三维星系相关的各向异性放大畸变：I。真实空间
Anisotropic Magnification Distortion of the 3D Galaxy Correlation: I. Real Space
摘要：
众所周知，引力透镜，主要通过放大偏差，修改所观察到的星系/类星体集群。这种讨论主要集中在2D角度相关性上。在这里，在一个配套文件（纸II），我们探讨放大偏差如何扭曲的3D关联函数和功率谱，首先考虑松原。有趣的是：失真是各向异性的。放大偏差优先增强了观察到的相关性的视线（LOS）的方向，特别是在大尺度上。例如，在LOS分离为~100 Mpc/h时，星系与星系之间的内在相关性相当弱，即使在z ~ 0.35的适度红移下，观测到的相关性也可以通过透镜效应增强几倍。机会：这种透镜各向异性是独特的，使得有可能分别测量星系-星系、星系-放大率和放大率-放大率的相关性，而不测量星系的形状。各向异性是区别于众所周知的变形由于特殊的运动，将讨论在文件II。挑战：随着精度的提高，在解释数据时必须考虑星系相关性的放大失真。例如，关联函数中~100 Mpc/h的重子声学振荡标度在LOS方向上移动了~3%，而在N-S方向上移动了~0.6%，这取决于星系偏置、红移和计数斜率。如果忽略哈勃参数和角直径距离的相应变化，可能会严重影响暗能量状态方程的测量。最后，放大失真提供了一个合理的解释，在笔形波束调查中看到的众所周知的过度相关。
英文摘要：
It is well known gravitational lensing, mainly via magnification bias, modifies the observed galaxy/quasar clustering. Such discussions have largely focused on the 2D angular correlation. Here and in a companion paper (Paper II) we explore how magnification bias distorts the 3D correlation function and power spectrum, as first considered by Matsubara. The interesting point is: the distortion is anisotropic. Magnification bias preferentially enhances the observed correlation in the line-of-sight (LOS) orientation, especially on large scales. For example at LOS separation of ~100 Mpc/h, where the intrinsic galaxy-galaxy correlation is rather weak, the observed correlation can be enhanced by lensing by a factor of a few, even at a modest redshift of z ~ 0.35. The opportunity: this lensing anisotropy is distinctive, making it possible to separately measure the galaxy-galaxy, galaxy-magnification and magnification-magnification correlations, without measuring galaxy shapes. The anisotropy is distinguishable from the well known distortion due to peculiar motions, as will be discussed in Paper II. The challenge: the magnification distortion of the galaxy correlation must be accounted for in interpreting data as precision improves. For instance, the ~100 Mpc/h baryon acoustic oscillation scale in the correlation function is shifted by up to ~3% in the LOS orientation, and up to ~0.6% in the monopole, depending on the galaxy bias, redshift and number count slope. The corresponding shifts in the inferred Hubble parameter and angular diameter distance, if ignored, could significantly bias measurements of the dark energy equation of state. Lastly, magnification distortion offers a plausible explanation for the well known excess correlations seen in pencil beam surveys.
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