Abstract

Beginning with the experiments by Michelson in the 1920's and continuing with more recent research activities around the world Michelson interferometry has evolved into a powerful tool for measuring the diameters of giant stars and separations and orbits of multiple star systems. This paper offers calculations of the wavelength dependent limiting sensitivity achievable using a two aperture interferometer, without or with partial adaptive optics corrections, based upon realistic assumptions in regard to system noise sources. Results are presented for the case of observing resolved stars characterized as spectral type G2V, the spectral classification of the sun.

© 1992 Optical Society of America