Joint analysis of Dark Energy Survey Year 3 data and CMB lensing from SPT and Planck. III. Combined cosmological constraints

Creators: Abbott, T. M. C.; Aguena, M.; Alarcon, A.; Alves, O.; Amon, A.; Andrade-Oliveira, F.; Annis, J.; Ansarinejad, B.; Avila, S.; Bacon, D.; Baxter, E. J.; Bechtol, K.; Becker, M. R.; Benson, B. A.; Bernstein, G. M.; Bertin, E.; Blazek, J.; Bleem, L. E.; Bocquet, S.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Camacho, H.; Campos, A.; Carlstrom, J. E.; Carnero Rosell, A.; Carrasco Kind, M.; Carretero, J.; Cawthon, R.; Chang, C.; Chang, C. L.; Chen, R.; Choi, A.¹; Chown, R.; Conselice, C.; Cordero, J.; Costanzi, M.; Crawford, T.; Crites, A. T.¹; Crocce, M.; da Costa, L. N.; Davis, C.; Davis, T. M.; de Haan, T.; De Vicente, J.; DeRose, J.; Desai, S.; Diehl, H. T.; Dobbs, M. A.; Dodelson, S.; Doel, P.; Doux, C.; Drlica-Wagner, A.; Eckert, K.; Eifler, T. F.; Elsner, F.; Elvin-Poole, J.; Everett, S.; Everett, W.; Fang, X.; Ferrero, I.; Ferté, A.; Flaugher, B.; Fosalba, P.; Friedrich, O.; Frieman, J.; García-Bellido, J.; Gatti, M.; George, E. M.; Giannantonio, T.; Giannini, G.; Gruen, D.; Gruendl, R. A.; Gschwend, J.; Gutierrez, G.; Halverson, N. W.; Harrison, I.; Herner, K.; Hinton, S. R.; Holder, G. P.; Hollowood, D. L.; Holzapfel, W. L.; Honscheid, K.; Hrubes, J. D.; Huang, H.; Huff, E. M.; Huterer, D.; Jain, B.; James, D. J.; Jarvis, M.; Jeltema, T.; Kent, S.; Knox, L.; Kovacs, A.; Krause, E.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Lee, A. T.; Leget, P.-F.; Lemos, P.; Liddle, A. R.; Lidman, C.; Luong-Van, D.; McMahon, J. J.; MacCrann, N.; March, M.; Marshall, J. L.; Martini, P.; McCullough, J.; Melchior, P.; Menanteau, F.; Meyer, S. S.; Miquel, R.; Mocanu, L.; Mohr, J. J.; Morgan, R.; Muir, J.; Myles, J.; Natoli, T.; Navarro-Alsina, A.; Nichol, R. C.; Omori, Y.; Padin, S.¹; Pandey, S.; Park, Y.; Paz-Chinchón, F.; Pereira, M. E. S.; Pieres, A.; Plazas Malagón, A. A.; Porredon, A.; Prat, J.; Pryke, C.; Raveri, M.; Reichardt, C. L.; Rollins, R. P.; Romer, A. K.; Roodman, A.; Rosenfeld, R.; Ross, A. J.; Ruhl, J. E.; Rykoff, E. S.; Sánchez, C.; Sanchez, E.; Sanchez, J.; Schaffer, K. K.; Secco, L. F.; Sevilla-Noarbe, I.; Sheldon, E.; Shin, T.; Shirokoff, E.; Smith, M.; Staniszewski, Z.; Stark, A. A.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; To, C.; Troxel, M. A.; Tutusaus, I.; Varga, T. N.; Vieira, J. D.; Weaverdyck, N.; Wechsler, R. H.; Weller, J.; Williamson, R.; Wu, W. L. K.; Yanny, B.; Yin, B.; Zhang, Y.; Zuntz, J.

1. California Institute of Technology

Abstract

We present cosmological constraints from the analysis of two-point correlation functions between galaxy positions and galaxy lensing measured in Dark Energy Survey (DES) Year 3 data and measurements of cosmic microwave background (CMB) lensing from the South Pole Telescope (SPT) and Planck. When jointly analyzing the DES-only two-point functions and the DES cross-correlations with SPT+𝑃⁢𝑙⁢𝑎⁢𝑛⁢𝑐⁢𝑘 CMB lensing, we find Ωm=0.344±0.030 and 𝑆8≡𝜎8⁢(Ωm/0.3)0.5=0.773±0.016, assuming Λ⁢CDM. When additionally combining with measurements of the CMB lensing autospectrum, we find Ωm=0.306+0.018−0.021 and 𝑆8=0.792±0.012. The high signal-to-noise of the CMB lensing cross-correlations enables several powerful consistency tests of these results, including comparisons with constraints derived from cross-correlations only, and comparisons designed to test the robustness of the galaxy lensing and clustering measurements from DES. Applying these tests to our measurements, we find no evidence of significant biases in the baseline cosmological constraints from the DES-only analyses or from the joint analyses with CMB lensing cross-correlations. However, the CMB lensing cross-correlations suggest possible problems with the correlation function measurements using alternative lens galaxy samples, in particular the redmagic galaxies and high-redshift maglim galaxies, consistent with the findings of previous studies. We use the CMB lensing cross-correlations to identify directions for further investigating these problems.

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Acknowledgement

The South Pole Telescope program is supported by the National Science Foundation (NSF) through the grant OPP-1852617. Partial support is also provided by the Kavli Institute of Cosmological Physics at the University of Chicago. Argonne National Laboratory’s work was supported by the U.S. Department of Energy, Office of Science, Office of High Energy Physics, under contract No. DE-AC02-06CH11357. Work at Fermi National Accelerator Laboratory, a DOE-OS, HEP User Facility managed by the Fermi Research Alliance, LLC, was supported under Contract No. DE-AC02-07CH11359. The Melbourne authors acknowledge support from the Australian Research Council’s Discovery Projects scheme (DP210102386). The McGill authors acknowledge funding from the Natural Sciences and Engineering Research Council of Canada, Canadian Institute for Advanced research, and the Fonds de recherche du Quúbec Nature et technologies. The CU Boulder group acknowledges support from NSF Grant No. AST-0956135. The Munich group acknowledges the support by the ORIGINS Cluster (funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy—EXC-2094–390783311), the MaxPlanck-Gesellschaft Faculty Fellowship Program, and the Ludwig-Maximilians-Universität München. J. V. acknowledges support from the Sloan Foundation. 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, 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 (ETH) Zürich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ciències de l’Espai (IEEC/CSIC), 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, NFS’s NOIRLab, 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 at NSF’s NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed 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 Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants No. ESP2017-89838, No. PGC2018-094773, No. PGC2018-102021, No. SEV-2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. 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’s Seventh Framework Program (FP7/2007-2013) including ERC grant agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant No. 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. We gratefully acknowledge the computing resources provided on Crossover (and/or Bebop and/or Swing and/or Blues), a high-performance computing cluster operated by the Laboratory Computing Resource Center at Argonne National Laboratory.

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