Autor(es):
Friedrich, O. ; Andrade-Oliveira, F. [UNESP] ; Camacho, H. [UNESP] ; Alves, O. [UNESP] ; Rosenfeld, R. [UNESP] ; Sanchez, J. ; Fang, X. ; Eifler, T. F. ; Krause, E. ; Chang, C. ; Omori, Y. ; Amon, A. ; Baxter, E. ; Elvin-Poole, J. ; Huterer, D. ; Palmese, A. ; Paz-Chinchon, F. ; Plazas, A. A. ; Sanchez, E. ; Scarpine, V. ; Serrano, S. ; Soares-Santos, M. ; Smith, M. ; Suchyta, E. ; Tarle, G. ; Thomas, D. ; Too, C. ; Varga, T. N. ; Weller, J. ; Wilkinson, R. D.
Data: 2022
Identificador Persistente: http://hdl.handle.net/11449/229920
Origem: Oasisbr
Assunto(s): cosmology: observations; large-scale structure of Universe
Descrição
Made available in DSpace on 2022-04-29T08:36:40Z (GMT). No. of bitstreams: 0 Previous issue date: 2021-12-01
We describe and test the fiducial covariance matrix model for the combined two-point function analysis of the Dark Energy Survey Year 3 (DES-Y3) data set. Using a variety of new ansatzes for covariance modelling and testing, we validate the assumptions and approximations of this model. These include the assumption of Gaussian likelihood, the trispectrum contribution to the covariance, the impact of evaluating the model at a wrong set of parameters, the impact of masking and survey geometry, deviations from Poissonian shot noise, galaxy weighting schemes, and other sub-dominant effects. We find that our covariance model is robust and that its approximations have little impact on goodness of fit and parameter estimation. The largest impact on best-fitting figure-of-merit arises from the so-called fsky approximation for dealing with finite survey area, which on average increases the χ2 between maximum posterior model and measurement by $3.7{{\ \rm per\ cent} (Δχ2 ≈ 18.9). Standard methods to go beyond this approximation fail for DES-Y3, but we derive an approximate scheme to deal with these features. For parameter estimation, our ignorance of the exact parameters at which to evaluate our covariance model causes the dominant effect. We find that it increases the scatter of maximum posterior values for ωm and σ8 by about $3{{\ \rm per\ cent} and for the dark energy equation-of-state parameter by about $5{{\ \rm per\ cent}.
Kavli Institute for Cosmology University of Cambridge, Madingley Road
Churchill College University of Cambridge
Instituto de Física Teórica Universidade Estadual Paulista
Laboratório Interinstitucional de e-Astronomia - LIneA, Rua Gal. José Cristino 77
Department of Physics University of Michigan
ICTP South American Institute for Fundamental Research Instituto de Física Teórica Universidade Estadual Paulista
Fermi National Accelerator Laboratory, PO Box 500
Department of Astronomy/Steward Observatory University of Arizona, 933 North Cherry Avenue
Jet Propulsion Laboratory California Institute of Technology, 4800 Oak Grove Drive
Department of Astronomy and Astrophysics University of Chicago
Kavli Institute for Cosmological Physics University of Chicago
Kavli Institute for Particle Astrophysics and Cosmology Stanford University, PO Box 2450
Department of Physics and Astronomy University of Hawaii, Watanabe 416, 2505 Correa Road
Center for Cosmology and Astro-Particle Physics Ohio State University
Department of Physics Ohio State University
Institut d'Estudis Espacials de Catalunya (IEEC)
Institute of Space Sciences ICE CSIC Campus UAB, Carrer de Can Magrans, s/n
SLAC National Accelerator Laboratory
National Center for Supercomputing Applications, 1205 West Clark Street
Department of Physics Stanford University, 382 Via Pueblo Mall
Centro de Investigaciones Energéticas Medioambientales y Tecnológicas (CIEMAT)
Institute of Cosmology and Gravitation University of Portsmouth
Department of Physics and Astronomy Pevensey Building University of Sussex
Institute of Astronomy University of Cambridge, Madingley Road
Department of Astrophysical Sciences Princeton University, Peyton Hall
School of Physics and Astronomy University of Southampton
Computer Science and Mathematics Division Oak Ridge National Laboratory
Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse
Universitäts-Sternwarte Fakultät für Physik Ludwig-Maximilians Universität München, Scheinerstr 1
Instituto de Física Teórica Universidade Estadual Paulista
ICTP South American Institute for Fundamental Research Instituto de Física Teórica Universidade Estadual Paulista
