Dynamics of Interacting Quintessence Models: Observational Constraints

Interacting quintessence models have been proposed to explain or, at least, alleviate the coincidence problem of late acceleration. In this paper we are concerned with two aspects of these kind of models: (i) which is the dynamical evolution of the model of Chimento {\em et al.} \cite{chimento}, i.e., under which conditions it gives rise to a right sequence of radiation, dark matter and dark energy dominated eras, and (ii) if it evades the limits imposed by Amendola {\em et al.} \cite{amendola-challenges}. After showing that the model correctly reproduces these eras, we correlate three data sets that constrain the interaction at three different redshift epochs:

z=10^{4}

,

z=10^{3}

, and

z=1

. We discuss the model selection and argue that notwithstanding the model under consideration evades the aforesaid limits it is heavily constrained by observation, so the prospects that the coincidence problem can be explained by the coupling of dark matter to dark energy are not clearly favored by the data.

Note:

13 pages, 6 figures and 4 tables

98.80.Jk
98.80.Es
98.80.Bp
expansion: acceleration
quintessence: interaction
cosmic coincidence
dark matter
dark energy
cosmic background radiation
power spectrum

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