标题： 二进制黑洞合并时间与宿主星系性质之间的便捷关系 显示英文标题

标题： Handy Relation Between Binary Black Hole Merger Times and Host Galaxy Properties

摘要： 在过去15年中，证据明确表明，大质量黑洞（MBH）双星合并时间尺度强烈依赖于其宿主星系的结构和运动学特性。 恒星密度、气体含量、形状和运动学都起作用，以非线性方式结合，影响双星的演化。 双星本身的特性，如偏心率、质量比和轨道平面，同样也很重要。 这使得准确估计宇宙学上的MBH双星合并率，或者生成反映星系宿主和轨道分布的合并率范围变得不那么直接。 我们使用一套广泛的高分辨率直接N体模拟，在这些模拟中，每个星系宿主的形状、结构和运动学特性都直接由观测结果提供，我们绘制出在不同星系宿主和MBH双星轨道下的MBH双星合并时间尺度。 这产生了一组方便的标度关系，用于确定MBH双星合并时间尺度——以及合并时间尺度的范围——作为基本可观测量的函数。 这样的标度关系可以很容易地作为子网格模型应用于宇宙学或半解析研究中，例如，用于模拟LISA或脉冲星计时的事件率。 显示英文摘要

摘要： Over the past 15 years, the evidence has clearly demonstrated that massive black hole (MBH) binary merger timescales depend strongly on the structural and kinematic properties of their host galaxy. Stellar density, gas content, shape and kinematics all play a role, combining in non-linear ways to effect the evolution of the binary. The binary properties themselves, such as eccentricity, mass ratio, and orbital plane, all matter as well. This makes it nontrivial to estimate accurate cosmological MBH binary merger rates, or to generate merger rate ranges that reflect the distribution of galaxy hosts and orbits. Using an extensive set of high-resolution direct N-body simulations in which the shape, structure, and kinematics of each galaxy host are directly informed by observations, we map out MBH binary merger timescales over a range of galaxy hosts and MBH binary orbits. This yields a convenient set of scaling relations to determine MBH binary merger timescales -- and the range of merger timescales -- as functions of basic observables. Such scaling relations can be readily employed as a subgrid model in cosmological or semi-analytic studies, for example, to model event rates for LISA or pulsar timing.