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M.W. M.Wood-VaseyYèche, ChristopheChristopheYècheZehavi, IditIditZehaviZhao, Gong-BoGong-BoZhaoBOSS Collaboration2020-03-252020-03-2520151550-7998http://hdl.handle.net/20.500.12386/23538We derive constraints on cosmological parameters and tests of dark energy models from the combination of baryon acoustic oscillation (BAO) measurements with cosmic microwave background (CMB) data and a recent reanalysis of Type Ia supernova (SN) data. In particular, we take advantage of high-precision BAO measurements from galaxy clustering and the Lyman-α forest (LyaF) in the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS). Treating the BAO scale as an uncalibrated standard ruler, BAO data alone yield a high confidence detection of dark energy; in combination with the CMB angular acoustic scale they further imply a nearly flat universe. Adding the CMB-calibrated physical scale of the sound horizon, the combination of BAO and SN data into an "inverse distance ladder" yields a measurement of H<SUB>0</SUB>=67.3 ±1.1 km s<SUP>-1</SUP> Mpc<SUP>-1</SUP> , with 1.7% precision. This measurement assumes standard prerecombination physics but is insensitive to assumptions about dark energy or space curvature, so agreement with CMB-based estimates that assume a flat Λ CDM cosmology is an important corroboration of this minimal cosmological model. For constant dark energy (Λ ), our BAO +SN +CMB combination yields matter density Ω<SUB>m</SUB>=0.301 ±0.008 and curvature Ω<SUB>k</SUB>=-0.003 ±0.003 . When we allow more general forms of evolving dark energy, the BAO +SN +CMB parameter constraints are always consistent with flat Λ CDM values at ≈1 σ . While the overall χ<SUP>2</SUP> of model fits is satisfactory, the LyaF BAO measurements are in moderate (2 - 2.5 σ ) tension with model predictions. Models with early dark energy that tracks the dominant energy component at high redshift remain consistent with our expansion history constraints, and they yield a higher H<SUB>0</SUB> and lower matter clustering amplitude, improving agreement with some low redshift observations. Expansion history alone yields an upper limit on the summed mass of neutrino species, ∑m<SUB>ν</SUB><0.56 eV (95% confidence), improving to ∑m<SUB>ν</SUB><0.25 eV if we include the lensing signal in the Planck CMB power spectrum. In a flat Λ CDM model that allows extra relativistic species, our data combination yields N<SUB>eff</SUB>=3.43 ±0.26 ; while the LyaF BAO data prefer higher N<SUB>eff</SUB> when excluding galaxy BAO, the galaxy BAO alone favor N<SUB>eff</SUB>≈3 . When structure growth is extrapolated forward from the CMB to low redshift, standard dark energy models constrained by our data predict a level of matter clustering that is high compared to most, but not all, observational estimates. <P />STAMPAenArticle10.1103/PhysRevD.92.1235162-s2.0-84952333924000366502800004http://arxiv.org/abs/1411.1074v3https://journals.aps.org/prd/abstract/10.1103/PhysRevD.92.1235162015PhRvD..92l3516AFIS/05 - ASTRONOMIA E ASTROFISICA