期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 366, 期 4, 页码 1455-1464出版社
OXFORD UNIV PRESS
DOI: 10.1111/j.1365-2966.2005.09943.x
关键词
large-scale structure of Universe
We investigate the properties of the pairwise velocity dispersion as a function of galaxy luminosity in the context of a halo model. We derive the distribution of velocities of pairs at a given separation taking into account both one- and two-halo contributions. We show that pairwise velocity distribution in real space is a complicated mixture of host-satellite, satellite-satellite (sat-sat) and two-halo pairs. The peak value is reached at around 1 h(-1) Mpc and does not reflect the velocity dispersion of a typical halo hosting these galaxies, but is instead dominated by the sat-sat pairs in high-mass clusters. This is true even for cross-correlations between bins separated in luminosity. As a consequence, the velocity dispersion at a given separation can decrease with luminosity, even if the underlying typical halo host mass is increasing, in agreement with recent observations. We compare our findings to numerical simulations and find a good agreement. Numerical simulations also suggest a luminosity-dependent velocity bias, which depends on the subhalo mass. We develop models of the auto- and cross-correlation functions of luminosity subsamples of galaxies in the observable r(proj)-pi space and calculate the inferred velocity dispersion as a function of wavevector if dispersion model is fit to the redshift-space power spectrum. We find that so-derived pairwise velocity dispersion also exhibits a bump at k similar to 1 h Mpc(-1).
作者
我是这篇论文的作者
点击您的名字以认领此论文并将其添加到您的个人资料中。
推荐
暂无数据