While interference fringes contain both amplitude and phase information, most
interferometric results published to date focus solely on the amplitude data. This is because …

Phase distortions due to atmospheric turbulence, as emphasized by Quirrenbach in Chapter
5, cause a variety of ill effects. They both limit the maximum useful size of a collecting …

The detection of high contrast companions at small angular separation appears feasible in
conventional direct images using the self-calibration properties of interferometric observable …

The high-spatial-frequency fringes that contain detailed information about a stellar image
are generally too weak to track. The Navy Prototype Optical Interferometer (NPOI) is the first …

In stellar interferometry the fringe visibility can be measured by modulating the optical path
difference between the two arms of an interferometer. This approach yields accurate …

Aims. Current and future ground-based interferometers require knowledge of the
atmospheric time constant t 0, but this parameter has diverse definitions. Moreover …

In the photon-starved regime, the signal-to-noise ratio of interferometric data depends on the
coherent integration time. To extend the integration time beyond the limit imposed by …

Context. Long-baseline optical interferometry uses the power spectrum and bispectrum
constructs as fundamental observables. Noise arising in the detection of the fringe pattern …

At present, the principal limitation on the resolution and contrast of astronomical imaging
instruments comes from aberrations in the optical path, which may be imposed by the Earth's …

Astronomical imaging can be broadly classified into two types. The first type is amplitude
interferometry, which includes conventional optical telescopes and very large baseline …