Introducing the Illustris Project: the evolution of galaxy populations across cosmic time

  title={Introducing the Illustris Project: the evolution of galaxy populations across cosmic time},
  author={Shy Genel and Mark Vogelsberger and Volker Springel and Debora Sijacki and Dylan Nelson and Gregory F. Snyder and Vicente Rodriguez-Gomez and Paul Torrey and Lars E. Hernquist},
  journal={Monthly Notices of the Royal Astronomical Society},
We present an overview of galaxy evolution across cosmic time in the Illustris Simulation. Illustris is an N-body/hydrodynamical simulation that evolves 2*1820^3 resolution elements in a (106.5Mpc)^3 box from cosmological initial conditions down to z=0 using the AREPO moving-mesh code. The simulation uses a state-of-the-art set of physical models for galaxy formation that was tuned to reproduce the z=0 stellar mass function and the history of the cosmic star-formation rate density. We find that… 
The Illustris simulation: the evolving population of black holes across cosmic time
We study the properties of black holes and their host galaxies across cosmic time in the Illustris simulation. Illustris is a large-scale cosmological hydrodynamical simulation which resolves a
The Illustris++ Project: The Next Generation of Cosmological Hydrodynamical Simulations of Galaxy Formation
Cosmological simulations of galaxy formation provide the most powerful technique for calculating the non-linear evolution of cosmic structure formation. This approach starts from initial conditions
Simulating galaxy formation with the IllustrisTNG model
We introduce an updated physical model to simulate the formation and evolution of galaxies in cosmological, large-scale gravity+magnetohydrodynamical simulations with the moving mesh code AREPO. The
The Horizon-AGN simulation: evolution of galaxy properties over cosmic time
We compare the predictions of Horizon-AGN, a hydro-dynamical cosmological simulation that uses an adaptive mesh refinement code, to observational data in the redshift range 0 6. We study the
The stellar mass assembly of galaxies in the Illustris simulation: growth by mergers and the spatial distribution of accreted stars
We use the Illustris simulation to study the relative contributions of in situ star formation and stellar accretion to the build-up of galaxies over an unprecedentedly wide range of masses (M_* =
The formation and evolution of dust in semi-analytic models of galaxy formation
The formation and evolution of galaxies is an interesting subject to study because it incorporates astrophysics from all scales, from the initial perturbations in the early universe creating the
The Auriga Project: the properties and formation mechanisms of disc galaxies across cosmic time
We introduce a suite of 30 cosmological magneto-hydrodynamical zoom simulations of the formation of galaxies in isolated Milky Way mass dark haloes. These were carried out with the moving mesh code
Cosmic Large-Scale Structure in the IllustrisTNG Simulations
We have finished two new, extremely large hydrodynamical simulations of galaxy formation that significantly advance the state of the art in cosmology. Together with accompanying dark matter only
The merger rate of galaxies in the Illustris simulation: a comparison with observations and semi-empirical models
We have constructed merger trees for galaxies in the Illustris simulation by directly tracking the baryonic content of subhaloes. These merger trees are used to calculate the galaxy–galaxy merger
First results from the IllustrisTNG simulations: matter and galaxy clustering
Hydrodynamical simulations of galaxy formation have now reached sufficient volume to make precision predictions for clustering on cosmologically relevant scales. Here we use our new IllustrisTNG


A model for cosmological simulations of galaxy formation physics: multi-epoch validation
We present a multi-epoch analysis of the galaxy populations formed within the cosmological hydrodynamical simulations presented in Vogelsberger et al. (2013). These simulations explore the
Shaping the galaxy stellar mass function with supernova- and AGN-driven winds
Cosmological hydrodynamical simulations of galaxy formation in representative regions of the Universe typically need to resort to subresolution models to follow some of the feedback processes crucial
The evolution of the galaxy stellar mass function is especially useful to test the current model of galaxy formation. Observational data have revealed a few inconsistencies with predictions from the
The formation of disc galaxies in high-resolution moving-mesh cosmological simulations
We present cosmological hydrodynamical simulations of eight Milky Way-sized haloes that have been previously studied with dark matter only in the Aquarius project. For the first time, we employ the
Galactic star formation and accretion histories from matching galaxies to dark matter haloes
We present a new statistical method to determine the relationship between the stellar masses of galaxies and the masses of their host dark matter haloes over the entire cosmic history from z � 4 to
The Evolution of Central Group Galaxies in Hydrodynamical Simulations
We trace the evolution of central galaxies in three ∼1013 M☉ galaxy groups simulated at high resolution in cosmological hydrodynamical simulations. In all three cases, the evolution in the group
A central challenge in observational studies of galaxy formation is how to associate progenitor galaxies with their descendants at lower redshifts. One promising approach is to link galaxies at fixed
A recipe for galaxy formation
We present a detailed prescription for how galaxy formation can be modelled in hierarchical theories of structure formation. Our model incorporates the formation and merging of dark matter halos, the
We discuss early results from the first N-body/hydrodynamical simulation to resolve the formation of galaxies in a volume large enough for their clustering properties to be reliably determined. The
Simulations of the formation, evolution and clustering of galaxies and quasars
It is shown that baryon-induced features in the initial conditions of the Universe are reflected in distorted form in the low-redshift galaxy distribution, an effect that can be used to constrain the nature of dark energy with future generations of observational surveys of galaxies.