Andrea Petri

Emulating the CFHTLenS weak lensing data: Cosmological constraints from moments and Minkowski functionals

Weak gravitational lensing is a powerful cosmological probe, with non-Gaussian features potentially containing the majority of the information. We examine constraints on the parameter triplet

Validity of the Born approximation for beyond Gaussian weak lensing observables

({\mathrm{\ensuremath{\Omega}}}_{m},w,{\ensuremath{\sigma}}_{8})

Do dark matter halos explain lensing peaks

from non-Gaussian features of the weak lensing convergence field, including a set of moments (up to fourth order) and Minkowski functionals, using publicly available data from the

CMB lensing beyond the power spectrum: Cosmological constraints from the one-point probability distribution function and peak counts

154\text{ }\text{ }{\mathrm{deg}}^{2}

Cosmology with photometric weak lensing surveys: Constraints with redshift tomography of convergence peaks and moments

CFHTLenS survey. We utilize a suite of ray-tracing N-body simulations spanning 91 points in

MassiveNuS: cosmological massive neutrino simulations

({\mathrm{\ensuremath{\Omega}}}_{m},w,{\ensuremath{\sigma}}_{8})

Mocking the weak lensing universe: The LensTools Python computing package ☆

parameter space, replicating the galaxy sky positions, redshifts and shape noise in the CFHTLenS catalogs. We then build an emulator that interpolates the simulated descriptors as a function of

Geometry and growth contributions to cosmic shear observables

({\mathrm{\ensuremath{\Omega}}}_{m},w,{\ensuremath{\sigma}}_{8})

CONSEQUENCES OF CCD IMPERFECTIONS FOR COSMOLOGY DETERMINED BY WEAK LENSING SURVEYS: FROM LABORATORY MEASUREMENTS TO COSMOLOGICAL PARAMETER BIAS

, and use it to compute the likelihood function and parameter constraints. We employ a principal component analysis to reduce dimensionality and to help stabilize the constraints with respect to the number of bins used to construct each statistic. Using the full set of statistics, we find

Cosmology Constraints from the Weak Lensing Peak Counts and the Power Spectrum in CFHTLenS

{\mathrm{\ensuremath{\Sigma}}}_{8}\ensuremath{\equiv}{\ensuremath{\sigma}}_{8}({\mathrm{\ensuremath{\Omega}}}_{m}/0.27{)}^{0.55}=0.75\ifmmode\pm\else\textpm\fi{}0.04