标题： 南小麦哲伦云的星团：结构参数 显示英文标题

标题： The Star Clusters of the Small Magellanic Cloud: Structural Parameters

摘要： 我们给出了来自小麦哲伦云的204个星团的结构参数，这些参数是通过对麦哲伦云光电巡天图像测得的V波段表面亮度轮廓拟合King模型和Elson, Fall, & Freeman（EFF）模型轮廓得到的。尽管King模型一般比Elson, Fall, 和Freeman的软幂律模型略好，并且对约90％的样本提供了统计上可接受的拟合，但King模型和EFF模型都很好地拟合了大多数轮廓。我们发现首选模型与星团年龄之间没有相关性。我们识别出的表面亮度轮廓中的唯一系统偏差是子样本中缺乏中心浓度，我们将这些星团称为“环形”星团。与先前的研究一致，我们发现SMC中的星团比银河系中的星团显著更椭圆。然而，考虑到平均年龄差异和这些系统的快速破坏，不应直接将SMC和银河系之间的比较解释为初始星团属性或其随后演化的差异。我们发现星团椭圆度与星团质量的相关性比与星团年龄的相关性更强。我们还确定了其他几个相关性（中心表面亮度与局部背景密度，核心半径与潮汐力，大小与距离），可以用来限制SMC中星团演化的模型。 显示英文摘要

摘要： We present structural parameters for 204 stellar clusters in the Small Magellanic Cloud derived from fitting King and Elson, Fall, & Freeman model profiles to the V-band surface brightness profiles as measured from the Magellanic Clouds Photometric Survey images. Both King and EFF profiles are satisfactory fits to the majority of the profiles although King profiles are generally slightly superior to the softened power-law profiles of Elson, Fall, and Freeman and provide statistically acceptable fits to ~90% of the sample. We find no correlation between the preferred model and cluster age. The only systematic deviation in the surface brightness profiles that we identify is a lack of a central concentration in a subsample of clusters, which we designate as "ring" clusters. In agreement with previous studies, we find that the clusters in the SMC are significantly more elliptical than those in the Milky Way. However, given the mean age difference and the rapid destruction of these systems, the comparison between SMC and MW should not directly be interpreted as either a difference in the initial cluster properties or their subsequent evolution. We find that cluster ellipticity correlates with cluster mass more strongly than with cluster age. We identify several other correlations (central surface brightness vs. local background density, core radius vs. tidal force, size vs. distance) that can be used to constrain models of cluster evolution in the SMC.