标题： 星系-晕/亚晕的联系：质量关系及其对某些卫星占据分布的影响 显示英文标题

标题： The Galaxy-Halo/Subhalo connection: Mass relations and implications for some satellite occupational distributions

摘要： 我们分别推断了中心星系和卫星星系的局部恒星-晕子晕质量关系(MRs)。 我们通过使用若干观测数据组合来约束这些关系，这些数据包括总星系恒星质量函数、将其分解为中心星系和卫星星系，以及在不同恒星质量区间测量的投影两点相关函数。 无论使用何种数据组合，得到的MRs之间的差异都在模型拟合不确定性范围内（非常小，小于星系与晕之间固有的散度）。 我们还假设中心晕(CH)和卫星子晕(SS) MRs周围的固有散度是常数，从而约束其值：sigma_c= 0.168±0.051 dex 和 sigma_s = 0.172±0.057 dex。 实际上，CH和SS MRs是不同的，特别是当我们考虑子晕在今天而不是吸积时的质量。 我们计算了几个人口统计量。 我们发现，即使是对于星团大小的晕，中心星系也不平均地位于最巨大卫星的质量分布中；也就是说，中心星系并不是卫星质量函数高端的一个简单实现；然而，对于> 3x10^13 msun 的晕，约15%的中心星系可能是。 我们还发现，具有N个麦哲伦云(MC)大小卫星的MW大小晕的概率与观测测量值一致；对于2x10^12 msun的晕质量，拥有2个MC的概率为5.4%，但如果排除那些卫星大于MC的系统，则概率下降到<2.2%。 显示英文摘要

摘要： We infer the local stellar-to-halo/subhalo mass relations (MRs) for central and satellite galaxies separately. We constraint this relations by using several combinations of observational data, consisting of the total galaxy stellar mass function, its decomposition into centrals and satellites, and the projected two-point correlation functions measured in different stellar mass bins. The differences among the resulting MRs are within the model-fit uncertainties (which are very small, smaller than the intrinsic scatter between galaxy and halo mass), no matter what combination of data are used. We also constrain the values of the intrinsic scatter around the central-halo (CH) and satellite-subhalo (SS) MRs assuming them to be constant: sigma_c= 0.168+-0.051 dex and sigma_s = 0.172+-0.057 dex, respectively. The CH and SS MRs are actually different, in particular when we take the subhalo mass at the present-day epoch instead of at their accretion time. We calculate several population statistics. We find that the central galaxy is not on average within the mass distribution of the most-massive satellite, even for cluster-sized halos, i.e., centrals are not a mere realization of the high-end of the satellite mass function; however for > 3x10^13 msun halos, ~15% of centrals could be. We also find that the probabilities of MW-sized halos of having N Magellanic-Clouds (MCs)-sized satellites agree well with observational measures; for a halo mass of 2x10^12 msun, the probability to have 2 MCs is 5.4%, but if we exclude those systems with satellites larger than the MCs, then the probability decreases to <2.2%.