Subtracting compact binary foregrounds to search for subdominant gravitational-wave backgrounds in next-generation ground-based observatories
Subtracting compact binary foregrounds to search for subdominant gravitational-wave backgrounds in next-generation ground-based observatories
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DOI：
10.1103/physrevd.108.064040
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发表时间：
2022-09
影响因子：
5
通讯作者：
Bei Zhou;L. Reali;E. Berti;Mesut Çalışkan;Cyril Creque-Sarbinowski;M. Kamionkowski;B. Sathyaprakash
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文献类型：
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作者：
Bei Zhou;L. Reali;E. Berti;Mesut Çalışkan;Cyril Creque-Sarbinowski;M. Kamionkowski;B. Sathyaprakash
随机引力波背景（SGWB）源自许多单独未解析的引力波（GW）信号的叠加。探测SGWB为我们提供了有关天体物理学、宇宙学和基础物理学的宝贵信息。在本文中，我们研究了下一代地面引力波天文台（宇宙探索者和爱因斯坦望远镜）网络中双星黑洞（BBH）和双中子星（BNS）聚结的SGWB，并确定了它们的测量效果；这就限制了我们观察其他次要的天体物理和宇宙学SGWB的能力。我们模拟全宇宙的 BBH 和 BNS 群体，并计算相应的 SGWB，其中包括 (i) 未检测到的信号和 (ii) 不完美去除已解析源的残留背景的叠加。两个分量的总和设定了观测其他SGWB的灵敏度。我们的结果表明，即使使用下一代天文台，残留背景也很大，限制了对其他SGWB的敏感性。对残余背景的主要贡献来自于推断检测到的信号的聚结相位和光度距离的不确定性。需要探索信号减法的替代方法，以尽量减少 BBH 和 BNS 前景，以便从其他次要的天体物理和宇宙学来源观察 SGWB。
Stochastic gravitational-wave backgrounds (SGWBs) derive from the superposition of numerous individually unresolved gravitational-wave (GW) signals. Detecting SGWBs provides us with invaluable information about astrophysics, cosmology, and fundamental physics. In this paper, we study SGWBs from binary black-hole (BBH) and binary neutron-star (BNS) coalescences in a network of next-generation ground-based GW observatories (Cosmic Explorer and Einstein Telescope) and determine how well they can be measured; this then limits how well we can observe other subdominant astrophysical and cosmological SGWBs. We simulate all-Universe populations of BBHs and BNSs and calculate the corresponding SGWBs, which consist of a superposition of (i) undetected signals, and (ii) the residual background from imperfect removal of resolved sources. The sum of the two components sets the sensitivity for observing other SGWBs. Our results show that, even with next-generation observatories, the residual background is large and limits the sensitivity to other SGWBs. The main contributions to the residual background arise from uncertainties in inferring the coalescence phase and luminosity distance of the detected signals. Alternative approaches to signal subtraction would need to be explored to minimize the BBH and BNS foreground in order to observe SGWBs from other subdominant astrophysical and cosmological sources.