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Figure 1. The light path through a Michelson interferometer.The two light rays with a common source combine at the half-silvered mirror to reach the detector. They may either interfere constructively (strengthening in intensity) if their light waves arrive in phase, or interfere destructively (weakening in intensity) if they arrive out of phase, depending on the exact distances between the ...
Dual-polarization interferometry; Fabry–Pérot interferometer; Fizeau interferometer; Fourier-transform interferometer; Fresnel interferometer (e.g. Fresnel biprism, Fresnel mirror or Lloyd's mirror) Fringes of Equal Chromatic Order interferometer (FECO) Gabor hologram; Gires–Tournois etalon; Heterodyne interferometer (see heterodyne ...
Lateral shearing interferometry is a self-referencing method of wavefront sensing. Instead of comparing a wavefront with a separate path reference wavefront, lateral shearing interferometry interferes a wavefront with a shifted version of itself. As a result, it is sensitive to the slope of a wavefront, not the wavefront shape per se. The ...
Rayleigh interferometer at the National Bureau of Standards. In optics, a Rayleigh interferometer is a type of interferometer which employs two beams of light from a single source.
Principle of the shearing interferometer. The shearing interferometer is an extremely simple means to observe interference and to use this phenomenon to test the collimation of light beams, especially from laser sources which have a coherence length which is usually significantly longer than the thickness of the shear plate (see graphics) so that the basic condition for interference is fulfilled.
A simple two-element optical interferometer. Light from two small telescopes (shown as lenses) is combined using beam splitters at detectors 1, 2, 3 and 4.The elements create a 1/4 wave delay in the light, allowing the phase and amplitude of the interference visibility to be measured, thus giving information about the shape of the light source.
To minimize image aberrations the angle plane of the glass wedges has to be placed orthogonal to the angle plane of the air-wedge. Because intensity of Fresnel reflections from a glass surface are polarization and angle dependent, it is necessary to keep the air-wedge plane nearly perpendicular to the incident beam (±5deg) to minimize instrumentally induced intensity variation.
An intensity interferometer is the name given to devices that use the Hanbury Brown and Twiss effect. [1] In astronomy, the most common use of such an astronomical interferometer is to determine the apparent angular diameter of a radio source or star.