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Interferometry typically uses electromagnetic waves and is an important investigative technique in the fields of astronomy, fiber optics, engineering metrology, optical metrology, oceanography, seismology, spectroscopy (and its applications to chemistry), quantum mechanics, nuclear and particle physics, plasma physics, biomolecular interactions ...
The result is an interferometer that exhibits the stability of the Sagnac topology while being insensitive to rotation. [46] The Laser Interferometer Gravitational-Wave Observatory (LIGO) consisted of two 4-km Michelson–Fabry–Pérot interferometers, and operated at a power level of about 100 watts of laser power at the beam splitter. After ...
While all three of these interferometers work with a white light source, only the first, the diffraction grating interferometer, is truly achromatic. [8] Here the vertical scanning or coherence probe interferometers are discussed in detail due to their extensive use for surface metrology in today’s high-precision industrial applications.
In 1962, M. E. Gertsenshtein and V. I. Pustovoit published the very first paper describing the principles for using interferometers for the detection of very long wavelength gravitational waves. [63] The authors argued that by using interferometers the sensitivity can be 10 7 to 10 10 times better than by using electromechanical experiments.
A vibrometer is generally a two beam laser interferometer that measures the frequency (or phase) difference between an internal reference beam and a test beam. The most common type of laser in an LDV is the helium–neon laser, although laser diodes, fiber lasers, and Nd:YAG lasers are also used.
Set-up of a self-mixing interferometer with laser diode and monitor photodiode. Self-mixing or back-injection laser interferometry is an interferometric technique in which a part of the light reflected by a vibrating target is reflected into the laser cavity, causing a modulation both in amplitude and in frequency of the emitted optical beam.
This principle is used by detectors such as LIGO and Virgo, which consist of a Michelson interferometer with a Fabry–Pérot cavity with a length of several kilometers in both arms. Smaller cavities, usually called mode cleaners , are used for spatial filtering and frequency stabilization of the main laser.
Optical heterodyne detection began to be studied at least as early as 1962, within two years of the construction of the first laser. [3] However, laser illumination is not the only way to produce spatially coherent light.
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