Nonminimal dark sector physics and cosmological tensions
By E. di Valentino, A. Melchiorri, O. Mena, S. Vagnozzi. Physical Review D, 2019
250 citations recorded by the source corpus.
We explore whether nonstandard dark sector physics might be required to solve the existing cosmological tensions. The properties we consider in combination are (a) an interaction between the dark matter and dark energy components and (b) a dark energy equation of state $w$ different from that of the canonical cosmological constant $w=\ensuremath{-}1$. In principle, these two parameters are independent. In practice, to avoid early-time, superhorizon instabilities, their allowed parameter spaces are correlated. Moreover, a clear degeneracy exists between these two parameters in the case of cosmic microwave background (CMB) data. We analyze three classes of extended interacting dark energy models in light of the 2019 Planck CMB results and Cepheid-calibrated local distance ladder ${H}_{0}$ measurements of Riess et al. (R19), as well as recent baryon acoustic oscillation (BAO) and type Ia supernovae (SNeIa) distance data. We find that in quintessence coupled dark energy models, where $wg\ensuremath{-}1$, the evidence for a nonzero coupling between the two dark sectors can surpass the $5\ensuremath{\sigma}$ significance. Moreover, for both $\mathrm{Planck}+\mathrm{BAO}$ or $\mathrm{Planck}+\mathrm{SNeIa}$, we find a preference for $wg\ensuremath{-}1$ at about three standard deviations. Quintessence models are, therefore, in excellent agreement with current data when an interaction is considered. On the other hand, in phantom coupled dark energy models, there is no such preference for a nonzero dark sector coupling. All the models we consider significantly raise the value of the Hubble constant, easing the ${H}_{0}$ tension. In the interacting scenario, the disagreement between $\mathrm{Planck}+\mathrm{BAO}$ and R19 is considerably reduced from $4.3\ensuremath{\sigma}$ in the case of the $\mathrm{\ensuremath{\Lambda}}$ cold dark matter ($\mathrm{\ensuremath{\Lambda}}\mathrm{CDM}$) model to about $2.5\ensuremath{\sigma}$. The addition of low-redshift BAO and SNeIa measurements leaves, therefore, some residual tension with R19 but at a level that could be justified by a statistical fluctuation. Bayesian evidence considerations mildly disfavor both the coupled quintessence and phantom models, while mildly favoring a coupled vacuum scenario, even when late-time datasets are considered. We conclude that nonminimal dark energy cosmologies, such as coupled quintessence, phantom, or vacuum models, are still an interesting route toward softening existing cosmological tensions, even when low-redshift datasets and Bayesian evidence considerations are taken into account.
Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics
View Paper: https://www.semanticscholar.org/paper/6494d870612d4d42d2bc839f73ec54ae7fd93a7f
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Citations in the corpus
- Cosmology Intertwined II: The Hubble Constant Tension (2020, unknown): “[63] E.”
- New physics in light of the H0 tension: An alternative view (2019, background): “[60–209] for what is inevitably an incomplete list of works examining these possibilities.”
- Interacting dark energy in the early 2020s: A promising solution to the H0 and cosmic shear tensions (2019, methodology): “nvector problem, and studying the modes which dominate the time evolution (which in this case will be those corresponding to the largest eigenvalue). These initial conditions turn out to be (see e.g. [172, 244, 257, 261, 264]): in x () = 3 2 (2˘ 1 w)(1 + w+ ˘=3) 12w2 2w 3w˘+ 7˘ 14 in (); (8) in x (x”