Cosmology with high-redshift galaxy survey: Neutrino mass and inflation
Cosmology with high-redshift galaxy survey: Neutrino mass and inflation
复制标题
DOI：
10.1103/physrevd.73.083520
复制
发表时间：
2005-12
影响因子：
5
通讯作者：
M. Takada;E. Komatsu;Toshifumi Futamase Tohoku Univ.;Japan.;U. T. A. Austin
中科院分区：
文献类型：
--
作者：
M. Takada;E. Komatsu;Toshifumi Futamase Tohoku Univ.;Japan.;U. T. A. Austin
高$z$星系红移巡天为精确测定中微子质量和暴胀模型开辟了令人兴奋的可能性。高$z$巡天比低$z$巡天对宇宙学更有用，因为在物质聚集、红移空间畸变和星系偏差方面的非线性要弱得多，这使我们能够使用星系功率谱到更小的空间尺度，这是低$z$巡天无法达到的。然后，我们可以利用线性功率谱在角和红移空间中的二维信息来测量中微子自由流对物质聚类的尺度依赖性抑制以及原始功率谱的形状。为了说明高$z$巡天在限制中微子质量和原始功率谱方面的能力，我们比较了未来在$0.5lzl2$、$2lzl4$和$3.5lzl6.5$覆盖300平方度的三个红移巡天。我们发现，结合普朗克卫星预期的宇宙微波背景数据，这些调查可以精确地确定中微子的总质量，预测误差分别为$\ensuremath{\sigma}({m}_{\ensuremath{\nu},\mathrm{tot}})=0.059$、0.043和0.025 eV，因此得出了中微子质量的正检测而不是上限，因为$\ensuremath{\sigma}({m}_{\ensuremath{\nu},\mathrm{tot}})$小于中微子振荡实验所隐含的中微子质量的下限。在最高的红移调查中，这一比例可达4倍。约束原始功率谱的倾斜和运行指数（$\ensuremath{\sigma}({n}_{s})=(3.8,3.7,3.0)\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}3}$和$\ensuremath{\sigma}({\ensuremath{\alpha}}_{s})=(5.9,5.7,2.4)\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}3}$，分别位于${k}_{0}=0.05\text{ }\text{ }{\mathrm{Mpc}}^{\ensuremath{-}1}$）的精度比当前的不确定性要小一个数量级以上，这将使我们能够区分候选的暴胀模型。特别是，未来最高红移巡天在${\ensuremath{\alpha}}_{s}$上的误差与一类简单暴胀模型的预测相差不远，这些模型是由具有自耦合的巨大标量场驱动的，${\ensuremath{\alpha}}_{s}=\ensuremath{-}(0.8\char21{}1.2)\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}3}$。
High-$z$ galaxy redshift surveys open up exciting possibilities for precision determinations of neutrino masses and inflationary models. The high-$z$ surveys are more useful for cosmology than low-$z$ ones owing to much weaker nonlinearities in matter clustering, redshift-space distortion, and galaxy bias, which allows us to use the galaxy power spectrum down to the smaller spatial scales that are inaccessible by low-$z$ surveys. We can then utilize the two-dimensional information of the linear power spectrum in angular and redshift space to measure the scale-dependent suppression of matter clustering due to neutrino free-streaming as well as the shape of the primordial power spectrum. To illustrate capabilities of high-$z$ surveys for constraining neutrino masses and the primordial power spectrum, we compare three future redshift surveys covering 300 square degrees at $0.5lzl2$, $2lzl4$, and $3.5lzl6.5$. We find that, combined with the cosmic microwave background data expected from the Planck satellite, these surveys allow precision determination of the total neutrino mass with the projected errors of $\ensuremath{\sigma}({m}_{\ensuremath{\nu},\mathrm{tot}})=0.059$, 0.043, and 0.025 eV, respectively, thus yielding a positive detection of the neutrino mass rather than an upper limit, as $\ensuremath{\sigma}({m}_{\ensuremath{\nu},\mathrm{tot}})$ is smaller than the lower limits to the neutrino masses implied from the neutrino oscillation experiments, by up to a factor of 4 for the highest redshift survey. The accuracies of constraining the tilt and running index of the primordial power spectrum, $\ensuremath{\sigma}({n}_{s})=(3.8,3.7,3.0)\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}3}$ and $\ensuremath{\sigma}({\ensuremath{\alpha}}_{s})=(5.9,5.7,2.4)\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}3}$ at ${k}_{0}=0.05\text{ }\text{ }{\mathrm{Mpc}}^{\ensuremath{-}1}$, respectively, are smaller than the current uncertainties by more than an order of magnitude, which will allow us to discriminate between candidate inflationary models. In particular, the error on ${\ensuremath{\alpha}}_{s}$ from the future highest redshift survey is not very far away from the prediction of a class of simple inflationary models driven by a massive scalar field with self-coupling, ${\ensuremath{\alpha}}_{s}=\ensuremath{-}(0.8\char21{}1.2)\ifmmode\times\else\texttimes\fi{}{10}^{\ensuremath{-}3}$.