论文标题
称重黑暗III：盖亚（Gaia）如何，但可能不会，天文统计会检测到自由浮动的黑洞
Weighing the Darkness III: How Gaia Could, but Probably Won't, Astrometrically Detect Free-Floating Black Holes
论文作者
论文摘要
众所周知，一个看不见的伴侣向光星的引力吸引力，会导致视差和恒星的正确运动。在本系列的上一篇论文中，我们认为天文宣教gaia可以通过精确测量这些弧线来识别长期周期二进制。恒星路径中的弧线也可能是由飞行型引起的 - 与另一个巨大物体的双曲线相遇。我们量化了伴侣恒星引起的明显加速度，这是冲击参数，相互作用速度和伴随质量的函数。原则上，盖亚可以用来符合星体统计学的识别大规模紧凑的光环对象对银河系的局部暗物质潜力的贡献。但是，在量化了其速率和盖亚的敏感性之后，我们发现蝇by是如此罕见，以至于盖亚（Gaia）可能永远不会观察到。因此，表现出天文加速度的GAIA数据库中的每个恒星都可能在带有另一个物体的长周期二进制中。然而，我们展示了中间质量的黑洞，如果它们存在于太阳能街区，它们会被它们在附近的恒星上诱导的异常大加速度检测到。
The gravitational pull of an unseen companion to a luminous star is well-known to cause deviations to the parallax and proper motion of a star. In a previous paper in this series, we argue that the astrometric mission Gaia can identify long-period binaries by precisely measuring these arcs. An arc in a star's path can also be caused by a fly-by -- the hyperbolic encounter with another massive object. We quantify the apparent acceleration over time induced by a companion star as a function of the impact parameter, velocity of interaction, and companion mass. In principle, Gaia could be used to astrometrically identify the contribution of massive compact halo objects to the local dark matter potential of the Milky Way. However, after quantifying their rate and Gaia's sensitivity, we find that fly-bys are so rare that Gaia will probably never observe one. Therefore every star in the Gaia database exhibiting astrometric acceleration is likely in a long-period binary with another object. Nevertheless, we show how intermediate mass black holes, if they exist in the Solar Neighborhood, could be detected by the anomalously large accelerations they induce on nearby stars.
