Dark Energy Survey Year 3 results: Cosmology with moments of weak lensing mass maps - Validation on simulations

We present a simulated cosmology analysis using the second and third moments of the weak lensing mass (convergence) maps. The second moment, or variances, of the convergence as a function of smoothing scale contains information similar to standard shear two-point statistics. The third moment, or the...

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Detalhes bibliográficos
Autores: Gatti, Marco, Crocce, Martín, Fosalba, Pablo, Gaztañaga, Enrique, Santiago, S., Zuntz, Joe A.
Formato: artículo
Estado:Versión publicada
Fecha de publicación:2020
País:España
Recursos:Consejo Superior de Investigaciones Científicas (CSIC)
Repositorio:DIGITAL.CSIC. Repositorio Institucional del CSIC
OAI Identifier:oai:digital.csic.es:10261/236754
Acesso em linha:http://hdl.handle.net/10261/236754
Access Level:acceso abierto
Palavra-chave:Cosmology: observations
Gravitational lensing: weak
Large-scale structure of the universe
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dc.title.none.fl_str_mv Dark Energy Survey Year 3 results: Cosmology with moments of weak lensing mass maps - Validation on simulations
title Dark Energy Survey Year 3 results: Cosmology with moments of weak lensing mass maps - Validation on simulations
spellingShingle Dark Energy Survey Year 3 results: Cosmology with moments of weak lensing mass maps - Validation on simulations
Gatti, Marco
Cosmology: observations
Gravitational lensing: weak
Large-scale structure of the universe
title_short Dark Energy Survey Year 3 results: Cosmology with moments of weak lensing mass maps - Validation on simulations
title_full Dark Energy Survey Year 3 results: Cosmology with moments of weak lensing mass maps - Validation on simulations
title_fullStr Dark Energy Survey Year 3 results: Cosmology with moments of weak lensing mass maps - Validation on simulations
title_full_unstemmed Dark Energy Survey Year 3 results: Cosmology with moments of weak lensing mass maps - Validation on simulations
title_sort Dark Energy Survey Year 3 results: Cosmology with moments of weak lensing mass maps - Validation on simulations
dc.creator.none.fl_str_mv Gatti, Marco
Crocce, Martín
Fosalba, Pablo
Gaztañaga, Enrique
Santiago, S.
Zuntz, Joe A.
author Gatti, Marco
author_facet Gatti, Marco
Crocce, Martín
Fosalba, Pablo
Gaztañaga, Enrique
Santiago, S.
Zuntz, Joe A.
author_role author
author2 Crocce, Martín
Fosalba, Pablo
Gaztañaga, Enrique
Santiago, S.
Zuntz, Joe A.
author2_role author
author
author
author
author
dc.contributor.none.fl_str_mv Henry Luce Foundation
Department of Energy (US)
National Science Foundation (US)
Ministerio de Ciencia, Innovación y Universidades (España)
Science and Technology Facilities Council (UK)
University of Illinois
Kavli Institute for Theoretical Physics
University of Chicago
The Ohio State University
Texas A&M University
Financiadora de Estudos e Projetos (Brasil)
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil)
Ministério da Ciência, Tecnologia e Inovação (Brasil)
German Research Foundation
European Commission
Generalitat de Catalunya
Fermilab
Consejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]
dc.subject.none.fl_str_mv Cosmology: observations
Gravitational lensing: weak
Large-scale structure of the universe
topic Cosmology: observations
Gravitational lensing: weak
Large-scale structure of the universe
description We present a simulated cosmology analysis using the second and third moments of the weak lensing mass (convergence) maps. The second moment, or variances, of the convergence as a function of smoothing scale contains information similar to standard shear two-point statistics. The third moment, or the skewness, contains additional non-Gaussian information. The analysis is geared towards the third year (Y3) data from the Dark Energy Survey (DES), but the methodology can be applied to other weak lensing data sets. We present the formalism for obtaining the convergence maps from the measured shear and for obtaining the second and third moments of these maps given partial sky coverage. We estimate the covariance matrix from a large suite of numerical simulations. We test our pipeline through a simulated likelihood analyses varying 5 cosmological parameters and 10 nuisance parameters and identify the scales where systematic or modelling uncertainties are not expected to affect the cosmological analysis. Our simulated likelihood analysis shows that the combination of second and third moments provides a 1.5 per cent constraint on S8 σ8(ωm/0.3)0.5 for DES Year 3 data. This is 20 per cent better than an analysis using a simulated DES Y3 shear two-point statistics, owing to the non-Gaussian information captured by the inclusion of higher order statistics. This paper validates our methodology for constraining cosmology with DES Year 3 data, which will be presented in a subsequent paper.
publishDate 2020
dc.date.none.fl_str_mv 2020
2021
2021
2021
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dc.identifier.none.fl_str_mv http://hdl.handle.net/10261/236754
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dc.publisher.none.fl_str_mv Blackwell Publishing
Oxford University Press
publisher.none.fl_str_mv Blackwell Publishing
Oxford University Press
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spelling Dark Energy Survey Year 3 results: Cosmology with moments of weak lensing mass maps - Validation on simulationsGatti, MarcoCrocce, MartínFosalba, PabloGaztañaga, EnriqueSantiago, S.Zuntz, Joe A.Cosmology: observationsGravitational lensing: weakLarge-scale structure of the universeWe present a simulated cosmology analysis using the second and third moments of the weak lensing mass (convergence) maps. The second moment, or variances, of the convergence as a function of smoothing scale contains information similar to standard shear two-point statistics. The third moment, or the skewness, contains additional non-Gaussian information. The analysis is geared towards the third year (Y3) data from the Dark Energy Survey (DES), but the methodology can be applied to other weak lensing data sets. We present the formalism for obtaining the convergence maps from the measured shear and for obtaining the second and third moments of these maps given partial sky coverage. We estimate the covariance matrix from a large suite of numerical simulations. We test our pipeline through a simulated likelihood analyses varying 5 cosmological parameters and 10 nuisance parameters and identify the scales where systematic or modelling uncertainties are not expected to affect the cosmological analysis. Our simulated likelihood analysis shows that the combination of second and third moments provides a 1.5 per cent constraint on S8 σ8(ωm/0.3)0.5 for DES Year 3 data. This is 20 per cent better than an analysis using a simulated DES Y3 shear two-point statistics, owing to the non-Gaussian information captured by the inclusion of higher order statistics. This paper validates our methodology for constraining cosmology with DES Year 3 data, which will be presented in a subsequent paper.Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana-Champaign, the Kavli Institute of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundac¸ao Carlos Chagas Filho de Amparo ˜ a Pesquisa do ` Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cient´ıfico e Tecnologico and the Minist ´ erio da Ci ´ encia, Tecnologia ˆ e Inovac¸ao, the Deutsche Forschungsgemeinschaft and the Collabo- ˜ rating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California, Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y ´ Tecnologicas-Madrid, the University of Chicago, University College ´ London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule (ETH) Z ¨ urich, Fermi ¨ National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ciencies de l’Espai (IEEC/CSIC), the ` Institut de F´ısica d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat M¨ unchen, and the ¨ associated Excellence Cluster Universe, the University of Michigan, the National Optical Astronomy Observatory, the University of Nottingham, the Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory, National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grant Numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under grants AYA2015- 71825, ESP2015-66861, FPA2015-68048, SEV-2016-0588, SEV2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union 7th Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) e-Universe (CNPq grant ˆ 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.Blackwell PublishingOxford University PressHenry Luce FoundationDepartment of Energy (US)National Science Foundation (US)Ministerio de Ciencia, Innovación y Universidades (España)Science and Technology Facilities Council (UK)University of IllinoisKavli Institute for Theoretical PhysicsUniversity of ChicagoThe Ohio State UniversityTexas A&M UniversityFinanciadora de Estudos e Projetos (Brasil)Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de JaneiroConselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil)Ministério da Ciência, Tecnologia e Inovação (Brasil)German Research FoundationEuropean CommissionGeneralitat de CatalunyaFermilabConsejo Superior de Investigaciones Científicas [https://ror.org/02gfc7t72]2021202120202021info:eu-repo/semantics/articlehttp://purl.org/coar/resource_type/c_dcae04bcPublisher's versioninfo:eu-repo/semantics/publishedVersionhttp://hdl.handle.net/10261/236754reponame:DIGITAL.CSIC. 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