斯巴鲁FMOS星系红移巡天（FastSound）。IV。$z\sim 1.4$红移空间畸变对引力理论的新约束
The Subaru FMOS galaxy redshift survey (FastSound). IV. New constraint on gravity theory from redshift space distortions at $z\sim 1.4$
摘要：
我们测量的红移空间相关函数的光谱样本的2783发射线星系的FastSound调查。这次调查使用了斯巴鲁望远镜，覆盖了$1.19<z<1.55$的红移范围，是第一次在如此高的红移范围内进行宇宙学研究。我们检测到明确的各向异性，由于红移空间失真（RSD）的相关函数作为分离平行和垂直的视线和四极矩的函数。在$z<1$，RSD已被广泛用于在宇宙学尺度上检验广义相对论。采用具有固定膨胀历史和无速度色散的LCDM宇宙学$σ_{\rm v}=0$，并使用8 Mpc/h以上尺度的RSD测量，我们在边缘化星系偏差参数$b(z)σ_8(z)$后，在$z\sim 1.4$上获得了红移处生长率的第一个约束$f(z)σ_8(z)=0.482\pm 0.116$。这对应于RSD的$4.2σ$检测。我们的约束是一致的广义相对论$fσ_8\sim 0.392$的$1-σ$置信水平内的预测。当我们允许$σ_{\rm v}$变化并将其边缘化时，增长率约束变为$fσ_8=0.494^{+0.126}_{-0.120}$。我们还证明，通过结合$fσ_8$上的低z约束，像FastSound这样的高z星系调查可以用于区分修改后的重力模型，而不依赖于CMB各向异性实验。
英文摘要：
We measure the redshift-space correlation function from a spectroscopic sample of 2783 emission line galaxies from the FastSound survey. The survey, which uses the Subaru Telescope and covers the redshift ranges of $1.19<z<1.55$, is the first cosmological study at such high redshifts. We detect clear anisotropy due to redshift-space distortions (RSD) both in the correlation function as a function of separations parallel and perpendicular to the line of sight and its quadrupole moment. RSD has been extensively used to test general relativity on cosmological scales at $z<1$. Adopting a LCDM cosmology with the fixed expansion history and no velocity dispersion $σ_{\rm v}=0$, and using the RSD measurements on scales above 8Mpc/h, we obtain the first constraint on the growth rate at the redshift, $f(z)σ_8(z)=0.482\pm 0.116$ at $z\sim 1.4$ after marginalizing over the galaxy bias parameter $b(z)σ_8(z)$. This corresponds to $4.2σ$ detection of RSD. Our constraint is consistent with the prediction of general relativity $fσ_8\sim 0.392$ within the $1-σ$ confidence level. When we allow $σ_{\rm v}$ to vary and marginalize it over, the growth rate constraint becomes $fσ_8=0.494^{+0.126}_{-0.120}$. We also demonstrate that by combining with the low-z constraints on $fσ_8$, high-z galaxy surveys like the FastSound can be useful to distinguish modified gravity models without relying on CMB anisotropy experiments.
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