Abstract

Ultra-high sensitivity interferometry is the most promising technique for detecting the gravitational radiation emitted by various astrophysical objects, as predicted by the theory of general relativity. The basic antenna will be a simple Michelson interferometer, with very long orthogonal arms (L≠3 km), each containing a similar ‘gravito-optic transducer’: a delay-line or a Fabry-Perot cavity. Shot-noise would prevent reaching the required sensitivity range unless the light power available inside the arms of the interferometer is of the order of 1 kW, an unusual value for single frequency uitrastable lasers. This why the use of the so-called ‘recycling interferometers’ has been proposed.

© 1988 Optical Society of America