The evolution of HI and CIV quasar absorption line systems at 1.9 < z < 3.2
The evolution of HI and CIV quasar absorption line systems at 1.9 < z < 3.2
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1.9 < z < 3.2 处 HI 和 CIV 类星体吸收线系统的演化
DOI：
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发表时间：
2013
期刊：
影响因子：
--
通讯作者：
UK.
中科院分区：
文献类型：
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作者：
Tae;A. Partl;R. Carswell;V. M. L. F. A. Potsdam;H Germany;D. O. Astronomy;U. Wisconsin;W. I. O. Astronomy;Madingley Road;Cambridge;UK.
在给定的速度范围内，我们研究了星系间3100个HI柱密度为log N(HI)=[12.75，17.0]，频率为1.9，12.2的星系间HI吸收体的分布和演化。整个HI柱密度分布函数(CDDF)可以描述为这两个特征良好的种群的组合，它们在log N(HI)~15处重叠。在log N(HI)15处，其分布函数与N(HI)^(-1.45)成正比。然而，在较低的N(HI)时，它开始变平，因为随着N(HI)的减少，森林富集度减少。在整个HI样本的CDDF中，在logN(HI)=[14，17]处显示的对幂定律的偏离是将具有不同CDDF形状的两个不同HI总体组合的结果。相对于临界密度的总HI质量密度为Omega(HI)~1.6×10^(-6)h^(-1)，其中富集林约占Omega(HI)的40%。
We have investigated the distribution and evolution of ~3100 intergalactic HI absorbers with HI column densities log N(HI) = [12.75, 17.0] at 1.9 12.2 within a given velocity range. The entire HI column density distribution function (CDDF) can be described as the combination of these two well-characterised populations which overlap at log N(HI) ~ 15. At log N(HI) 15, with its distribution function proportional to N(HI)^(-1.45). However, it starts to flatten out at lower N(HI), since the enriched forest fraction decreases with decreasing N(HI). The deviation from the power law at log N(HI) = [14, 17] shown in the CDDF for the entire HI sample is a result of combining two different HI populations with a different CDDF shape. The total HI mass density relative to the critical density is Omega(HI) ~ 1.6 x 10^(-6) h^(-1), where the enriched forest accounts for ~40% of Omega(HI).
DOI：
10.1086/511749
发表时间：
2006-12
期刊：
The Astrophysical Journal
影响因子：
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作者：
N. Lehner;B. Savage;P. Richter;K. Sembach;T. Tripp;B. P. W. U. O. N. Dame;U. Wisconsin;U. Bonn;Space Telescope Science Institute;U. O. Massachusetts
通讯作者：
N. Lehner;B. Savage;P. Richter;K. Sembach;T. Tripp;B. P. W. U. O. N. Dame;U. Wisconsin;U. Bonn;Space Telescope Science Institute;U. O. Massachusetts