标题： 银河系的逃逸速度轮廓来自盖亚DR3 显示英文标题

标题： The Escape Velocity Profile of the Milky Way from Gaia DR3

摘要： 银河系的逃逸速度分布提供了对其潜在质量分布和暗物质特性的关键且独立的测量。 使用来自盖亚DR3的恒星样本，该样本具有6D运动学和严格的质量筛选条件，我们从4千秒差距到11千秒差距的银河中心半径范围内获得了银河系的逃逸速度分布。 为了推断径向区间的逃逸速度，我们用传统的幂律模型和一种新的函数形式对恒星速度分布的尾部进行建模，这是我们引入的新函数形式。 虽然幂律模型倾向于依赖于高速度的外推，但我们发现新的函数形式能最真实地表示观测到的分布。 使用这一逃逸速度分布，我们对以纳瓦罗-弗伦克-怀特轮廓建模的银河系暗物质晕的特性进行了限制。 结合太阳位置处的圆轨道速度的限制，我们得到了浓度和质量分别为$c_{200\rm{c}}^{\rm{DM}} = 13.9^{+6.2}_{-4.3}$和$\rm{M}_{200\rm{c}}^{\rm{DM}} = 0.55^{+0.15}_{-0.14}\times 10^{12} M_\odot$。 这对应于银河系的总质量为$\rm{M}_{200\rm{c}} = 0.64^{+0.15}_{-0.14}\times 10^{12} M_\odot$，这处于银河系质量历史范围的低端，但与其他最近的估计一致。 显示英文摘要

摘要： The escape velocity profile of the Milky Way offers a crucial and independent measurement of its underlying mass distribution and dark matter properties. Using a sample of stars from Gaia DR3 with 6D kinematics and strict quality cuts, we obtain an escape velocity profile of the Milky Way from 4 kpc to 11 kpc in Galactocentric radius. To infer the escape velocity in radial bins, we model the tail of the stellar speed distribution with both traditional power law models and a new functional form that we introduce. While power law models tend to rely on extrapolation to high speeds, we find our new functional form gives the most faithful representation of the observed distribution. Using this for the escape velocity profile, we constrain the properties of the Milky Way's dark matter halo modeled as a Navarro-Frenck-White profile. Combined with constraints from the circular velocity at the solar position, we obtain a concentration and mass of $c_{200\rm{c}}^{\rm{DM}} = 13.9^{+6.2}_{-4.3}$ and $\rm{M}_{200\rm{c}}^{\rm{DM}} = 0.55^{+0.15}_{-0.14}\times 10^{12} M_\odot$. This corresponds to a total Milky Way mass of $\rm{M}_{200\rm{c}} = 0.64^{+0.15}_{-0.14}\times 10^{12} M_\odot$, which is on the low end of the historic range of the Galaxy's mass, but in line with other recent estimates.