Identification of Cosmic Voids as Massive Cluster Counterparts

Abstract

We develop a method to identify cosmic voids from the matter density field by adopting a physically-motivated concept that voids are the counterpart of massive clusters. To prove the concept we use a pair of $\Lambda$CDM simulations, a reference and its initial density-inverted mirror simulation, and study the relation between the effective size of voids and the mass of corresponding clusters. Galaxy cluster-scale dark matter halos are identified in the Mirror simulation at $z=0$ by linking dark matter particles. The void corresponding to each cluster is defined in the Reference simulation as the region occupied by the member particles of the cluster. We study the voids corresponding to the halos more massive than $10^{13}{h}^{-1}{M}_{\odot }$. We find a power-law scaling relation between the void size and the corresponding cluster mass. Voids with corresponding cluster mass above $10^{15}{h}^{-1}{M}_{\odot }$ occupy $\sim 1\%$ of the total simulated volume, whereas this fraction increases to $\sim 54\%$ for voids with corresponding cluster mass above $10^{13}{h}^{-1}{M}_{\odot }$. It is also found that the density profile of the identified voids follows a universal functional form. Based on these findings, we propose a method to identify cluster-counterpart voids directly from the matter density field without their mirror information by utilizing three parameters such as the smoothing scale, density threshold, and minimum core fraction. We recover voids corresponding to clusters more massive than $3\times 10^{14}{h}^{-1}{M}_{\odot }$ at 70--74 \% level of completeness and reliability. Our results suggest that we are able to identify voids in a way to associate them with clusters of a particular mass-scale.

arXiv commentPublished in ApJ

References in corpus (57)

• Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Likelihoods and Parameters from the WMAP data
• The persistent cosmic web and its filamentary structure I: Theory and implementation
• The Las Campanas Redshift Survey
• Properties of Dark Matter Haloes in Clusters, Filaments, Sheets and Voids
• A hierarchy of voids: Much ado about nothing
• Evolution of the cosmic web
• ZOBOV: a parameter-free void-finding algorithm
• The Void Phenomenon
• Multiscale Phenomenology of the Cosmic Web
• A Cosmic Watershed: the WVF Void Detection Technique
• Cosmic Voids in Sloan Digital Sky Survey Data Release 7
• NEXUS: Tracing the Cosmic Web Connection
• Precision cosmography with stacked voids
• Voids in the 2dF Galaxy Redshift Survey
• The Aspen--Amsterdam Void Finder Comparison Project
• The structure of voids
• Universal Density Profile for Cosmic Voids
• Testing Gravity using Cosmic Voids
• Halos and Voids in f(R) Gravity
• Counting voids to probe dark energy
• Voids in a $\Lambda$CDM Universe
• The darkness that shaped the void: dark energy and cosmic voids
• Precision cosmology with voids: definition, methods, dynamics
• The abundance of voids and the excursion set formalism
• The Hierarchical Structure and Dynamics of Voids
• Second-order Lagrangian perturbation theory initial conditions for resimulations
• Structure Formation With a Long-Range Scalar Dark Matter Interaction
• Cosmic Voids: structure, dynamics and galaxies
• Morphology of the supercluster-void network in LCDM cosmology
• Sparse sampling, galaxy bias, and voids
• The Evidence of Absence: Galaxy Voids in the Excursion Set Formalism
• Only the Lonely: H I Imaging of Void Galaxies
• Clues on void evolution I: Large scale galaxy distributions around voids
• Galaxy and Mass Assembly (GAMA): Fine filaments of galaxies detected within voids
• GOTPM: A Parallel Hybrid Particle-Mesh Treecode
• Shapes and Sizes of Voids in the LCDM Universe: Excursion Set Approach
• The Challenge of the Largest Structures in the Universe to Cosmology
• Constraining the Dark Energy Equation of State with Cosmic Voids
• The Evolution of Voids in the Adhesion Approximation
• The Size and Shape of Local Voids
• The Void Size Function in Dynamical Dark Energy Cosmologies
• Large-Scale Clustering of Cosmic Voids
• The orientation of galaxy dark matter haloes around cosmic voids
• Void Ellipticity Distribution as a Probe of Cosmology
• Alignments of Voids in the Cosmic Web
• The nature of voids: I. Watershed void finders and their connection with theoretical models
• Inverted initial conditions: exploring the growth of cosmic structure and voids
• Assembly of filamentary void galaxy configurations
• The dark matter of galaxy voids
• The view from the boundary: a new void stacking method
• HectoMAP and Horizon Run 4: Dense Structures and Voids in the Real and Simulated Universe
• A Detection of $z$~2.3 Cosmic Voids from 3D Lyman-$\alpha$ Forest Tomography in the COSMOS Field
• Testing spherical evolution for modelling void abundances
• Constraining Cosmology with Big Data Statistics of Cosmological Graphs
• How to Build a Catalogue of Linearly-Evolving Cosmic Voids
• Alcock-Paczynski Test with the Evolution of Redshift-Space Galaxy Clustering Anisotropy
• Cosmological Information from the Small-scale Redshift Space Distortions

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• Why Cosmic Voids Matter: Nonlinear Structure & Linear Dynamics
• Catalogues of voids as antihalos in the local Universe
• Observational Constraints on the Dark Energy with a Quadratic Equation of State
• Unveiling the Universe with Emerging Cosmological Probes
• A possible role for the merger of clusters/voids in the cosmological expansion
• Cluster-counterpart Voids: Void Identification from Galaxy Density Field
• The Molecular and Atomic Hydrogen Gas Content of the Boötes Void galaxy CG 910
• An Anti-halo Void Catalogue of the Local Super-Volume
• Cosmological constraints from the density gradient weighted correlation function