Properties of galaxies reproduced by a hydrodynamic simulation

By M. Vogelsberger, Shy Genel, Volker Springel, P. Torrey, D. Sijacki, Da Xu, Gregory F. Snyder, Simeon Bird, D. Nelson, Lars Hernquist Mit and 5 more. Nature, 2014

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Previous simulations of the growth of cosmic structures have broadly reproduced the ‘cosmic web’ of galaxies that we see in the Universe, but failed to create a mixed population of elliptical and spiral galaxies, because of numerical inaccuracies and incomplete physical models. Moreover, they were unable to track the small-scale evolution of gas and stars to the present epoch within a representative portion of the Universe. Here we report a simulation that starts 12 million years after the Big Bang, and traces 13 billion years of cosmic evolution with 12 billion resolution elements in a cube of 106.5 megaparsecs a side. It yields a reasonable population of ellipticals and spirals, reproduces the observed distribution of galaxies in clusters and characteristics of hydrogen on large scales, and at the same time matches the ‘metal’ and hydrogen content of galaxies on small scales.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

FIRE in the field: Simulating the threshold of galaxy formation (2016, methodology): “Both the Illustris (Vogelsberger et al. 2014) and EAGLE (Schaye et al. 2015) simulations, which are hydrodynamic simulations with homogeneous mass resolution that cover large volumes at significantly lower resolution (dark matter particle masses of ∼ 106 M ) than our zoom-ins, find that halos in the”
The Illustris simulation: the evolving population of black holes across cosmic time (2014, methodology): “For further details of the simulations see Vogelsberger et al. (2014) and Genel et al. (2014).”
The IllustrisTNG simulations: public data release (2018, methodology): “Recent examples reaching z = 0 include Illustris (Vogelsberger et al. 2014a; Genel et al. 2014), EAGLE (Schaye et al. 2015; Crain et al. 2015), Horizon-AGN (Dubois et al. 2014), Romu-lus (Tremmel et al. 2017), Simba (Davé et al. 2019), Mag-neticum (Dolag et al. 2016), among others.”
First results from the IllustrisTNG simulations: radio haloes and magnetic fields (2017, methodology): “The IllustrisTNG1 simulation series is the follow-up project of the Illustris simulation suite (Vogelsberger et al. 2014a,b; Genel et al. 2014; Nelson et al. 2015; Sijacki et al. 2015).”
How to Measure Galaxy Star Formation Histories. II. Nonparametric Models (2018, methodology): “Appendix A compares the chosen prior for log(SFR(t)/SFR(t+ ∆t)) against a distribution of this quantity measured from realistic star formation histories taken from the Illustris hydrodynamical simulation (Vogelsberger et al. 2014a,b; Torrey et al. 2014).”
Consistent modelling of the meta-galactic UV background and the thermal/ionization history of the intergalactic medium (2018, background): “Many state of the art cosmological hydrodynamical simulation projects, such as, e.g, Illustris (Vogelsberger et al. 2014) or Eagle (Schaye et al. 2015), follow photoionization and photoheating under the simplifying assumption of ionization equilibrium in the presence of an external UV background.”
Three-phase Interstellar Medium in Galaxies Resolving Evolution with Star Formation and Supernova Feedback (TIGRESS): Algorithms, Fiducial Model, and Convergence (2016, background): “…(e.g., Behroozi et al. 2013; Moster et al. 2013), the Kennicutt-Schmidt relation (Kennicutt 1998), star formation history, and other properties (e.g., Hopkins et al. 2014; Vogelsberger et al. 2014; Crain et al. 2015; Schaye et al. 2015; Agertz & Kravtsov 2016; Davé et al. 2016; Keller et al. 2016).”
Introducing the Illustris Project: simulating the coevolution of dark and visible matter in the Universe (2014, background): “The total matter power spectrum of Illustris-1 and Illustris-Dark-1 was presented and discussed in Vogelsberger et al. (2014).”
The Horizon-AGN Simulation: Morphological Diversity of Galaxies ,Promoted by AGN Feedback (2016, background): “…simulations including the necessary physics to produce a morphological mix of galaxies such as Horizon-AGN (Dubois et al. 2014), Illustris (Vogelsberger et al. 2014), or Eagle (Schaye et al. 2015), it now becomes feasible to investigate in detail, and with statistical significance the…”
Core Cosmology Library: Precision Cosmological Predictions for LSST (2018, background): “…impact of baryonic physics on the distribution of matter, which is known to exceed the per cent level at scales k & 1 Mpc−1 (van Daalen et al. 2011; Vogelsberger et al. 2014; Hellwing et al. 2016; Springel et al. 2017; Chisari et al. 2018) and can affect the extraction of cosmological parameters…”
First results from the TNG50 simulation: galactic outflows driven by supernovae and black hole feedback (2019, background): “…clarified the need for efficient outflows in order to make realistic galaxy populations whose characteristics and integral properties are roughly in agreement with observational constraints (Vogelsberger et al. 2014; Genel et al. 2014; Crain et al. 2015; Schaye et al. 2015; Dubois et al. 2016).”
The size evolution of star-forming and quenched galaxies in the IllustrisTNG simulation (2017, background): “1011 M in the original Illustris simulation (Vogelsberger et al. 2014a,b; Genel et al. 2014) are larger than observed galaxies by roughly a factor of 2 (Snyder et al. 2015; Bottrell et al. 2017; Furlong et al. 2017).”
The optical morphologies of galaxies in the IllustrisTNG simulation: a comparison to Pan-STARRS observations (2018, methodology): “…Digital Sky Survey (SDSS, York et al. 2000), and on the theoretical side with largescale hydrodynamic cosmological simulations such as Illustris (Vogelsberger et al. 2014a,b; Genel et al. 2014), EAGLE (Schaye et al. 2015; Crain et al. 2015), and Horizon-AGN (Dubois et al. 2014). c© 0000 The…”
The stellar mass assembly of galaxies in the Illustris simulation: growth by mergers and the spatial distribution of accreted stars (2015, methodology): “…we note that we also examined the dependence of the ex situ stellar mass fraction on galaxy overdensity (not shown), using a definition based on the distance to the 5th nearest neighbour with an r-band magnitude brighter than −19.5 (Vogelsberger et al. 2014b), but found no significant correlation.”
Physical Models of Galaxy Formation in a Cosmological Framework (2014, methodology): “They produced a bimodal color magnitude diagram, with a red galaxy fraction as a function of stellar mass and environment in good agreement with observations by Peng et al. (2010) and others (Vogelsberger et al. 2014a).”
The EAGLE project: Simulating the evolution and assembly of galaxies and their environments (2014, methodology): “…radiative losses in the ISM are to generate the outflow outside the galaxy or to turn off the hydrodynamic interaction between the wind and the ISM (e.g. Springel & Hernquist 2003; Oppenheimer & Davé 2006; Oppenheimer et al. 2010; Puchwein & Springel 2013; Vogelsberger et al. 2013, 2014b).”
The star formation main sequence and stellar mass assembly of galaxies in the Illustris simulation (2014, background): “Genel et al. (2014) and Vogelsberger et al. (2014a) found similar deviations between the Illustris simulation and abundance matching results when analysing the high- and lowmass ends of the stellar mass function.”
An Older, More Quiescent Universe from Panchromatic SED Fitting of the 3D-HST Survey (2018, methodology): “The prior is tuned to allow similar transitions in SFR(t) to those of galaxies in the Illustris hydrodynamical simulations (Torrey et al. 2014; Vogelsberger et al. 2014a, 2014b; Diemer et al. 2017), though it is deliberately set to encompass broader behavior than is seen in these simulations.”
Galaxy formation in the Planck cosmology – I. Matching the observed evolution of star formation rates, colours and stellar masses (2014, background): “…and cosmological hydrodynamics simulations form low-mass galaxies too early, leading to an overabundance of lower mass galaxies (M⋆ ∼ 1010 M⊙) at z > 1 (Fontanot et al. 2009; Henriques et al. 2011; Guo et al. 2011; Weinmann et al. 2012; Lu et al. 2013; Genel et al. 2014; Vogelsberger et al. 2014).”