All-sky search for continuous gravitational waves from isolated neutron stars in the early O3 LIGO data
All-sky search for continuous gravitational waves from isolated neutron stars in the early O3 LIGO data
复制标题
全天搜索来自早期 O3 LIGO 数据中孤立中子星的连续引力波
DOI：
10.1103/physrevd.104.082004
复制
发表时间：
2021
影响因子：
5
通讯作者：
and the KAGRA Collaboration),
中科院分区：
文献类型：
--
作者：
R. Abbott et al. (The LIGO Scientific Collaboration;the Virgo Collaboration;and the KAGRA Collaboration),
我们报告了在20-2000 Hz频段和频率时间导数范围内的连续引力波的全天搜索。这样的信号可能是由我们银河系附近的一颗旋转的、稍微非轴对称的孤立中子星星产生的。这次搜索使用了Advanced LIGO和Advanced Virgo第三次观测运行O3的前六个月的LIGO数据。没有观测到周期性引力波信号，95%置信水平（CL）频率论的上限是根据它们的强度来确定的。最坏情况（线极化）应变振幅的最低上限接近200 Hz。对于圆偏振源（最有利的方向），最低上限为。这些严格的频率论上限指的是所有天空位置和频率导数值的整个范围。对于天空位置和恒星方向的总体平均系综，最低95% C.L.应变幅度的上限为。这些上限改进了我们以前发表的全天结果，在更高的频率上看到了最大的改进（因子），部分原因是量子压缩相对于第二次观测运行O2显着提高了探测器的噪声水平。这些限制是迄今为止搜索的大多数参数空间中最具约束性的。
We report on an all-sky search for continuous gravitational waves in the frequency band 20–2000 Hz and with a frequency time derivative in the range of. Such a signal could be produced by a nearby, spinning and slightly nonaxisymmetric isolated neutron star in our Galaxy. This search uses the LIGO data from the first six months of Advanced LIGO’s and Advanced Virgo’s third observational run, O3. No periodic gravitational wave signals are observed, and 95% confidence-level (C.L.) frequentist upper limits are placed on their strengths. The lowest upper limits on worst-case (linearly polarized) strain amplitudearenear 200 Hz. For a circularly polarized source (most favorable orientation), the lowest upper limits are. These strict frequentist upper limits refer to all sky locations and the entire range of frequency derivative values. For a population-averaged ensemble of sky locations and stellar orientations, the lowest 95% C.L. upper limits on the strain amplitude are. These upper limits improve upon our previously published all-sky results, with the greatest improvement (factor of) seen at higher frequencies, in part because quantum squeezing has dramatically improved the detector noise level relative to the second observational run, O2. These limits are the most constraining to date over most of the parameter space searched.