TY - JOUR
T1 - The fundamental plane of EDisCS galaxies The effect of size evolution
AU - Saglia...[et al.], RP
AU - Sanchuez-Blazques, P.
AU - Bender, R.
AU - Milvang-Jensen, Bo
PY - 2010/11/19
Y1 - 2010/11/19
N2 - 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 Re, surface brightness Ie, and velocity dispersions s) for 154 cluster and 68 field galaxies. On average, we achieve precisions of 10% in Re, 0.1 dex in logIe, and 10% in s. 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 I1 = 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 δlog M/LB = (-0.54 ± 0.01)z = (-1.61 ± 0.01) log(1 + z) in clusters, independent of their velocity dispersion. The evolution is stronger (δlog M/LB = (-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 a and ß 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 × 1011 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 Re . (1 + z)-0.5±0.2 and s . (1 + z)0.41±0.08, at fixed dynamical masses, and Re . (1 + z)-0.68±0.4 and s . (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 LB . (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 (≤1011 M) cluster galaxies are old (with a formation redshift zf ≥ 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.
AB - 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 Re, surface brightness Ie, and velocity dispersions s) for 154 cluster and 68 field galaxies. On average, we achieve precisions of 10% in Re, 0.1 dex in logIe, and 10% in s. 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 I1 = 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 δlog M/LB = (-0.54 ± 0.01)z = (-1.61 ± 0.01) log(1 + z) in clusters, independent of their velocity dispersion. The evolution is stronger (δlog M/LB = (-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 a and ß 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 × 1011 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 Re . (1 + z)-0.5±0.2 and s . (1 + z)0.41±0.08, at fixed dynamical masses, and Re . (1 + z)-0.68±0.4 and s . (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 LB . (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 (≤1011 M) cluster galaxies are old (with a formation redshift zf ≥ 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.
U2 - 10.1051/0004-6361/201014703
DO - 10.1051/0004-6361/201014703
M3 - Journal article
SN - 0004-6361
VL - 524
SP - A6
JO - Astronomy and Astrophysics Supplement Series
JF - Astronomy and Astrophysics Supplement Series
ER -