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 modelling the sensitivities of current and future generations of gravitational wave detectors across the entire gravitational-wave spectrum of coalescing black-hole binaries. We provide methods to generate sensitivity curves for pulsar timing arrays (PTAs) using a novel realistic PTA sensitivity curve generator, space-based interferometers using adaptive models that can represent a wide range of proposed detector designs, and ground-based interferometers using realistic noise models that can reproduce current, second, and third generation designs, as well as novel variations of the essential design parameters. To model the signal from black-hole binaries at any mass scale, we use phenomenological waveforms capable of modelling the inspiral, merger, and ringdown for sources with varying mass ratios and spins. Using this adaptable framework, we produce signal-to-noise ratios for the combination of any modelled 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.

中文翻译：

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当前和未来探测器在黑洞二元引力波谱中的灵敏度

已知黑洞的质量至少跨越 9 个数量级：从激光干涉仪引力波天文台科学合作和处女座合作观测到的恒星质量物体，到像事件视界观测到的超大质量黑洞M87 核心的望远镜。无论质量大小如何，预计所有这些物体都会形成双星并最终发射可观测的引力辐射，而质量更大的物体会以更低的引力波频率发射。我们展示了工具 gwent，用于对当前和未来几代引力波探测器在合并黑洞双星的整个引力波谱中的灵敏度进行建模。我们提供了使用新颖的现实 PTA 灵敏度曲线发生器生成脉冲星定时阵列 (PTA) 灵敏度曲线的方法，使用自适应模型的天基干涉仪可以代表广泛的提议探测器设计，以及使用现实噪声模型的地面干涉仪可以再现当前、第二和第三代设计，以及基本设计参数的新变化。为了对来自任何质量尺度的黑洞双星的信号进行建模，我们使用了能够对具有不同质量比和自旋的源的内旋、合并和振铃进行建模的现象学波形。使用这种适应性强的框架，我们为与探测器或源相关的任何建模参数的组合生成信噪比。通过允许每个检测器和源参数的变化，我们可以确定最重要的因素，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。