MUFASA: Galaxy Formation Simulations With Meshless Hydrodynamics
By R. Dav'e, Robert J. Thompson, P. Hopkins. 2016
223 citations recorded by the source corpus.
We present the mufasa suite of cosmological hydrodynamic simulations, which employs the gizmo meshless finite mass (MFM) code including H_2-based star formation, nine-element chemical evolution, two-phase kinetic outflows following scalings from the Feedback in Realistic Environments zoom simulations, and evolving halo mass-based quenching. Our fiducial (50 h^(−1) Mpc)^3 volume is evolved to z = 0 with a quarter billion elements. The predicted galaxy stellar mass functions (GSMFs) reproduces observations from z = 4 → 0 to ≲ 1.2σ in cosmic variance, providing an unprecedented match to this key diagnostic. The cosmic star formation history and stellar mass growth show general agreement with data, with a strong archaeological downsizing trend such that dwarf galaxies form the majority of their stars after z ∼ 1. We run 25 and 12.5 h^(−1) Mpc volumes to z = 2 with identical feedback prescriptions, the latter resolving all hydrogen-cooling haloes, and the three runs display fair resolution convergence. The specific star formation rates broadly agree with data at z = 0, but are underpredicted at z ∼ 2 by a factor of 3, re-emphasizing a longstanding puzzle in galaxy evolution models. We compare runs using MFM and two flavours of smoothed particle hydrodynamics, and show that the GSMF is sensitive to hydrodynamics methodology at the ∼×2 level, which is sub-dominant to choices for parametrizing feedback.
Subfields: Astronomy and Astrophysics, Instrumentation
View Paper: https://www.semanticscholar.org/paper/8c0beb6cddf374d21f1164730181e6ae1e638831
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Citations in the corpus
- FIRE-2 simulations: physics versus numerics in galaxy formation (2017, methodology): “Similarly, Davé et al. (2016) compare low-resolution cosmological large-volume simulations using a simplified, non-FIRE subgrid ISM and feedback model and MFM and “P-SPH” (FIRE-1 SPH) methods in GIZMO.”
- Near infrared spectroscopy and star-formation histories of 3 ≤ z ≤ 4 quiescent galaxies (2018, methodology): “…exceeds that predicted by state-of-the-art cosmological simulations, with and without AGN feedback (e.g., Wellons et al. 2015; Sparre et al. 2015; Davé et al. 2016), and requires a formation channel at z > 5 with SFRs larger than observed in the mostly dustfree Lyman-break galaxies (LBGs; e.g.,…”
- simba: Cosmological simulations with black hole growth and feedback (2019, methodology): “The Simba simulations utilise much of the framework of the Mufasa simulations as described in Davé et al. (2016), but there are a number of updates and additions based on recent theoretical and observations results, in addition to the major change of modeling black hole growth and feedback as well…”
- RECONCILING DWARF GALAXIES WITH ΛCDM COSMOLOGY: SIMULATING A REALISTIC POPULATION OF SATELLITES AROUND A MILKY WAY–MASS GALAXY (2016, background): “That said, several tests (Hopkins 2015; Davé et al. 2016; Hopkins et al., in prep.) also show that using MFM versus P-SPH does not significantly change (.”
- First results from the IllustrisTNG simulations: the galaxy colour bimodality (2017, background): “In concert with other large-volume efforts (Dubois et al. 2016; Dolag et al. 2016; Davé et al. 2016) these projects have convincingly demonstrated that hydrodynamical simulations of structure formation at kilo-parsec spatial resolution can reasonably reproduce the fundamental properties and…”
- 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).”
- HIRAX: a probe of dark energy and radio transients (2016, methodology): “In addition, these simulations will use combinations of analytical models, hydrodynamical N-body code (See Ref.13) and treatment of instrumental effects and of polarized foregrounds (See Ref.14).”
- UniverseMachine: The correlation between galaxy growth and dark matter halo assembly from z = 0−10 (2018, unknown): “This coincides with existing tensions between SSFRs from observations and SSFRs from modern hydrodynamical simulations (e.g., Sparre et al. 2015; Davé et al. 2016), as well as tensions between IR and SED-fit SFR indicators (Fang et al. 2018): SFRobs−SFRtrue = µ +κ exp ( − (z−2) 2 2 ) (25) The prior…”
- Inferring the star formation histories of massive quiescent galaxies with bagpipes: evidence for multiple quenching mechanisms (2017, methodology): “(14) MNRAS 000, 1–23 (2017) 4.3 Generating mock observations of Mufasa galaxies Mufasa (Davé et al. 2016) is a suite of cosmological hydrodynamic simulations which correctly reproduces many of the observed properties of the population of quenched galaxies at z = 0, including the slope of the red…”