高级检测器时代通过GRB触发的检索检测GW吸气的展望
Outlook for detection of GW inspirals by GRB-triggered searches in the Advanced detector era
摘要：
短而硬的伽马射线暴（GRB）被认为起源于两颗中子星（NS）或一颗中子星和一个黑洞（BH）的合并。如果这种情况是正确的，那么短伽马射线暴将伴随着强引力波（GW）的发射，可以被LIGO，Virgo，KAGRA和LIGO-India等GW天文台检测到。与全天候、全天时的GW搜索相比，外部触发的GW搜索具有时间和天空位置已知、GW幅度增大等优点。基于最近的联合LIGO-Virgo数据，我们的分析估计，和我们的蒙特卡罗模拟候选紧凑的二进制合并事件的信噪比的分布，我们找到了一个有效的敏感体积GRB触发的搜索，是约2倍以上的全天空，所有的时间搜索。对于NS-NS系统，喷流角为20度，伽马射线卫星视场为天空的10%，并且具有通常旋进的自旋，这使NS-NS短GRB和NS-BH短GRB关联的数量增加了一倍，达到NS-NS和NS-BH所有检测的3-4%。我们还调查的权力测试统计过剩的阈下事件列表中，并表明，这些是不太可能揭示一个阈下人口，直到发现GW协会短伽玛暴已经是例行的。最后，我们提供了有用的公式计算GW振幅的先验分布，从一个紧凑的二进制合并，对于一个给定的GW探测器网络和给定的天空位置。
英文摘要：
Short, hard gamma-ray bursts (GRBs) are believed to originate from the coalescence of two neutron stars (NSs) or a NS and a black hole (BH). If this scenario is correct, then short GRBs will be accompanied by the emission of strong gravitational waves (GWs), detectable by GW observatories such as LIGO, Virgo, KAGRA, and LIGO-India. As compared with blind, all-sky, all-time GW searches, externally triggered searches for GW counterparts to short GRBs have the advantages of both significantly reduced detection threshold due to known time and sky location and enhanced GW amplitude because of face-on orientation. Based on the distribution of signal-to-noise ratios in candidate compact binary coalescence events in the most recent joint LIGO-Virgo data, our analytic estimates, and our Monte Carlo simulations, we find an effective sensitive volume for GRB-triggered searches that is about 2 times greater than for an all-sky, all-time search. For NS-NS systems, a jet angle of 20 degrees, a gamma-ray satellite field of view of 10% of the sky, and priors with generally precessing spin, this doubles the number of NS-NS short-GRB and NS-BH short-GRB associations, to ~3-4% of all detections of NS-NSs and NS-BHs. We also investigate the power of tests for statistical excesses in lists of subthreshold events, and show that these are unlikely to reveal a subthreshold population until finding GW associations to short GRBs is already routine. Finally, we provide useful formulas for calculating the prior distribution of GW amplitudes from a compact binary coalescence, for a given GW detector network and given sky location.
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