Numerical study of halo concentrations in dark-energy cosmologies
Numerical study of halo concentrations in dark-energy cosmologies
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DOI：
10.1051/0004-6361:20031757
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发表时间：
2003-09
影响因子：
6.5
通讯作者：
K. Dolag;M. Bartelmann;F. Perrotta;C. Baccigalupi;L. Moscardini;M. Meneghetti;G. Tormen
中科院分区：
文献类型：
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作者：
K. Dolag;M. Bartelmann;F. Perrotta;C. Baccigalupi;L. Moscardini;M. Meneghetti;G. Tormen
用常量和时变状态方程研究了不同暗能量宇宙中暗物质晕的浓度参数及其与质量的依赖关系和红移演化，并与标准的ACDM和OCDM模型进行了比较。我们发现，以前提出的用于预测晕浓度的算法可以很好地适应暗能量模型。当以分析预期值为中心时，晕浓度呈对数正态分布，标准偏差为∼0.2。平均晕浓度与质量和红移的关系符合(1+z)c=c0(M/M0)α的形式，整个过程的α为-0.1.我们发现，团簇的浓度依赖于团簇形成时的暗能量状态方程，即通过线性生长因子D+(Zcoll)红移zcoll。作为对暗能量宇宙论的一种简单修正，我们提出了用线性生长因子的比率c0→c0 D+(Z Coll)/D+.ACDM(Z Coll)来标度c0。
We study the concentration parameters, their mass dependence and redshift evolution, of dark-matter halos in different dark-energy cosmologies with constant and time-variable equation of state, and compare them with standard ACDM and OCDM models. We find that previously proposed algorithms for predicting halo concentrations can be well adapted to dark-energy models. When centred on the analytically expected values, halo concentrations show a log-normal distribution with a uniform standard deviation of ∼0.2. The dependence of averaged halo concentrations on mass and redshift permits a simple fit of the form (1 + z) c = c 0 (M/M 0 ) α , with α -0.1 throughout. We find that the cluster concentration depends on the dark energy equation of state at the cluster formation redshift z coll through the linear growth factor D + (z coll ). As a simple correction accounting for dark-energy cosmologies, we propose scaling c 0 from ACDM with the ratio of linear growth factors, c 0 → c 0 D + (Z coll )/D +.ACDM (z coll ).