论文标题
有针对性地搜索银河脉冲星人口的随机重力波背景
Targeted search for the stochastic gravitational-wave background from the galactic millisecond pulsar population
论文作者
论文摘要
毫秒普尔萨尔（Pulsars），具有高频$ \ MATHCAL {O} $（kHz）的旧物体旋转，从其球形形状中持续变形，可能会发出重力波（GW）。这些是在基于地面的GW探测器中观察到的各向异性随机重力波背景（SGWB）的潜在候选者之一。在这里，我们通过分析先进的Ligo和高级处女座检测器的前三个观测运行中的数据来介绍基于千分之一的脉冲星，以基于千分之一的脉冲星对SGWB的有针对性搜索的结果。我们假设SGWB功率光谱和天空分布的形状是从总体合成模型中知道的\ textit {a先验{a先验{a先验。集合源属性的信息，即脉冲机的内数，$ n _ {\ textrm {obs}} $和平均椭圆度，$μ_ε$是在最大可能的可能性统计量中编码的。我们找不到来自所考虑的源人群的SGWB信号的重要证据。该参数的最佳贝叶斯上限为$ 95 \％$的信心为$ n _ {\ textrm {obs}} \ leq8.8 \ times10^{4} $和$μ_i_ε\ leq1.4 \ leq1.4 \ times10^{ - 6} $，与均值均与eLlipt culipt coption相提并论。 Finally, we show that for the plausible case of $N_{\textrm{obs}}=40,000$, with the one year of observations, the one-sigma sensitivity on $μ_ε$ might reach $1.5\times10^{-7}$ and $4.1\times10^{-8}$ for the second-generation detector network having A+ sensitivity and third-generation detector network, 分别。
The millisecond pulsars, old-recycled objects spinning with high frequency $\mathcal{O}$ (kHz) sustaining the deformation from their spherical shape, may emit gravitational waves (GW). These are one of the potential candidates contributing to the anisotropic stochastic gravitational-wave background (SGWB) observable in the ground-based GW detectors. Here, we present the results from a likelihood-based targeted search for the SGWB due to millisecond pulsars in the Milky Way, by analyzing the data from the first three observing runs of Advanced LIGO and Advanced Virgo detector. We assume that the shape of SGWB power spectra and the sky distribution is known \textit{a priori} from the population synthesis model. The information of the ensemble source properties, i.e., the in-band number of pulsars, $N_{\textrm{obs}}$ and the averaged ellipticity, $μ_ε$ is encoded in the maximum likelihood statistic. We do not find significant evidence for the SGWB signal from the considered source population. The best Bayesian upper limit with $95\%$ confidence for the parameters are $N_{\textrm{obs}}\leq8.8\times10^{4}$ and $μ_ε\leq1.4\times10^{-6}$, which is comparable to the bounds on mean ellipticity with the GW observations of the individual pulsars. Finally, we show that for the plausible case of $N_{\textrm{obs}}=40,000$, with the one year of observations, the one-sigma sensitivity on $μ_ε$ might reach $1.5\times10^{-7}$ and $4.1\times10^{-8}$ for the second-generation detector network having A+ sensitivity and third-generation detector network, respectively.
