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• W2960759715 abstract "Abstract We report the constraints of H 0 obtained from Wilkinson Microwave Anisotropy Probe (WMAP) 9-year data combined with the latest baryonic acoustic oscillations (BAO) measurements. We use the BAO measurements from 6dF Galaxy Survey (6dFGS), the SDSS DR7 main galaxies sample (MGS), the BOSS DR12 galaxies, and the eBOSS DR14 quasars. Adding the recent BAO measurements to the cosmic microwave background (CMB) data from WMAP, we constrain cosmological parameters Ω m = 0.298 ± 0.005, <?CDATA ${H}_{0}={68.36}_{-0.52}^{+0.53}{rm{km}}cdot {{rm{s}}}^{-1}cdot {{rm{Mpc}}}^{-1}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML overflow=scroll> <mml:mrow> <mml:msub> <mml:mi>H</mml:mi> <mml:mn>0</mml:mn> </mml:msub> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>68.36</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.52</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.53</mml:mn> </mml:mrow> </mml:msubsup> <mml:mi mathvariant=normal>km</mml:mi> <mml:mo>⋅</mml:mo> <mml:msup> <mml:mi mathvariant=normal>s</mml:mi> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> <mml:mo>⋅</mml:mo> <mml:msup> <mml:mrow> <mml:mi mathvariant=normal>Mpc</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> </mml:mrow> </mml:math> , <?CDATA ${sigma }_{8}={0.8170}_{-0.0175}^{+0.0159}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML overflow=scroll> <mml:mrow> <mml:msub> <mml:mi>σ</mml:mi> <mml:mn>8</mml:mn> </mml:msub> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>0.8170</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.0175</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.0159</mml:mn> </mml:mrow> </mml:msubsup> </mml:mrow> </mml:math> in a spatially flat Λ cold dark matter (Λ CDM ) model, and Ω m = 0.302 ± 0.008, H 0 = 67.63 ± 1.30 km ⋅ s −1 ⋅ Mpc −1 , <?CDATA ${sigma }_{8}={0.7988}_{-0.0338}^{+0.0345}$?> <mml:math xmlns:mml=http://www.w3.org/1998/Math/MathML overflow=scroll> <mml:mrow> <mml:msub> <mml:mi>σ</mml:mi> <mml:mn>8</mml:mn> </mml:msub> <mml:mo>=</mml:mo> <mml:msubsup> <mml:mrow> <mml:mn>0.7988</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>0.0338</mml:mn> </mml:mrow> <mml:mrow> <mml:mo>+</mml:mo> <mml:mn>0.0345</mml:mn> </mml:mrow> </mml:msubsup> </mml:mrow> </mml:math> in a spatially flat wCDM model, respectively. Our measured H 0 results prefer a value lower than 70 km ⋅ s −1 ⋅ Mpc −1 , consistent with the recent data on CMB constraints from Planck (2018), but in 3.1 and 3.5 σ tension with local measurements of SH0ES (2018) in Λ CDM and wCDM framework, respectively. Our results indicate that there is a systematic tension on the Hubble constant between SH0ES and the combination of CMB and BAO datasets ." @default.
• W2960759715 created "2019-07-23" @default.
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• W2960759715 date "2019-07-01" @default.
• W2960759715 modified "2023-10-03" @default.
• W2960759715 title "Constraints on H₀ from WMAP and BAO Measurements*" @default.
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• W2960759715 doi "https://doi.org/10.1088/0253-6102/71/7/826" @default.
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