Recent Structural Evolution of Early‐Type Galaxies: Size Growth from z = 1 to z = 0

Abstract

Strong size and internal density evolution of early-type galaxies between z ∼ 2 and the present has been reported by several authors. Here we analyze samples of nearby and distant (z ∼1) galaxies with dynamically measured masses in order to confirm the previous, model-dependent results and constrain the uncertainties that may play a role. Velocity dispersion (σ) measurements are taken from the literature for 50 morphologically selected 0.8 < z < 1.2 field and cluster early-type galaxies with typical masses M dyn = 2 ×10 11 M ̇ . Sizes (R eff ) are determined with Advanced Camera for Surveys imaging. We compare the distant sample with a large sample of nearby(0.04 < z < 0.08) early-type galaxies extracted from the Sloan Digital Sky Survey for which we determine sizes, masses, and densities in a consistent manner, using simulations to quantify systematic differences between the size measurements of nearby and distant galaxies. We find a highly significant difference between the σ-R eff distributions of the nearby and distant samples, regardless of sample selection effects. The implied evolution in R eff at fixed mass between z = 1 and the present is a factor of 1.97 ±0.15. This is in qualitative agreement with semianalytic models; however, the observed evolution is much faster than the predicted evolution. Our results reinforce and are quantitatively consistent with previous, photometric studies that found size evolution of up to a factor of 5 since z ∼ 2. A combination of structural evolution of individual galaxies through the accretion of companions and the continuous formation of early-type galaxies through increasingly gas-poor mergers is one plausible explanation of the observations. © 2008. The American Astronomical Society. All rights reserved.