Local Group自行动力学
Local Group Proper Motion Dynamics
摘要：
我们对本星系群中星系的动力学和质量的了解长期以来一直受到这样一个事实的限制，即只有视线速度是可观测的。这在动力学模型中引入了显著的退化，这只能通过测量垂直于视线的速度分量来解决。然而，在太阳邻域之外，相应的自行通常太小而无法测量。在过去的十年里，这种情况发生了巨大的变化，特别是由于哈勃太空望远镜的角分辨率和稳定性。现在可以在整个本地组中可靠地测量适当的运动，例如，HSTPROMO协作的工作。在这篇评论中，我总结了自行的重要性，本地集团科学，我描述了当前和未来的观测方法和设施，可用于测量自行。我强调最近的结果，各种银河系人口（球状星团，隆起，贫金属晕，超高速恒星，潮汐流），矮卫星星系，麦哲伦星云和仙女座星系。
英文摘要：
Our knowledge of the dynamics and masses of galaxies in the Local Group has long been limited by the fact that only line-of-sight velocities were observationally accessible. This introduces significant degeneracies in dynamical models, which can only be resolved by measuring also the velocity components perpendicular to the line of sight. However, beyond the solar neighborhood, the corresponding proper motions have generally been too small to measure. This has changed dramatically over the past decade, especially due to the angular resolution and stability available on the Hubble Space Telescope. Proper motions can now be reliably measured throughout the Local Group, as illustrated by, e.g., the work of the HSTPROMO collaboration. In this review, I summarize the importance of proper motions for Local Group science, and I describe the current and future observational approaches and facilities available to measure proper motions. I highlight recent results on various Milky Way populations (globular clusters, the bulge, the metal-poor halo, hypervelocity stars, and tidal streams), dwarf satellite galaxies, the Magellanic Clouds and the Andromeda System.
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