Cluster Probes of Dark Energy Clustering

Abstract

Cluster abundances are oddly insensitive to canonical early dark energy. Early dark energy with sound speed equal to the speed of light cannot be distinguished from a quintessence model with the equivalent expansion history for $z<2$ but negligible early dark energy density, despite the different early growth rate. However, cold early dark energy, with a sound speed much smaller than the speed of light, can give a detectable signature. Combining cluster abundances with cosmic microwave background power spectra can determine the early dark energy fraction to 0.3 % and distinguish a true sound speed of 0.1 from 1 at 99 % confidence. We project constraints on early dark energy from the Euclid cluster survey, as well as the Dark Energy Survey, using both current and projected Planck CMB data, and assess the impact of cluster mass systematics. We also quantify the importance of dark energy perturbations, and the role of sound speed during a crossing of $w=-1$.

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Cited by in corpus (10)

• Variable sound speed in interacting dark energy models
• Comparing halo bias from abundance and clustering
• Nonlinear bulk viscosity and the stability of accelerated expansion in FRW spacetime
• Full Investigation on the Dynamics of Power-Law Kinetic Quintessence
• Effects of ghost dark energy perturbations on the evolution of spherical overdensities
• A short review on clustering dark energy
• Combined constraints on deviations of dark energy from an ideal fluid from Euclid and Planck
• Dark energy homogeneity in general relativity: Are we applying it correctly?
• Towards a Solution to the H0 Tension: the Price to Pay
• Observational constraints on thawing quintessence scalar field model