Key points are not available for this paper at this time.
The prototype gravitational-wave detector at Garching is described: in a laser-illuminated Michelson interferometer having arms 30 m in length, a folded optical path of 3 km is realized. The origin, action, and magnitude of possible noise sources are given. The agreement between the expected and measured noise is good. For a band of astrophysical interest, extending from 1 to 6 kHz, the quantum shot noise corresponding to a light power of P=0. 23 W is dominant. In terms of the dimensionless strain h the best sensitivity in a 1-kHz bandwidth is h=310^-18, comparable to the most sensitive Weber-bar-type antennas.
Shoemaker et al. (1988) studied this question.