Cluster number counts dependence on dark energy inhomogeneities and coupling to dark matter

Abstract

Cluster number counts can be used to test dark energy models. We investigate dark energy candidates which are coupled to dark matter. We analyze the cluster number counts dependence on the amount of dark matter coupled to dark energy. Further more, we study how dark energy inhomogeneities affect cluster abundances. It is shown that increasing the coupling reduces significantly the cluster number counts, and that dark energy inhomogeneities increases cluster abundances. Wiggles in cluster number counts are shown to be a specific signature of coupled dark energy models. Future observations will possibly detect such oscillations and discriminate among the different dark energy models.

arXiv comment9 pages, 8 figures. Further extensions on section on discriminating models with future surveys. Accepted for publication in Mon. Not. Roy. Astro. Soc

References in corpus (62)

• Measurements of Omega and Lambda from 42 High-Redshift Supernovae
• First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters
• Simulating the joint evolution of quasars, galaxies and their large-scale distribution
• Type Ia Supernova Discoveries at z>1 From the Hubble Space Telescope: Evidence for Past Deceleration and Constraints on Dark Energy Evolution
• 4D Gravity on a Brane in 5D Minkowski Space
• Large scale bias and the peak background split
• Quintessence, Cosmic Coincidence, and the Cosmological Constant
• Coupled Quintessence
• Mass function of dark matter halos
• Chameleon Fields: Awaiting Surprises for Tests of Gravity in Space
• Chameleon Cosmology
• Cosmological Tracking Solutions
• Quintessence and the Rest of the World
• Accelerated expansion of the universe driven by tachyonic matter
• Cluster Abundance Constraints on Quintessence Models
• Cosmology with a Primordial Scaling Field
• Galaxy Clustering in Early SDSS Redshift Data
• Quintessence arising from exponential potentials
• Cosmology with tachyon field as dark energy
• Big Bang nucleosynthesis and physics beyond the Standard Model
• Detecting Dark Energy in Orbit -- the Cosmological Chameleon
• Interacting Dark Matter and Dark Energy
• Cardassian Expansion: a Model in which the Universe is Flat, Matter Dominated, and Accelerating
• Can the clustered dark matter and the smooth dark energy arise from the same scalar field ?
• Cosmic Background Anisotropies in CDM Cosmology
• Constraints on Cosmological Parameters from Future Galaxy Cluster Surveys
• Quintessence and Supergravity
• Stationary dark energy: the present universe as a global attractor
• The South Pole Telescope
• Observational constraints on low redshift evolution of dark energy: How consistent are different observations?
• On the spherical collapse model in dark energy cosmologies
• Galaxy clusters at 0.3 < z < 0.4 and the value of Ω_0
• Galaxy Cluster Abundance Evolution and Cosmological Parameters
• Varying Alpha in a More Realistic Universe
• Self-Calibration of Cluster Dark Energy Studies: Observable-Mass Distribution
• Baryon bias and structure formation in an accelerating universe
• Cosmology with massive neutrinos coupled to dark energy
• The Mass Power Spectrum in Quintessence Cosmological Models
• Quintessential Haloes around Galaxies
• Self-similar cosmological solutions with a non-minimally coupled scalar field
• Stationary dark energy with a baryon-dominated era: solving the coincidence problem with a linear coupling
• Structure Formation in Inhomogeneous Dark Energy Models
• Local and Global Variations of The Fine Structure Constant
• Self-Calibration of Cluster Dark Energy Studies: Counts in Cells
• Primordial Magnetic Fields via Spontaneous Breaking of Lorentz Invariance
• Properties of Galaxy Clusters: Mass and Correlation Functions
• Inhomogeneous Gravity
• CDM-Variant Cosmological Models - I: Simulations and Preliminary Comparisons
• Observational Constraints on General Relativistic Energy Conditions, Cosmic Matter Density and Dark Energy from X-Ray Clusters of Galaxies and Type-Ia Supernovae
• On virialization with dark energy
• Constraining the Evolution of Dark Energy with a Combination of Galaxy Cluster Observables
• Dark energy and the evolution of spherical overdensities
• Models of quintessence coupled to the electromagnetic field and the cosmological evolution of alpha
• The Amplitude of Mass Fluctuations
• Cosmon dark matter?
• Large scale structure in non-standard cosmologies
• Dark Matter and Dark Energy from the solution of the strong CP problem
• Gauge-Invariant Perturbations of Varying-Alpha Cosmologies
• Are Galaxies Cosmon Lumps?
• Observational constraints on the dark energy density evolution
• Tracing the Nature of Dark Energy with Galaxy Distribution
• Dynamical quintessence fields Press-Schechter mass function: detectability and effect on dark haloes

Cited by in corpus (107)

• Cosmology and Fundamental Physics with the Euclid Satellite
• Cosmology and fundamental physics with the Euclid satellite
• Dark Energy
• Dark Matter and Dark Energy Interactions: Theoretical Challenges, Cosmological Implications and Observational Signatures
• Probing the Coupling between Dark Components of the Universe
• Thermodynamics of dark energy interacting with dark matter and radiation
• Hydrodynamical N-body simulations of coupled dark energy cosmologies
• Gauss-Bonnet Quintessence: Background Evolution, Large Scale Structure and Cosmological Constraints
• Interacting Dark Energy -- constraints and degeneracies
• Constraining Interactions in Cosmology's Dark Sector
• Signature of the interaction between dark energy and dark matter in galaxy clusters
• Structure formation in the presence of dark energy perturbations
• Interacting models may be key to solve the cosmic coincidence problem
• Phase-space analysis of interacting phantom cosmology
• The Growth of Structure in Interacting Dark Energy Models
• Spherical collapse in quintessence models with zero speed of sound
• Simultaneous Falsification of LCDM and Quintessence with Massive, Distant Clusters
• Cosmological constraints on interacting dark energy with redshift-space distortion after Planck data
• Hubble expansion and structure formation in the "running FLRW model" of the cosmic evolution
• Growth factor parametrization and modified gravity
• Signature of the interaction between dark energy and dark matter in observations
• Physical approximations for the nonlinear evolution of perturbations in dark energy scenarios
• Dynamics of interacting dark energy model in Einstein and Loop Quantum Cosmology
• The impact of Early Dark Energy on non-linear structure formation
• Large Scale Structures in Kinetic Gravity Braiding Model That Can Be Unbraided
• Confronting Dark Energy Models using Galaxy Cluster Number Counts
• High-z massive clusters as a test for dynamical coupled dark energy
• The imprint of the interaction between dark sectors in galaxy clusters
• The latitude dependence of the rotation measures of NVSS sources
• The spherical collapse model and cluster formation beyond the $\Lambda$ cosmology: Indications for a clustered dark energy?
• The High Redshift Integrated Sachs-Wolfe Effect
• Combined analysis of weak lensing and X-ray blind surveys
• How to Distinguish Dark Energy and Modified Gravity?
• Voids of dark energy
• Distinguishing interacting dark energy from wCDM with CMB, lensing, and baryon acoustic oscillation data
• Late universe dynamics with scale-independent linear couplings in the dark sector
• Growth factor parametrization in curved space
• Interacting Energy Components and Observational $H(z)$ Data
• On the Magnitude of Dark Energy Voids and Overdensities
• The transient acceleration from time-dependent interacting dark energy models
• The spherical collapse model in time varying vacuum cosmologies
• Early Dark Energy at High Redshifts: Status and Perspectives
• Dynamical Mutation of Dark Energy
• Coupled Quintessence and Phantom Based On a Dilaton
• Spherical Collapse in Chameleon Models
• On the implementation of the spherical collapse model for dark energy models
• The signature of dark energy perturbations in galaxy cluster surveys
• Galaxy cluster number count data constraints on cosmological parameters
• Probing Dark Energy at Galactic and Cluster Scales
• Reconstructing a String-Inspired Quintom Model of Dark Energy
• Halo Mass Functions in Early Dark Energy Cosmologies
• Fixed points in interacting dark energy models
• Cluster scaling relations from cosmological hydrodynamic simulations in dark energy dominated universe
• Constraining dark energy fluctuations with supernova correlations
• Effects of early dark energy on strong cluster lensing
• Higher-order coupled quintessence
• Clustering dark energy and halo abundances
• The integrated Sachs-Wolfe effect in cosmologies with coupled dark matter and dark energy
• Cosmological Models and Latest Observational Data
• Testing flatness of the universe with probes of cosmic distances and growth
• A short review on clustering dark energy
• Notes on interacting holographic dark energy model in a closed universe
• Dark energy interacting with dark matter and unparticle
• What do cluster counts really tell us about the Universe?
• Dilaton Coupled Quintessence Model in the $\omega -{\omega }^{\prime }$ Plane
• Effective dark energy equation of state in interacting dark energy models
• Higher neutrino mass allowed if Cold Dark Matter and Dark Energy are coupled
• Indistinguishable Macroscopic Behaviour of Palatini Gravities and General Relativity
• Robust constraints on dark energy and gravity from galaxy clustering data
• Mass Varying Neutrinos, Quintessence, and the Accelerating Expansion of the Universe
• Gravitational Lensing Constraints on Dynamical and Coupled Dark Energy
• Probing Dark Energy Inhomogeneities with Supernovae
• Probing dark energy with the next generation X-ray surveys of galaxy clusters
• Dynamics and constraints of the dissipative Liouville cosmology
• Dynamics and Constraints of the Massive Gravitons Dark Matter Flat Cosmologies
• Testing model independent modified gravity with future large scale surveys
• The mass and the coupling of the Dark Particle
• Cosmological Perturbations and the Running Cosmological Constant Model
• Scalar field-perfect fluid correspondence and nonlinear perturbation equations
• Cluster Probes of Dark Energy Clustering
• Dynamics of minimally coupled dark energy in spherical halos of dark matter
• Constraining thawing and freezing models with cluster number counts
• Simulations of structure formation in interacting dark energy cosmologies
• Evolution of Spherical Overdensity in Thawing Dark energy Models
• ISW-LSS cross-correlation in coupled Dark Energy models with massive neutrinos
• Detecting dark matter-dark energy coupling with the halo mass function
• Structure and evolution of Zel'dovich pancakes as probes of dark energy models
• Effects of Rastall parameter on perturbation of dark sectors of the Universe
• Constraining Thawing Dark Energy using Galaxy Cluster Number Counts
• Unifying static analysis of gravitational structures with a scale-dependent scalar field gravity as an alternative to dark matter
• Spherical collapse and cluster number counts in dark energy models disformally coupled to dark matter
• Spherical collapse in coupled quintessence with a $\Lambda$CDM background
• Voids and overdensities of coupled Dark Energy
• Interacting dark energy collapse with matter components separation
• Halos in Dark Ages: formation and chemistry
• High-precision spectra for dynamical Dark Energy cosmologies from constant-w models
• Spherical collapse of non-top-hat profiles in the presence of dark energy with arbitrary sound speed
• Observational constraint on dynamical evolution of dark energy
• High accuracy power spectra including baryonic physics in dynamical Dark Energy models
• Linear dark energy equation of state revealed by supernovae?
• The Cosmological Supersymmetron
• CMB Anomalies from Imperfect Dark Energy: Confrontation with the Data
• Skewness of matter distribution in clustering dark energy cosmologies
• Beyond Spherical Top Hat Collapse
• Holes within galaxies: the egg or the hen?
• SZ effect or Not? - Detecting most galaxy clusters' main foreground effect
• Halos of dark energy