Dark MaGICC: the effect of Dark Energy on galaxy formation. Cosmology does matter

Abstract

We present the Dark MaGICC project, which aims to investigate the effect of Dark Energy (DE) modeling on galaxy formation via hydrodynamical cosmological simulations. Dark MaGICC includes four dynamical Dark Energy scenarios with time varying equations of state, one with a self-interacting Ratra-Peebles model. In each scenario we simulate three galaxies with high resolution using smoothed particle hydrodynamics (SPH). The baryonic physics model is the same used in the Making Galaxies in a Cosmological Context (MaGICC) project, and we varied only the background cosmology. We find that the Dark Energy parameterization has a surprisingly important impact on galaxy evolution and on structural properties of galaxies at z=0, in striking contrast with predictions from pure Nbody simulations. The different background evolutions can (depending on the behavior of the DE equation of state) either enhance or quench star formation with respect to a LCDM model, at a level similar to the variation of the stellar feedback parameterization, with strong effects on the final galaxy rotation curves. While overall stellar feedback is still the driving force in shaping galaxies, we show that the effect of the Dark Energy parameterization plays a larger role than previously thought, especially at lower redshifts. For this reason, the influence of Dark Energy parametrization on galaxy formation must be taken into account, especially in the era of precision cosmology.

11 pages, 13 figures

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Cited by in corpus (28)

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• On the origin of the chemical bimodality of disk stars: A tale of merger and migration
• NIHAO XV: The environmental impact of the host galaxy on galactic satellite and field dwarf galaxies
• Faint dwarfs as a test of DM models: WDM vs. CDM
• NIHAO XIV: Reproducing the observed diversity of dwarf galaxy rotation curve shapes in LCDM
• NIHAO-UHD: The properties of MW-like stellar disks in high resolution cosmological simulations
• NIHAO project II: Halo shape, phase-space density and velocity distribution of dark matter in galaxy formation simulations
• NIHAO X: Reconciling the local galaxy velocity function with Cold Dark Matter via mock HI observations
• NIHAO XIX: How supernova feedback shapes the galaxy baryon cycle
• The edge of galaxy formation I: formation and evolution of MW-satellites analogues before accretion
• Simulated ΛCDM analogues of the thin Plane of Satellites around the Andromeda galaxy are not kinematically coherent structures
• The challenge of simultaneously matching the observed diversity of chemical abundance patterns in cosmological hydrodynamical simulations
• Evidence for Early Filamentary Accretion from the Andromeda Galaxy's Thin Plane of Satellites
• The edge of galaxy formation II: evolution of Milky Way satellite analogues after infall
• The impact of early massive mergers on the chemical evolution of Milky Way-like galaxies: insights from NIHAO-UHD simulations
• Strongly Coupled Dark Energy Cosmologies: preserving LCDM success and easing low scale problems II - Cosmological simulations
• The response of dark matter haloes to elliptical galaxy formation: a new test for quenching scenarios
• Simulation techniques for modified gravity
• The BAHAMAS project: Effects of dynamical dark energy on large-scale structure
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• Time evolution of the local gravitational parameters and gravitational wave polarizations in a relativistic MOND theory
• Effects of Coupled Dark Energy on the Milky Way and its Satellites
• NIHAO XXVIII: Collateral effects of AGN on dark matter concentration and stellar kinematics
• HELLO project: High-$z$ Evolution of Large and Luminous Objects
• The Origin of the Metal-Poor Common Proper Motion Pair HD 134439/134440: Insights from New Elemental Abundances
• Clues to the nature of dark matter from first galaxies
• Quenching vs. Quiescence: forming realistic massive ellipticals with a simple starvation model