Introducing the Illustris Project: simulating the coevolution of dark and visible matter in the Universe

Vogelsberger, Mark; Genel, Shy; Springel, Volker; Torrey, Paul; Sijacki, Debora; Xu, D.; Snyder, Gregory F.; Nelson, Dylan; Hernquist, Lars

doi:10.1093/mnras/stu1536

Cited by 2,235 publications

(1,921 citation statements)

References 134 publications

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“…The energy-driven scalings we predict are consistent with those assumed in state-of-the-art simulations that match observed properties of galaxies and the CGM (Dave et al 2013;Ford et al 2014;Genel et al 2014;Vogelsberger et al 2014). They are, however, somewhat different from that predicted by the Feedback in Realistic Galaxies (FIRE) suite of zoom simulations that also self-consistently drive outflows; the FIRE simulations find a shallower dependence for > v 60 circ km s −1 and a steeper dependence for smaller systems (Muratov et al 2015).…”

Section: Mass Loading Factor Evolutionsupporting

confidence: 76%

In-N-Out: The Gas Cycle From Dwarfs to Spiral Galaxies

Christensen

Davé

Governato

et al. 2016

ApJ

211

250

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We examine the scalings of galactic outflows with halo mass across a suite of 20 high-resolution cosmological zoom galaxy simulations covering halo masses in the range - . These simulations self-consistently generate outflows from the available supernova energy in a manner that successfully reproduces key galaxy observables, including the stellar mass-halo mass, Tully-Fisher, and mass-metallicity relations. We quantify the importance of ejective feedback to setting the stellar mass relative to the efficiency of gas accretion and star formation. Ejective feedback is increasingly important as galaxy mass decreases; we find an effective mass loading factor that scales asv circ 2.2 , with an amplitude and shape that are invariant with redshift. These scalings are consistent with analytic models for energy-driven wind, based solely on the halo potential. Recycling is common: about half of the outflow mass across all galaxy masses is later reaccreted. The recycling timescale is typically ∼1 Gyr, virtually independent of halo mass. Recycled material is reaccreted farther out in the disk and with typically ∼2-3 times more angular momentum. These results elucidate and quantify how the baryon cycle plausibly regulates star formation and alters the angular momentum distribution of disk material across the halo mass range where most cosmic star formation occurs.

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Section: Mass Loading Factor Evolutionsupporting

confidence: 76%

In-N-Out: The Gas Cycle From Dwarfs to Spiral Galaxies

Christensen

Davé

Governato

et al. 2016

ApJ

211

250

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“…At higher mass, it has been shown that additional feedback recipes are needed to prevent overcooling (e.g. Vernaleo & Reynolds 2006;Gabor et al 2011;Vogelsberger et al 2014;Schaye et al 2015).…”

Section: Merger Tree Selectionmentioning

confidence: 99%

Star formation in mergers with cosmologically motivated initial conditions

Karman

Macciò

Kannan

et al. 2015

Mon. Not. R. Astron. Soc.

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We use semi-analytic models and cosmological merger trees to provide the initial conditions for multi-merger numerical hydrodynamic simulations, and exploit these simulations to explore the effect of galaxy interaction and merging on star formation (SF). We compute numerical realisations of twelve merger trees from z = 1.5 to z = 0. We include the effects of the large hot gaseous halo around all galaxies, following recent obervations and predictions of galaxy formation models. We find that including the hot gaseous halo has a number of important effects. Firstly, as expected, the star formation rate on long timescales is increased due to cooling of the hot halo and refuelling of the cold gas reservoir. Secondly, we find that interactions do not always increase the SF in the long term. This is partially due to the orbiting galaxies transferring gravitational energy to the hot gaseous haloes and raising their temperature. Finally we find that the relative size of the starburst, when including the hot halo, is much smaller than previous studies showed. Our simulations also show that the order and timing of interactions are important for the evolution of a galaxy. When multiple galaxies interact at the same time, the SF enhancement is less than when galaxies interact in series. All these effects show the importance of including hot gas and cosmologically motivated merger trees in galaxy evolution models.

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“…Hence one needs to asses the relative importance of mergers versus smooth accretion driven by the cosmic environment and to study its induced morphological diversity. With the advent of large-scale albeit fairly well resolved cosmological hydrodynamical simulations such as Horizon-AGN , see as well Devriendt et al 2010;Khandai et al 2014;Vogelsberger et al 2014;Schaye et al 2015 for similar simulations performed with different numerical techniques), it has recently become feasible to investigate these different physical processes in detail and with sufficient statistics, a necessary requirement to truly unravel the impact of galaxy environment on their properties.…”

Section: Introductionmentioning

confidence: 99%

The rise and fall of stellar across the peak of cosmic star formation history: effects of mergers versus diffuse stellar mass acquisition

Welker

Dubois

Devriendt

et al. 2016

Mon. Not. R. Astron. Soc.

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Building galaxy merger trees from a state-of-the-art cosmological hydrodynamics simulation, Horizon-AGN, we perform a statistical study of how mergers and smooth accretion drive galaxy morphologic properties above z > 1. More specifically, we investigate how stellar densities, effective radii and shape parameters derived from the inertia tensor depend on mergers of different mass ratios. We find strong evidence that smooth accretion tends to flatten small galaxies over cosmic time, leading to the formation of disks. On the other hand, mergers, and not only the major ones, exhibit a propensity to puff up and destroy stellar disks, confirming the origin of elliptical galaxies. We also find that elliptical galaxies are more susceptible to grow in size through mergers than disc galaxies with a size-mass evolution r 0.5 ∝ M 1.2 s instead of r 0.5 ∝ M −0.5 s − M 0.5 depending on the merger mass ratio. The gas content drive the size-mass evolution due to merger with a faster size growth for gas-poor galaxies r 0.5 ∝ M 2 s than for gas-rich galaxies r 0.5 ∝ M s .

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Introducing the Illustris Project: simulating the coevolution of dark and visible matter in the Universe

Cited by 2,235 publications

References 134 publications

In-N-Out: The Gas Cycle From Dwarfs to Spiral Galaxies

In-N-Out: The Gas Cycle From Dwarfs to Spiral Galaxies

Star formation in mergers with cosmologically motivated initial conditions

The rise and fall of stellar across the peak of cosmic star formation history: effects of mergers versus diffuse stellar mass acquisition

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