绘制银河系的黑暗世界 I：银河系黑洞运动学、速率和人口统计学的综合模拟
Charting the Galactic Underworld I: Comprehensive simulations of the kinematics, rates, and demographics of Milky Way black holes
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中文总结 AI 辅助
该研究利用cogsworth模拟银河系黑洞固有种群，考虑其双星演化等，报告黑洞速率等人统计学及运动学，分析其对多种因素的敏感性，指出黑洞质量分布等对相关模型敏感，观测可约束相关标准，还探讨了银河系引力场时间演化及双星相互作用的影响。
中文摘要 AI 辅助
随着即将来自罗曼、盖亚 DR4 和光谱巡天的数据，我们很快将拥有一个前所未有的银河系黑洞数据集来约束它们的形成和演化。为做好准备，我们用cogsworth模拟银河系黑洞的固有种群，自洽地考虑它们的双星演化和在银河系引力场中的轨迹。我们报告了这些黑洞的速率、人口统计学和运动学，以及它们对双星演化、超新星物理和银河系引力场中32种变化的敏感性。在基准模型中，银河系中已形成约1.7×10⁸个黑洞（尽管在我们的各种变化中总数跨越一个数量级），其中绝大多数（约91%）目前是孤立的，约3%已逃离银河系。双星系统中的约10⁷个黑洞大多有另一个黑洞或白矮星伴星，但约10⁵个有发光恒星伴星。黑洞比可见星分布更分散，标高约大2.5倍。黑洞质量与当前位置相关：质量最大的黑洞优先靠近银盘。这种相关性在黑洞-恒星双星中尤其强烈，它们分为紧密的、低质量的共包层后系统和宽的、高质量的非相互作用系统。黑洞质量分布和运动学对残余质量规定和出生时的反冲模型高度敏感，因此观测可以约束可爆性标准和黑洞反冲。考虑银河系引力场的时间演化使逃逸率增加一倍多，并使束缚种群的标高增加约20%，而忽略双星相互作用则高估了30%。
英文摘要
With upcoming data from Roman, Gaia DR4, and spectroscopic surveys, we will soon have an unprecedented dataset of Milky Way black holes (BHs) to constrain their formation and evolution. To prepare, we simulate the intrinsic population of Milky Way BHs with cogsworth, self-consistently accounting for their binary evolution and trajectories through the Galactic potential. We report the rate, demographics, and kinematics of these BHs, and their sensitivity to 32 variations in binary evolution, supernova physics, and Galactic potentials. In the fiducial model, ~$1.7 \times 10^8$ BHs have formed in the Milky Way (though this total spans an order of magnitude across our variations), where the vast majority (~91%) are currently isolated and ~3% have escaped the Galaxy. Most of the ~$10^7$ BHs in binaries have another BH or a white dwarf companion, but ~$10^5$ retain a luminous stellar companion. BHs are distributed more diffusely than visible stars, with a scale height around ~$2.5\times$ larger. BH masses correlate with present-day location: the most massive BHs are preferentially close to the Galactic plane. This correlation is especially strong for BH-star binaries, which separate into tight, low-mass post-common-envelope systems and wide, high-mass non-interacting ones. The BH mass distribution and kinematics are highly sensitive to the remnant mass prescription and natal kick model, so observations could constrain explodability criteria and BH kicks. Accounting for the time-evolution of the Galactic potential more than doubles the escape fraction and increases the bound population's scale height by ~20%, whilst neglecting binary interactions overestimates it by 30%.
