NIHAO project II: Halo shape, phase-space density and velocity distribution of dark matter in galaxy formation simulations

Abstract

We use the NIHAO (Numerical Investigation of Hundred Astrophysical Objects) cosmological simulations to study the effects of galaxy formation on key properties of dark matter (DM) haloes. NIHAO consists of $\simeq 90$ high-resolution SPH simulations that include (metal-line) cooling, star formation, and feedback from massive stars and SuperNovae, and cover a wide stellar and halo mass range: $10^6<M_{\ast }/M_{\odot }<10^{11}$ ( $10^{9.5}<M_{\mathrm{halo}}/M_{\odot }<10^{12.5}$). When compared to DM-only simulations, the NIHAO haloes have similar shapes at the virial radius, R_{\rm vir}, but are substantially rounder inside $\simeq 0.1R_{\mathrm{vir}}$. In NIHAO simulations $c/a$ increases with halo mass and integrated star formation efficiency, reaching $\sim 0.8$ at the Milky Way mass (compared to 0.5 in DM-only), providing a plausible solution to the long-standing conflict between observations and DM-only simulations. The radial profile of the phase-space $Q$ parameter ($\rho /{\sigma }^3$) is best fit with a single power law in DM-only simulations, but shows a flattening within $\simeq 0.1R_{\mathrm{vir}}$ for NIHAO for total masses $M>10^{11}{M}_{\odot }$. Finally, the global velocity distribution of DM is similar in both DM-only and NIHAO simulations, but in the solar neighborhood, NIHAO galaxies deviate substantially from Maxwellian. The distribution is more symmetric, roughly Gaussian, with a peak that shifts to higher velocities for Milky Way mass haloes. We provide the distribution parameters which can be used for predictions for direct DM detection experiments. Our results underline the ability of the galaxy formation processes to modify the properties of dark matter haloes.

19 pages, 17 figures, analysis strongly improved, main conclusions unchanged, accepted for publication in MNRAS

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• NIHAO VI. The hidden discs of simulated galaxies
• The impact of going beyond the Maxwell distribution in direct dark matter detection rates
• The impact of baryons on dark matter haloes
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Cited by in corpus (71)

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• Simulated Milky Way analogues: implications for dark matter indirect searches
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• Assessing Astrophysical Uncertainties in Direct Detection with Galaxy Simulations
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• Dependency of halo concentration on mass, redshift and fossilness in Magneticum hydrodynamic simulations
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• Advances in Constraining Intrinsic Alignment Models with Hydrodynamic Simulations
• nIFTy Galaxy Cluster simulations IV: Quantifying the Influence of Baryons on Halo Properties
• Baryonic Imprints on DM Halos: Population Statistics from Dwarf Galaxies to Galaxy Clusters
• Origin of the Local Group satellite planes
• Magnetization of the intergalactic medium in the IllustrisTNG simulations: the importance of extended, outflow-driven bubbles
• Creating a galaxy lacking dark matter in a dark matter dominated universe
• A Plane of High Velocity Galaxies Across the Local Group
• Constraint on the velocity dependent dark matter annihilation cross section from Fermi-LAT observations of dwarf galaxies
• The impact of galactic feedback on the shapes of dark-matter haloes
• DM halo morphological types of MW-like galaxies in the TNG50 simulation: Simple, Twisted, or Stretched
• Bracketing the impact of astrophysical uncertainties on local dark matter searches
• Shapes of Milky-Way-Mass Galaxies with Self-Interacting Dark Matter
• Evolution and Statistics of Non-Sphericity of Dark Matter Halos from Cosmological N-Body Simulation
• From EMBER to FIRE: predicting high resolution baryon fields from dark matter simulations with Deep Learning
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• Projected Axis Ratios of Galaxy Clusters in the Horizon-AGN Simulation: Impact of Baryon Physics and Comparison with Observations
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• The impact of inelastic self-interacting dark matter on the dark matter structure of a Milky Way halo
• Cosmological Magnetogenesis: The Biermann Battery during the Epoch of Reionization
• On the Cosmic Web Elongation in Fuzzy Dark Matter Cosmologies: Effects on Density Profiles, Shapes and Alignments of Halos
• The oblateness of the Milky Way dark matter halo from the stellar streams of NGC 3201, M68, and Palomar 5
• Astrophysical Tests of Dark Matter Self-Interactions
• Dark matter capture by the Sun: revisiting velocity distribution uncertainties
• Dark Matter Response to Galaxy Assembly History
• The Doppler effect on indirect detection of dark matter using dark matter only simulations
• Major mergers between dark matter haloes -- I. Predictions for size, shape, and spin
• The Milky Way, Coming into Focus: Precision Astrometry Probes its Evolution, and its Dark Matter
• Joint Gas and Stellar Dynamical Models of WLM: An isolated dwarf galaxy within a cored, prolate DM halo
• The dynamical structure of broken power-law and double power-law models for dark matter haloes
• Self-gravitating Equilibria of Non-minimally Coupled Dark Matter Halos
• Direct Detection Anomalies in light of $Gaia$ Data
• Testing the Impact of Satellite Anisotropy on Large and Small Scale Intrinsic Alignments using Hydrodynamical Simulations
• Observationally inferred dark matter phase-space distribution and direct detection experiments
• Probing the shape of the Milky Way dark matter halo with hypervelocity stars: a new method
• Sliding into DM: Determining the local dark matter density and speed distribution using only the local circular speed of the Galaxy
• Galaxy shapes in Magneticum. I. Connecting stellar and dark matter shapes to dynamical and morphological galaxy properties and the large-scale structure
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• SpheCow: flexible dynamical models for galaxies and dark matter haloes
• The spatial distribution of satellites in galaxy clusters
• Power law pseudo phase-space density profiles of dark matter halos: fluke of physics?
• Evaluating the variance of individual halo properties in constrained cosmological simulations
• The shape of dark matter halos: a new fundamental cosmological invariance
• A MARVEL-ous study of how well galaxy shapes reflect Dark Matter halo shapes in Cold Dark Matter Simulations
• The effect of hydrodynamical simulation inspired dark matter velocity profile on directional detection of dark matter
• Sensitivity of Halo Shape Measurements
• Dark Matter Velocity Distributions for Direct Detection: Astrophysical Uncertainties are Smaller Than They Appear
• Milky Way Halo Vibrations and Incommensurate Stream Velocities
• Structural and dynamical modeling of WINGS clusters. III. The pseudo phase-space density profile
• Self-consistent dynamical models with a finite extent -- II. Radially truncated models
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• Towards characterizing dark matter subhalo perturbations in stellar streams with graph neural networks
• Search for Leptophilic Dark Matter at the LHeC
• How to Build an Empirical Speed Distribution for Dark Matter in the Solar Neighborhood
• Constraining the population of dark matter halo shapes using hierarchical inference with extragalactic stellar streams