We employ Gaia DR2 proper motions for 151 Milky Way globular clusters from Vasiliev (2019) in tandem with distances and line-of-sight velocities to derive their kinematical properties. To assign clusters to the Milky Way thick disk, bulge, and halo we follow the approach of Posti et al. (2018) who distinguished among different Galactic stellar components using stars's orbits. In particular, we use the ratio $L_{z}/e$, the $Z$ projection of the angular momentum to the eccentricity, as population tracer, which we complement with chemical abundances extracted from the literature and Monte-Carlo simulations. We find that 20 globular clusters belong to the bar/bulge of the Milky Way, 35 exhibit disk properties, and 96 are members of the halo. Moreover, we find that halo globular clusters have close to zero rotational velocity with average value $ $ =1$\pm$ 4 km s$^{-1}$. On the other hand, the sample of clusters that belong to the thick disk possesses a significant rotation with average rotational velocity 179 $\pm$ 6 km s$^{-1}$. The twenty globular clusters orbiting within the bar/bulge region of the Milky Way galaxy have average rotational velocity of 49 $\pm$ 11 km s$^{-1}$.

中文翻译：

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使用 Gaia DR2 和 HST 数据的球状星团运动学中的银河系子系统

我们对来自 Vasiliev (2019) 的 151 个银河系球状星团采用 Gaia DR2 自行结合距离和视线速度来推导它们的运动学特性。为了将星团分配给银河系厚盘、凸起和光晕，我们遵循 Posti 等人的方法。（2018）谁使用恒星的轨道区分不同的银河系恒星成分。特别是，我们使用比率 $L_{z}/e$，即角动量对偏心率的 $Z$ 投影，作为种群示踪剂，我们补充了从文献和蒙特卡罗模拟中提取的化学丰度。我们发现 20 个球状星团属于银河系的棒/球状星团，35 个具有圆盘特性，96 个是光晕的成员。而且，我们发现晕球状星团的旋转速度接近于零，平均值 $ $ =1$\pm$ 4 km s$^{-1}$。另一方面，属于厚盘的簇样本具有显着的旋转，平均旋转速度为 179 $\pm$ 6 km s$^{-1}$。二十个球状星团在银河系的棒/球区域内运行，平均旋转速度为 49 $\pm$ 11 km s$^{-1}$。