The eagle simulations of galaxy formation: the importance of the hydrodynamics scheme

Schaller, Matthieu; Vecchia, Claudio Dalla; Schaye, Joop; Bower, Richard G.; Theuns, Tom; Crain, Robert A.; Furlong, Michelle; McCarthy, Ian G.

doi:10.1093/mnras/stv2169

Cited by 700 publications

(1,047 citation statements)

References 91 publications

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“…This is due to the fact that the fluctuations in the density and velocity field in SPH simulations are on the order of a percent level, while the magnitude of other sources of errors, such as gas cooling rate and supernova feedback, are much larger (Zhu et al 2015). For example, Schaller et al (2015) compared the results obtained with "Anar-chy SPH" and the original Gadget formulation. They conclude that the properties of the most galaxies such as stellar masses and galaxy size are not significantly affected by the choice of SPH solver.…”

Section: Numerical Methods Vs Physical Modelsmentioning

confidence: 99%

The Formation of a Milky Way-Sized Disk Galaxy. I. A Comparison of Numerical Methods

Zhu

2016

ApJ

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The long-standing challenge of creating a Milky Way-like disk galaxy from cosmological simulations has motivated significant developments in both numerical methods and physical models. We investigate these two fundamental aspects in a new comparison project using a set of cosmological hydrodynamic simulations of a Milky Way-size galaxy. In this study, we focus on the comparison of two particle-based hydrodynamics methods: an improved smoothed particle hydrodynamics (SPH) code Gadget, and a Lagrangian Meshless Finite-Mass (MFM) code Gizmo. All the simulations in this paper use the same initial conditions and physical models, which include star formation, "energy-driven" outflows, metaldependent cooling, stellar evolution and metal enrichment. We find that both numerical schemes produce a late-type galaxy with extended gaseous and stellar disks. However, notable differences are present in a wide range of galaxy properties and their evolution, including star formation history, gas content, disk structure and kinematics. Compared to Gizmo, Gadget simulation produced a larger fraction of cold, dense gas at high redshift which fuels rapid star formation and results in a higher stellar mass by 20% and a lower gas fraction by 10% at z = 0, and the resulting gas disk is smoother and more coherent in rotation due to damping of turbulent motion by the numerical viscosity in SPH, in contrast to the Gizmo simulation which shows more prominent spiral structure. Given its better convergence properties and lower computational cost, we argue that MFM method is a promising alternative to SPH in cosmological hydrodynamic simulations.

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Section: Numerical Methods Vs Physical Modelsmentioning

confidence: 99%

The Formation of a Milky Way-Sized Disk Galaxy. I. A Comparison of Numerical Methods

Zhu

2016

ApJ

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“…The main modifications to the entropy-conserving SPH implementation of the GADGET-3 code (Springel & Hernquist 2003a) comprise (i) the pressure-entropy SPH formulation described by Hopkins (2013), (ii) the artificial viscosity switch of Cullen & Dehnen (2010), (iii) the artificial conduction switch of Price (2008), (iv) the time step limiter from Durier & Dalla Vecchia (2012) to improve energy conservation during sudden changes of internal energy, and (v) a C2 Wendland (1995) 58-neighbour kernel to suppress particlepairing instabilities (Dehnen & Aly 2012). Collectively, these updates are referred to as 'Anarchy' (Dalla Vecchia, in preparation; see also appendix A of S15) and the impact of their inclusion on the galaxy population was explored by Schaller et al (2015).…”

Section: The Eagle Simulation Codementioning

confidence: 99%

Bimodality of low-redshift circumgalactic O vi in non-equilibrium eagle zoom simulations

Oppenheimer¹,

Crain

Schaye

et al. 2016

Mon. Not. R. Astron. Soc.

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208

271

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Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details.

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“…The simulations were performed by using a modified version of the GADGET-3 smoothed particle hydrodynamics (SPH) code (last described by Springel 2005). The modifications to the SPH implementation are collectively referred to as ANARCHY (Dalla Vecchia, in preparation; see also Schaller et al 2015).…”

Section: T H E E Ag L E S I M U L At I O N Smentioning

confidence: 99%

Galaxy metallicity scaling relations in the EAGLE simulations

Rossi

Bower

Font

et al. 2017

Monthly Notices of the Royal Astronomical Society

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138

136

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Citation for published item:he ossiD w r¡ % imili nd fowerD i h rd qF nd pontD endree F nd h yeD toop nd heunsD om @PHIUA 9q l xy met lli ity s ling rel tions in the ieqvi simul tionsF9D wonthly noti es of the oy l estronomi l o ietyFD RUP @QAF ppF QQSREQQUUF Further information on publisher's website: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTWe quantify the correlations between gas-phase and stellar metallicities and global properties of galaxies, such as stellar mass, halo mass, age and gas fraction, in the Evolution and Assembly of GaLaxies and their Environments suite of cosmological hydrodynamical simulations. The slope of the correlation between stellar mass and metallicity of star-forming (SF) gas (M * -Z SF,gas relation) depends somewhat on resolution, with the higher resolution run reproducing a steeper slope. This simulation predicts a non-zero metallicity evolution, increasing by ≈0.5 dex at ∼10 9 M since z = 3. The simulated relation between stellar mass, metallicity and star formation rate at z 5 agrees remarkably well with the observed fundamental metallicity relation. At M * 10 10.3 M and fixed stellar mass, higher metallicities are associated with lower specific star formation rates, lower gas fractions and older stellar populations. On the other hand, at higher M * , there is a hint of an inversion of the dependence of metallicity on these parameters. The fundamental parameter that best correlates with the metal content, in the simulations, is the gas fraction. The simulated gas fraction-metallicity relation exhibits small scatter and does not evolve significantly since z = 3. In order to better understand the origin of these correlations, we analyse a set of lower resolution simulations in which feedback parameters are varied. We find that the slope of the simulated M * -Z SF,gas relation is mostly determined by stellar feedback at low stellar masses (M * 10 10 M ), and at high masses (M * 10 10 M ) by the feedback from active galactic nuclei.

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The eagle simulations of galaxy formation: the importance of the hydrodynamics scheme

Cited by 700 publications

References 91 publications

The Formation of a Milky Way-Sized Disk Galaxy. I. A Comparison of Numerical Methods

The Formation of a Milky Way-Sized Disk Galaxy. I. A Comparison of Numerical Methods

Bimodality of low-redshift circumgalactic O vi in non-equilibrium eagle zoom simulations

Galaxy metallicity scaling relations in the EAGLE simulations

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