与紧凑双星聚合相关的伽马射线暴的速率和射束角

Shasvath J. Kapadia, Dimple, Dhruv Jain, Kuntal Misra, K. G. Arun and Resmi Lekshmi
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摘要

据认为,双中子星(BNS)凝聚和一部分中子星-黑洞(NSBH)合并,即使不是全部,也会产生足够的质量抛射,为伽马射线暴(GRBs)提供能量。然而,这一比例以及与BNS相关的伽玛射线暴的射束角分布都很难从观测中得到证实。最近的工作应用机器学习工具分析了费米/伽玛射线暴监测仪(GBM)和斯威夫特/爆发警报望远镜(BAT)观测到的伽玛射线暴光变曲线。GRB被分为多个不同的星团,其中一个星团(BNS星团)可能与BNS有关,而另一个星团(NSBH星团)可能与NSBH有关。作为一个原理证明,假设费米/GBM 和斯威夫特/BAT 探测到的所有与 BNSs(NSBHs)相关的 GRBs 都位于 BNS(NSBH)星团中,我们估算了它们的速率(Gpc-3 yr-1)。我们将这些速率与LIGO-Virgo-KAGRA(LVK)合作组织在前三次观测运行(O1、O2、O3)中估算的相应BNS和NSBH速率进行比较。我们发现,假定束流分数分布均匀(fb∈ [0.01, 0.1]),BNS速率与LVK的速率估计值一致。反过来,使用 LVK 的 BNS 率估计值,假设所有 BNS 合并都产生了 GRB,我们就能以 90% 的置信度将束角分布限制在 θj∈ [0.°8, 33.°5] 。同样,我们利用费米/GBM(斯威夫特/BAT)数据将GRB-bright NSBHs的比例限制为fB∈[1.3%, 63%](fB∈[0.4%, 15%])。
本文章由计算机程序翻译,如有差异,请以英文原文为准。
Rates and Beaming Angles of Gamma-Ray Bursts Associated with Compact Binary Coalescences
Some, if not all, binary neutron star (BNS) coalescences, and a fraction of neutron star–black hole (NSBH) mergers, are thought to produce sufficient mass ejection to power gamma-ray bursts (GRBs). However, this fraction, as well as the distribution of beaming angles of BNS-associated GRBs, is poorly constrained from observation. Recent work applied machine learning tools to analyze GRB light curves observed by Fermi/Gamma-Ray Burst Monitor (GBM) and Swift/Burst Alert Telescope (BAT). GRBs were segregated into multiple distinct clusters, with the tantalizing possibility that one of them (BNS cluster) could be associated with BNSs and another (NSBH cluster) with NSBHs. As a proof of principle, assuming that all GRBs detected by Fermi/GBM and Swift/BAT associated with BNSs (NSBHs) lie in the BNS (NSBH) cluster, we estimate their rates (Gpc−3 yr−1). We compare these rates with corresponding BNS and NSBH rates estimated by the LIGO–Virgo–KAGRA (LVK) collaboration from the first three observing runs (O1, O2, O3). We find that the BNS rates are consistent with LVK’s rate estimates, assuming a uniform distribution of beaming fractions (fb ∈ [0.01, 0.1]). Conversely, using the LVK’s BNS rate estimates, assuming all BNS mergers produce GRBs, we are able to constrain the beaming angle distribution to θj ∈ [0.°8, 33.°5] at 90% confidence. We similarly place limits on the fraction of GRB-bright NSBHs as fB ∈ [1.3%, 63%] (fB ∈ [0.4%, 15%]) with Fermi/GBM (Swift/BAT) data.
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