The telescope is a part of the "'URAN "'( Ukrainian Radio Interferometer of NASU ) decametric VLBI system, which includes another four significantly smaller low-frequency radio telescopes.
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Each antenna will be a different distance from the radio source, and as with the short baseline radio interferometer the delays incurred by the extra distance to one antenna must be added artificially to the signals received at each of the other antennas.
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Developed predominantly for use with the then under-construction VLA, the generality inherent in its design allowed it to become the standard data-reduction package for most radio interferometers, including VLBI . Limited single-dish capability is also featured.
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Very Long Baseline Interferometry uses a technique related to the closure phase to combine telescopes separated by thousands of kilometers to form a radio interferometer with a resolution which would be given by a hypothetical single dish with an aperture thousands of kilometers in diameter.
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Initial usage was focused on the VLA, but it has gone on to be used to reduce data from practically all radio interferometers, including MERLIN and the GMRT and, to a lesser extent, the 12-m radio telescope and the 91-m transit telescope.
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Optical interferometers are extremely complex, unfilled aperture photon-collecting telescopes in the visual ( sometimes the near infrared, too ), which produce synthesized images and fringe data " on the fly " ( unlike radio interferometers which are privileged to record the data for " later " synthesis ), essentially by taking an inverse Fourier transform of the incoming data.
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