Journal article

Dark Energy Survey Year 1 results: Methodology and projections for joint analysis of galaxy clustering, galaxy lensing, and CMB lensing two-point functions

EJ Baxter, Y Omori, C Chang, T Giannantonio, D Kirk, E Krause, J Blazek, L Bleem, A Choi, TM Crawford, S Dodelson, TF Eifler, O Friedrich, D Gruen, GP Holder, B Jain, M Jarvis, N MacCrann, A Nicola, S Pandey Show all

Physical Review D: Particles, Fields, Gravitation and Cosmology | American Physical Society | Published : 2019

Abstract

Optical imaging surveys measure both the galaxy density and the gravitational lensing-induced shear fields across the sky. Recently, the Dark Energy Survey (DES) Collaboration used a joint fit to two-point correlations between these observables to place tight constraints on cosmology (T. M. C. Abbott (Dark Energy Survey Collaboration), Phys. Rev. D 98, 043526 (2018)PRVDAQ2470-001010.1103/PhysRevD.98.043526). In this work, we develop the methodology to extend the DES Year 1 joint probes analysis to include cross-correlations of the optical survey observables with gravitational lensing of the cosmic microwave background as measured by the South Pole Telescope (SPT) and Planck. Using simulated ..

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University of Melbourne Researchers

Grants

Awarded by U.S. Department of Energy


Awarded by Australian Research Council


Awarded by MINECO


Awarded by DOE


Awarded by Sloan Foundation


Awarded by NASA through Einstein Postdoctoral Fellowship - Chandra X-ray Center


Awarded by NASA


Awarded by National Science Foundation


Awarded by European Research Council under the European Union's Seventh Framework Program


Awarded by ERC


Awarded by Australian Research Council Centre of Excellence for All-sky Astrophysics


Awarded by NSF Physics Frontier Center


Awarded by Gordon and Betty Moore Foundation


Awarded by U.S. Department of Energy, Office of Science, Office of High Energy Physics


Funding Acknowledgements

The contour plots in this paper were made using CHAINCONSUMER<SUP>7</SUP> [90]. E. B. is partially supported by the U.S. Department of Energy Grant No. DE-SC0007901. The Reichardt and Bianchini acknowledge support from the Australian Research Council's Future Fellowships scheme (Grant No. FT150100074). P.F. is funded by MINECO, Projects No. ESP2013-48274-C3-1-P, No. ESP2014-58384-C3-1-P, and No. ESP2015-66861-C3-1-R. E. R. is supported by DOE Grant No. DE-SC0015975 and by the Sloan Foundation, Grant No. FG-2016-6443. Support for D. G. was provided by NASA through Einstein Postdoctoral Fellowship Grant No. PF5-160138 awarded by the Chandra X-ray Center, which is operated by the Smithsonian Astrophysical Observatory for NASA under Contract No. NAS8-03060. 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 andAstro-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, Fundacao Carlos Chagas Filho de Amparo 'a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientifico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovacao, 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 Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenossische Technische Hochschule Zurich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciencies de l'Espai, the Institut de Fisica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universitat Munchen 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 is 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 ERDF funds from the European Union. Institut de Fisica d'Altes Energies is partially funded by the Centres de Recerca de Catalunya 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 (Grant No. FP7/2007-2013) including ERC 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. The South Pole Telescope program is supported by the National Science Foundation through Grant No. PLR-1248097. Partial support is also provided by the NSF Physics Frontier Center Grant No. PHY-0114422 to the Kavli Institute of Cosmological Physics at the University of Chicago, the Kavli Foundation, and the Gordon and Betty Moore Foundation through Grant No. 947 to the University of Chicago. Argonne National Laboratory's work was supported under the U.S. Department of Energy Contract No. DE-AC02-06CH11357. 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.