Morphological Evolution of Galaxies to $z \sim 4$

Abstract

Galaxies have clearly evolved since the universe was 1 Gyr old, but methods to trace and quantify this evolution are still in their infancy. In this paper I demonstrate that with the careful use of a 'physical morphology' it is possible to determine quantitatively how the process of galaxy evolution is occurring out to z ∼ 4. Using a system of parameters that traces star formation and galaxy interactions, I show how distinct galaxy populations at high-z can be identified in deep high-resolution optical and NIR images. These tools are also used to measure a potential merger fraction of galaxies from 0 < z < 4. If these methods are reliable, as is suggested by a local galaxy calibration, the merger fraction of galaxies scales α (1+z) 2.1±0.5 , peaks near z ∼ 2, and declines thereafter. I also discuss how this system is likely part of the ultimate physical classification of galaxies.