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    Galaxy clustering, CMB and supernova data constraints on ϕ\phiCDM model with massive neutrinos

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    We investigate a scalar field dark energy model (i.e., ϕ\phiCDM model) with massive neutrinos, where the scalar field possesses an inverse power-law potential, i.e., V(ϕ)ϕαV(\phi)\propto {\phi}^{-\alpha} (α>0\alpha>0). We find that the sum of neutrino masses Σmν\Sigma m_{\nu} has significant impacts on the CMB temperature power spectrum and on the matter power spectrum. In addition, the parameter α\alpha also has slight impacts on the spectra. A joint sample, including CMB data from Planck 2013 and WMAP9, galaxy clustering data from WiggleZ and BOSS DR11, and JLA compilation of Type Ia supernova observations, is adopted to confine the parameters. Within the context of the ϕ\phiCDM model under consideration, the joint sample determines the cosmological parameters to high precision. It turns out that α<4.995\alpha <4.995 at 95% CL for the ϕ\phiCDM model. And yet, the Λ\LambdaCDM scenario corresponding to α=0\alpha = 0 is not ruled out at 95% CL. Moreover, we get Σmν<0.262\Sigma m_{\nu}< 0.262 eV at 95% CL for the ϕ\phiCDM model, while the corresponding one for the Λ\LambdaCDM model is Σmν<0.293\Sigma m_{\nu} < 0.293 eV. The allowed scale of Σmν\Sigma m_\nu in the ϕ\phiCDM model is a bit smaller than that in the Λ\LambdaCDM model. It is consistent with the qualitative analysis, which reveals that the increases of α\alpha and Σmν\Sigma m_\nu both can result in the suppression of the matter power spectrum. As a consequence, when α\alpha is larger, in order to avoid suppressing the matter power spectrum too much, the value of Σmν\Sigma m_\nu should be smaller.Comment: 15 pages, 4 figures, 1 tabl
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