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...
In order to increase the science reach of GW detectors, it is fundamental to reduce the quantum noise, composed of radiation pressure noise (RPN) at low frequencies (roughly < 100 Hz) and shot noise (SN) at high frequencies (roughly > 100 Hz). Since the quantum noise is generated by vacuum fluctuations entering the interferometer, the injection of phase-squeezed vacuum states reduces the SN...
Gravitational waves (GWs) are opening a new window to investigate our Universe. As an effort to broaden the frequency band of GW observation, LISA will be the first-ever spaceborne GW detector, aiming to detect the GW signals from various astrophysical and cosmological sources in the frequency band from 0.1 mHz to 1 Hz. To study the noises and how to reduce them at the required levels allowing...
Pulsar Timing Array (PTA) experiments aim to detect nHz gravitational waves (GW) from supermassive black hole binaries. This is done by looking for correlated variations of the Time of Arrivals (TOA) across an array of ultra-stable millisecond pulsars. Regular observations have been taken and collected over the last 2 or so decades. Three established PTA collaborations: the North American...
