标题： 微弱星系的聚类：$\w $，由弱引力透镜引起 显示英文标题

标题： Clustering of Faint Galaxies: $\w $, Induced by Weak Gravitational Lensing

摘要： 弱引力透镜效应由大尺度结构引起，通过“放大偏差”影响暗弱星系的计数数量，从而影响角度两点相关函数$\w $的测量。 在暗弱亮度下，聚类幅度随极限亮度的变化将与从 Limber 方程预期的不同。 幅度将达到一个最小值，然后随着极限亮度的增加而上升。 这种行为发生是因为 $\w$由于聚类会随着距离的增加而减少，而弱透镜引起的“放大偏差”则随着距离的增加而增加。 视亮度 $m_{min}$ 是放大偏差开始主导观测聚类的亮度，这取决于模型和颜色。 它由 $\omega(m=m_{min},\theta=5^\prime) \approx (1\ -\ 2)\times 10^{-3}(5s-2)^2 \Omega_0^2 \sigma_8^2$给出，其中$s$是数量计数的对数斜率。 已发表的在$R=25$处的$\w$测量可能受到“放大偏差”的强烈影响。 可以设计一个利用天空中蓝色和红色数量计数比值的实验，以最小化“真实”聚类的影响。 放大偏差是对质量聚类的测量。 这个弱透镜实验不需要测量星系的形状和位置角。 我推导了一个包含放大偏差效应的修正的 Limber 方程。 显示英文摘要

摘要： Weak gravitational lensing by large scale structure affects the number counts of faint galaxies through the ``magnification bias'' and thus affects the measurement of the angular two-point correlation function $\w $. At faint magnitudes the clustering amplitude will decrease differently with limiting magnitude than expected from Limber's equation. The amplitude will hit a minimum and then rise with limiting magnitude. This behavior occurs because $\w$ due to clustering decreases with distance, while the ``magnification bias'' due to weak lensing increases with distance. The apparent magnitude $m_{min}$ at which the magnification bias starts to dominate the observed clustering is model and color dependent. It is given by $\omega(m=m_{min},\theta=5^\prime) \approx (1\ -\ 2)\times 10^{-3}(5s-2)^2 \Omega_0^2 \sigma_8^2$, where $s$ is the logarithmic slope of the number counts. Already published measurements of $\w$ at $R=25$ may be strongly influenced by the ``magnification bias''. An experiment using the ratio of blue and red number counts across the sky can be designed such that the effects of the ``true'' clustering is minimized. The magnification bias is a measurement of the clustering of the mass. This weak lensing experiment does not require measuring shapes and position angles of galaxies. I derive a revised Limber's Equation including the effects of magnification bias.