https://hal-insu.archives-ouvertes.fr/insu-03644953Simon, P.P.SimonSemboloni, E.E.Sembolonivan Waerbeke, L.L.van WaerbekeHoekstra, H.H.HoekstraErben, T.T.ErbenFu, L.L.FuHarnois-Déraps, J.J.Harnois-DérapsHeymans, C.C.HeymansHildebrandt, H.H.HildebrandtKilbinger, M.M.KilbingerIAP - Institut d'Astrophysique de Paris - INSU - CNRS - Institut national des sciences de l'Univers - SU - Sorbonne Université - CNRS - Centre National de la Recherche ScientifiqueKitching, T. D.T. D.KitchingMiller, L.L.MillerSchrabback, T.T.SchrabbackCFHTLenS: a Gaussian likelihood is a sufficient approximation for a cosmological analysis of third-order cosmic shear statisticsHAL CCSD2015gravitational lensing: weakmethods: statisticalcosmology: observationsdark matterAstrophysics - Cosmology and Nongalactic Astrophysics[SDU] Sciences of the Universe [physics][SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph]Gestionnaire, Hal Sorbonne Université2022-04-26 09:14:432023-03-13 11:17:182022-04-26 09:14:44enJournal articleshttps://hal-insu.archives-ouvertes.fr/insu-03644953/document10.1093/mnras/stv339application/pdf1We study the correlations of the shear signal between triplets of sources in the Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS) to probe cosmological parameters via the matter bispectrum. In contrast to previous studies, we adopt a non-Gaussian model of the data likelihood which is supported by our simulations of the survey. We find that for state-of-the-art surveys, similar to CFHTLenS, a Gaussian likelihood analysis is a reasonable approximation, albeit small differences in the parameter constraints are already visible. For future surveys we expect that a Gaussian model becomes inaccurate. Our algorithm for a refined non-Gaussian analysis and data compression is then of great utility especially because it is not much more elaborate if simulated data are available. Applying this algorithm to the third-order correlations of shear alone in a blind analysis, we find a good agreement with the standard cosmological model: Σ _8=σ _8(Ω _m/0.27)^{0.64}=0.79^{+0.08}_{-0.11} for a flat Λ cold dark matter cosmology with h = 0.7 ± 0.04 (68 per cent credible interval). Nevertheless our models provide only moderately good fits as indicated by χ<SUP>2</SUP>/dof = 2.9, including a 20 per cent rms uncertainty in the predicted signal amplitude. The models cannot explain a signal drop on scales around 15 arcmin, which may be caused by systematics. It is unclear whether the discrepancy can be fully explained by residual point spread function systematics of which we find evidence at least on scales of a few arcmin. Therefore we need a better understanding of higher order correlations of cosmic shear and their systematics to confidently apply them as cosmological probes.