一个典型的星系巡天几何学会导致不同间距和视线角度的星系对具有不同的红移分布，从而产生不同的有效红移。然而，聚类测量分析假设的聚类是在一个单一的有效红移的代表。我们调查的影响，在星系对有效红移的大规模集群测量星系巡天的变化。我们发现，星系调查跨越一个大的红移范围有不同的有效红移作为一个函数的对分离和角度。此外，当考虑示踪剂的聚类幅度随红移强烈演变时，这种组合可以导致额外的尺度依赖的聚类各向异性。我们证明了这种影响的大小的eBOSS DR 16类星体样本，并表明，虽然对磁的影响是可以忽略不计的，忽略这种影响可能会导致大规模的倾斜$\sim 4\%$和$\sim40\%$在四极和十六极，分别。我们讨论的策略，以减轻这种影响时，进行测量。
英文摘要：
A typical galaxy survey geometry results in galaxy pairs of different separation and angle to the line-of-sight having different distributions in redshift and consequently a different effective redshift. However, clustering measurements are analysed assuming that the clustering is representative of that at a single effective redshift. We investigate the impact of variations in the galaxy-pair effective redshift on the large-scale clustering measured in galaxy surveys. We find that galaxy surveys spanning a large redshift range have different effective redshifts as a function of both pair separation and angle. Furthermore, when considering tracers whose clustering amplitude evolves strongly with redshift, this combination can result in an additional scale-dependent clustering anisotropy. We demonstrate the size of this effect on the eBOSS DR16 Quasar sample and show that, while the impact on monopole is negligible, neglecting this effect can result in a large-scale tilt of $\sim 4\%$ and $\sim40\%$ in quadrupole and hexadecapole, respectively. We discuss strategies to mitigate this effect when making measurements.
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: a tomographic analysis of structure growth and expansion rate from anisotropic galaxy clustering
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: anisotropic clustering analysis in configuration-space
The clustering of galaxies in the completed SDSS-III Baryon Oscillation Spectroscopic Survey: a tomographic measurement of structure growth and expansion rate from anisotropic galaxy clustering in Fourier space
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: Anisotropic Baryon Acoustic Oscillations measurements in Fourier-space with optimal redshift weights
利用扩展的重子振荡光谱巡天数据Release 14类星体样品，测量了具有最佳红移权的各向异性和各向同性的重子声学振荡（BAO）。应用红移权重将对BAO膨胀参数$α(z_{\rm eff})$的约束提高了17\ %。我们重建了$0.8<z<2.2$红移范围内BAO距离指标的演化历史。本文是分析eBOSS DR 14类星体样本的一组中的一部分。
The Clustering of Galaxies in the SDSS-III DR9 Baryon Oscillation Spectroscopic Survey: Testing Deviations from $Λ$ and General Relativity using anisotropic clustering of galaxies
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: Effect of smoothing of density field on reconstruction and anisotropic BAO analysis
The clustering of galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey: measurements of the growth of structure and expansion rate at z=0.57 from anisotropic clustering
我们分析了斯隆数字巡天III重子振荡光谱巡天（BOSS）数据发布9（DR 9）样本中大质量星系的各向异性聚类，该样本由264，283个星系组成，红移范围为0.43 < z < 0.7，跨度为3，275平方度。这两个奇特的速度和错误的假设红移距离关系（“Alcock-Paczynski效应”）产生的聚类幅度和方向之间的相关性，相对于视线。我们对四极和四极关联函数的宽带形状的测量与尖锐的重子声学振荡（BAO）标准尺一起，同时约束了共动角直径距离（2190 +/- 61 Mpc）到z=0.57，哈勃膨胀率在z=0.57（92.4 +/- 4.5 km/s/Mpc），以及在相同红移下的结构增长率（d σ 8/d ln a = 0.43 +/- 0.069）。我们的分析提供了目前最好的直接测定DA和H的星系聚类数据使用这种技术。如果我们进一步假设LCDM扩展历史，我们的增长约束收紧到d σ 8/d ln a = 0.415 +/- 0.034。结合宇宙微波背景，我们对DA、H和生长的测量都分别需要z > 0.57的暗能量，当结合起来时意味着Ω_Λ = 0.74 +/- 0.016，与z<0.57的宇宙演化无关。在我们的配套论文（Samushia et al. prep）中，我们进一步探讨了这些观测的宇宙学意义。
The Clustering of Galaxies in the SDSS-III Baryon Oscillation Spectroscopic Survey (BOSS): measuring growth rate and geometry with anisotropic clustering
Model-Independent Measurements of Cosmic Expansion and Growth at z=0.57 Using the Anisotropic Clustering of CMASS Galaxies From the Sloan Digital Sky Survey Data Release 9
The Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: Growth rate of structure measurement from anisotropic clustering analysis in configuration space between redshift 0.6 and 1.1 for the Emission Line Galaxy sample
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: Measuring the anisotropic Baryon Acoustic Oscillations with redshift weights
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 LRG sample: structure growth rate measurement from the anisotropic LRG correlation function in the redshift range 0.6 < z < 1.0
Reconstruction of halo power spectrum from redshift-space galaxy distribution: cylinder-grouping method and halo exclusion effect
星系巡天观测中红移空间畸变（RSD）测量到的奇特速度场为研究大尺度结构的生长提供了独特的途径。然而，系统的影响时，包括卫星星系的聚类分析。由于卫星星系倾向于居住在具有更大晕偏差的大质量晕中，因此包含物增强了集群能力。此外，维里运动的卫星星系的非线性RSD效应导致了显着的抑制集群的权力。我们发展了一种新的方法来恢复红移空间功率谱的晕从观测到的星系分布，通过最大限度地减少污染的卫星星系。我们研究的圆柱分组方法（CGM）有效地将卫星星系从星系样本中排除。然而，我们发现，这种技术产生明显的各向异性在重建的晕分布在所有规模模仿RSD。在小尺度上，明显的各向异性聚类是由CGM使用的各向异性圆柱体内的晕排除引起的。在大尺度上，将沿视线排列的大尺度结构中的不同晕错误识别为同一CGM组，通过它们与CGM晕的互相关引起明显的各向异性聚类。我们构建了一个经验模型的CGM晕功率谱，其中包括使用CGM窗口函数在小尺度以及线性物质功率谱乘以一个简单的各向异性函数在大尺度上导出的校正项。我们将这个模型应用到z=0.5的模拟星系表中，设计成类似于SDSS-III BOSS CMASS星系，发现我们的模型可以预测宿主晕的四极和四极功率谱，直到k<0.5 h/Mpc，误差在5%以内。
Constraining Primordial Power Asymmetry from Galaxy Clustering and Peculiar Velocity Information
Kyoto University（京都大学）；Yukawa Institute for Theoretical Physics, Kyoto University（京都大学汤川理论物理研究所）；Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo（东京大学前沿科学高等研究院宇宙物理数学卡弗里研究所（WPI））；Korea Institute for Advanced Study（韩国高等科学研究院）；Academia Sinica Institute of Astronomy and Astrophysics (ASIAA)（中央研究院天文及天文物理学研究所）；Onomichi City University（尾道市立大学）
Anisotropic redshift distributions in photometric galaxy clustering and their cosmological impact
Ludwig-Maximilians Universität München（慕尼黑大学）；Excellence Cluster ORIGINS（ORIGINS卓越集群）；Institut de Física d’Altes Energies (IFAE), The Barcelona Institute of Science and Technology（巴塞罗那科技高等物理研究所）；ETH Zurich（苏黎世联邦理工学院）；Nagoya University（名古屋大学）；Kobayashi-Maskawa Institute for the Origin of Particles and the Universe (KMI)（小林-益川粒子宇宙起源研究所）
The Completed SDSS-IV extended Baryon Oscillation Spectroscopic Survey: BAO and RSD measurements from anisotropic clustering analysis of the Quasar Sample in configuration space between redshift 0.8 and 2.2
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: structure growth rate measurement from the anisotropic quasar power spectrum in the redshift range $0.8<z<2.2$
Clustering of emission line galaxies with IllustrisTNG -- II. cosmology challenge with anisotropic correlation functions and ELG-halo connections
Center for Frontier Science, Chiba University（千叶大学前沿科学中心）；Department of Physics, Graduate School of Science, Chiba University（千叶大学理学研究科物理系）；RIKEN Center for Advanced Intelligence Project（理化学研究所先进智能项目中心）；Kavli Institute for the Physics and Mathematics of the Universe, The University of Tokyo Institutes for Advanced Study（东京大学高等研究院宇宙物理数学研究所卡弗里）；Academia Sinica Institute of Astronomy and Astrophysics（中央研究院天文及天文物理研究所）
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: measuring the evolution of the growth rate using redshift space distortions between redshift 0.8 and 2.2
A new look at lines of sight: using Fourier methods for the wide-angle anisotropic 2-point correlation function
星系的各向异性两点关联函数（2PCF）测量成对聚集作为对分离的角度的函数的视线。后者通常被定义为双星系对三角形的角平分线或从观测者到分离中点的矢量。在这里，我们展示了如何使用傅立叶变换来加速这些测量中的任何一个，使用Yamamoto et al.（2006）估计器的轻微推广，其中对中的每个成员连续用作视线。我们还提出了扰动理论预测我们的广义估计，包括广角校正。
The clustering of the SDSS-IV extended Baryon Oscillation Spectroscopic Survey DR14 quasar sample: measurement of the growth rate of structure from the anisotropic correlation function between redshift 0.8 and 2.2
