arXiv 2510.063522025-10astro-ph.HEastro-ph.CO

LIGO-Virgo-KAGRA探测到的所有双黑洞都遵循统一的时间延迟分布吗？可能不是

Are all Binary Black Holes Detected by LIGO-Virgo-KAGRA Following the Universal Time-Delay Distributions? Probably Not

Tata Institute of Fundamental Research（塔塔基础研究所）；Indian Institute of Technology Bombay（印度理工学院孟买分校）

Samsuzzaman Afroz, Navdha, Suvodip Mukherjee

备注：: 15 + 5 (references and appendix) Pages, 5 + 3 (appendix) figures

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AI总结：

该研究利用GWTC-4星表的双黑洞，采用基于网格的非参数框架重建时间延迟分布，发现双黑洞并合的时间延迟分布存在质量依赖特征，单一幂律无法同时描述两个质量区间的分布。

摘要：

双黑洞（BBH）并合的时间延迟分布（DTD）编码了恒星形成历史与引力波（GW）辐射之间的演化联系。我们利用来自GWTC-4星表的双黑洞，采用避免限制性幂律假设的基于网格的框架，对DTD进行非参数重建。我们将双黑洞群体划分为20-40倍太阳质量和40-100倍太阳质量两个质量区间，在三种不同的恒星形成率密度（SFRD）模型下，使用基于网格的轨迹分别重建每个区间的DTD。我们发现，两个质量区间均倾向于中等至长延迟时间的延展平台，而非单一特征时标，且两个区间的重建并合率ℛ(z)均从本地值上升，在中等红移处达到峰值后下降。两个区间的差异是程度上的而非本质上的：20-40倍太阳质量区间的约束较宽泛，本地率R₀约为18-23 Gpc⁻³·yr⁻¹，在z≈0.8-1.05处达到并合率峰值；而40-100倍太阳质量区间偏好更清晰的约2-4 Gyr的中等延迟范围，对长延迟时间的抑制更剧烈，处于证据明显更严格的轨迹集合中，本地率R₀约为9-13 Gpc⁻³·yr⁻¹，且峰值向稍高红移z≈1.0-1.05偏移。结果表明，单一幂律DTD可能不足以同时描述两个质量区间，这指向可能存在与质量相关的双黑洞演化路径，需要用更大的引力波星表进一步研究。

英文摘要：

The delay time distribution (DTD) of binary black hole (BBH) mergers encodes the evolutionary link between stellar formation history and gravitational-wave (GW) emission. We present a non-parametric reconstruction of the DTD using BBHs from the GWTC-4 catalog, employing a grid-based framework that avoids restrictive power-law assumptions. We divide the BBH population into two mass bins, $20$--$40\,M_\odot$ and $40$--$100\,M_\odot$, and reconstruct the DTD independently for each bin using grid-based trajectories, under three different star formation rate density (SFRD) models. We find that both mass bins favor an extended plateau of intermediate-to-long delay times rather than a single characteristic timescale, and that in both bins the reconstructed merger rate $\mathcal{R}(z)$ rises from its local value to a peak at intermediate redshift before declining. The two bins differ in degree rather than kind: the $20$--$40\,M_\odot$ bin is broadly constrained, with a local rate of $R_0 \approx 18$--$23\,\mathrm{Gpc^{-3}\,yr^{-1}}$ and a merger rate peaking at $z \sim 0.8$--$1.05$, while the $40$--$100\,M_\odot$ bin prefers a more sharply defined intermediate delay range of $\sim$2--4 Gyr with a steeper suppression of long delay times, within a noticeably tighter set of high-evidence trajectories, a lower local rate of $R_0 \approx 9$--$13\,\mathrm{Gpc^{-3}\,yr^{-1}}$, and a peak shifted to slightly higher redshift, $z \sim 1.0$--$1.05$. The results indicate that a single power-law DTD may not be sufficient to simultaneously describe both mass bins, pointing toward possible mass-dependent binary evolution pathways that merit further investigation with larger GW catalogs.

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