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

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dc.creatorSchimd, Carlo
dc.creatorTereno, Ismael
dc.creatorUzan, Jean-Philippe
dc.creatorMellier, Yannick
dc.creatorvan Waerbeke, Ludovic
dc.creatorSemboloni, Elisabetta
dc.creatorHoekstra, Henk
dc.creatorFu, Liping
dc.creatorRiazuelo, Alain
dc.date2006-03-07
dc.date.accessioned2026-07-07T11:42:30Z
dc.date.available2026-07-07T11:42:30Z
dc.descriptionDark 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.
dc.description20 pages, 13 figures; abridged abstract
dc.identifierhttps://arxiv.org/abs/astro-ph/0603158
dc.identifierhttp://arxiv.org/abs/astro-ph/0603158
dc.identifierAstron.Astrophys.463:405-421,2007
dc.identifierdoi:10.1051/0004-6361:20065154
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/200907
dc.subjectAstrophysics
dc.subjectHigh Energy Physics - Phenomenology
dc.titleTracking quintessence by cosmic shear - Constraints from VIRMOS-Descart and CFHTLS and future prospects
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