Dependence on the environment of the abundance function of light-cone simulation dark matter haloes

Abstract

Aims.We study the dependence of the halo abundance function (AF) on different environments in a whole-sky $\Lambda$CDM light-cone halo catalogue extending to z < 0.65, using a simple and well-defined halo isolation criterion. Methods. The isolation status of each individual dark matter halo is determined by the distance to its nearest neighbour, which defines the maximum spherical region devoid of halos above a threshold mass around it (although the true size of such region may be much larger since it is not necessarily spherical). A versatile double power-law Schechter function is used to fit the dark matter halo AF, and its derived parameters are studied as a function of halo isolation status. Results. (a) Our function fits the halo abundances for all halo isolation statuses extremely well, while the well-established theoretical mass functions, integrated over the volume of the light-cone, provide an adequate but poorer fit than our phenomenological model. (b) As expected, and in agreement with other studies based on snap-shot simulations, we find significant differences of the halo abundance function as a function of halo isolation, indicating different rates of halo formation. The slope of the power law and the characteristic mass of the Schechter-like fitting function decrease with isolation, a result consistent with the formation of less massive haloes in lower density regions. (c) We find an unexpected upturn of the characteristic mass of the most isolated haloes of our sample. This upturn originates and characterises only the higher redshift regime (z > 0.45), which probably implies a significant and recent evolution of the isolation status of the most isolated and most massive haloes.

arXiv comment8 pages, 9 figures

References in corpus (58)

• emcee: The MCMC Hammer
• A Universal Density Profile from Hierarchical Clustering
• Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Cosmological Interpretation
• Efficient Computation of CMB anisotropies in closed FRW models
• Large scale bias and the peak background split
• Profiles of dark haloes: evolution, scatter, and environment
• Cosmological Hydrodynamics with Adaptive Mesh Refinement: a new high resolution code called RAMSES
• Ellipsoidal collapse and an improved model for the number and spatial distribution of dark matter haloes
• Mass function of dark matter halos
• Improved Cosmological Constraints from New, Old and Combined Supernova Datasets
• Concentrations of Dark Halos from their Assembly Histories
• How Filaments are Woven into the Cosmic Web
• The Large Scale Bias of Dark Matter Halos: Numerical Calibration and Model Tests
• Environmental Effects on Late-Type Galaxies in Nearby Clusters
• Galaxy Star-Formation as a Function of Environment in the Early Data Release of the Sloan Digital Sky Survey
• The age dependence of halo clustering
• The subhalo populations of LCDM dark haloes
• The Dependence of Halo Clustering on Halo Formation History, Concentration, and Occupation
• Precision Determination of the Mass Function of Dark Matter Halos
• Assembly bias in the clustering of dark matter haloes
• The halo mass function from the dark ages through the present day
• Tracing the cosmic web
• Halo assembly bias and its effects on galaxy clustering
• On the environmental dependence of halo formation
• The Evolution of Dark Matter Halo Properties in Clusters, Filaments, Sheets and Voids
• The halo mass function through the cosmic ages
• A marked correlation function analysis of halo formation times in the Millennium Simulation
• Measures of Galaxy Environment - I. What is "Environment"?
• Next Generation Cosmology: Constraints from the Euclid Galaxy Cluster Survey
• A kinematic classification of the cosmic web
• Initial Conditions for Large Cosmological Simulations
• What aspects of galaxy environment matter?
• A Systematic Study of X-Ray Substructure of Galaxy Clusters Detected in the ROSAT All-Sky Survey
• A simple multigrid scheme for solving the Poisson equation with arbitrary domain boundaries
• The velocity shear tensor: tracer of halo alignment
• Imprints of dark energy on cosmic structure formation: II) Non-Universality of the halo mass function
• The preferred direction of infalling satellite galaxies in the Local Group
• The dependence on environment of Cold Dark Matter Halo properties
• The Dependence of the Mass Assembly History of Cold Dark Matter Halos on Environment
• The cosmic web and the orientation of angular momenta
• Disentangling galaxy environment and host halo mass
• The Dependence of the Occupation of Galaxies on the Halo Formation Time
• The universal nature of subhalo accretion
• Galaxy And Mass Assembly (GAMA): The galaxy luminosity function within the cosmic web
• Imprints of Dark Energy on Cosmic Structure Formation I) Realistic Quintessence Models and the Non-Linear Matter Power Spectrum
• The Cluster Substructure - Alignment Connection
• Properties of Dark Matter Halos as a Function of Local Environment Density
• Toward a Universal Formulation of the Halo Mass Function
• The dark matter assembly of the Local Group in constrained cosmological simulations of a LambdaCDM universe
• Galaxy properties and the cosmic web in simulations
• The Bias and Mass Function of Dark Matter Halos in Non-Markovian Extension of the Excursion Set Theory
• Environmental Influences on the Morphology and Dynamics of Group Size Haloes
• Halo abundances within the cosmic web
• Groups of galaxies: relationship between environment and galaxy properties
• Filaments from the galaxy distribution and from the velocity field in the local universe
• Mass functions and bias of dark matter halos
• eROSITA cluster cosmology forecasts: cluster temperature substructure bias
• The abundance and environment of dark matter haloes

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