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>DETECTION RATE ESTIMATES OF GRAVITY WAVES EMITTED DURING PARABOLIC ENCOUNTERS OF STELLAR BLACK HOLES IN GLOBULAR CLUSTERS
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DETECTION RATE ESTIMATES OF GRAVITY WAVES EMITTED DURING PARABOLIC ENCOUNTERS OF STELLAR BLACK HOLES IN GLOBULAR CLUSTERS
The rapid advance of gravitational wave (GW) detector facilities makes it very important to estimate the event rates of possible detection candidates. We consider an additional possibility of GW bursts produced during parabolic encounters (PEs) of stellar-mass compact objects in globular clusters (GCs). We estimate the rate of successful detections for specific detectors: the initial Laser Interferometric Gravitational-Wave Observatory (InLIGO), the French-Italian gravitational wave antenna VIRGO, the near-future Advanced-LIGO (AdLIGO), the space-based Laser Interferometric Space Antenna (LISA), and the Next Generation LISA (NGLISA). Simple GC models are constructed to account for the compact object mass function, mass segregation, number density distribution, and velocity distribution. We both calculate encounters classically and account for general relativistic corrections by extrapolating the results for infinite mass ratios. We also include the cosmological redshift of waveforms and event rates. We find that typical PEs with masses m_1 = m_2 = 40 solar mass are detectable with matched filtering over a signal-to-noise ratio S /N = 5 within a distance d_L ～ 200 Mpc for InLIGO and VIRGO, z = 1 for AdLIGO, 0.4 Mpc for LISA, and 1 Gpc for NGLISA. We estimate single data stream detection rates of 5.5 x 10~(-5) yr~(-1) for InLIGO, 7.2 x 10~(-5) yr~(-1) for VIRGO, 0.063 yr~(-1) for AdLIGO, 2.9 x 10~(-6) yr~(-1) for LISA, and 1.0 yr~(-1) for NGLISA, for reasonably conservative assumptions. These estimates are subject to uncertainties in the GC parameters, most importantly the total number and mass distribution of BHs in the cluster core. In reasonably optimistic cases, we get approx > 1 detection for AdLIGO per year. We expect that a coincident analysis using multiple detectors and accounting for GW recoil capture significantly increases the detection rates. The regular detection of GWs during PEs would provide a unique observational probe for constraining the stellar BH mass function of dense clusters.
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机译：重力波（GW）检测器设备的快速发展使得估算可能的检测候选者的事件发生率变得非常重要。我们认为球状星团（GC）中恒星质量致密物体的抛物线相遇（PE）产生GW爆发的另一种可能性。我们估算特定探测器的成功探测率：初始激光干涉重力波天文台（InLIGO），法国-意大利重力波天线VIRGO，近未来Advanced-LIGO（AdLIGO），空基激光干涉空间天线（LISA）和下一代LISA（NGLISA）。构建简单的GC模型以说明紧凑的对象质量函数，质量分离，数量密度分布和速度分布。我们都经典地计算相遇，并通过外推无限质量比的结果来说明广义相对论校正。我们还包括波形和事件发生率的宇宙学红移。我们发现，对于InLIGO和VIRGO，在信噪比S / N = 5内，对于质量为m_1 = m_2 = 40太阳质量的典型PE，可以在信噪比S / N = 5的情况下进行匹配滤波，对于InLIGO和VIRGO，z = 1，对于AdLIGO， LISA为0.4 Mpc，NGLIS为1 Gpc。我们估计InLIGO的单个数据流检测率分别为5.5 x 10〜（-5）yr〜（-1），VIRGO的7.2 x 10〜（-5）yr〜（-1），0.063 yr〜（-1） AdLIGO，对于LISA为2.9 x 10〜（-6）yr〜（-1），对于NGLISA为1.0 yr〜（-1）（出于合理的保守假设）。这些估计值受GC参数不确定性的影响，最重要的是，簇芯中BH的总数和质量分布不确定。在合理乐观的情况下，我们每年大约会检测到1次以上的AdLIGO。我们期望使用多个检测器并考虑到GW反冲捕获的同时分析可以显着提高检测率。在PE期间对GW的常规检测将为约束密集簇的恒星BH质量函数提供独特的观察探针。
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