In division of wavefront, different spatial portions of an incident wavefront are selected and propagated so that their fields overlap. Double-slit interference is an example. The selected portions need sufficient spatial optical coherence for stable interference fringes.
In division of amplitude, a partially reflecting interface sends parts of the same incident wavefront into separate paths that are later recombined. A Michelson interferometer is an example. The resulting interference visibility depends on relative optical path length, polarization of waves, intensity balance and optical coherence.
An interferogram records detected light intensity produced by interference as a controlled position, phase or delay is varied. In Fourier transform spectroscopy, the variable is the delay between two copies of the same field. Removing the constant background gives a correlation signal whose Fourier transform determines the source's spectral power density, subject to the measured delay window and instrumental response.
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 , where is the full angular diameter. Different surface-brightness laws, including limb darkening, change the null.
