标题： 大麦哲伦云中53个富星团的表面亮度分布与结构参数 显示英文标题

标题： Surface Brightness Profiles and Structural Parameters for 53 Rich Stellar Clusters in the Large Magellanic Cloud

摘要： 我们从哈勃太空望远镜档案中编译了一个伪快照数据集，包含53个富丽马尼亚星团的双色观测数据，这些星团的年龄在10^6到10^10年之间。我们展示了整个样本的表面亮度分布，并为每个星团推导出结构参数，包括核心半径以及光度和质量估计值。 由于我们预计这里呈现的结果将成为几个进一步项目的基石，我们详细描述了数据处理和表面亮度分布构建的过程，并将我们的结果与以前地面研究的结果进行了比较。 表面亮度分布显示出大量的细节，包括年轻星团分布中的不规则性（如凸起、凹陷和陡峭的肩部），以及双重星团和后核坍缩（PCC）星团的证据。 特别是，我们在几个候选PCC星团的内部区域发现了幂律分布，其斜率约为-0.7，但表现出相当大的变化。 我们估计，丽女星系团的老年星团中有20%±7%已经进入了PCC演化阶段，这一比例与银河球状星团系统的比例相似。 此外，我们详细检查了R136的分布，并表明它可能不是一个PCC星团。 我们还观察到了核心半径随年龄的变化趋势，这一趋势已在多位作者先前的不同出版物中发现和讨论过。 然而，我们的图表分辨率更高，并似乎在几百Myr时显示出了分支。 我们认为，这种观察到的关系反映了丽女星系团的真实物理演化，其中一些星团由于质量损失而经历了小规模的核心膨胀，而另一些则由于某种未识别的特征或物理过程而经历了大规模的核心膨胀。 显示英文摘要

摘要： We have compiled a pseudo-snapshot data set of two-colour observations from the Hubble Space Telescope archive for a sample of 53 rich LMC clusters with ages 10^6-10^10 yr. We present surface brightness profiles for the entire sample, and derive structural parameters for each cluster, including core radii, and luminosity and mass estimates. Because we expect the results presented here to form the basis for several further projects, we describe in detail the data reduction and surface brightness profile construction processes, and compare our results with those of previous ground-based studies. The surface brightness profiles show a large amount of detail, including irregularities in the profiles of young clusters (such as bumps, dips, and sharp shoulders), and evidence for both double clusters and post core-collapse (PCC) clusters. In particular we find power-law profiles in the inner regions of several candidate PCC clusters, with slopes of approximately -0.7, but showing considerable variation. We estimate that 20 +/- 7 % of the old cluster population of the LMC has entered PCC evolution, a similar fraction to that for the Galactic globular cluster system. In addition, we examine the profile of R136 in detail and show that it is probably not a PCC cluster. We also observe a trend in core radius with age that has been discovered and discussed in several previous publications by different authors. Our diagram has better resolution however, and appears to show a bifurcation at several hundred Myr. We argue that this observed relationship reflects true physical evolution in LMC clusters, with some experiencing small scale core expansion due to mass loss, and others large scale expansion due to some unidentified characteristic or physical process.