论文标题
DESI传统调查中的星系聚类及其在CMB上的烙印
Galaxy clustering in the DESI Legacy Survey and its imprint on the CMB
论文作者
论文摘要
我们使用DESI传统调查成像中的数据来探测覆盖红移范围$ 0 <z <0.8 $的层析成像切片中的星系密度场。经过仔细考虑完整性校正和银河系切割后，我们获得了$ 4.9 \ times 10^7 $的样本，覆盖17 739°$^2 $的星系。我们以精度$σ_z/（1+z）= 0.012-0.015 $得出光度红移，并与其他估计值进行比较。层析成像图与CMB温度的普朗克图和透镜收敛的互相关探测结构的生长，因为$ z = 0.8 $。信号与基准Planck $λ$ CDM型号进行了比较，并且需要整体比例$a_κ= 0.901 \ pm 0.026 $，用于镜头互相关，$ a _ {\ rm isw} = 0.984 \ pm 0.349 $ 0.349 $ for温度交叉效果，以换句话说，以synected synelf synected sectected synelf。 ISW振幅与基准$λ$ CDM预测一致，但显着位于Rácz等人的Avera模型的预测。 （2017年），已被提议作为宇宙加速的替代解释。在$λ$ CDM之内，与Planck结果相比，镜头互相关的低振幅需要减少波动归一化或物质密度，因此$ω_m^{0.78}σ_8= 0.297 \ 0.297 \ pm 0.009 $。结合CMB镜头的总幅度，这主要有利于密度转移：$ω_m= 0.274 \ pm0.024 $。我们与替代证据讨论了该图的一致性。镜头和主要CMB约束之间的保守妥协将需要$ω_m= 0.296 \ pm0.006 $，其中两个探针的95％置信区都重叠。
We use data from the DESI Legacy Survey imaging to probe the galaxy density field in tomographic slices covering the redshift range $0<z<0.8$. After careful consideration of completeness corrections and galactic cuts, we obtain a sample of $4.9\times 10^7$ galaxies covering 17 739 deg$^2$. We derive photometric redshifts with precision $σ_z/(1+z)=0.012 - 0.015$, and compare with alternative estimates. Cross-correlation of the tomographic galaxy maps with Planck maps of CMB temperature and lensing convergence probe the growth of structure since $z=0.8$. The signals are compared with a fiducial Planck $Λ$CDM model, and require an overall scaling in amplitude of $A_κ=0.901\pm 0.026$ for the lensing cross-correlation and $A_{\rm ISW} = 0.984 \pm 0.349$ for the temperature cross-correlation, interpreted as the Integrated Sachs-Wolfe effect. The ISW amplitude is consistent with the fiducial $Λ$CDM prediction, but lies significantly below the prediction of the AvERA model of Rácz et al. (2017), which has been proposed as an alternative explanation for cosmic acceleration. Within $Λ$CDM, our low amplitude for the lensing cross-correlation requires a reduction either in fluctuation normalization or in matter density compared to the Planck results, so that $Ω_m^{0.78}σ_8=0.297\pm 0.009$. In combination with the total amplitude of CMB lensing, this favours a shift mainly in density: $Ω_m=0.274\pm0.024$. We discuss the consistency of this figure with alternative evidence. A conservative compromise between lensing and primary CMB constraints would require $Ω_m=0.296\pm0.006$, where the 95% confidence regions of both probes overlap.
