论文标题
使用Illustris tng50模拟，在银河系中流浪的中间质量黑洞的动力学
Dynamics of Intermediate-Mass Black Holes Wandering in the Milky Way Galaxy Using the Illustris TNG50 Simulation
论文作者
论文摘要
矮星系中的中间质量黑洞（IMBH）的检测对于缩小黑洞的质量分布的差距至关重要（$ \ sim 3 \，\ rm m _ {\ odot} $ to $ \ sim 5 \ sim 5 \ sim 5 \ times 10^{10} {10} {10} {10} \，\ rm m m _ _} IMBHS最初位于矮人的中心，后来与银河系相撞，可能在我们的银河系中徘徊，未被发现。我们使用TNG50是Illustristng项目的最高分辨率运行，用于研究适当的质量范围的恒星簇的运动学和动力学，在MW模拟星系中充当IMBH代理。我们证明了我们所研究的IMBH的$ \ sim 87 \％$向内漂移。这些下沉的IMBH的径向速度的中位数为$ \ sim 0.44 \，\ rm ckpc \，h^{ - 1} \，gyr^{ - 1} $，对黑洞质量不依赖。中央$ 1 \，\ rm ckpc \，h^{ - 1} $在银河系中的IMBH数量最高。开发了具有线性阻力的物理玩具模型，以随着时间的流逝来解释轨道圆形。这些发现限制了IMBH的空间分布，表明未来的搜索应集中在银河系的中央区域。此外，我们发现IMBH相对于银河中心的3D速度分布的平均值为$ \ sim 180 \，\ rm km \，s^{ - 1} $，较大的方差，半径降低。值得注意的是，相对于本地气体的速度分布显示出明显较低的值，平均值为$ \ sim 88 \，\ rm km \，s^{ - 1} $。这些结果有助于预测IMBH的积聚和辐射特性，从而通过未来的调查来促进它们的检测。
The detection of Intermediate-Mass Black Holes (IMBHs) in dwarf galaxies is crucial to closing the gap in the wide mass distribution of black holes ($\sim 3 \, \rm M_{\odot}$ to $\sim 5 \times 10^{10} \, \rm M_{\odot}$). IMBHs originally located at the center of dwarfs that later collide with the Milky Way (MW) could be wandering, undetected, in our Galaxy. We used TNG50, the highest-resolution run of the IllustrisTNG project, to study the kinematics and dynamics of star clusters, in the appropriate mass range, acting as IMBH proxies in a MW analog galaxy. We showed that $\sim 87\%$ of our studied IMBHs drift inward. The radial velocity of these sinking IMBHs has a median magnitude of $\sim 0.44 \, \rm ckpc \, h^{-1} \, Gyr^{-1}$ and no dependence on the black hole mass. The central $1 \, \rm ckpc \, h^{-1}$ has the highest number density of IMBHs in the galaxy. A physical toy model with linear drag forces was developed to explain the orbital circularization with time. These findings constrain the spatial distribution of IMBHs, suggesting that future searches should focus on the central regions of the Galaxy. Additionally, we found that the 3D velocity distribution of IMBHs with respect to the galactic center has a mean of $\sim 180 \, \rm km \, s^{-1}$ and larger variance with decreasing radius. Remarkably, the velocity distribution relative to the local gas shows significantly lower values, with a mean of $\sim 88 \, \rm km \, s^{-1}$. These results are instrumental for predicting the accretion and radiation properties of IMBHs, facilitating their detection with future surveys.
