The precision of radial-velocity determinations of solar-type stars by cross-correlation

The theoretical limit to the precision (defined as the inverse of the square of the random error) of a radial-velocity determination of a solar-type star obtained from the technique of digital cross-correlation is constructed as a function of simple parameters of the recording of a stellar spectrum.The relationship is used to establish conditions for maximizing the precision for a given object, exposure time, and observing instrument. Both fibre-fed and Cassegrain-mounted spectrographs are considered.