@article{07f3da689c7f40dca1dd136ce2c70280,
title = "DES Y1 results: Splitting growth and geometry to test ΛcDM",
abstract = "We analyze Dark Energy Survey (DES) data to constrain a cosmological model where a subset of parameters - focusing on ωm - are split into versions associated with structure growth (e.g., ωmgrow) and expansion history (e.g., ωmgeo). Once the parameters have been specified for the ΛCDM cosmological model, which includes general relativity as a theory of gravity, it uniquely predicts the evolution of both geometry (distances) and the growth of structure over cosmic time. Any inconsistency between measurements of geometry and growth could therefore indicate a breakdown of that model. Our growth-geometry split approach therefore serves both as a (largely) model-independent test for beyond-ΛCDM physics, and as a means to characterize how DES observables provide cosmological information. We analyze the same multiprobe DES data as [Phys. Rev. Lett. 122, 171301 (2019)PRLTAO0031-900710.1103/PhysRevLett.122.171301]: DES Year 1 (Y1) galaxy clustering and weak lensing, which are sensitive to both growth and geometry, as well as Y1 BAO and Y3 supernovae, which probe geometry. We additionally include external geometric information from BOSS DR12 BAO and a compressed Planck 2015 likelihood, and external growth information from BOSS DR12 RSD. We find no significant disagreement with ωmgrow=ωmgeo. When DES and external data are analyzed separately, degeneracies with neutrino mass and intrinsic alignments limit our ability to measure ωmgrow, but combining DES with external data allows us to constrain both growth and geometric quantities. We also consider a parametrization where we split both ωm and w, but find that even our most constraining data combination is unable to separately constrain ωmgrow and wgrow. Relative to ΛCDM, splitting growth and geometry weakens bounds on σ8 but does not alter constraints on h.",
author = "{(DES Collaboration)} and J. Muir and E. Baxter and V. Miranda and C. Doux and A. Fert{\'e} and Leonard, {C. D.} and D. Huterer and B. Jain and P. Lemos and M. Raveri and S. Nadathur and A. Campos and A. Chen and S. Dodelson and J. Elvin-Poole and S. Lee and Secco, {L. F.} and Troxel, {M. A.} and N. Weaverdyck and J. Zuntz and D. Brout and A. Choi and M. Crocce and Davis, {T. M.} and D. Gruen and E. Krause and C. Lidman and N. Maccrann and A. M{\"o}ller and J. Prat and Ross, {A. J.} and M. Sako and S. Samuroff and C. S{\'a}nchez and D. Scolnic and B. Zhang and Abbott, {T. M.C.} and M. Aguena and S. Allam and J. Annis and S. Avila and D. Bacon and E. Bertin and S. Bhargava and Bridle, {S. L.} and D. Brooks and Burke, {D. L.} and {Carnero Rosell}, A. and {Carrasco Kind}, M. and J. Carretero",
note = "Funding Information: This paper has gone through internal review by the DES Collaboration. J. M. has been supported by the Porat Fellowship at Stanford University, and by the Rackham Graduate School through a Predoctoral Fellowship. The analysis made use of the software tools s ci p y , n um p y , matplotlib , camb , g et d ist , m ulti n est , p olychord , anesthetic , c osmo sis , and c osmo l ike . It was supported through computational resources and services provided by the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DE-AC02-05CH11231, and by the Sherlock cluster, supported by Stanford University and the Stanford Research Computing Center. 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, Funda{\c c}{\~a}o Carlos Chagas Filho de Amparo {\`a} Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cient{\'i}fico e Tecnol{\'o}gico and the Minist{\'e}rio da Ci{\^e}ncia, Tecnologia e Inova{\c c}{\~a}o, 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 Energ{\'e}ticas, Medioambientales y Tecnol{\'o}gicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgen{\"o}ssische Technische Hochschule (ETH) Z{\"u}rich, Fermi National Accelerator Laboratory, the University of Illinois at Urbana-Champaign, the Institut de Ci{\`e}ncies de l{\textquoteright}Espai (IEEC/CSIC), the Institut de F{\'i}sica d{\textquoteright}Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit{\"a}t M{\"u}nchen and the associated Excellence Cluster Universe, the University of Michigan, NFS{\textquoteright}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{\textquoteright}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{\textquoteright}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 Ci{\^e}ncia e Tecnologia (INCT) do e-Universo (CNPq Grant No. 465376/2014-2). This manuscript has been authored by the 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. Publisher Copyright: {\textcopyright} 2021 American Physical Society.",
year = "2021",
month = jan,
day = "21",
doi = "10.1103/PhysRevD.103.023528",
language = "English (US)",
volume = "103",
journal = "Physical Review D",
issn = "2470-0010",
publisher = "American Physical Society",
number = "2",
}