Population of Merging Compact Binaries Inferred Using Gravitational Waves through GWTC-3
Population of Merging Compact Binaries Inferred Using Gravitational Waves through GWTC-3
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DOI：
10.1103/physrevx.13.011048
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发表时间：
2021-11
影响因子：
12.5
通讯作者：
The Ligo Scientific Collaboration;The Virgo Collaboration;T. Abbott;T. Abbott;F. Acernese;K. Ackley
中科院分区：
文献类型：
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作者：
The Ligo Scientific Collaboration;The Virgo Collaboration;T. Abbott;T. Abbott;F. Acernese;K. Ackley
我们报告了通过GWTC - 3以每年低于1次误报率探测到的76个紧凑双星并合的总体性质。该目录包含三类双星并合：双黑洞（BBH）、双中子星（BNS）和中子星 - 黑洞（NSBH）并合。我们推断双中子星并合率在10 ${\rm{Gpc^{-3} yr^{-1}}}$到1700 ${\rm{Gpc^{-3} yr^{-1}}}$之间，中子星 - 黑洞并合率在7.8 ${\rm{Gpc^{-3}\, yr^{-1}}}$到140 ${\rm{Gpc^{-3} yr^{-1}}}$之间，这里假设速率密度相对于共动体积是常数，并取本工作中所用方法的90%置信区间的并集。考虑到双黑洞并合率随红移演化，我们发现在一个基准红移（z = 0.2）处，双黑洞并合率在17.9 ${\rm{Gpc^{-3}\, yr^{-1}}}$到44 ${\rm{Gpc^{-3}\, yr^{-1}}}$之间。我们得到了一个广泛的中子星质量分布，其范围从$1.2^{+0.1}_{-0.2} M_\odot$到$2.0^{+0.3}_{-0.3} M_\odot$。我们能够确定地识别出在类中子星质量和类黑洞质量之间，并合率相对于组分质量的快速下降，但没有证据表明并合率在10 $M_\odot$之前再次上升。我们还发现双黑洞质量分布相对于幂律分布存在局部的过密和欠密区域。虽然我们继续发现双星中较大质量组分的质量分布作为主质量的函数强烈下降，但我们没有观察到在约60 $M_\odot$以上并合率被强烈抑制的证据。观测到双黑洞并合率随红移以与$(1 + z)^{\kappa}$成正比的速率增加，对于$z\lesssim 1$，$\kappa = 2.9^{+1.7}_{-1.8}$。观测到的黑洞自旋较小，一半的自旋大小低于$\chi_i \simeq 0.25$。我们在总体中观察到负对齐自旋的证据，并且对于质量比更不相等的系统，自旋大小增加。
We report on the population properties of 76 compact binary mergers detected with gravitational waves below a false alarm rate of 1 per year through GWTC-3. The catalog contains three classes of binary mergers: BBH, BNS, and NSBH mergers. We infer the BNS merger rate to be between 10 $\rm{Gpc^{-3} yr^{-1}}$ and 1700 $\rm{Gpc^{-3} yr^{-1}}$ and the NSBH merger rate to be between 7.8 $\rm{Gpc^{-3}\, yr^{-1}}$ and 140 $\rm{Gpc^{-3} yr^{-1}}$ , assuming a constant rate density versus comoving volume and taking the union of 90% credible intervals for methods used in this work. Accounting for the BBH merger rate to evolve with redshift, we find the BBH merger rate to be between 17.9 $\rm{Gpc^{-3}\, yr^{-1}}$ and 44 $\rm{Gpc^{-3}\, yr^{-1}}$ at a fiducial redshift (z=0.2). We obtain a broad neutron star mass distribution extending from $1.2^{+0.1}_{-0.2} M_\odot$ to $2.0^{+0.3}_{-0.3} M_\odot$. We can confidently identify a rapid decrease in merger rate versus component mass between neutron star-like masses and black-hole-like masses, but there is no evidence that the merger rate increases again before 10 $M_\odot$. We also find the BBH mass distribution has localized over- and under-densities relative to a power law distribution. While we continue to find the mass distribution of a binary's more massive component strongly decreases as a function of primary mass, we observe no evidence of a strongly suppressed merger rate above $\sim 60 M_\odot$. The rate of BBH mergers is observed to increase with redshift at a rate proportional to $(1+z)^{\kappa}$ with $\kappa = 2.9^{+1.7}_{-1.8}$ for $z\lesssim 1$. Observed black hole spins are small, with half of spin magnitudes below $\chi_i \simeq 0.25$. We observe evidence of negative aligned spins in the population, and an increase in spin magnitude for systems with more unequal mass ratio.