Sensitivity of present and future detectors across the black-hole binary gravitational wave spectrum
Sensitivity of present and future detectors across the black-hole binary gravitational wave spectrum
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DOI：
10.1088/1361-6382/abd4f6
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发表时间：
2021-03
影响因子：
3.5
通讯作者：
A. Kaiser;S. McWilliams
中科院分区：
文献类型：
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作者：
A. Kaiser;S. McWilliams
已知黑洞的质量跨越至少 9 个数量级：从激光干涉仪引力波天文台科学合作组织和 Virgo 合作组织观测到的恒星质量天体，到 M87 中心事件视界望远镜观测到的超大质量黑洞。无论质量规模如何，所有这些物体都预计会形成双星并最终发射可观测到的引力辐射，质量更大的物体会以更低的引力波频率发射。我们推出了 gwent 工具，用于对当前和未来几代引力波探测器在聚结黑洞双星 (BHB) 整个引力波谱上的灵敏度进行建模。我们提供了使用新颖的真实 PTA 灵敏度曲线生成器（Hazboun、Romano 和 Smith 2019 Phys. Rev. D 100 104028）生成脉冲星定时阵列（PTA）灵敏度曲线的方法，使用可以代表各种拟议探测器设计的自适应模型的天基干涉仪（Amaro-Seoane 等人 2017 arXiv:1702.00786）以及地面干涉仪 使用可以再现电流的真实噪声模型的干涉仪（Abbott 等人 2016 Phys. Rev. Lett. 116 061102）、第二代和第三代设计（Hild 等人 2011 Class. Quantum Grav. 28 094013）以及基本设计参数的新颖变体。为了对任何质量尺度的 BHB 信号进行建模，我们使用唯象波形，能够对具有不同质量比和自旋的源的吸气、合并和振铃进行建模（Khan 等人 2016 Phys. Rev. D 93 044007；Husa 等人 2016 Phys. Rev. D 93 044006）。使用这种适应性强的框架，我们可以为与探测器或源相关的任何建模参数的组合生成信噪比 (SNR)。通过允许每个探测器和源参数的变化，我们可以查明最重要的因素，以确定特定仪器设计的最佳性能。我们的探测器和信号模型的适应性可以轻松扩展到新的探测器设计和其他引力波信号模型。
Black-holes are known to span at least 9 orders of magnitude in mass: from the stellar-mass objects observed by the Laser Interferometer Gravitational-Wave Observatory Scientific Collaboration and Virgo Collaboration, to supermassive black-holes like the one observed by the Event Horizon Telescope at the heart of M87. Regardless of the mass scale, all of these objects are expected to form binaries and eventually emit observable gravitational radiation, with more massive objects emitting at ever lower gravitational-wave frequencies. We present the tool, gwent, for modeling the sensitivities of current and future generations of gravitational wave detectors across the entire gravitational-wave spectrum of coalescing black-hole binaries (BHBs). We provide methods to generate sensitivity curves for pulsar timing arrays (PTAs) using a novel realistic PTA sensitivity curve generator (Hazboun, Romano and Smith 2019 Phys. Rev. D 100 104028), space-based interferometers using adaptive models that can represent a wide range of proposed detector designs (Amaro-Seoane et al 2017 arXiv:1702.00786), and ground-based interferometers using realistic noise models that can reproduce current (Abbott et al 2016 Phys. Rev. Lett. 116 061102), second, and third generation designs (Hild et al 2011 Class. Quantum Grav. 28 094013), as well as novel variations of the essential design parameters. To model the signal from BHBs at any mass scale, we use phenomenological waveforms capable of modeling the inspiral, merger, and ringdown for sources with varying mass ratios and spins (Khan et al 2016 Phys. Rev. D 93 044007; Husa et al 2016 Phys. Rev. D 93 044006). Using this adaptable framework, we produce signal-to-noise ratios (SNR) for the combination of any modeled parameter, associated with either the detector or the source. By allowing variation across each detector and source parameter, we can pinpoint the most important factors to determining the optimal performance for particular instrument designs. The adaptability of our detector and signal models can easily be extended to new detector designs and other models of gravitational wave signals.