论文标题
银河系球形集群动力学：它们优先是共旋转吗？
Milky Way globular cluster dynamics: are they preferentially co-rotating?
论文作者
论文摘要
银河系的重型成分的运动受到银河系的发光和暗物质含量的控制。因此，银河系的动力学可以用作将星系的质量模型推断为较大半径的示踪剂。在这项工作中，我们使用直接可观察的视线速度来测试球状簇种群的动力学是否与银河系的轴对称重力潜力一致。为此，我们从数值上计算球状簇群体的相空间分布，其中轨道是随机定向的，或相对于恒星磁盘的共同旋转。然后，我们将观测到的位置和视线速度分布与$ \ sim $ 150球形簇与模型的速度分布进行比较。我们发现，对于采用的质量模型，共旋转场景是基于各种统计检验的最受欢迎的模型。我们进行了与早期合并事件祖细胞相关的GC的分析。该分析可以在不久的将来进行扩展，以包括精确和大量数据，以更好地将银河电位限制为大半径。
The motion of the baryonic components of the Milky Way is governed by both luminous and dark matter content of the Galaxy. Thus, the dynamics of the Milky Way globular clusters can be used as tracers to infer the mass model of the Galaxy up to a large radius. In this work, we use the directly observable line-of-sight velocities to test if the dynamics of the globular cluster population is consistent with an assumed axisymmetric gravitational potential of the Milky Way. For this, we numerically compute the phase space distribution of the globular cluster population where the orbits are either oriented randomly or co-/counter- rotating with respect to the stellar disk. Then we compare the observed position and line-of-sight velocity distribution of $\sim$ 150 globular clusters with that of the models. We found that, for the adopted mass model, the co-rotating scenario is the favored model based on various statistical tests. We do the analysis with and without the GCs associated to the progenitors of early merger events. This analysis can be extended in the near future to include precise and copious data to better constrain the Galactic potential up to a large radius.
