Number counts in homogeneous and inhomogeneous dark energy models

Abstract

In the simple case of a constant equation of state, redshift distribution of collapsed structures may constrain dark energy models. Different dark energy models having the same energy density today but different equations of state give quite different number counts. Moreover, we show that introducing the possibility that dark energy collapses with dark matter (``inhomogeneous'' dark energy) significantly complicates the picture. We illustrate our results by comparing four dark energy models to the standard $\Lambda$-model. We investigate a model with a constant equation of state equal to -0.8, a phantom energy model and two scalar potentials (built out of a combination of two exponential terms). Although their equations of state at present are almost indistinguishable from a $\Lambda$-model, both scalar potentials undergo quite different evolutions at higher redshifts and give different number counts. We show that phantom dark energy induces opposite departures from the $\Lambda$-model as compared with the other models considered here. Finally, we find that inhomogeneous dark energy enhances departures from the $\Lambda$-model with maximum deviations of about 15% for both number counts and integrated number counts. Larger departures from the $\Lambda$-model are obtained for massive structures which are rare objects making it difficult to statistically distinguish between models.

10 pages, 11 figures. Version accepted for publication in A&A

References in corpus (27)

• Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant
• Measurements of Omega and Lambda from 42 High-Redshift Supernovae
• First Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Determination of Cosmological Parameters
• Cosmology and the Fate of Dilatation Symmetry
• Quintessence, Cosmic Coincidence, and the Cosmological Constant
• An alternative to quintessence
• A Dynamical Solution to the Problem of a Small Cosmological Constant and Late-time Cosmic Acceleration
• Coupled Quintessence
• Quintessence arising from exponential potentials
• Cosmology with tachyon field as dark energy
• Structure formation with a self-tuning scalar field
• Cosmological scaling solutions of non-minimally coupled scalar fields
• Can the clustered dark matter and the smooth dark energy arise from the same scalar field ?
• Constraints on Cosmological Parameters from Future Galaxy Cluster Surveys
• Quintessence and Supergravity
• The Cluster Abundance in Flat and Open Cosmologies
• Could supermassive black holes be quintessential primordial black holes?
• Self Calibration in Cluster Studies of Dark Energy: Combining the Cluster Redshift Distribution, the Power Spectrum and Mass Measurements
• The Mass Power Spectrum in Quintessence Cosmological Models
• Quintessential Haloes around Galaxies
• Constraining cosmological parameters using Sunyaev-Zel'dovich cluster surveys
• An alternative to the cosmological 'concordance model'
• Tracking Extended Quintessence
• On virialization with dark energy
• Constraining dark energy with Sunyaev-Zel'dovich cluster surveys
• Dark energy and the evolution of spherical overdensities
• Halo properties in models with dynamical Dark Energy

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• Generalized Layzer-Irvine equation: the role of dark energy perturbations in cosmic structure formation
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