Abstract
The problems associated with the photometry of fast-moving asteroids are discussed. The effect of noise in CCD observations on the photometric accuracy is analyzed. A photometric accuracy limitation is shown to exist for observations of asteroids, which is determined by the angular rate of the object and the ratio of the flux from the object and noise due to sky background and dark current. The effective exposure for observing a moving object is determined. The method of overlapping areas is analyzed, which is used for obtaining the lightcurves of fast-moving asteroids. This method includes the determination of the mutual magnitude differences for the entire ensemble of comparison stars, the reduction of the magnitudes of all these stars to the magnitude of one of them adopted as the primary comparison star, the determination of the magnitude of the “average star” on each frame of the entire series of CCD observations, and the computation of the lightcurve as the difference between the magnitude of the asteroid and that of the average star.
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