Abstract

The formation of a photographic image of a star on a plate by having a telescope assume the functions of the camera is described. The factors which contribute to the spreading of the light from a star on the emulsion, and those which bring about deviations from a “flawless” (usually gnomonic) projection of the stars onto the plate are analyzed. The amount by which the measured position of an image deviates from the position prescribed by the flawless projection depends on the position of the image on the plate, the intensity, and the spectrum of the star. Methods are given to show how measured positions can be freed from these deviations and thus reduced to “flawless” positions, and examples are quoted showing where and how these methods have been applied.

© 1963 Optical Society of America

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