Laser power stabilization for Advanced VIRGO
Résumé
Second generation of laser interferometer gravitational wave detectors can now detect the fusion of compact stellar object pair weekly. To increase the sensitivity, an important change of design between first and second generation gravitational wave detectors is the use of homodyne detection instead of heterodyne. This modification has strongly increased the requirement on laser power stabilization for Advanced VIRGO [1] . The relative intensity noise (RIN) requirement depends on the effective defects of the interferometer mirrors and its operational state. It spans between 10 -8 Hz -1/2 and 1.2×10 -9 Hz -1/2 at 30 Hz for the most sensitive future configuration (2024).
Mots clés
Sensitivity
Laser noise
Power lasers
Gravitational waves
Europe
Detectors
Laser stability
gravitational wave detectors
gravitational waves
homodyne detection
light interferometers
interferometer mirrors
laser power stabilization
laser interferometer gravitational wave detectors
compact stellar object pair
generation gravitational wave detectors
Advanced VIRGO
relative intensity noise requirement
relative intensity noise
frequency 30.0 Hz
laser: stability
laser: interferometer
gravitational radiation detector: interferometer
noise
VIRGO
sensitivity