论文标题
修订和新的适当动作，以确认和候选银河系矮星系
Revised and new proper motions for confirmed and candidate Milky Way dwarf galaxies
论文作者
论文摘要
提出了新的全身性卫星卫星卫星运动的新推导，并使用GAIA数据发布2列出了59个已确认或候选矮人银河卫星。这构成了所有已知的银河系矮星系（以及可能是2020年5月的候选人），截至2020年5月，截至2020年，截至2020射手座矮星系。我们首次为印度河1，DES J0225+0304，CETUS 2，PICTOR 2和LEO T得出系统性适当的运动，但请注意，后三个依赖于质量差的光度法比其他样品的质量差。我们无法解析引导4，Cetus 3，Indus 2，Pegasus 3或处女座1的信号。我们的方法灵感来自PACE＆LI（2019）的最大似然方法，并同时检查了空间，色彩障碍和源的适当运动分布。出于系统性适当的运动而无需识别确认的径向速度成员，尽管这些恒星的适当运动在可用的地方通过模型上的先验纳入了分析中。与现有文献值相比，系统正确运动的相关不确定性平均要$ \ sim 1.4 $。对卫星的隐含成员资格分布的分析表明，我们准确地识别出污染率小于20分之一的成员恒星。
A new derivation of systemic proper motions of Milky Way satellites is presented, and applied to 59 confirmed or candidate dwarf galaxy satellites using Gaia Data Release 2. This constitutes all known Milky Way dwarf galaxies (and likely candidates) as of May 2020 except the Magellanic Clouds, the Canis Major and Hydra 1 stellar overdensities, and the tidally disrupting Bootes III and Sagittarius dwarf galaxies. We derive systemic proper motions for the first time for Indus 1, DES J0225+0304, Cetus 2, Pictor 2 and Leo T, but note that the latter three rely on photometry that is of poorer quality than for the rest of the sample. We cannot resolve a signal for Bootes 4, Cetus 3, Indus 2, Pegasus 3, or Virgo 1. Our method is inspired by the maximum likelihood approach of Pace & Li (2019) and examines simultaneously the spatial, color-magnitude, and proper motion distribution of sources. Systemic proper motions are derived without the need to identify confirmed radial velocity members, although the proper motions of these stars, where available, are incorporated into the analysis through a prior on the model. The associated uncertainties on the systemic proper motions are on average a factor of $\sim 1.4$ smaller than existing literature values. Analysis of the implied membership distribution of the satellites suggests we accurately identify member stars with a contamination rate less than 1 in 20.
