Virialization of cosmological structures in models with time varying equation of state

Abstract

We study the virialization of the cosmic structures in the framework of flat cosmological models where the dark energy component plays an important role in the global dynamics of the universe. In particular, our analysis focuses on the study of the spherical matter perturbations, as the latter decouple from the background expansion and start to ``turn around'' and finally collapse. We generalize this procedure taking into account models with an equation of state which vary with time, and provide a complete formulation of the cluster virialization attempting to address the nonlinear regime of structure formation. In particular, assuming that clusters have collapsed prior to the epoch of $z_{\mathrm{f}}\simeq 1.4$, in which the most distant cluster has been found, we show that the behavior of the spherical collapse model depends on the functional form of the equation of state.

arXiv comment8 pages, 4 figures, MNRAS in press

References in corpus (24)

• First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters
• The Cosmological Constant and Dark Energy
• Cosmological parameters from SDSS and WMAP
• Cosmological Imprint of an Energy Component with General Equation of State
• A Phantom Menace? Cosmological consequences of a dark energy component with super-negative equation of state
• Final Results from the Hubble Space Telescope Key Project to Measure the Hubble Constant
• Exploring the Expansion History of the Universe
• Accelerating Universes with Scaling Dark Matter
• Cluster Abundance Constraints on Quintessence Models
• On the spherical collapse model in dark energy cosmologies
• The foundations of observing dark energy dynamics with the Wilkinson Microwave Anisotropy Probe
• The XMM Cluster Survey: A Massive Galaxy Cluster at z=1.45
• Structure Formation in Inhomogeneous Dark Energy Models
• Constraining cosmological parameters using Sunyaev-Zel'dovich cluster surveys
• Cosmological structure formation in a homogeneous dark energy background
• Supernovae and the Nature of the Dark Energy
• Dark energy and the evolution of spherical overdensities
• Non-linear Structure Formation in Cosmologies with Early Dark Energy
• The Postcollapse Equilibrium Structure of Cosmological Haloes in a Low-Density Universe
• Modeling Dynamical Dark Energy
• Virialization in Dark Energy Cosmology
• The APM cluster-galaxy cross-correlation function : Constraints on Omega and galaxy bias
• Cluster Formation Rate in Models with Dark Energy
• Cosmological constrains from X-ray AGN clustering and SNIa data

Cited by in corpus (20)

• Observational constraints on one-parameter dynamical dark-energy parametrizations and the $H_0$ tension
• Hubble expansion and structure formation in the "running FLRW model" of the cosmic evolution
• The spherical collapse model and cluster formation beyond the $\Lambda$ cosmology: Indications for a clustered dark energy?
• Combined analysis of weak lensing and X-ray blind surveys
• The spherical collapse model in time varying vacuum cosmologies
• Cluster abundances and S-Z power spectra: effects of non-Gaussianity and early dark energy
• Probing Dark Energy at Galactic and Cluster Scales
• Spherical collapse model with non-clustering dark energy
• Halo Mass Functions in Early Dark Energy Cosmologies
• Testing flatness of the universe with probes of cosmic distances and growth
• Spherical collapse model and cluster number counts in power law $f(T)$ gravity
• Dynamics and constraints of the Unified Dark Matter flat cosmologies
• Constraints on shear and rotation with massive galaxy clusters
• Spherical collapse model in agegraphic dark energy cosmologies
• Constraining thawing and freezing models with cluster number counts
• Evolution of Spherical Overdensity in Thawing Dark energy Models
• Constraining Thawing Dark Energy using Galaxy Cluster Number Counts
• Two Component Baryonic-Dark Matter Structure Formation in Top-Hat Model
• End equilibrium state of a spherical gravitational collapse in the presence of matter and scalar field
• Holes within galaxies: the egg or the hen?