Astronomical interferometer

An astronomical interferometer combines observations from separated collecting locations to infer angular source structure. Its projected interferometric baseline determines the angular spatial frequency sampled. Amplitude and intensity interferometers measure different coherence observables; a Michelson stellar interferometer combines optical field amplitudes.

The Michelson stellar interferometer, associated with Albert Abraham Michelson, uses separated collectors and beam-redirection optics to produce interference fringes. The collector spacing determines sensitivity to a stellar angular diameter, independently of the final beam spacing at the combiner. The first null for a uniform disk is $D=1.21967\lambda /\alpha$, where $\alpha$ is the full angular diameter. Different surface-brightness laws, including limb darkening, change the null.