贝克勒尔86和87两个年轻的疏散星团及其邻域：结合多色photometry与Gaia DR3测光
Two young open clusters in Cygnus and their vicinity: combining multicolor photometry with Gaia DR3 astrometry
AI总结：
研究贝克勒尔86和87星团的消光特性及其空间运动，结合多色photometry和Gaia数据确定星团年龄和质量，揭示其可能的共同起源。
摘要：
我们研究了贝克勒尔86和87两个邻近的疏散星团，重点在于评估视场内和跨星团的消光特性。我们还分析了它们在空间和时间上的运动行为，以确定其可能的共同起源和与Cyg~OB1关联的关系。通过在维尔纽斯七色系统中获得的新的CCD测光数据（在这些两个星团的区域内测到V=19.0 mag），我们根据光谱和光度分类来分类恒星，并确定个体的星际消光值。通过基于Gaia DR3的五参数空间，确定了可能的星团成员。通过使用H-R图来推导星团的年龄和恒星质量。为了获得星团的三维运动学并追溯其历史轨道，我们结合了基于Gaia的自行和距离以及文献中的径向速度。估计的星团特性表明，这两个星团几乎等距（1.7 kpc）且几乎同时形成，平均年龄分别为6.1±0.5和6.5±0.4 Myr，年龄分散为3 Myr。每个星团内部的消光非均匀性明显，尤其是在贝克勒尔86的面朝方向，最质量大的恒星显示出显著的亚结构。通过将观测到的质量函数外推到最小的恒星质量，我们得到了贝克勒尔86和87的质量分别为519 M(Sun)和1551 M(Sun)。尽管这两个星团有非常相似的性质，但它们的轨道路径表明它们没有共同的出生地，然而贝克勒尔87和其邻居NGC 6913很可能是一起诞生的。
英文摘要：
We investigate two neighboring clusters in the Cygnus complex, Berkeley 86 and Berkeley 87, with a primary emphasis on the evaluation of extinction in the field of view towards and across the clusters. We also analyze their kinematic behavior in space and time to discern their possible common origin and relation to the Cyg~OB1 association. New CCD photometry in the Vilnius seven-color system, obtained down to V=19.0 mag in the fields of these two clusters, is used to classify stars in terms of spectral and luminosity classes and to determine the individual values of interstellar extinction. The probable cluster members are identified in a 5-parameter space based on Gaia DR3. The cluster ages and stellar masses are derived through the use of the HR diagrams. To obtain the 3D kinematics of the clusters and trace their orbits back in time, we combine the Gaia-based proper-motions and distances with radial velocities from the literature. The estimated cluster properties show that both clusters are almost equidistant (1.7 kpc) and nearly coeval, with average ages of 6.1$\pm$0.5 and 6.5$\pm$0.4 Myr, respectively, and age dispersion of 3 Myr. The nonuniformity of extinction is evident within each cluster, especially pronounced across the face of Berkeley 86 where the most-massive stars show substantial substructure. By extrapolating the observed mass function to a minimum stellar mass, we obtain cluster masses of 519 M(Sun) and 1551 M(Sun) for Berkeley 86 and 87, respectively. Although both clusters share very similar properties, their orbital paths show no indication that they had a common birthplace, however Berkeley 87 and its neighbor NGC 6913 are very likely to have been born in pair.
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