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首页> 外文期刊>The Astrophysical journal >KINEMATICS OF TIDAL DEBRIS FROM ω CENTAURI'S PROGENITOR GALAXY
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KINEMATICS OF TIDAL DEBRIS FROM ω CENTAURI'S PROGENITOR GALAXY

机译：ωCENTAURI的祖先星系的潮汐碎屑运动学

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摘要

We present the kinematic properties of a tidally disrupted dwarf galaxy in the Milky Way, based on the hypothesis that its central part once contained the most massive Galactic globular cluster, ω Cen. Dynamical evolution of a self-gravitating progenitor galaxy that follows the present-day and likely past orbits of ω Cen is calculated numerically and the kinematic nature of their tidal debris is analyzed, combined with randomly generated stars comprising spheroidal halo and flat disk components. We show that the retrograde rotation of the debris stars at ～-100 km s~(-1) accords with a recently discovered large radial velocity stream at ～300 km s~(-1) toward the Galactic longitude of ～270°. These stars also contribute, only in part, to a reported retrograde motion of the outer halo at the north Galactic pole. The prospects for future debris searches and the implications for the early evolution of the Galaxy are briefly presented.
机译：我们基于银河系中心部分曾经包含最大质量银河系球状星团ωCen的假设，介绍了银河系中经潮汐破坏的矮星系的运动学特性。数值计算自引力银河系的动态演化，该自引力银河系遵循ωCen的当前轨道和可能过去的轨道，并分析其潮汐碎片的运动学性质，并结合随机产生的包括球形晕和平盘成分的恒星。我们发现，碎片星在〜-100 km s〜（-1）处逆行自转与最近发现的在〜300 km s〜（-1）处朝向270°银河系的大径向速度流一致。这些恒星也仅部分报告了银河系北极外晕的逆行运动。简要介绍了未来碎片搜索的前景以及对银河早期发展的影响。

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