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Abstracts |
P. Fritschel (MIT), M. Zucker (MIT), R. Bork (Caltech), N. Mavalvala (Caltech), D. Ouimette (Caltech), G. Gonzalez (Pennsylvania State University), H. Rong (LIGO Hanford Observatory), D. Sigg (LIGO Hanford
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 to the power of minus 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 interferometric lengths to within 0.2-pm of the operating point. We also highlight the restrictions imposed by couplings of noise into the gravitation wave readout signal and the required immunity against them.
{*} Work supported by National Science Foundation cooperative agreement PHY-9210038 and grant PHY-9870032
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C011127
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ICALEPCS 2001
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