We aim to demonstrate the accuracy of the method to simulated fields, and then proceed to apply it to the mass reconstruction of the HST/ACS COSMOS field. We introduce a novel methodology that enables the efficient sampling of the high-dimensional Bayesian posterior of the weak lensing mass-mapping problem, relying on simulations to define a fully non-Gaussian prior.
#Inverse fourier transform full
Weak lensing mass-mapping is a useful tool for accessing the full distribution of dark matter on the sky, but because of intrinsic galaxy ellipticies, finite fields, and missing data, the recovery of dark matter maps constitutes a challenging, ill-posed inverse problemĪims. Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, JapanĬenter for Gravitational Physics, Yukawa Institute for Theoretical Physics, Kyoto University, Kitashirakawa Oiwakecho, Sakyo-ku, Kyoto 606-8502, JapanĪrgelander-Institut für Astronomie, Universität Bonn, Auf dem Hügel 71, 53121 Bonn, GermanyĬontext. Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 93720, USA University College London, Gower St, London, UKīerkeley Center for Cosmological Physics, University of California, 341 Campbell Hall, Berkeley, CA 94720, USA Schrabback 8ĪIM, CEA, CNRS, Université Paris-Saclay, Université Paris Diderot, Sorbonne Paris Cité, 91191 Gif-sur-Yvette, FranceĮ-mail: de Physique de l’École Normale Supérieure, ENS, Université PSL, CNRS, Sorbonne Université, Université de Paris, Paris, France
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