A model for cosmological simulations of galaxy formation physics: multi-epoch validation

By P. Torrey, M. Vogelsberger, Shy Genel, D. Sijacki, Volker Springel, Lars Hernquist HarvardCfA, I. Cambridge, Hits. 2013

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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 performance of a recently implemented feedback model which includes primordial and metal line radiative cooling with self-shielding corrections; stellar evolution with associated mass loss and chemical enrichment; feedback by stellar winds; black hole seeding, growth and merging; and AGN quasar- and radio-mode heating with a phenomenological prescription for AGN electro-magnetic feedback. We illustrate the impact of the model parameter choices on the resulting simulated galaxy population properties at high and intermediate redshifts. We demonstrate that our scheme is capable of producing galaxy populations that broadly reproduce the observed galaxy stellar mass function extending from redshift z=0 to z=3. We also characterise the evolving galactic B-band luminosity function, stellar mass to halo mass ratio, star formation main sequence, Tully-Fisher relation, and gas-phase mass-metallicity relation and confront them against recent observational estimates. This detailed comparison allows us to validate elements of our feedback model, while also identifying areas of tension that will be addressed in future work.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/4f9c7a8a3ff85b8a7b577665dc206e8ee73ed319

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Citations in the corpus

Supermassive black holes and their feedback effects in the IllustrisTNG simulation (2017, methodology): “We employ a similar scaling in the thermal mode, where we use the approach of Vogelsberger et al. (2013) and reduce the accretion rate by a factor of (Pext/Pref) 2 whenever Pext < Pref.”
Vertical disc heating in Milky Way-sized galaxies in a cosmological context (2015, methodology): “We briefly summarise here some of the most important physical processes implemented in arepo, and re- MNRAS 000, 1–1 (2015) fer the interested reader to Vogelsberger et al. (2013) and Marinacci et al. (2014a) for more details.”
Introducing the Illustris Project: simulating the coevolution of dark and visible matter in the Universe (2014, methodology): “Our implementation is described in detail in Vogelsberger et al. (2013) and Torrey et al. (2014).”
Gusty, gaseous flows of FIRE: Galactic winds in cosmological simulations with explicit stellar feedback (2015, background): “We focus on comparing our results to the Illustris project (Vogelsberger et al. 2013, hereafter V13), as well as the simulations presented in Ford et al. (2014, hereafter F14).”
A new class of accurate, mesh-free hydrodynamic simulation methods (2014, methodology): “This has been used in a wide range of previous and current work on cosmological galaxy formation (e.g. Springel & Hernquist 2003b; Robertson et al. 2004; Di Matteo et al. 2005; Hopkins et al. 2006, 2008a,b; Narayanan et al. 2006; Vogelsberger et al. 2013).”
Ingredients for 21 cm Intensity Mapping (2018, methodology): “The numerical methods and subgrid physics models build upon Vogelsberger et al. (2013), and are specified in full in Weinberger et al. (2017a,b) and Pillepich et al. (2017b).”
Radiative feedback and the low efficiency of galaxy formation in low-mass haloes at high redshift (2013, background): “Torrey et al. (2014) report fstars=0.4-0.7% atz = 2 for the same halo mass.”
Theoretical Challenges in Galaxy Formation (2016, background): “…specific implementations see e.g. Ceverino & Klypin 2009; Kravtsov 2003; Oppenheimer & Davé 2006; Scannapieco et al. 2005; Tornatore et al. 2007; Vogelsberger et al. 2013; Wiersma, Schaye & Smith 2009) of gas in the presence of the UV/X-ray background radiation from quasars and galaxies (e.g.…”
Dancing in the dark: galactic properties trace spin swings along the cosmic web (2014, background): “Vogelsberger et al. (2013) manage to reproduce the low-mass tail of the stellar-to-halo mass relation by decoupling hydrodynamically the launched wind gas from the dense star-forming gas (as introduced by Springel & Hernquist 2003).”
Massive Black Hole Binary Mergers in Dynamical Galactic Environments (2016, neutral): “For a comprehensive presentation of the galaxy formation models (e.g. cooling, inter-stellar medium, stellar evolution, chemical enrichment) see the papers: Vogelsberger et al. (2013) and Torrey et al. (2014).”
Galaxy morphology and star formation in the Illustris Simulation at z = 0 (2015, methodology): “Torrey et al. (2014) showed that the Illustris model approximately reproduces this trend at z = 0, and we find again that its location and slope in this plot is the same as that found by Whitaker et al. (2012).”
The Illustris simulation: the evolving population of black holes across cosmic time (2014, methodology): “Here we are specifically interested in the basic black hole properties, while the convergence of other quantities has been discussed in Vogelsberger et al. (2013); Torrey et al. (2014); Genel et al. (2014).”
The origin and evolution of the galaxy mass–metallicity relation (2015, background): “At z = 0, Torrey et al. (2014) and the Lu model show steeper slopes at the low-mass end, due to the low metal retention efficiency in low-mass galaxies, a consequence of invoking strong outflows to suppress star formation in these galaxies5.”
(Star)bursts of FIRE: observational signatures of bursty star formation in galaxies (2015, background): “This relation is also important because its normalisation and scatter may provide important constraints on galaxy formation physics (Torrey et al. 2014; Sparre et al. 2015; Furlong et al. 2015; Mitra et al. 2015; but cf. Kelson 2014).”
The illustris simulation: Public data release (2015, methodology): “ty eects. For complete details on the behavior, implementation, parameter selection, and validation of these physical models, see Vogelsberger et al. (2013), which describes the feedback models, and Torrey et al. (2014), which compares the model output with observations from z= 0 to z= 3. The Illust”
First results from the TNG50 simulation: galactic outflows driven by supernovae and black hole feedback (2019, background): “…simulations sometimes including such hard-coded directionality by hand (Springel & Hernquist 2003), including in the original Illustris model (Vogelsberger et al. 2013), but this was removed in TNG mainly as an opportunity to simplify an unnecessarily complex model feature (Pillepich et al.…”
Neutral hydrogen in galaxy haloes at the peak of the cosmic star formation history (2014, background): “These include temporarily suppressing hydrodynamical interactions (e.g., Hernquist & Springel 2003; Oppenheimer & Davé 2006; Vogelsberger et al. 2013; Ford et al. 2013; Marinacci et al. 2014) or gas cooling (e.g., Stinson et al. 2006; Governato et al. 2007; Shen et al. 2010; Guedes et al. 2011) as…”