大尺度结构中的银河系角动量和angular momentum耦合
Galactic angular momenta and angular momentum couplings in the large-scale structure
摘要：
本文重新讨论了利用潮汐剪切获得星系角动量的问题，并从峰值限制的高斯随机过程中计算了角动量方差σ_L^2和角动量关联函数C_L（r）。这种描述初始条件的随机过程将潮汐剪切和惯性视为动力场，并明确说明了惯性场的离散性。我们描述的方式，在角动量的相关性的结果，从长期的相关性的相互作用的潮汐剪切，和短期的相关性在惯性场，这反映了这两个对称张量的本征系统之间的相关性。我们提出了一种新的形式的角动量关联函数，它是能够区分平行和反平行的角动量矢量的对齐，并评论的内在对齐弱透镜测量的影响。我们确定了缩放L/M propto。M^{2/3}，并发现银河系大小的晕的角动量分布在~1 Mpc/h的尺度上是相关的。关联函数可用C_L（r）propto形式的经验关系式拟合。exp（-[r/r_0]^beta）。
英文摘要：
In this paper, we revisit the aquisition of angular momentum of galaxies by tidal shearing and compute the angular momentum variance sigma_L^2 as well as the angular momentum correlation function C_L(r) from a peak-restricted Gaussian random process. This stochastic process describing the initial conditions treats both the tidal shear as well as the inertia as dynamical fields and explicitly accounts for the discreteness of the inertia field. We describe the way in which the correlations in angular momentum result from an interplay of long-ranged correlations in the tidal shear, and short ranged correlations in the inertia field and which reflects the correlation between the eigensystems of these two symmetric tensors. We propose a new form of the angular momentum correlation function which is able to distinguish between parallel and antiparallel alignment of angular momentum vectors, and comment on implications of intrinsic alignments for weak lensing measurements. We confirm the scaling L/M propto. M^{2/3} and find the angular momentum distribution of Milky Way-sized haloes to be correlated on scales of ~1 Mpc/h. The correlation function can be well fitted by an empirical relation of the form C_L(r) propto. exp(-[r/r_0]^beta).
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