Detecting a stochastic gravitational wave background in the presence of a galactic foreground and instrument noise
Detecting a stochastic gravitational wave background in the presence of a galactic foreground and instrument noise
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DOI：
10.1103/physrevd.89.022001
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发表时间：
2014-01-14
影响因子：
5
通讯作者：
Cornish, Neil J.
中科院分区：
文献类型：
--
作者：
Adams, Matthew R.;Cornish, Neil J.
探测随机引力波背景需要我们首先理解和模拟任何天体物理前景。在毫赫兹频段，占主导地位的前景信号将来自银河系中尚未解决的白色矮双星。我们建立在我们以前的工作表明，一个随机的引力波背景可以检测到的仪器噪声和银河系的混乱前景的存在。我们的方法的关键是准确地建模的各种信号分量的频谱。我们模拟数据千兆激光干涉仪空间天线工作在毫赫兹频段与六个和四个链接。我们得到后验分布函数的仪器噪声参数，星系的水平和调制参数，和随机背景能量密度。我们发现，我们能够检测到一个尺度不变的随机背景的能量密度低至Ω（gw）= 2 × 10（-13）的六链接干涉仪和Ω（gw）= 5 × 10（-13）的四链接干涉仪与一年的数据。
Detecting a stochastic gravitational wave background requires that we first understand and model any astrophysical foregrounds. In the millihertz frequency band, the predominate foreground signal will be from unresolved white dwarf binaries in the galaxy. We build on our previous work to show that a stochastic gravitational wave background can be detected in the presence of both instrument noise and a galactic confusion foreground. The key to our approach is accurately modeling the spectra for each of the various signal components. We simulate data for a gigameter Laser Interferometer Space Antenna operating in the millihertz frequency band with both six and four links. We obtain posterior distribution functions for the instrument noise parameters, the galaxy level and modulation parameters, and the stochastic background energy density. We find that we are able to detect a scale-invariant stochastic background with energy density as low as Omega(gw) = 2 x 10(-13) for a six-link interferometer and Omega(gw) = 5 x 10(-13) for a four-link interferometer with one year of data.