Phenomenological aspects of dark energy dominated by Pier Stefano Corasaniti; University of Sussex

By Pier Stefano Corasaniti; University of Sussex

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Larger values of ΩX ). As we will show later, extending the likelihood analysis to the slope of the tracker potential enables us to find models that simultaneously fit the whole data. 6 (2σ). In a different approach Saini et al. 2 Parameterized quintessence potential 37 they have been able to reconstruct the redshift dependence of the dark energy equation of state. 83. Waga and Frieman have constrained the slope of the Inverse Power Law potential α (see Eq. 10)) by making use of the Sn Ia and lensing statistic data [116].

5). In this case we can distinguish two different evolutionary regimes of the gravitational potential. At redshift z > 10 the Universe is matter dominated and the quintessence is in the tracker solution with an equation of state very close to the matter value. Therefore during this period the expansion rate is the same as in the Λ model and we would expect Φ/ΦΛ ≈ 1. The fact this ratio deviates from unity is due to the presence of the dark energy perturbations. On the other hand the evolution of the gravitational potential at z << 10 is caused by the accelerated phase of expansion.

In this Chapter we will review some of the constraints obtained in previous works. Then we will describe the analysis of the Sn Ia data and the measured position of the CMB peaks that we performed to constrain the shape of a general quintessence potential [110]. We will comment on our results and compare them to those obtained in other related work. 1 Upper bounds on the cosmic equation of state Different dark energy models are usually constrained assuming that the dark energy behaves as a perfect fluid with a constant equation of state wX = pX /ρX ≤ −1.

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