Abstract
Abstract The optimum pixel size ϵ of a detector under given observational conditions depends on a priori information about the object in focus, the Point Spread Function (PSF), the signal-to-noise ratio, etc. The Rayleigh criterion, according to which the theoretically attainable resolution is of the order of the PSF width Δ, leads to the generally accepted value of ϵ= Δ/2. It is shown that this conventional approach does not take into account important information concerning the image smoothing. Image restoration technique allows to reach much higher resolving power under typical conditions of observations, so that much smaller pixel size should be chosen to provide the theoretically attainable resolving power. Unmatched telescope and detector have significant losses in the resolving power and limiting magnitude. The formulae are given for approximate calculation of the corresponding parameters. As an example, the problem of the resolving power of the Hubble Space Telescope is discussed.
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