USING MEMBER GALAXY LUMINOSITIES AS HALO MASS PROXIES OF GALAXY GROUPS
USING MEMBER GALAXY LUMINOSITIES AS HALO MASS PROXIES OF GALAXY GROUPS
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DOI：
10.1088/0004-637x/804/1/55
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发表时间：
2015-03
期刊：
影响因子：
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通讯作者：
Yi Lu;Xiaohu Yang;S. Shen
中科院分区：
文献类型：
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作者：
Yi Lu;Xiaohu Yang;S. Shen
可靠的星系晕质量估计在宇宙学和星系形成研究中起着重要的作用。在这里，我们着手寻找一种方法来改善晕质量估计的星系系统中，有限数量的最明亮的成员星系已被观察到。使用四个模拟星系样本构造半解析形成模型，subhalo丰度匹配方法，和条件光度函数，分别，我们发现，最亮的和随后的最亮的成员星系之间的光度差距在一个晕（组），可以用来减少显着的分散在晕质量估计的基础上的最亮的星系的光度单独。测试表明，这些修正可以显着减少在晕质量估计的分散的1.50%至1.70%，在大质量的晕取决于成员星系被认为是。与传统的排序方法相比，我们发现这种方法更适合于少于五个成员的群体，或者在非常明亮的震级截止的观测中。
Reliable halo mass estimation for a given galaxy system plays an important role in both cosmology and galaxy formation studies. Here we set out to find a way to improve halo mass estimation of those galaxy systems in which a limited number of brightest member galaxies have been observed. Using four mock galaxy samples constructed from semi-analytical formation models, the subhalo abundance matching method, and the conditional luminosity functions, respectively, we find that the luminosity gap between the brightest and the subsequent brightest member galaxies in a halo (group) can be used to reduce significantly the scatter in the halo mass estimation based on the luminosity of the brightest galaxy alone. Tests show that these corrections can significantly reduce the scatter in the halo mass estimations by ∼50% to ∼70% in massive halos depending on which member galaxies are considered. Compared to the traditional ranking method, we find that this method works better for groups with less than five members, or in observations with a very bright magnitude cutoff.