Claudio Dalla Vecchia
Pedro Alonso Palicio, Chris Brook, Andrea Negri, Arianna Di Cintio, Mónica Hernández Sánchez
A. Sánchez (Max Planck Institute for Extraterrestrial Physics, Garching); S. Khochfar (Royal Observatory, Edinburgh); T. Theuns (Institute for Computational Cosmology, Durham); I. McCarthy (John Moores University, Liverpool); R. Crain (John Moores University, Liverpool); S. Kay (University of Manchester); Y. Bahé (Leiden Observatory, Leiden); J. Schaye (Leiden Observatory, Leiden); A, Maccio (NYUAD); A. Obreja (University Observatory Munich)
How galaxies formed and evolved through cosmic time is one of the key questions of modern astronomy and astrophysics. Cosmological time- and length-scales are so large that the evolution of individual galaxies cannot be directly observed. Only through numerical simulations can one follow the emergence of cosmic structures within the current cosmological paradigm.
The main physical processes in galaxy formation and evolution are gravity, hydrodynamics, gas cooling, star formation, stellar evolution, supernova (SN) and black hole (BH) feedback. These are highly non-linear, thus difficult to describe with analytic models. Moreover, the presence of baryonic matter induces biases that collisionless (“dark matter”) simulations alone cannot reproduce (e.g. van Daalen et al. 2014, MNRAS, 440, 2997; Velliscig et al. 2014, MNRAS, 442, 2641). Semi-analytic models based on these simulations require ad hoc corrections to account for these biases. Hydrodynamical, cosmological simulations are therefore the preferred tool for conducting “controlled experiments” of galaxy formation and evolution.
After three decades of advances in numerical simulations, theorists have only recently been able to reproduce simultaneously the observed properties of the present day galaxy population and the inter-galactic medium (e.g. EAGLE, Schaye et al. 2015, MNRAS, 446, 521; ILLUSTRIS, Vogelsberger et al., 2014, Nature, 509, 177). In particular, the luminosity and mass function of galaxies, the galaxy size- and metallicity-mass relations, and many other properties are now reproduced over a large range of galaxy stellar masses.
Numerical tools are available for investigating the physics of galaxy formation and evolution with unprecedented detail. To date, little effort has been concentrated in studying the properties of the full galaxy population in group and cluster environments. Galaxy groups and clusters are excellent laboratories for studying physical processes, such as mergers, tidal stripping and ram-pressure stripping. It is known these processes shape galaxies at any epoch in cosmic history, but it is not known how, combined, they yield the observed population of cluster galaxies. Moreover, little effort has been put in studying the secular evolution of galaxies with self-consistent models of galaxy formation, and much has to be done to link secular processes to galaxy evolution. Finally, cosmological simulations are reaching the sophistication required to describe the Local Group environment in great detail. New theoretical results in these fields will be useful for interpreting the data of current and future ground- and space-based galaxy surveys like MANGA, WEAVE, GAIA and EUCLID.