Dark Energy Survey Year 1 Results: Constraints on Extended Cosmological Models from Galaxy Clustering and Weak Lensing
Creators: name: DES Collaboration
name: Abbott, T. M. C.
name: Abdalla, F. B.
name: Avila, S.
name: Banerji, M.
name: Baxter, E.
name: Bechtol, K.
name: Becker, M. R.
name: Bertin, E.
name: Blazek, J.
name: Bridle, S. L.
name: Brooks, D.
name: Brout, D.
name: Burke, D. L.
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: Crocce, M.
name: Cunha, C. E.
name: da Costa, L. N.
name: Davis, C.
name: De Vicente, J.
name: DeRose, J.
name: Desai, S.
name: Di Valentino, E.
name: Diehl, H. T.
name: Dietrich, J. P.
name: Dodelson, S.
name: Doel, P.
name: Drlica-Wagner, A.
name: Eifler, T. F.
name: Elvin-Poole, J.
name: Evrard, A. E.
name: Fernandez, E.
name: Ferté, A.
name: Flaugher, B.
name: Fosalba, P.
name: Frieman, J.
name: García-Bellido, J.
name: Gaztanaga, E.
name: Gerdes, D. W.
name: Giannantonio, T.
name: Gruen, D.
name: Gruendl, R. A.
name: Gschwend, J.
name: Gutierrez, G.
name: Hartley, W. G.
name: Hollowood, D. L.
name: Honscheid, K.
name: Hoyle, B.
name: Huterer, D.
name: Jain, B.
name: Jeltema, T.
name: Johnson, M. W. G.
name: Johnson, M. D.
name: Kim, A. G.
name: Krause, E.
name: Kuehn, K.
name: Kuropatkin, N.
name: Lahav, O.
name: Lee, S.
name: Lemos, P.
name: Leonard, C. D.
name: Li, T. S.
name: Liddle, A. R.
name: Lima, M.
name: Lin, H.
name: Maia, M. A. G.
name: Marshall, J. L.
name: Martini, P.
name: Menanteau, F.
name: Miller, C. J.
name: Miquel, R.
name: Miranda, V.
name: Mohr, J. J.
name: Muir, J.
name: Nichol, R. C.
name: Nord, B.
name: Ogando, R. L. C.
name: Plazas, A. A.
name: Raveri, M.
name: Rollins, R. P.
name: Romer, A. K.
name: Roodman, A.
name: Rosenfeld, R.
name: Samuroff, S.
name: Sanchez, E.
name: Scarpine, V.
name: Schindler, R.
name: Schubnell, M.
name: Scolnic, D.
name: Secco, L. F.
name: Serrano, S.
name: Sevilla-Noarbe, I.
name: Smith, M.
name: Soares-Santos, M.
name: Sobreira, F.
name: Suchyta, E.
name: Swanson, M. E. C.
name: Tarle, G.
name: Thomas, D.
name: Troxel, M. A.
name: Vikram, V.
name: Walker, A. R.
name: Weaverdyck, N.
name: Wechsler, R. H.
name: Weller, J.
name: Yanny, B.
name: Zhang, Y.
name: Zuntz, J.
Publisher: name: arXiv
Year: 2018
Subjects: subject: Cosmology and Nongalactic Astrophysics (astro-ph.CO)
subject: General Relativity and Quantum Cosmology (gr-qc)
subject: High Energy Physics - Phenomenology (hep-ph)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We present constraints on extensions of the minimal cosmological models dominated by dark matter and dark energy, $Λ$CDM and $w$CDM, by using a combined analysis of galaxy clustering and weak gravitational lensing from the first-year data of the Dark Energy Survey (DES Y1) in combination with external data. We consider four extensions of the minimal dark energy-dominated scenarios: 1) nonzero curvature $Ω_k$, 2) number of relativistic species $N_{\rm eff}$ different from the standard value of 3.046, 3) time-varying equation-of-state of dark energy described by the parameters $w_0$ and $w_a$ (alternatively quoted by the values at the pivot redshift, $w_p$, and $w_a$), and 4) modified gravity described by the parameters $μ_0$ and $Σ_0$ that modify the metric potentials. We also consider external information from Planck CMB measurements; BAO measurements from SDSS, 6dF, and BOSS; RSD measurements from BOSS; and SNIa information from the Pantheon compilation. Constraints on curvature and the number of relativistic species are dominated by the external data; when these are combined with DES Y1, we find $Ω_k=0.0020^{+0.0037}_{-0.0032}$ at the 68% confidence level, and $N_{\rm eff}&lt;3.28\, (3.55)$ at 68% (95%) confidence. For the time-varying equation-of-state, we find the pivot value $(w_p, w_a)=(-0.91^{+0.19}_{-0.23}, -0.57^{+0.93}_{-1.11})$ at pivot redshift $z_p=0.27$ from DES alone, and $(w_p, w_a)=(-1.01^{+0.04}_{-0.04}, -0.28^{+0.37}_{-0.48})$ at $z_p=0.20$ from DES Y1 combined with external data; in either case we find no evidence for the temporal variation of the equation of state. For modified gravity, we find the present-day value of the relevant parameters to be $Σ_0= 0.43^{+0.28}_{-0.29}$ from DES Y1 alone, and $(Σ_0, μ_0)=(0.06^{+0.08}_{-0.07}, -0.11^{+0.42}_{-0.46})$ from DES Y1 combined with external data, consistent with predictions from GR.
description: 22 pages, 7 figures, matches the published version