Einstein@Home All-sky Search for Continuous Gravitational Waves in LIGO O2 Public Data
Einstein@Home All-sky Search for Continuous Gravitational Waves in LIGO O2 Public Data
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DOI：
10.3847/1538-4357/abc7c9
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发表时间：
2020-09
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影响因子：
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通讯作者：
B. Steltner;M. Papa;H. Eggenstein;B. Allen;V. Dergachev;R. Prix;B. Machenschalk;S. Walsh;S. Zhu;O. Behnke;S. Kwang
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作者：
B. Steltner;M. Papa;H. Eggenstein;B. Allen;V. Dergachev;R. Prix;B. Machenschalk;S. Walsh;S. Zhu;O. Behnke;S. Kwang
我们在汉福德和利文斯顿探测器的LIGO O2数据中进行了一次全天搜索，以寻找连续的引力波。我们搜索频率为20.0赫兹≤f≤585.15赫兹和自旋下降赫兹S−1的近单色信号。我们将搜索部署在爱因斯坦@家庭志愿者计算项目上，并通过八个进一步的搜索阶段跟踪与最重要结果相关的波形，达到了高达500赫兹的全天测量所达到的最佳灵敏度。检查的六个波形通过了所有阶段，但它们都与硬件注入有关，硬件注入是在LIGO探测器处模拟的假信号，用于验证目的。我们用一致的参数恢复所有这些假信号。没有其他波形幸存下来，所以我们没有发现在我们搜索的可探测水平上有连续引力波信号的证据。我们将探测器处连续引力波的h0振幅限制为信号频率的函数，单位为半赫兹。在163.0赫兹，在90%的置信度水平下，最受约束的上限是h0=1.3×10−25。我们的结果不包括赤道椭圆度大于10−7的中子星旋转速度大于5ms，更接近100pc。根据一些模型，这些变形是中子星外壳可以很容易地支持的。
We conduct an all-sky search for continuous gravitational waves in the LIGO O2 data from the Hanford and Livingston detectors. We search for nearly monochromatic signals with frequency 20.0 Hz ≤ f ≤ 585.15 Hz and spin-down Hz s−1. We deploy the search on the Einstein@Home volunteer-computing project and follow-up the waveforms associated with the most significant results with eight further search stages, reaching the best sensitivity ever achieved by an all-sky survey up to 500 Hz. Six of the inspected waveforms pass all the stages but they are all associated with hardware injections, which are fake signals simulated at the LIGO detector for validation purposes. We recover all these fake signals with consistent parameters. No other waveform survives, so we find no evidence of a continuous gravitational wave signal at the detectability level of our search. We constrain the h 0 amplitude of continuous gravitational waves at the detector as a function of the signal frequency, in half-Hz bins. The most constraining upper limit at 163.0 Hz is h 0 = 1.3 × 10−25, at the 90% confidence level. Our results exclude neutron stars rotating faster than 5 ms with equatorial ellipticities larger than 10−7 closer than 100 pc. These are deformations that neutron star crusts could easily support, according to some models.