Fingerprinting dark energy

Abstract

Dark energy perturbations are normally either neglected or else included in a purely numerical way, obscuring their dependence on underlying parameters like the equation of state or the sound speed. However, while many different explanations for the dark energy can have the same equation of state, they usually differ in their perturbations so that these provide a fingerprint for distinguishing between different models with the same equation of state. In this paper we derive simple yet accurate approximations that are able to characterize a specific class of models (encompassing most scalar-field models) which is often generically called "dark energy". We then use the approximate solutions to look at the impact of the dark energy perturbations on the dark matter power spectrum and on the integrated Sachs-Wolfe effect in the cosmic microwave background radiation.

11 pages, 5 figures, minor changes to match published version

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Cited by in corpus (68)

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• The phenomenological approach to modeling the dark energy
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• Dark Energy in Practice
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• Consistent perturbations in an imperfect fluid
• A New Class of Parametrization for Dark Energy without Divergence
• Spherical collapse of dark energy with an arbitrary sound speed
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• Fingerprinting Dark Energy II: weak lensing and galaxy clustering tests
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• Fingerprinting Dark Energy III: distinctive marks of viscosity
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• The Integrated Sachs-Wolfe Effect in Time Varying Vacuum Model
• Reconstruction of the null-test for the matter density perturbations
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• What kind of science is cosmology?
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• The Effective Fluid approach for Modified Gravity and its applications
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• Scrutinizing coupled vector dark energy in light of data
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• Lensing convergence and anisotropic dark energy in galaxy redshift surveys
• ${\mathbf{\Omega }}_1{\mathbf{\Omega }}_2$-$\mathbf{\Lambda }$CDM: A promising phenomenological extension of the standard model of cosmology
• Probing dynamical embeddings in a five-dimensional spacetime in light of DESI BAO
• Can dark energy explain a high growth index?
• Constraining Dark Energy Perturbations: the Role of Early Dark Energy
• Matter growth in extended $\Lambda$CDM cosmology