论文标题
新灯中的二进制黑洞人口和宇宙学：PISN质量和地层频道的签名
Binary black holes population and cosmology in new lights: Signature of PISN mass and formation channel in GWTC-3
论文作者
论文摘要
二进制黑洞（BBHS）跨宇宙红移的质量，自旋和合并速率分布提供了一种独特的方式，可以在其地层通道上发光。随着BBH合并速率的红移依赖性，BBH的质量分布还可以表现出由于不同的形成通道以及对父恒星金属性的依赖而导致的红移依赖性。我们探索了BBH质量分布的红移依赖性，并从Ligo-Virgo-Kagra协作的第三个重力波（GW）目录GWTC-3共同演变。我们研究了BBHS质谱中的峰状特征与与超新星物理学和时间延迟分布有关的过程之间的可能连接。我们偏爱恒星形成和BBH合并之间的短期延迟。使用电源定律表格用于时间延迟分布（$（t^{\ rm min} _d）^{d} $），我们找到$ d <-0.7 $可信，$ 90 \％$ $ interval。 BBHS {可以拟合的质量分布，并带有{红移依赖性峰值功能，可以将其链接到该对恒星金属$ z _*$的对配对不稳定性超级novae（pisn）质量尺度$ m _ {\ rm pisn}（z _*）$。对于恒星金属性的基准价值$ z _*= 10^{ - 4} $，我们找到了$ \ rm m _ {\ rm pisn}（z _*）= 44.4^{+7.9} _ {+7.9} _ { - 6.3} $ $ \ $ \ $ \ rm m_ \ odot $。规模和与以前的分析不同。尽管我们发现PISN值对金属性有很强的依赖性，但是我们探索的模型并不高于那些不考虑金属性的模型，因为贝叶斯因素尚无定论。将来有了更多的数据，PISN的金属性依赖性的证据将对我们对恒星物理学的理解产生重大影响。
The mass, spin, and merger rate distribution of the binary black holes (BBHs) across cosmic redshifts provide a unique way to shed light on their formation channel. Along with the redshift dependence of the BBH merger rate, the mass distribution of BBHs can also exhibit redshift dependence due to different formation channels and dependence on the metallicity of the parent stars. We explore the redshift dependence of the BBH mass distribution jointly with the merger rate evolution from the third gravitational wave (GW) catalog GWTC-3 of the LIGO-Virgo-KAGRA collaboration. We study possible connections between peak-like features in the mass spectrum of BBHs and processes related to supernovae physics and time-delay distributions. We obtain a preference for short-time delays between star formation and BBH mergers. Using a power law form for the time delay distribution ($(t^{\rm min}_d)^{d}$) we find $d<-0.7$ credible at $90\%$ interval. The mass distribution of the BBHs {could be fitted} with a power-law form with {a redshift-dependent peak feature that can be linked to the pair instability supernovae (PISN) mass scale $M_{\rm PISN}(Z_*)$ at a stellar metallicity $Z_*$. For a fiducial value of the stellar metallicity $Z_*= 10^{-4}$, we find the $\rm M_{\rm PISN}(Z_*)=44.4^{+7.9}_{-6.3} $ $\rm M_\odot$.} This is in accordance with the theoretical prediction of the lower edge of the PISN mass scale and differs from previous analyses. Although we find a strong dependence of the PISN value on metallicity, the model that we explored is not strongly favored over those that do not account for metallicity as the Bayes factors are inconclusive. In the future with more data, evidence towards metallicity dependence of the PISN will have a significant impact on our understanding of stellar physics.
