Coupled and extended quintessence: Theoretical differences and structure formation

By Valeria Pettorino, C. Baccigalupi. 2008

155 citations recorded by the source corpus.

The case of a coupling between dark energy and matter [coupled quintessence (CQ)] or gravity [extended quintessence (EQ)] has recently attracted a deep interest and has been widely investigated both in the Einstein and in the Jordan frames (EF, JF), within scalar-tensor theories. Focusing on the simplest models proposed so far, in this paper we study the relation existing between the two scenarios, isolating the Weyl scaling which allows one to express them in the EF and JF. Moreover, we perform a comparative study of the behavior of linear perturbations in both scenarios, which turn out to behave in a markedly different way. In particular, while the clustering is enhanced in the considered CQ models with respect to the corresponding quintessence ones where the coupling is absent and to the ordinary cosmologies with a cosmological constant and cold dark matter ($\ensuremath{\Lambda}\mathrm{CDM}$), structures in EQ models may grow slower. This is likely to have direct consequences on the inner properties of nonlinear structures, like cluster concentration, as well as on the weak lensing shear on large scales. Finally, we specialize our study for interfacing linear dynamics and N-body simulations in these cosmologies, giving a recipe for the corrections to be included in N-body codes in order to take into account the modifications to the expansion rate, growth of structures, and strength of gravity.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/970c7888165d78ce1913b7c45bbb955e576a231b

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Nuclear and High Energy Physics

Citations in the corpus

Hydrodynamical N-body simulations of coupled dark energy cosmologies (2008, methodology): “…investigated, for β(φ) given by a constant, both in its background and linear perturbation features (Wetterich 1995; Amendola 2000) as well as with regard to the effects on structure formation (Amendola 2004; Pettorino & Baccigalupi 2008) , and via a first N-body simulation (Macciò et al. 2004).”
Observational constraints on an interacting dark energy model (2009, unknown): “…in Amendola et al. (2003); Koivisto (2005); Olivares et al. (2006); Mainini & Bonometto (2007); Bean et al. (2008); Vergani et al. (2009); Pettorino & Baccigalupi (2008); Schäfer (2008); Schaefer et al. (2008); La Vacca & Colombo (2008); He et al. (2009); Bean et al. (2008); Corasaniti…”
Interacting dark energy in the early 2020s: A promising solution to the H0 and cosmic shear tensions (2019, background): “[130–239], for a recent comprehensive review see [200]).”
The growth of structure in interacting dark energy models (2009, background): “[41–45]) in order to construct an accurate lensing signal, and this could involve N-body simulations for interacting dark matter [46–48].”
Cosmology and Fundamental Physics with the Euclid Satellite (2012, methodology): “Various choices of couplings have been investigated in literature, including constant and varying β(φ) [45, 818, 47, 690, 557, 990, 992, 947, 502].”