The Structure of Dark Matter Haloes in Hierarchical Clustering Models

Abstract

We use a set of large cosmological N-body simulations to study the internal structure of dark matter haloes which form in scale-free models. We find that the radius r_178 corresponding to a mean interior overdensity of 178 accurately delineates the quasi-static halo interior from the surrounding infalling material, in agreement with the simple spherical collapse model. The interior velocity dispersion correlates with mass, again in good agreement with the spherical collapse model. Interior to the virial radius r_178, the spherical averaged density, circular velocity and velocity dispersion profiles are well fit by a simple 2-parameter analytic model proposed by Navarro etal (1995). This model has density going as 1/r at small radii, steepening to 1/r^3 at large radii, and fits our haloes to the resolution limit of the simulations. The two model parameters, scalelength and mass, are tightly correlated. Lower mass haloes are more centrally concentrated, and so have scalelengths which are a smaller fraction of their virial radius than those of their higher mass counterparts. This reflects the earlier formation times of low mass haloes. The haloes are moderately aspherical, with typical axial ratios 1:0.8:0.65 at their virial radii. These shapes are maintained by an anisotropic velocity dispersion tensor. The median value of the spin parameter is lambda=0.04, with a weak trend for lower lambda at higher halo mass. We also investigate how the halo properties depend on the algorithm used to identify them, using both friends-of-friends and spherical overdensity methods. We find that for groups selected at mean overdensities 100-400 by either method the properties are insensitive to how the haloes are selected, if the halo centre is taken as the position of the most bound particle

arXiv commentRevised version with one extra figure accepted for publication in MNRAS. Large figures available by anonymous ftp at ftp://star-ftp.dur.ac.uk/pub/preprints/cl3_figs.ps.tar.gz and complete paper available as gzipped postscript file at ftp://star-ftp.dur.ac.uk/pub/preprints/cl3.ps.gz

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• Profiles of dark-matter haloes at high redshift
• A Comparison of Simple Mass Estimators for Galaxy Clusters
• Hydrodynamic Approach to the Evolution of Cosmic Structures II: Study of N-body Simulations at z=0
• Stochastic Model of the Spin Distribution of Dark Matter Halos
• The morphology of star-forming gas and its alignment with galaxies and dark matter haloes in the EAGLE simulations
• The Distribution of Dark Matter in Galaxies: Constant-Density Dark Halos Envelop the Stellar Disks
• SED-inferred properties and morphology of Lyman-break galaxies at $z\sim 1$ in the CDF-S
• Made-To-Measure Models of Self-Similar Triaxial Halos with Steep Inner Density Gradients
• Exact potential-density pairs for flattened dark haloes
• An expanded merger-tree description of cluster evolution
• Cosmic accretion shocks as a tool to measure the dark matter mass of galaxy clusters
• Cosmological Simulations with Scale-Free Initial Conditions I: Adiabatic Hydrodynamics
• Anisotropic Models of Dark Halos
• What Could be the Observational Signature of Dark Matter in Globular Clusters?
• Radial density and temperature profiles of the intracluster gas constructed jointly from the X-ray surface brightness measurement and the universal density profile
• Gravitational Collapse in an Expanding Universe: Scaling Relations for Two-Dimensional Collapse Revisited
• Probing baryonic processes and gastrophysics in the formation of the Milky Way dwarf satellites: I. metallicity distribution properties
• Accurate dark matter halo elongation from weak-lensing stacking analysis
• Optimizing the Recovery of Fisher Information in the Dark Matter Power Spectrum
• Shapes of dark matter haloes with discrete globular cluster dynamics: The example of NGC 5128 (Centaurus A)
• The eventful life journey of galaxy clusters. I. Impact of DM halo and ICM properties on their full assembly histories
• The Orbital Structure of Dark Matter Halos with Gas
• Intrinsic alignments of the extended radio continuum emission of galaxies in the EAGLE simulations
• Making use of sub-resolution halos in N-body simulations
• Shape and connectivity of groups and clusters: Impact of dynamical state and accretion history
• Stacked phase-space density of galaxies around massive clusters: Comparison of dynamical and lensing masses
• Simulation-based marginal likelihood for cluster strong lensing cosmology
• Quantifying the collisionless nature of dark matter and galaxies in A1689
• Devouring The Centaurus A Satellites: Modeling Dwarf Galaxies with Galacticus
• Convergence of halo statistics: code comparison between Rockstar and CompaSO using scale-free simulations
• Energetic particles and high-energy processes in cosmological filaments and their astronomical implications
• Measurement of the dark matter velocity anisotropy profile in galaxy clusters
• Star formation losses due to tidal debris in `hierarchical' galaxy formation
• Three-dimensional shapelets and an automated classification scheme for dark matter haloes
• Density profiles of dark matter halos with anisotropic velocity tensors
• A necessary condition for best fitting analytical to simulated density profiles in dark matter haloes
• Predicting the Scaling Relations between the Dark Matter Halo Mass and Observables from Generalised Profiles II: Intracluster Gas Emission
• Star formation and chemical evolution of damped Lyman $\alpha$ systems
• Angular momentum and morphological sequence of massive galaxies through Dark Sage
• Observational tests of the delta_c-M_vir relation in hierarchical clustering models
• A Random Walk Model for Halo Triaxiality
• Distribution Function in Center of Dark Matter Halo
• The halo finding problem revisited: a deep revision of the ASOHF code
• A dynamics-based density profile for dark haloes. I. Algorithm and basic results
• A Non-parametric Method for the Inference of Halo Occupation Distributions
• Comparison of Modeling SPARC spiral galaxies' rotation curves: halo models vs MOND
• Hubble Expansion Signature on Simulated Halo Density Profiles: A Path to Observing the Turnaround Radius