Modelling the evolution of galaxies as a function of environment

Abstract

In this review, I provide an overview of theoretical aspects related to the evolution of galaxies as a function of environment. I discuss the main physical processes at play, their characteristic time-scales and environmental dependency, and comment on their treatment in the framework of hierarchical galaxy formation models. I briefly summarize recent results and the main open issues.

Invited Review given at the Workshop "Environment and the Formation of Galaxies: 30 years later" held in Lisbon, 6-7 September 2010

References in corpus (11)

• From dwarf spheroidals to cDs: Simulating the galaxy population in a LCDM cosmology
• A Semi-Analytic Model for the Co-evolution of Galaxies, Black Holes, and Active Galactic Nuclei
• The effect of galaxy mass ratio on merger--driven starbursts
• Ram pressure stripping the hot gaseous halos of galaxies in groups and clusters
• The Importance of Mergers for the Origin of Intracluster Stars in Cosmological Simulations of Galaxy Clusters
• Ram pressure stripping of disc galaxies orbiting in clusters. I. Mass and radius of the remaining gas disc
• Modelling and interpreting the dependence of clustering on the spectral energy distributions of galaxies
• A semi-analytic model comparison - gas cooling and galaxy mergers
• Ram pressure histories of cluster galaxies
• The dependence of AGN activity on stellar and halo mass in Semi-Analytic Models
• Gas cooling in semi-analytic models and SPH simulations: are results consistent?

Cited by in corpus (6)

• The environmental history of group and cluster galaxies in a LambdaCDM Universe
• The GALEX Ultraviolet Virgo Cluster Survey (GUViCS). IV: The role of the cluster environment on galaxy evolution
• Spectacular tails of ionised gas in the Virgo cluster galaxy NGC 4569
• The influence of the environmental history on quenching star formation in a $\Lambda$CDM universe
• Galaxy evolution in protoclusters
• The Stellar Mass Assembly of Low Redshift, Massive, Central Galaxies in SDSS and the TNG300 simulation