引力波携带超出有效自旋参数的信息，但难以提取
Gravitational waves carry information beyond effective spin parameters but it is hard to extract
AI总结：
本研究针对引力波观测中自旋信息维度缩减的问题，通过模拟三类同有效自旋分布、不同自旋大小与倾角分布的天体物理族群并开展参数估计，发现现有模型可定性区分族群，但准确恢复分布和诊断模型误设偏差仍具挑战。
摘要：
双黑洞并合的引力波观测通过双星自旋（即每个组成黑洞的自旋大小和方向，共由六个自由度描述）来探究其天体物理起源。然而，发出的信号主要取决于两个有效自旋参数，这些参数将自旋自由度凝聚为与轨道平面平行和垂直的两类。鉴于物理相关问题与通常可测量量之间存在这种维度缩减，我们重新探讨了以下问题：能否通过引力波观测成功恢复组成黑洞自旋大小和方向的信息，还是我们只是在推断有效自旋参数分布的信息。为此，我们模拟了三个具有相同底层有效自旋分布但自旋大小和倾角分布不同的天体物理族群，并在其上开展完整的单事件和族群层面的参数估计。我们发现，在当前灵敏度下，参数化族群模型确实能够定性区分具有不同自旋大小和倾角分布的族群。然而，无论是准确恢复真实分布，还是诊断由模型误设导致的偏差，仍然具有挑战性。我们将前者归因于处理高维后验分布的实际困难，将后者归因于每个单事件携带的关于全部六个自旋自由度的信息极少这一事实。
英文摘要：
Gravitational wave observations of binary black hole mergers probe their astrophysical origins via the binary spin, namely the spin magnitudes and directions of each component black hole, together described by six degrees of freedom. However, the emitted signals primarily depend on two effective spin parameters that condense the spin degrees of freedom to those parallel and those perpendicular to the orbital plane. Given this reduction in dimensionality between the physically relevant problem and what is typically measurable, we revisit the question of whether information about the component spin magnitudes and directions can successfully be recovered via gravitational-wave observations, or if we simply extrapolate information about the distributions of effective spin parameters. To this end, we simulate three astrophysical populations with the same underlying effective-spin distribution but different spin magnitude and tilt distributions, on which we conduct full individual-event and population-level parameter estimation. We find that parameterized population models can indeed qualitatively distinguish between populations with different spin magnitude and tilt distributions at current sensitivity. However, it remains challenging to either accurately recover the true distribution or to diagnose biases due to model misspecification. We attribute the former to practical challenges of dealing with high-dimensional posterior distributions, and the latter to the fact that each individual event carries very little information about the full six spin degrees of freedom.
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