On the assembly history of dark matter haloes
On the assembly history of dark matter haloes
复制标题
论暗物质晕的组装历史
DOI：
10.1111/j.1365-2966.2007.11942.x
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发表时间：
2005-10
影响因子：
4.8
通讯作者：
Li, Yun
中科院分区：
文献类型：
--
作者：
Mo, H. J.;van den Bosch, Frank C.;Lin, W. P.;Li, Yun
我们研究了暗物质晕的质量组装历史。我们比较MAH使用（i）合并树构建扩展的Press-Schechter（EPS）形式主义，（ii）数值模拟和（iii）拉格朗日微扰代码PINOCCHIO。我们表明，皮诺乔MAH是在使用数值模拟得到的非常好的协议，而EPS形式主义预测MAH发生得太晚。PINOCCHIO比N体模拟的CPU消耗少得多，可以在简单的个人计算机上运行，并且不需要任何劳动密集型的模拟后分析，因此提供了一个独特而强大的工具来研究暗物质晕的生长历史。使用一套55 PINOCCHIO模拟，每个256（3）粒子，我们研究了12 924冷暗物质（CDM）晕在Lambda CDM和谐宇宙学的MAH。这是迄今为止用于任何此类分析的最大的晕集。对于每个MAH，我们得到四个不同的形成红移，其特征在于不同的时代在组装历史的暗物质晕。我们表明，晕的质量小于特征的非线性质量尺度建立他们的潜在威尔斯之前，他们获得大部分的质量。当一个晕达到其最大维里速度的时间大致分为两个阶段，一个快速吸积阶段，这是占主导地位的主要合并，和一个缓慢吸积阶段占主导地位的次要合并。每一个光环都经历了大约3 +/- 2次大的合并，因为它的主要祖先的质量等于最终光环质量的1%。这个主要的合并统计被发现是几乎独立的晕质量。然而，这些主要合并发生的平均红移强烈依赖于质量，更大质量的晕经历他们的主要合并。
We study the mass assembly history (MAH) of dark matter haloes. We compare MAHs obtained using (i) merger trees constructed with the extended Press-Schechter (EPS) formalism, (ii) numerical simulations and (iii) the Lagrangian perturbation code PINOCCHIO. We show that the PINOCCHIO MAHs are in excellent agreement with those obtained using numerical simulations, while the EPS formalism predicts MAHs that occur too late. PINOCCHIO, which is much less CPU intensive than N-body simulation, can be run on a simple personal computer, and does not require any labour intensive post-simulation analysis, therefore provides a unique and powerful tool to investigate the growth history of dark matter haloes. Using a suite of 55 PINOCCHIO simulations, with 256(3) particles each, we study the MAHs of 12 924 cold dark matter (CDM) haloes in a Lambda CDM concordance cosmology. This is by far the largest set of haloes used for any such analysis. For each MAH we derive four different formation redshifts, which characterize different epochs during the assembly history of a dark matter halo. We show that haloes less massive than the characteristic non-linear mass scale establish their potential wells much before they acquire most of their mass. The time when a halo reaches its maximum virial velocity roughly divides its mass assembly into two phases, a fast-accretion phase which is dominated by major mergers, and a slow-accretion phase dominated by minor mergers. Each halo experiences about 3 +/- 2 major mergers since its main progenitor had a mass equal to 1 per cent of the final halo mass. This major merger statistic is found to be virtually independent of halo mass. However, the average redshift at which these major mergers occur is strongly mass dependent, with more massive haloes experiencing their major mergers later.
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DOI：
10.1046/j.1365-8711.2002.05441.x
发表时间：
2001-09
影响因子：
4.8
作者：
G. Taffoni;P. Monaco;T. Theuns
通讯作者：
G. Taffoni;P. Monaco;T. Theuns
DOI：
10.1086/340190
发表时间：
2001-09
期刊：
The Astrophysical Journal
影响因子：
--
作者：
S. M. Khairul Alam;J. Bullock;David H. Weinberg
通讯作者：
S. M. Khairul Alam;J. Bullock;David H. Weinberg
影响因子：
1
作者：
V. Avila-Reese;C. I. D. Astronomia;Unam;M. O. A. D. Brera;Italy.
通讯作者：
V. Avila-Reese;C. I. D. Astronomia;Unam;M. O. A. D. Brera;Italy.
DOI：
10.1086/174501
发表时间：
1993-07
期刊：
arXiv: Astrophysics
影响因子：
--
作者：
E. Bertschinger;B. Jain
通讯作者：
E. Bertschinger;B. Jain
影响因子：
4.8
作者：
D. D. C. Rodrigues-D.;P. Thomas
通讯作者：
D. D. C. Rodrigues-D.;P. Thomas