Interacting dark energy: constraints and degeneracies
By Timothy Clemson, K. Koyama, Gong-Bo Zhao, R. Maartens, J. Valiviita. 2011
151 citations recorded by the source corpus.
Institute of Theoretical Astrophysics, University of Oslo, N-0315 Oslo, Norway(Dated: October 14, 2011)In standard cosmologies, dark energy interacts only gravitationally with dark matter. Therecould be a non-gravitational interaction in the dark sector, leading to changes in the effective DEequation of state, in the redshift dependence of the DM density and in structure formation. Weuse CMB, BAO and SNIa data to constrain a model where the energy transfer in the dark sector isproportional to the DE density. There are two subclasses, defined by the vanishing of momentumtransfer either in the DM or the DE frame. We conduct a Markov-Chain Monte-Carlo analysis toobtain best-fit parameters. The background evolution allows large interaction strengths, and theconstraints from CMB anisotropies are weak. The growth of DM density perturbations is muchmore sensitive to the interaction, and can deviate strongly from the standard case. However, thedeviations are degenerate with galaxy bias and thus more difficult to constrain. Interestingly, theISW signature is suppressed since the non-standard background evolution can compensate for highgrowth rates. We also discuss the partial degeneracy between interacting DE and modified gravity,and how this can be broken.I. INTRODUCTION
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/8cf7ec9a0368eab501b94d843fd8d1a3e0503e7e
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Citations in the corpus
- Interacting scenarios with dynamical dark energy: Observational constraints and alleviation of the H0 tension (2019, background): “Additionally, for an interacting universe the conservation equations become [103, 104, 105]”
- Interacting dark energy in the early 2020s: A promising solution to the H0 and cosmic shear tensions (2019, methodology): “ities, leading to curvature perturbations blowing up on superhorizon scales. For the ˘CDM model in which Q/ˆ x, the instabilities present when w6= 1 are absent if the signs of ˘and (1+w) are opposite [144, 161, 261, 265, 266] (see also [267{273] for alternative approaches to avoiding these instabili”
- Nonminimal dark sector physics and cosmological tensions (2019, background): “Apart from the gravitational instabilities present when w = −1 [151, 228], there may also be early-time instabilities [151, 152, 157, 227–229], and avoiding them leads to imposing stability conditions on w and ξ.”
- Tale of stable interacting dark energy, observational signatures, and the H0 tension (2018, methodology): “Within the perturbed FLRW metric, the perturbation equations for the fluid A are given by the following [9, 10, 12]:”
- Interacting dark energy with time varying equation of state and the H0 tension (2018, methodology): “For simplicity, we assume that momentum transfer potential is zero in the rest frame of the dark matter [51, 52, 53] which directs k(2)fA = QA(θ − θc) where k is the wave number and θ = θ μ, θc are respectively the volume expansion scalar of the total fluid and the volume expansion scalar for the CD”