Supernova constraints on multi-coupled dark energy

Abstract

The persisting consistency of ever more accurate observational data with the predictions of the standard ΛCDM cosmological model puts severe constraints on possible alternative scenarios, but still does not shed any light on the fundamental nature of the cosmic dark sector. As large deviations from a ΛCDM cosmology are ruled out by data, the path to detect possible features of alternative models goes necessarily through the definition of cosmological scenarios that leave almost unaffected the background and -to a lesser extent -the linear perturbations evolution of the universe. In this context, the Multi-coupled DE (McDE) model was proposed by Baldi [9] as a particular realization of an interacting Dark Energy field characterized by an effective screening mechanism capable of suppressing the effects of the coupling at the background and linear perturbation level. In the present paper, for the first time, we challenge the McDE scenario through a direct comparison with real data, in particular with the luminosity distance of Type Ia supernovae. By studying the existence and stability conditions of the critical points of the associated background dynamical system, we select only the cosmologically consistent solutions, and confront their background expansion history with data. Confirming previous qualitative results, the McDE scenario appears to be fully consistent with the adopted sample of Type Ia supernovae, even for coupling values corresponding to an associated scalar fifth-force about four orders of magnitude stronger than standard gravity. Our analysis demonstrates the effectiveness of the McDE background screening, and shows some new non-trivial asymptotic solutions for the future evolution of the universe. Clearly, linear perturbation data and, even more, nonlinear structure formation properties are expected to put much tighter constraints on the allowed coupling range. Nonetheless, our results show how the background expansion history might be highly insensitive to the fundamental nature and to the internal complexity of the dark sector.PACS numbers: 95.36.+x, 95.35.+d, 97.60.Bw, 98.80.Es.

Multifield coupled quintessence

“…It is immediately obtained that i x The matter dominated solution is the fixed point characterized by x i , y i = 0, (or y = 0) and which essentially means that the partial derivative with respect to the field φ i of the sum of all the dark matter contributions must vanish. This solution was discussed in a number of recent publications for a single field system and two dark matter components with symmetric couplings [45][46][47][48]. For the simple system of two fields and two dark matter components we obtain that the field must settle at the bottom of a valley defined by the flat direction in the φ 1 -φ 2 plane,…”

“…[44,45] and the phenomenology of such a set up was investigated and compared to observations in Refs. [46][47][48].…”

Linear density perturbations in multifield coupled quintessence

“…From the 0 − 0 component we get 20) from the 0 − i componentψ 21) from the trace of the i − j componenẗ 22) and from the trace-free part of the i − j componenṫ…”

“…In a series of recent papers [20,21,24], perturbations in the McDE model have been calculated numerically and compared with present and future large scale structure experiments. Taking this line of investigation, one can model the dark sector of the universe as being made up of N fluids interacting with M scalar fields.…”

“…One example is coupled quintessence. In this model a scalar field, which makes up the dark energy (DE) component of the universe and produces acceleration, is coupled to a pressureless dark matter fluid [10][11][12][13][14][15][16][17][18][19][20][21][22][23]. Recent extensions which have been investigated include Multicoupled Dark Energy (McDE) (see e.g.…”