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We present cosmological constraints from 2D weak gravitational lensing by the large-scale structure in the Canada–France–Hawaii Telescope Lensing Survey (CFHTLenS) which spans 154 deg² in five optical bands. Using accurate photometric redshifts and measured shapes for 4. 2 million galaxies between redshifts of 0. 2 and 1. 3, we compute the 2D cosmic shear correlation function over angular scales ranging between 0. 8 and 350 arcmin. Using non-linear models of the dark-matter power spectrum, we constrain cosmological parameters by exploring the parameter space with Population Monte Carlo sampling. The best constraints from lensing alone are obtained for the small-scale density-fluctuations amplitude σ₈ scaled with the total matter density Ωm. For a flat Λcold dark matter (ΛCDM) model we obtain σ₈ (Ωₘ/0. 27) 0. 6 = 0. 79 ± 0. 03. combine the CFHTLenS data with 7-year Wilkinson Microwave Anisotropy Probe (WMAP7), baryonic acoustic oscillations (BAO): SDSS-III (BOSS) and a Hubble Space Telescope distance-ladder prior on the Hubble constant to get joint constraints. For a flat ΛCDM model, we find Ωₘ = 0. 283 ± 0. 010 and σ₈ = 0. 813 ± 0. 014. In the case of a curved wCDM universe, we obtain Ωₘ = 0. 27 ± 0. 03, σ₈ = 0. 83 ± 0. 04, w0 = −1. 10 ± 0. 15 and ΩK = 0. 006^ (+0. 006) _ (− 0. 004). calculate the Bayesian evidence to compare flat and curved ΛCDM and dark-energy CDM models. From the combination of all four probes, we find models with curvature to be at moderately disfavoured with respect to the flat case. A simple dark-energy model is indistinguishable from ΛCDM. Our results therefore do not necessitate any deviations from the standard cosmological model.
Kilbinger et al. (Sat,) studied this question.