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Data acquired by the Virgo interferometer during the second part of the O3scientific run, referred to as O3b, were analysed with the aim ofcharacterising the onset and time evolution of scattered light noise inconnection with the variability of microseismic noise in the environmentsurrounding the detector. The adaptive algorithm used, called pytvfemd, issuitable for the analysis of time series which are both nonlinear andnonstationary. It allowed to obtain the first oscillatory mode of thedifferential arm motion degree of freedom of the detector during days affectedby scattered light noise. The mode's envelope i.e., its instantaneousamplitude, is then correlated with the motion of the West end bench, a knownsource of scattered light during O3. The relative velocity between the West endtest mass and the West end optical bench is used as a predictor of scatteredlight noise. Higher values of correlation are obtained in periods of higherseismic noise in the microseismic frequency band. This is also confirmed by thesignal-to-noise ratio (SNR) of scattered light glitches from GravitySpy for theJanuary-March 2020 period. Obtained results suggest that the adoptedmethodology is suited for scattered light noise characterisation and monitoringin gravitational wave interferometers.

Daily monitoring of scattered light noise due to microseismic variability at the Virgo interferometer