The idea that the resolution of optical instruments is limited due to the
wave nature of light is familiar to students of optics and is embodied in the
Rayleigh's criterion which states that the angular resolution of a
telescope/microscope is ultimately diffraction limited and is given by
where is some measure of the aperture size. The need for higher angular resolution has led to the development of instruments with larger size and which operate at smaller wavelengths. In radioastronomy, the wavelengths are so large that even though the sizes of radio telescopes are large, the angular resolution is still poor compared to optical instruments. Thus while the human eye has a diffraction limit of and even modest optical telescopes have diffraction limits2.4of , even the largest radio telescopes (300m in diameter) have angular resolutions of only at 1 metre wavelength. To achieve higher resolutions one has to either increase the diameter of the telescope further (which is not practical) or decrease the observing wavelength. The second option has led to a tendency for radio telescopes to operate at centimetre and millimetre wavelengths, which leads to high angular resolutions. These telescopes are however restricted to studying sources that are bright at cm and mm wavelengths. To achieve high angular resolutions at metre wavelengths one need telescopes with apertures that are hundreds of kilometers in size. Single telescopes of this size are clearly impossible to build. Instead radio astronomers achieve such angular resolutions using a technique called aperture synthesis. Aperture synthesis is based on interferometry, the principles of which are familiar to most physics students. There is in fact a deep analogy between the double slit experiment with quasi-monochromatic light and the radio two element interferometer. Instead of setting up this analogy we choose the more common route to radio interferometry via the van Cittert-Zernike theorem.