2001/11/09 by D. Sigg, H. Rong, P. Fritschel +5
Physics and Astronomy · #physics.ins-det
published as eConf C011127 (2001) WEcT003 · Presentation at ICALEPCS 2001, San Jose, November 2001, (WECT003), 3 pages
arxiv created 2001/11/09 · arxiv updated 2009/12/01
Interferometric gravitational wave antennas are based on Michelson interferometers whose sensitivity to small differential length changes has been enhanced by adding multiple coupled optical resonators. The use of optical cavities is essential for reaching the required sensitivity, but sets challenges for the control system which must maintain the cavities near resonance. The goal for the strain sensitivity of the Laser Interferometer Gravitational-wave Observatory (LIGO) is 10-21 rms, integrated over a 100 Hz bandwidth centered at 150 Hz. 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 10-14 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.