Abstract
A variety of astronomical problems require detailed information on the structure of radio sources for their solution. There is a corresponding need to increase the angular resolution of radio telescopes, the resolution being proportional to the size of the telescope aperture. As is well known, enlarging the size of the classic instruments of radio astronomy, fully steerable dish antennas, is hindered by limitations of a technological nature. The idea of fulfilling the high angular resolution requirements with small antennas, which was proposed in the 1950s, was therefore quite revolutionary. These instruments became known as aperture synthesis systems. In what follows, we will outline the main theoretical relations describing the way that aperture synthesis systems work and the data processing methods used in these systems.t
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