本文提出了一種基於迭代密度估計的新方法,用於從重力波觀測中重建合併黑洞雙星的質量分佈,發現雙星質量比並不如先前研究所認為的那樣傾向於接近相等,且質量比分佈會隨著主星質量的變化而改變。
This research introduces a novel iterative density estimation method to accurately reconstruct the mass distribution of merging black hole binaries from gravitational wave observations, revealing a weaker preference for near-equal mass binaries than previously thought and suggesting a more complex relationship between primary and secondary black hole masses.