标题： 三十年代中期的危机：解析35倍太阳质量峰值附近的引力波源特性 显示英文标题

标题： A Mid-Thirties Crisis: Dissecting the Properties of Gravitational Wave Sources Near the 35 Solar Mass Peak

摘要： 二进制黑洞（BBH）在引力波天文学第一个十年中观测到的合并的一个显著特点是，在$35\,\mathrm{M}_{\odot}$附近的组件质量事件有过剩。 已经提出了多种形成通道来解释这种过剩。 为了区分这些通道，有必要检查它们在其他参数上的预测种群分布。 在这项工作中，我们关注接近$35\,\mathrm{M}_{\odot}$峰值的 BBH 合并，并推断主质量（$m_1$）、质量比（$q$）、有效自旋（$\chi_{\rm eff}$）和红移（$z$）的种群分布。 我们观察到合并率随着$m_1$逐渐增加，从$20\,\mathrm{M}_{\odot}$到大约$34\,\mathrm{M}_{\odot}$时增加了$3$倍，随后在$50\,\mathrm{M}_{\odot}$时急剧下降了一个数量级。 这一种群还表现出对等质量合并的微弱偏好，并具有一个向正值倾斜的$\chi_{\rm eff}$分布，中位数为零，在大约$90\%$置信度下被排除。 我们发现在 $35\, \mathrm{M}_{\odot}$ 峰值星群中不存在显著的 $q-\chi_{\rm eff}$ 相关性，这表明低质量系统 ($m_1<20\,\mathrm{M}_{\odot}$) 可能是导致在完整 BBH 合并星表中观测到的 $q-\chi_{\rm eff}$ 负相关性的原因。 合并速率的红移演化与宇宙恒星形成速率一致。 我们将我们的发现与来自各种形成通道的预测进行了比较。 我们发现，对不稳定性超新星情景的常见变体以及分层合并模型与 $35\,\mathrm{M}_{\odot}$ 星群的观测特征不相容。 最终，我们所考虑的任何形成通道都无法解释该星群中观测到的全部甚至大部分特征。 黑洞合并的“三十年代中期”正处于危机之中。 显示英文摘要

摘要： One striking feature of binary black hole (BBH) mergers observed in the first decade of gravitational-wave astronomy is an excess of events with component masses around $35\,\mathrm{M}_{\odot}$. Multiple formation channels have been proposed to explain this excess. To distinguish among these channels, it is essential to examine their predicted population-level distributions across additional parameters. In this work, we focus on BBH mergers near the $35\,\mathrm{M}_{\odot}$ peak and infer the population distributions of primary mass ($m_1$), mass ratio ($q$), effective spin ($\chi_{\rm eff}$), and redshift ($z$). We observe a gradual increase in the merger rate with $m_1$, rising by a factor of $3$ from $20\,\mathrm{M}_{\odot}$ to a peak around $34\,\mathrm{M}_{\odot}$, followed by a sharp, order-of-magnitude decline by $50\,\mathrm{M}_{\odot}$. This population also shows a weak preference for equal-mass mergers and has a $\chi_{\rm eff}$ distribution skewed toward positive values, with a median of zero excluded at approximately $90\%$ confidence. We find no significant $q-\chi_{\rm eff}$ correlation in the $35\, \mathrm{M}_{\odot}$ peak population, suggesting that lower-mass systems ($m_1<20\,\mathrm{M}_{\odot}$) likely drive the $q-\chi_{\rm eff}$ anti-correlation observed in the full BBH merger catalog. The redshift evolution of the merger rate is consistent with the cosmic star formation rate. We compare our findings with predictions from a wide range of formation channels. We find that common variants of the pair-instability supernova scenario, as well as hierarchical merger models, are incompatible with the observed features of the $35\,\mathrm{M}_{\odot}$ population. Ultimately, none of the formation channels we consider can explain all or even most of the features observed in this population. The ''mid-thirties'' of black hole mergers are in crisis.