Evolution of galaxy clustering
Evolution of galaxy clustering
复制标题
星系团的演化
DOI：
10.1046/j.1365-8711.1998.01788.x
复制
发表时间：
1997
影响因子：
4.8
通讯作者：
J. Bagla
中科院分区：
文献类型：
--
作者：
J. Bagla
我们研究了CDM类模型中暗物质晕相关函数的演化。我们表明，晕相关函数不演变的相关函数的基础质量分布的比例。最早坍缩的晕，对应于密度场中罕见的峰值，非常强烈地聚集在一起。晕相关函数的振幅从其初始的大值减小。这种下降一直持续到平均峰值崩溃，之后幅度缓慢增长。这种行为被证明是通用的，最小振幅的时代只取决于在相关规模的质量的均方根波动，并在一个小得多的程度上，在该规模的功率谱的斜率。我们讨论的相关性，这一结果的解释观测星系和类星体集群。
We study the evolution of the correlation function of dark matter haloes in the CDM class of models. We show that the halo correlation function does not evolve in proportion with the correlation function of the underlying mass distribution. The earliest haloes to collapse, which correspond to rare peaks in the density field, cluster very strongly. The amplitude of the halo correlation function decreases from its initial, large, value. This decrease continues until the average peaks have collapsed, after which the amplitude grows slowly. This behaviour is shown to be generic and the epoch of minimum amplitude depends only on the rms fluctuations in mass at the relevant scale and, to a much smaller extent, on the slope of the power spectrum at that scale. We discuss the relevance of this result for interpretation of observations of galaxy and quasar clustering.