Diluted-aperture Stellar Interferometry
Success in radio interferometry caught the attention of astronomers working at optical and infrared (IR) wavelengths, spanning the whole range from 0.35 to 20 μm. Thus, a long baseline optical interferometer (LBOI) came into existence offering unprecedented resolution. As stated earlier in Sect. 3.2, stellar interfero- metry can be achieved with a single telescope into which light from a distant object can pass through two (or more) apertures in a mask covering the telescope and then combine the two light beams to produce fringes. Another way to achieve stellar interferometry is to use two or more telescopes looking at the same star and reflect-ing light beams into a single receiver.
KeywordsFringe Pattern Celestial Object Baseline Vector Vernal Equinox Celestial Equator
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