银河系疏散星团的聚类特征
Cluster characteristics of Galactic open clusters
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中文总结 AI 辅助
研究银河系疏散星团的聚类特征，采用保守方法估计其总质量和半径，利用多种光度源轨迹网格及相关方法研究三维特征与局限性，估计约7000个星团参数，为未来盖亚数据更精确研究提供基础。
中文摘要 AI 辅助
星团非常适合用于研究恒星及其宿主星系的形成、演化和动力学。为此，需要估计星团的总质量、半径和形状，这些参数强烈影响它们在宿主星系中的命运，但文献中对此类特征尚无定论，已发表的值差异很大。我们采用非常保守的方法估计总质量和星团半径，即计算成员质量并求和。此外，研究了疏散星团的三维特征及其局限性。使用了不同光度源（包括2MASS、盖亚和泛星计划）常用的演化轨迹网格，用ASteCA构建的合成星团测试插值方法。利用著名的银河坐标和视差倒数分布估计三维形状。估计了约7000个疏散星团的总质量和半径，并观测到潮汐尾迹。个别值可用于未来盖亚数据发布以获得更精确的值，当前的DR3仅允许研究距离达500秒差距的三维形状，超过此距离，由于观测视差的不确定性，会发现明显的针状形状。
英文摘要
Star clusters are perfectly suited for studying the formation, evolution, and dynamics of stars and their host galaxies. For this, we need to estimate total masses, radii and shapes of star clusters. These parameters strongly influence their fates in the host galaxies. However, there is no agreement about these characteristics in the literature. The published values widely disagree. We estimated total masses and cluster radii using a very conservative approach: calculating member masses and summing them. Furthermore, we investigated the three-dimensional characteristics of open clusters and their limitations. We used a commonly used grid of evolutionary tracks for different photometric sources, including 2MASS, Gaia, and Pan-STARRS. The interpolation method was tested using synthetic clusters built with ASteCA. To estimate three-dimensional shapes, we used the distribution of the well-known Galactic coordinates and inverse parallaxes. We estimated the total masses and radii of about 7000 open clusters and observed traces of tidal tails. Individual values can be used in future $Gaia$ data releases to obtain even more precise values. The current DR3 allows the study of only three-dimensional shapes up to 500 pc. Beyond this distance, we find a significant needle-like shape due to uncertainties in observed parallaxes.
