Subtracting compact binary foreground sources to reveal primordial gravitational-wave backgrounds
Subtracting compact binary foreground sources to reveal primordial gravitational-wave backgrounds
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DOI：
10.1103/physrevd.102.024051
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发表时间：
2020-02
影响因子：
5
通讯作者：
S. Sachdev;T. Regimbau;B. Sathyaprakash
中科院分区：
文献类型：
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作者：
S. Sachdev;T. Regimbau;B. Sathyaprakash
探测早期宇宙相变期间产生的原始引力波背景是未来地面探测器的一个关键科学目标。致密双星合并的速率是如此之大，以至于它们的宇宙学人口产生了一种混乱的背景，可能掩盖了潜在的原始随机背景的检测。在本文中，我们研究了当前和未来的检测器，以解决混乱的背景，揭示有趣的原始背景的能力。目前的LIGO和Virgo探测器网络以及即将到来的KAGRA和LIGO-India探测器网络将无法分辨宇宙学紧凑双星源群，其对随机背景的敏感性将受到这些源的混乱背景的限制。我们发现，由宇宙探测器和爱因斯坦望远镜的三个（和五个）第三代（3G）探测器组成的网络可以分辨出双星黑洞产生的混乱背景，只剩下约0.013%（分别为0.00075%）的未分辨，而高达25%（分别为7.7%）的双星中子星星源仍然未分辨。因此，双黑洞人口可能不会限制原始背景的观测，但双中子星星人口将限制3G探测器的灵敏度为10 Hz时的$\Omega_{\rm GW} \sim 10^{-11}$（分别为$\Omega_{\rm GW} \sim 3\times 10^{-12}$）。
Detection of primordial gravitational-wave backgrounds generated during the early universe phase transitions is a key science goal for future ground-based detectors. The rate of compact binary mergers is so large that their cosmological population produces a confusion background that could masquerade the detection of potential primordial stochastic backgrounds. In this paper we study the ability of current and future detectors to resolve the confusion background to reveal interesting primordial backgrounds. The current detector network of LIGO and Virgo and the upcoming KAGRA and LIGO-India will not be able to resolve the cosmological compact binary source population and its sensitivity to stochastic background will be limited by the confusion background of these sources. We find that a network of three (and five) third generation (3G) detectors of Cosmic Explorer and Einstein Telescope will resolve the confusion background produced by binary black holes leaving only about 0.013\% (respectively, 0.00075\%) unresolved; in contrast, as many as 25\% (respectively, 7.7\%) of binary neutron star sources remain unresolved. Consequently, the binary black hole population will likely not limit observation of primordial backgrounds but the binary neutron star population will limit the sensitivity of 3G detectors to $\Omega_{\rm GW} \sim 10^{-11}$ at 10 Hz (respectively, $\Omega_{\rm GW} \sim 3\times 10^{-12}$).