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Photometric-standard stars are a series of stars that have had their light output in various passbands of photometric system, measured very carefully. Other objects can be observed using CCD cameras or photoelectric photometers connected to a telescope, and the flux, or amount of light received, can be compared to a photometric-standard star to determine the exact brightness, or stellar magnitude, of the object.
The current set of photometric-standard stars for UBVRI photometry most often used by astronomers[original research?] is that published by Arlo U. Landolt in 1992 in the Astronomical Journal, vol. 104, no. 1, p. 340-371.
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