Tracking quintessence by cosmic shear - Constraints from VIRMOS-Descart and CFHTLS and future prospects

TL;DR

This paper constrains quintessence dark energy models using cosmic shear, supernovae, and CMB data, exploring the impact of non-linear regimes and future survey prospects to improve understanding of dark energy.

Contribution

It presents the first weak lensing analysis of high-energy motivated dark energy models, incorporating non-linear regime descriptions and future survey simulations.

Findings

Constraints on quintessence slope parameter alpha: <1 without supergravity, ~2 with supergravity.

Estimated dark energy density Omega_Q: approximately 0.75.

Analysis of large-scale weak lensing data reduces dependence on non-linear modeling.

Abstract

Dark energy can be investigated in two complementary ways, by considering either general parameterizations or physically well-defined models. Following the second route, we explore the constraints on quintessence models where the acceleration is driven by a slow-rolling scalar field. The analysis focuses on cosmic shear, combined with supernovae Ia and CMB data. Using a Boltzmann code including quintessence models and the computation of weak lensing observables, we determine several two-point shear statistics. The non-linear regime is described by two different mappings. The likelihood analysis is based on a grid method. The data include the "gold set" of supernovae Ia, the WMAP-1 year data and the VIRMOS-Descart and CFHTLS-deep and -wide data for weak lensing. This is the first analysis of high-energy motivated dark energy models that uses weak lensing data. We explore larger angular scales, using a synthetic realization of the complete CFHTLS-wide survey as well as next space-based missions surveys. Two classes of cosmological parameters are discussed: i) those accounting for quintessence affect mainly geometrical factors; ii) cosmological parameters specifying the primordial universe strongly depend on the description of the non-linear regime. This dependence is addressed using wide surveys, by discarding the smaller angular scales to reduce the dependence on the non-linear regime. Special care is payed to the comparison of these physical models with parameterizations of the equation of state. For a flat universe and a quintessence inverse power law potential with slope alpha, we obtain alpha < 1 and Omega_Q=0.75^{+0.03}_{-0.04} at 95% confidence level, whereas alpha=2^{+18}_{-2}, Omega_Q=0.74^{+0.03}_{-0.05} when including supergravity corrections.