是什么决定了星系中质量最大的星团的质量：统计学，物理学还是破坏？
What determines the mass of the most massive star cluster in a galaxy: statistics, physics or disruption?
摘要：
在许多不同的星系环境中，星系团初始质量函数（CIMF）都符合指数为-2的幂律分布。这意味着最大质量星系团的质量（M_max）与星系团的个数之间存在线性关系。假设团簇形成速率恒定，且最大质量团簇不发生破裂，则在对数年龄区间内确定M_max时，M_max随年龄线性增加。在我们的样本中，七个星系中有五个观测到了这种增加，这表明M_max是由样本的大小决定的。这也意味着大规模集群对破坏非常稳定，与本次会议上提出的质量独立破坏（MID）模型不一致。对于M51和银河系中的星团，样本大小的预测在10^6 M_sun附近破裂，这表明这是这些星系中星团质量的物理上限。在这种方法中，MID和CIMF截断之间存在退化。我们展示了如何集群光度函数可以作为一种工具来区分两者。
英文摘要：
In many different galactic environments the cluster initial mass function (CIMF) is well described by a power-law with index -2. This implies a linear relation between the mass of the most massive cluster (M_max) and the number of clusters. Assuming a constant cluster formation rate and no disruption of the most massive clusters it also means that M_max increases linearly with age when determining M_max in logarithmic age bins. We observe this increase in five out of the seven galaxies in our sample, suggesting that M_max is determined by the size of the sample. It also means that massive clusters are very stable against disruption, in disagreement with the mass independent disruption (MID) model presented at this conference. For the clusters in M51 and the Antennae galaxies the size-of-sample prediction breaks down around 10^6 M_sun, suggesting that this is a physical upper limit to the masses of star clusters in these galaxies. In this method there is a degeneracy between MID and a CIMF truncation. We show how the cluster luminosity function can serve as a tool to distinguish between the two.
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