http://arxiv.org/abs/1603.07115
We investigate two dark energy cosmological models (i.e., the $\Lambda$CDM and $\phi$CDM models) with massive neutrinos in both the spatially flat and non-flat scenarios, where in the $\phi$CDM model the scalar field possesses an inverse power-law potential, $V(\phi)\propto {\phi}^{-\alpha}$ ($\alpha>0$). Cosmic microwave background data from Planck 2015, baryon acoustic oscillations data from 6dFGS, SDSS-MGS, BOSS-LOWZ and BOSS CMASS-DR11, the JLA compilation of Type Ia supernova apparent magnitude observations, and the Hubble Space Telescope $H_0$ prior, are jointly employed to constrain the model parameters. In the spatially flat (non-flat) $\Lambda$CDM model, the sum of neutrino masses is bounded as $\Sigma m_{\nu} < 0.166 (0.354)$ eV at 95\% confidence level (CL). Correspondingly, in the flat (non-flat) $\phi$CDM model, we find $\Sigma m_{\nu} < 0.164 (0.364)$ eV at 95\% CL. The inclusion of spatial curvature as a free parameter results in a significant broadening of confidence regions for $\Sigma m_{\nu}$ and other parameters. However, the curvature density parameter is constrained to $-0.0017 < \Omega_k < 0.0092$ for the $\Lambda$CDM model and $-0.0019 < \Omega_k < 0.0096$ for the $\phi$CDM model at 95\% CL, which is very close to zero.
Y. Chen, B. Ratra, M. Biesiada, et. al.
Thu, 24 Mar 16
39/60
Comments: 6 pages, 3 figures, 1 table
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