  In gravitational wave astronomy, non-Gaussian noise, such as scattered light
noise disturbs stable interferometer operation, limiting the interferometer's
sensitivity, and reducing the reliability of the analyses. In scattered light
noise, the non-Gaussian noise dominates the sensitivity in a low frequency
range of less than a few hundred Hz, which is sensitive to gravitational waves
from compact binary coalescence. This non-Gaussian noise prevents reliable
parameter estimation, since several analysis methods are optimized only for
Gaussian noise. Therefore, identifying data contaminated by non-Gaussian noise
is important. In this work, we extended the conventional method to evaluate
non-Gaussian noise, Rayleigh statistic, by using a statistical hypothesis test
to determine a threshold for non-Gaussian noise. First, we estimated the
distribution of the Rayleigh statistic against Gaussian noise, called the
background distribution, and validated that our extension serves as the
hypothetical test. Moreover, we investigated the detection efficiency by
assuming two non-Gaussian noise models. For example, for the model with strong
scattered light noise, the true positive rate was always above 0.7 when the
significance level was 0.05. The results showed that our extension can
contribute to an initial detection of non-Gaussian noise and lead to further
investigation of the origin of the non-Gaussian noise.
