arXiv 2408.040642024-08astro-ph.HEgr-qc

长伽马射线暴是并合双黑洞的前身天体吗？

Are long gamma-ray bursts progenitors to merging binary black holes?

Tom Y. Wu, Maya Fishbach

备注：: 8 pages, 4 figures. Matches version accepted by ApJ
发表信息：: The Astrophysical Journal, Volume 977, Number 2 (2024)
DOI：: 10.3847/1538-4357/ad98ed

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AI总结：

本文用长伽马射线暴发生率替代恒星形成率，推断其与双黑洞并合之间的延迟时间分布，发现幂律斜率约为-0.96，支持LGRB追踪BBH前身形成，但仅至多约4%的LGRB能演化为并合双黑洞。

摘要：

双黑洞（BBH）前身天体形成与其引力波（GW）并合之间的延迟时间分布，为了解其未知的形成历史提供了重要线索。在推断延迟时间分布时，通常假设BBH前身天体的形成率跟随恒星形成率（SFR）。本工作不采用恒星形成率，而是考虑长伽马射线暴（LGRB）的发生率。LGRB被认为对应于（可能自旋的）黑洞的形成，因此可能与BBH前身天体群体相关。通过比较Ghirlanda & Salvaterra（2022）推断的LGRB发生率随红移的演化与LIGO-Virgo-KAGRA（LVK）观测推断的BBH并合率，我们发现LGRB与BBH并合之间的延迟时间分布可以用幂律很好地描述，其最小延迟时间为$10$ Myr，斜率$α={-0.96}^{+0.64}_{-0.76}$（90%置信度）。这与BBH延迟时间分布的理论预期相符，从而支持了LGRB追踪BBH前身天体形成的假说。然而，比较这两个群体的绝对发生率，我们发现至多只有$f = {4}^{+10}_{-2}\\%$的LGRB可能演化为并合BBH。我们还考虑了LGRB仅产生具有较大顺向自旋（有效旋进自旋$χ_\mathrm{eff} > 0.2$）的BBH系统的可能性。在这种情况下，我们发现$f = 0.3^{+1.0}_{-0.2}\\%$，且延迟时间分布倾向于我们所考虑的最陡的幂律斜率（$α= -2$）。我们认为，LGRB与GW的异步观测为研究宇宙历史中黑洞生命周期的多信使探测提供了有力手段。

英文摘要：

The distribution of delay times between the formation of binary black hole (BBH) progenitors and their gravitational-wave (GW) merger provides important clues about their unknown formation histories. When inferring the delay time distribution, it is typically assumed that BBH progenitor formation traces the star formation rate (SFR). In this work, we consider the rate of long gamma-ray bursts (LGRBs) instead of the SFR. LGRBs are thought to correspond to the formation of (possibly spinning) black holes, and may therefore be related to the BBH progenitor population. By comparing the redshift evolution of the LGRB rate as inferred by Ghirlanda & Salvaterra (2022) and the BBH merger rate inferred by LIGO-Virgo-KAGRA (LVK) observations, we find that the delay time distribution between LGRBs and BBH mergers is well-described by a power law with minimum delay time $10$ Myr and slope $α={-0.96}^{+0.64}_{-0.76}$ (90% credibility). This matches theoretical expectations for the BBH delay time distribution, which in turn lends support to the hypothesis that LGRBs trace BBH progenitor formation. However, comparing the absolute rates of these two populations, we find that at most $f = {4}^{+10}_{-2}\%$ of LGRBs may evolve into merging BBH. We also consider the possibility that LGRBs only produce BBH systems with large aligned spins (with effective inspiral spin $χ_\mathrm{eff} > 0.2$). In this case, we find $f = 0.3^{+1.0}_{-0.2}\%$ and the delay time distribution favors the steepest power-law slopes we consider ($α= -2$). We argue that asynchronous observations of LGRBs and GWs provide a powerful multimessenger probe of black hole lifecycles across cosmic history.

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