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arXiv 1507.02008astro-ph.CO
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星系成团、CMB和超新星数据对含大质量中微子的$ϕ$ CDM模型的约束

Galaxy clustering, CMB and supernova data constraints on $ϕ$CDM model with massive neutrinos

Yun Chen, Lixin Xu

备注：
15 pages, 4 figures, 1 table
发表信息：
Phys. Lett. B 752 (2016) 66-75
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摘要：

我们研究了标量场暗能量模型（即，$ϕ$ CDM模型），其中标量场具有逆幂律势，即，$V(ϕ)\propto ϕ^{-α}$（$α>0$）。我们发现中微子质量之和$Σm_ν$对CMB温度功率谱和物质功率谱有显著的影响。此外，参数$α$对光谱也有轻微的影响。采用Planck 2013和WMAP 9的CMB数据、WiggleZ和BOSS DR 11的星系团数据以及JLA汇编的Ia型超新星观测数据等联合样本来限制参数。在考虑中的$ϕ$ CDM模型的背景下，联合样本确定宇宙学参数的高精度。结果表明，$ϕ$ CDM模型的$α<4.995$为95% CL。然而，在95% CL下，不排除与$α= 0$对应的$Λ$ CDM情况。此外，我们得到$ϕ$ CDM模型在95%CL下的$Σm_ν< 0.262$ eV，而$Λ$ CDM模型的相应的一个是$Σm_ν < 0.293$ eV。$ϕ$ CDM模型中的$Σm_ν$的允许规模比$Λ$ CDM模型中的小一些。这与定性分析结果一致，即$α$和$Σm_ν$的增加都会导致物质功率谱的抑制。因此，当$α$较大时，为了避免过多地抑制物质功率谱，$Σm_ν$的值应该较小。

英文摘要：

We investigate a scalar field dark energy model (i.e., $ϕ$CDM model) with massive neutrinos, where the scalar field possesses an inverse power-law potential, i.e., $V(ϕ)\propto ϕ^{-α}$ ($α>0$). We find that the sum of neutrino masses $Σm_ν$ has significant impacts on the CMB temperature power spectrum and on the matter power spectrum. In addition, the parameter $α$ 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 $ϕ$CDM model under consideration, the joint sample determines the cosmological parameters to high precision. It turns out that $α<4.995$ at 95% CL for the $ϕ$CDM model. And yet, the $Λ$CDM scenario corresponding to $α= 0$ is not ruled out at 95% CL. Moreover, we get $Σm_ν< 0.262$ eV at 95% CL for the $ϕ$CDM model, while the corresponding one for the $Λ$CDM model is $Σm_ν < 0.293$ eV. The allowed scale of $Σm_ν$ in the $ϕ$CDM model is a bit smaller than that in the $Λ$CDM model. It is consistent with the qualitative analysis, which reveals that the increases of $α$ and $Σm_ν$ both can result in the suppression of the matter power spectrum. As a consequence, when $α$ is larger, in order to avoid suppressing the matter power spectrum too much, the value of $Σm_ν$ should be smaller.

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