发表机构
Research Center for the Early Universe (RESCEU), Graduate School of Science, The University of Tokyo; TAPIR, California Institute of Technology; Graduate School of Science, The University of Tokyo; Department of Physics, Graduate School of Science, Chiba University（东京大学理学研究系早期宇宙研究中心; 加州理工学院 TAPIR; 东京大学理学研究系; 千叶大学理学研究系物理学科）
机构由 AI 辅助整理，请以论文原文为准。AI 中文总结
该研究利用星系成团性，构建引力波定位区域内的寄主星系类型似然，推断双黑洞并合事件的寄主星系种群占比，预测第三代探测器时代前可实现相关推断。
AI 中文摘要
星系成团性编码了双黑洞（BBH）并合事件寄主星系的信息，即便单个寄主星系仍未被识别，因为邻近星系的分布在统计上依赖于寄主星系总体。我们在引力波定位区域内，基于寄主星系条件下的星系计数分布构建事件级别的寄主星系类型似然，并将其结合以推断不同星系种群所寄主的BBH并合事件占比。该框架适用于常见和稀有的星系种群，无需预设形成效率或并合延迟时间分布。利用已测量的恒星形成星系和宁静星系的成团性，假设所有并合事件均发生在宁静星系中的理想化一年预测，对O5、后O5及第三代探测器网络，宁静寄主星系占比的单侧90%后验可信下限中位数分别为0.19、0.48和0.92。这些预测展示了在第三代探测器时代之前开展寄主星系种群推断的潜力。
英文摘要
Galaxy clustering encodes information about the host galaxies of binary black hole (BBH) mergers even when individual hosts remain unidentified, because the distribution of neighboring galaxies depends statistically on the host-galaxy population. We construct event-level host-type likelihoods from host-conditioned galaxy-count distributions within gravitational-wave localization regions and combine them to infer the fractions of BBH mergers hosted by different galaxy populations. The framework applies to common and rare galaxy populations without prescribing formation efficiencies or merger delay-time distributions. Using measured star-forming and quenched galaxy clustering, idealized one-year forecasts assuming all mergers occur in quenched galaxies yield median one-sided 90% lower credible limits of 0.19, 0.48, and 0.92 on the quenched-host fraction for O5, post-O5, and third-generation networks. These forecasts illustrate the potential for host-galaxy population inference before the third-generation detector era.
Comments10 pages, 4 figures
