Orateur
Michal Was
(LAPP)
Description
Scattered light has limited at times all interferometric gravitational wave (GW) detectors to date. We describe how some of the scattered light noise contribution have been subtracted from strain data of Advanced Virgo during O3. We model in detail the scattered light coupling from suspended end benches and show how further noise subtraction can be achieved. The fitted model parameters can be used to characterize the interferometer optical properties. In particular it provides a new method to calibrate GW detectors that is fully independent from previously used methods (free swinging Michelson fringes, photon calibration and Newtonian calibration).
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Author
Michal Was
(LAPP)
