TY - JOUR
T1 - Physical Models of Galaxy Formation in a Cosmological Framework
AU - Somerville, Rachel S.
AU - Davé, Romeel
PY - 2015/8/1
Y1 - 2015/8/1
N2 - Modeling galaxy formation in a cosmological context presents one of the
greatest challenges in astrophysics today due to the vast range of
scales and numerous physical processes involved. Here we review the
current status of models that employ two leading techniques to simulate
the physics of galaxy formation: semianalytic models and numerical
hydrodynamic simulations. We focus on a set of observational targets
that describe the evolution of the global and structural properties of
galaxies from roughly cosmic high noon (z â¼ 2-3) to the
present. Although minor discrepancies remain, overall, models show
remarkable convergence among different methods and make predictions that
are in qualitative agreement with observations. Modelers have converged
on a core set of physical processes that are critical for shaping galaxy
properties. This core set includes cosmological accretion, strong
stellar-driven winds that are more efficient at low masses, black hole
feedback that preferentially suppresses star formation at high masses,
and structural and morphological evolution through merging and
environmental processes. However, all cosmological models currently
adopt phenomenological implementations of many of these core processes,
which must be tuned to observations. Many details of how these diverse
processes interact within a hierarchical structure formation setting
remain poorly understood. Emerging multiscale simulations are helping to
bridge the gap between stellar and cosmological scales, placing models
on a firmer, more physically grounded footing. Concurrently, upcoming
telescope facilities will provide new challenges and constraints for
models, particularly by directly constraining inflows and outflows
through observations of gas in and around galaxies.
AB - Modeling galaxy formation in a cosmological context presents one of the
greatest challenges in astrophysics today due to the vast range of
scales and numerous physical processes involved. Here we review the
current status of models that employ two leading techniques to simulate
the physics of galaxy formation: semianalytic models and numerical
hydrodynamic simulations. We focus on a set of observational targets
that describe the evolution of the global and structural properties of
galaxies from roughly cosmic high noon (z â¼ 2-3) to the
present. Although minor discrepancies remain, overall, models show
remarkable convergence among different methods and make predictions that
are in qualitative agreement with observations. Modelers have converged
on a core set of physical processes that are critical for shaping galaxy
properties. This core set includes cosmological accretion, strong
stellar-driven winds that are more efficient at low masses, black hole
feedback that preferentially suppresses star formation at high masses,
and structural and morphological evolution through merging and
environmental processes. However, all cosmological models currently
adopt phenomenological implementations of many of these core processes,
which must be tuned to observations. Many details of how these diverse
processes interact within a hierarchical structure formation setting
remain poorly understood. Emerging multiscale simulations are helping to
bridge the gap between stellar and cosmological scales, placing models
on a firmer, more physically grounded footing. Concurrently, upcoming
telescope facilities will provide new challenges and constraints for
models, particularly by directly constraining inflows and outflows
through observations of gas in and around galaxies.
U2 - 10.1146/annurev-astro-082812-140951
DO - 10.1146/annurev-astro-082812-140951
M3 - Article
SN - 0066-4146
VL - 53
SP - 51
EP - 113
JO - Annual Review of Astronomy and Astrophysics
JF - Annual Review of Astronomy and Astrophysics
ER -