Dark Energy Survey Year 3 Results: Constraints on extensions to $Λ$CDM with weak lensing and galaxy clustering
Creators: name: DES Collaboration
name: Abbott, T. M. C.
name: Aguena, M.
name: Alarcon, A.
name: Alves, O.
name: Amon, A.
name: Annis, J.
name: Avila, S.
name: Bacon, D.
name: Baxter, E.
name: Bechtol, K.
name: Becker, M. R.
name: Bernstein, G. M.
name: Birrer, S.
name: Blazek, J.
name: Bocquet, S.
name: Brandao-Souza, A.
name: Bridle, S. L.
name: Brooks, D.
name: Burke, D. L.
name: Camacho, H.
name: Campos, A.
name: Rosell, A. Carnero
name: Kind, M. Carrasco
name: Carretero, J.
name: Castander, F. J.
name: Cawthon, R.
name: Chang, C.
name: Chen, A.
name: Chen, R.
name: Choi, A.
name: Conselice, C.
name: Cordero, J.
name: Costanzi, M.
name: Crocce, M.
name: da Costa, L. N.
name: Pereira, M. E. S.
name: Davis, C.
name: Davis, T. M.
name: DeRose, J.
name: Desai, S.
name: Di Valentino, E.
name: Diehl, H. T.
name: Dodelson, S.
name: Doel, P.
name: Doux, C.
name: Drlica-Wagner, A.
name: Eckert, K.
name: Eifler, T. F.
name: Elsner, F.
name: Elvin-Poole, J.
name: Everett, S.
name: Fang, X.
name: Farahi, A.
name: Ferrero, I.
name: Ferté, A.
name: Flaugher, B.
name: Fosalba, P.
name: Friedel, D.
name: Friedrich, O.
name: Frieman, J.
name: García-Bellido, J.
name: Gatti, M.
name: Giani, L.
name: Giannantonio, T.
name: Giannini, G.
name: Gruen, D.
name: Gruendl, R. A.
name: Gschwend, J.
name: Gutierrez, G.
name: Hamaus, N.
name: Harrison, I.
name: Hartley, W. G.
name: Herner, K.
name: Hinton, S. R.
name: Hollowood, D. L.
name: Honscheid, K.
name: Huang, H.
name: Huff, E. M.
name: Huterer, D.
name: Jain, B.
name: James, D. J.
name: Jarvis, M.
name: Jeffrey, N.
name: Jeltema, T.
name: Kovacs, A.
name: Krause, E.
name: Kuehn, K.
name: Kuropatkin, N.
name: Lahav, O.
name: Lee, S.
name: Leget, P. -F.
name: Lemos, P.
name: Leonard, C. D.
name: Liddle, A. R.
name: Lima, M.
name: Lin, H.
name: MacCrann, N.
name: Marshall, J. L.
name: McCullough, J.
name: Mena-Fernández, J.
name: Menanteau, F.
name: Miquel, R.
name: Miranda, V.
name: Mohr, J. J.
name: Muir, J.
name: Myles, J.
name: Nadathur, S.
name: Navarro-Alsina, A.
name: Nichol, R. C.
name: Ogando, R. L. C.
name: Omori, Y.
name: Palmese, A.
name: Pandey, S.
name: Park, Y.
name: Paterno, M.
name: Paz-Chinchón, F.
name: Percival, W. J.
name: Pieres, A.
name: Malagón, A. A. Plazas
name: Porredon, A.
name: Prat, J.
name: Raveri, M.
name: Rodriguez-Monroy, M.
name: Rogozenski, P.
name: Rollins, R. P.
name: Romer, A. K.
name: Roodman, A.
name: Rosenfeld, R.
name: Ross, A. J.
name: Rykoff, E. S.
name: Samuroff, S.
name: Sánchez, C.
name: Sanchez, E.
name: Sanchez, J.
name: Cid, D. Sanchez
name: Scarpine, V.
name: Scolnic, D.
name: Secco, L. F.
name: Sevilla-Noarbe, I.
name: Sheldon, E.
name: Shin, T.
name: Smith, M.
name: Soares-Santos, M.
name: Suchyta, E.
name: Tabbutt, M.
name: Tarle, G.
name: Thomas, D.
name: To, C.
name: Troja, A.
name: Troxel, M. A.
name: Tutusaus, I.
name: Varga, T. N.
name: Vincenzi, M.
name: Walker, A. R.
name: Weaverdyck, N.
name: Wechsler, R. H.
name: Weller, J.
name: Yanny, B.
name: Yin, B.
name: Zhang, Y.
name: Zuntz, J.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We constrain extensions to the $Λ$CDM model using measurements from the Dark Energy Survey's first three years of observations and external data. The DES data are the two-point correlation functions of weak gravitational lensing, galaxy clustering, and their cross-correlation. We use simulated data and blind analyses of real data to validate the robustness of our results. In many cases, constraining power is limited by the absence of nonlinear predictions that are reliable at our required precision. The models are: dark energy with a time-dependent equation of state, non-zero spatial curvature, sterile neutrinos, modifications of gravitational physics, and a binned $σ_8(z)$ model which serves as a probe of structure growth. For the time-varying dark energy equation of state evaluated at the pivot redshift we find $(w_{\rm p}, w_a)= (-0.99^{+0.28}_{-0.17},-0.9\pm 1.2)$ at 68% confidence with $z_{\rm p}=0.24$ from the DES measurements alone, and $(w_{\rm p}, w_a)= (-1.03^{+0.04}_{-0.03},-0.4^{+0.4}_{-0.3})$ with $z_{\rm p}=0.21$ for the combination of all data considered. Curvature constraints of $Ω_k=0.0009\pm 0.0017$ and effective relativistic species $N_{\rm eff}=3.10^{+0.15}_{-0.16}$ are dominated by external data. For massive sterile neutrinos, we improve the upper bound on the mass $m_{\rm eff}$ by a factor of three compared to previous analyses, giving 95% limits of $(ΔN_{\rm eff},m_{\rm eff})\leq (0.28, 0.20\, {\rm eV})$. We also constrain changes to the lensing and Poisson equations controlled by functions $Σ(k,z) = Σ_0 Ω_Λ(z)/Ω_{Λ,0}$ and $μ(k,z)=μ_0 Ω_Λ(z)/Ω_{Λ,0}$ respectively to $Σ_0=0.6^{+0.4}_{-0.5}$ from DES alone and $(Σ_0,μ_0)=(0.04\pm 0.05,0.08^{+0.21}_{-0.19})$ for the combination of all data. Overall, we find no significant evidence for physics beyond $Λ$CDM.
description: Updated to match published version and fix a citation reference. 46 pages, 25 figures, data available at https://dev.des.ncsa.illinois.edu/releases/y3a2/Y3key-extensions