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Dark Energy Survey year 1 results: Cosmological constraints from galaxy clustering and weak lensing

Abbott, T. M. C. and Eifler, T. F. (2018) Dark Energy Survey year 1 results: Cosmological constraints from galaxy clustering and weak lensing. Physical Review D, 98 (4). Art. No. 043526. ISSN 2470-0010. https://resolver.caltech.edu/CaltechAUTHORS:20180828-110124712

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Abstract

We present cosmological results from a combined analysis of galaxy clustering and weak gravitational lensing, using 1321 deg^2 of griz imaging data from the first year of the Dark Energy Survey (DES Y1). We combine three two-point functions: (i) the cosmic shear correlation function of 26 million source galaxies in four redshift bins, (ii) the galaxy angular autocorrelation function of 650,000 luminous red galaxies in five redshift bins, and (iii) the galaxy-shear cross-correlation of luminous red galaxy positions and source galaxy shears. To demonstrate the robustness of these results, we use independent pairs of galaxy shape, photometric-redshift estimation and validation, and likelihood analysis pipelines. To prevent confirmation bias, the bulk of the analysis was carried out while “blind” to the true results; we describe an extensive suite of systematics checks performed and passed during this blinded phase. The data are modeled in flat ΛCDM and wCDM cosmologies, marginalizing over 20 nuisance parameters, varying 6 (for ΛCDM) or 7 (for wCDM) cosmological parameters including the neutrino mass density and including the 457×457 element analytic covariance matrix. We find consistent cosmological results from these three two-point functions and from their combination obtain S_8 ≡ σ_8(Ω_m/0.3)^(0.5) = 0.773^(+0.026)_(−0.020) and Ω_m = 0.267^(+0.030)_(−0.017) for ΛCDM; for wCDM, we find S_8 = 0.782^(+0.036)_(−0.024), Ω_m = 0.284^(+0.033)_(−0.030), and w = −0.82^(+0.21)_(−0.20) at 68% C.L. The precision of these DES Y1 constraints rivals that from the Planck cosmic microwave background measurements, allowing a comparison of structure in the very early and late Universe on equal terms. Although the DES Y1 best-fit values for S_8 and Ω_m are lower than the central values from Planck for both ΛCDM and wCDM, the Bayes factor indicates that the DES Y1 and Planck data sets are consistent with each other in the context of ΛCDM. Combining DES Y1 with Planck, baryonic acoustic oscillation measurements from SDSS, 6dF, and BOSS and type Ia supernovae from the Joint Lightcurve Analysis data set, we derive very tight constraints on cosmological parameters: S_8 = 0.802±0.012 and Ω_m=0.298±0.007 in ΛCDM and w = −1.00^(+0.05)_(−0.04) in wCDM. Upcoming Dark Energy Survey analyses will provide more stringent tests of the ΛCDM model and extensions such as a time-varying equation of state of dark energy or modified gravity.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.1103/PhysRevD.98.043526DOIArticle
https://arxiv.org/abs/1708.01530arXivDiscussion Paper
https://link.aps.org/doi/10.1103/Physics.11.85Featured InPhysics: Viewpoint
ORCID:
AuthorORCID
Eifler, T. F.0000-0002-1894-3301
Additional Information:© 2018 American Physical Society. Received 10 August 2017; published 27 August 2018. 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 Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovação, the Deutsche Forschungsgemeinschaft, and the collaborating institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai, the Institut de Física d’Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München 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. This work was 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 under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-88861, No. FPA2015-68048, No. SEV-2012-0234, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include European Research Development Fund (ERDF) funds from the European Union. I. F. A. E. is partially funded by the Centres de Recerce de Catalunya (CERCA) program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including European Research Council Grants No. 240672, No. 291329, and No. 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics, through Project No. CE110001020. 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. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a nonexclusive, paid-up, irrevocable, worldwide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. We are grateful to Anže Slosar for helpful communications. Many of the figures in this paper were produced with chainconsumer [151]. This research used resources of the National Energy Research Scientific Computing Center, a DOE Office of Science User Facility supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231.
Funders:
Funding AgencyGrant Number
Ministerio de Educación y Ciencia (MEC)UNSPECIFIED
Science and Technology Facilities Council (STFC)UNSPECIFIED
Higher Education Funding Council for EnglandUNSPECIFIED
University of Illinois Urbana-ChampaignUNSPECIFIED
University of ChicagoUNSPECIFIED
Ohio State UniversityUNSPECIFIED
Texas A&M UniversityUNSPECIFIED
Financiadora de Estudos e Projetos (FINEP)UNSPECIFIED
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ)UNSPECIFIED
Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq)UNSPECIFIED
Ministério da Ciência, Tecnologia e InovaçãoUNSPECIFIED
Deutsche Forschungsgemeinschaft (DFG)UNSPECIFIED
Argonne National LaboratoryUNSPECIFIED
University of California Santa CruzUNSPECIFIED
University of CambridgeUNSPECIFIED
Centro de Investigaciones Energéticas, Medioambientales y TecnológicasUNSPECIFIED
University College LondonUNSPECIFIED
DES-Brazil ConsortiumUNSPECIFIED
University of EdinburghUNSPECIFIED
ETH ZurichUNSPECIFIED
Fermi National Accelerator LaboratoryUNSPECIFIED
Institut de Ciències de l’EspaiUNSPECIFIED
Institut de Física d’Altes EnergiesUNSPECIFIED
Lawrence Berkeley National LaboratoryUNSPECIFIED
Ludwig-Maximilians Universität MünchenUNSPECIFIED
Excellence Cluster UniverseUNSPECIFIED
University of MichiganUNSPECIFIED
National Optical Astronomy ObservatoryUNSPECIFIED
University of NottinghamUNSPECIFIED
University of PennsylvaniaUNSPECIFIED
University of PortsmouthUNSPECIFIED
Stanford Linear Accelerator CenterUNSPECIFIED
Stanford UniversityUNSPECIFIED
University of SussexUNSPECIFIED
OzDES Membership ConsortiumUNSPECIFIED
NSFAST-1138766
NSFAST-1536171
Ministerio de Economía, Industria y Competitividad (MINECO)AYA2015-71825
Ministerio de Economía, Industria y Competitividad (MINECO)ESP2015-88861
Ministerio de Economía, Industria y Competitividad (MINECO)FPA2015-68048
Centro de Excelencia Severo OchoaSEV-2012-0234
Centro de Excelencia Severo OchoaSEV-2016-0597
Ministerio de Economía, Industria y Competitividad (MINECO)MDM-2015-0509
European Regional Development Fund (ERDF)UNSPECIFIED
Generalitat de CatalunyaUNSPECIFIED
European Research Council (ERC)240672
European Research Council (ERC)291329
European Research Council (ERC)306478
Australian Research CouncilCE110001020
Department of Energy (DOE)DE-AC02-07CH11359
Department of Energy (DOE)DE-AC02-05CH11231
Issue or Number:4
Record Number:CaltechAUTHORS:20180828-110124712
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20180828-110124712
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:89213
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:28 Aug 2018 18:23
Last Modified:09 Mar 2020 13:18

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