标题： 紧凑性峰值：对合并双黑洞质量分布的天体物理解释 显示英文标题

标题： Compactness peaks: An astrophysical interpretation of the mass distribution of merging binary black holes

摘要： 随着对双黑洞合并检测数量的增加，我们开始探索质量分布中的结构。 施耐德等人最近的一项研究提出，孤立双星演化中被剥离的恒星自然会在啁啾质量分布中的$\sim 8 M_\odot$和$14 M_\odot$处产生峰值，并解释了啁啾质量在$\approx 10-12 M_\odot$之间的黑洞缺失现象。 啁啾质量的间隙来自于组件质量分布中$m_1, m_2 \approx 10-15 M_\odot$之间的明显间隙以及这些黑洞的特定配对。 这个组件质量间隙来自于前身星核心致密性的变化，其中碳氧核心质量的致密性下降将不再形成黑洞。 我们开发了一个受此情景启发的人口模型，以探究由两个种群组成的双黑洞组件质量分布的结构：1）两个峰值成分，用来表示在致密性峰值处形成的黑洞，2）一个幂律成分，用来解释任何污染事件，这些是可能来自不同渠道（例如动力学）的双星。 我们使用分层贝叶斯推断来分析使用该模型的第三引力波瞬变目录（GWTC-3）中的事件。 我们发现，较低质量峰值在$\sim 11 M_\odot$处急剧下降，而较高质量峰值在$\sim 13 M_\odot$处开始，这与施耐德等人的预测一致。 然而，没有明确的证据表明存在间隙。 我们还发现两个种群具有不同的自旋分布的轻微支持。 除了这些种群结果外，我们还强调了一些与从被剥离恒星形成的致密物体预期种群分布不同的观测事件。 显示英文摘要

摘要： With the growing number of detections of binary black hole mergers, we are beginning to probe structure in the distribution of masses. A recent study by Schneider et al. proposes that isolated binary evolution of stripped stars naturally gives rise to the peaks at chirp masses $\sim 8 M_\odot$, $14 M_\odot$ in the chirp mass distribution and explains the dearth of black holes between $\approx 10-12 M_\odot$ in chirp mass. The gap in chirp mass results from an apparent gap in the component mass distribution between $m_1, m_2 \approx 10-15 M_\odot$ and the specific pairing of these black holes. This component mass gap results from the variation in core compactness of the progenitor, where a drop in compactness of Carbon-Oxygen core mass will no longer form black holes from core collapse. We develop a population model motivated by this scenario to probe the structure of the component mass distribution of binary black holes consisting of two populations: 1) two peak components to represent black holes formed in the compactness peaks, and 2) a powerlaw component to account for any polluting events, these are binaries that may have formed from different channels (e.g. dynamical). We perform hierarchical Bayesian inference to analyse the events from the third gravitational-wave transient catalogue (GWTC-3) with this model. We find that there is a preference for the lower mass peak to drop off sharply at $\sim 11 M_\odot$ and the upper mass peak to turn on at $\sim 13 M_\odot$, in line with predictions from Schneider et al. However, there is no clear evidence for a gap. We also find mild support for the two populations to have different spin distributions. In addition to these population results, we highlight observed events of interest that differ from the expected population distribution of compact objects formed from stripped stars.