A stochastic search for intermittent gravitational-wave backgrounds
A stochastic search for intermittent gravitational-wave backgrounds
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DOI：
10.1103/physrevd.107.103026
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发表时间：
2023-01
影响因子：
5
通讯作者：
J. Lawrence;K. Turbang;A. Matas;A. Renzini;N. van Remortel;J. Romano
中科院分区：
文献类型：
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作者：
J. Lawrence;K. Turbang;A. Matas;A. Renzini;N. van Remortel;J. Romano
高级LIGO、Virgo和KAGRA探测器频带中的引力波背景（GWB）的一个可能来源是整个宇宙中无法分辨的恒星质量双星黑洞（BBH）合并的信号叠加。由于BBH合并带（$\sim\！1~{\rm s}$）比相邻合并之间的预期间隔（$\sim\！10^3~{\rm s}$）时，观察到的信号将是“爆米花状“或间歇的，占空比为10 ^{-3}$。然而，目前由LIGO-Virgo-KAGRA合作进行的随机GWB的标准互相关搜索是基于连续高斯信号模型，该模型没有考虑背景的间歇性。后者更好地描述了高斯混合模型，其中包括一个占空比参数，量化的程度的磁阻。基于Drasco和Flanagan的早期论文，我们提出了一种基于随机信号的间歇性GWB搜索。对于这样的信号，这种搜索比标准的连续互相关搜索执行得更好。我们目前的结果，我们的随机信号为基础的方法间歇GWB适用于模拟数据的一些简单的模型，并比较其性能的其他搜索方法，无论是在检测和信号表征。对更真实的模拟数据集进行额外测试，例如，由天体物理学激发的BBH合并信号注入到有色检测器噪声包含噪声瞬态，将需要在此方法可以应用于真实的引力波数据的信心。
A likely source of a gravitational-wave background (GWB) in the frequency band of the Advanced LIGO, Virgo and KAGRA detectors is the superposition of signals from the population of unresolvable stellar-mass binary-black-hole (BBH) mergers throughout the Universe. Since the duration of a BBH merger in band ($\sim\!1~{\rm s}$) is much shorter than the expected separation between neighboring mergers ($\sim\!10^3~{\rm s}$), the observed signal will be"popcorn-like"or intermittent with duty cycles of order $10^{-3}$. However, the standard cross-correlation search for stochastic GWBs currently performed by the LIGO-Virgo-KAGRA collaboration is based on a continuous-Gaussian signal model, which does not take into account the intermittent nature of the background. The latter is better described by a Gaussian mixture-model, which includes a duty cycle parameter that quantifies the degree of intermittence. Building on an earlier paper by Drasco and Flanagan, we propose a stochastic-signal-based search for intermittent GWBs. For such signals, this search performs better than the standard continuous cross-correlation search. We present results of our stochastic-signal-based approach for intermittent GWBs applied to simulated data for some simple models, and compare its performance to the other search methods, both in terms of detection and signal characterization. Additional testing on more realistic simulated data sets, e.g., consisting of astrophysically-motivated BBH merger signals injected into colored detector noise containing noise transients, will be needed before this method can be applied with confidence on real gravitational-wave data.