamental parameters
Record Number:CaltechAUTHORS:20101220-114217618
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20101220-114217618
Official Citation:The fundamental plane of EDisCS galaxies - The effect of size evolution R. P. Saglia, P. Sánchez-Blázquez, R. Bender, L. Simard, V. Desai, A. Aragón-Salamanca, B. Milvang-Jensen, C. Halliday, P. Jablonka, S. Noll, B. Poggianti, D. I. Clowe, G. De Lucia, R. Pelló, G. Rudnick, T. Valentinuzzi, S. D. M. White and D. Zaritsky A&A 524 A6 (2010) DOI: 10.1051/0004-6361/201014703
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:21444
Collection:CaltechAUTHORS
Deposited By: Jason Perez
Deposited On:21 Dec 2010 18:44
Last Modified:03 Oct 2019 02:24

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