Interferometric gravitational wave antennas are based on enhanced Michelson interferometers. The sensitivity goal of the Laser Interferometer Gravitational-wave Observatory (LIGO) is 10/sup -21/ rms, integrated over a 100 Hz bandwidth centered at 150 Hz. The use of Fabry-Perot cavities is essential for reaching the required sensitivity, but sets challenges for the control system which must maintain the cavities near resonance. We present the major design features of the LIGO length and frequency sensing and control system which will hold the differential length to within 5/spl times/10/sup -14/ m of the operating point. We also highlight the restrictions imposed by couplings of noise into the gravitational wave readout signal and the required immunity against them.
LIGO interferometry
2005 Quantum Electronics and Laser Science Conference ; 2 ; 764-766 Vol. 2
2005-01-01
1495317 byte
Conference paper
Electronic Resource
English
TIBKAT | 2021
|TIBKAT | 2021
|Astrophysical Cosmology Using a Lunar LIGO
British Library Conference Proceedings | 1996
|The Laser Interferometer Gravitational-Wave Observatory LIGO
British Library Conference Proceedings | 2000
|The Laser Interferometer Gravitational-wave Observatory (LIGO)
British Library Online Contents | 1995
|