Clustering Properties of Dynamical Dark Energy Models

Abstract

We provide a generic but physically clear discussion of the clustering properties of dark energy models. We explicitly show that in quintessence-type models the dark energy fluctuations, on scales smaller than the Hubble radius, are of the order of the perturbations to the Newtonian gravitational potential, hence necessarily small on cosmological scales. Moreover, comparable fluctuations are associated with different gauge choices. We also demonstrate that the often used homogeneous approximation is unrealistic, and that the so-called dark energy mutation is a trivial artifact of an effective, single fluid description. Finally, we discuss the particular case where the dark energy fluid is coupled to dark matter.

5 pages

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• The effect of pressure gradients on luminosity distance - redshift relations
• Lagrangian description of cosmic fluids: mapping dark energy into unified dark energy
• Constraints on the dark matter sound speed from galactic scales: the cases of the Modified and Extended Chaplygin Gas
• Evolution of perturbations in distinct classes of canonical scalar field models of dark energy
• Scalar field dark energy perturbations and the Integrated Sachs Wolfe effect
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• Impact of the matter density uncertainty on the dark energy reconstruction
• Layzer-Irvine equation: new perspectives and the role of interacting dark energy
• Assessing the viability of successful reconstruction of the dynamics of dark energy using varying fundamental couplings
• Interacting Dark Energy and Its Implications for Unified Dark Sector