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Photometry (astronomy)
Photometry is a technique of astronomy concerned with measuring the flux, or intensity of an astronomical object's electromagnetic radiation.〔 When photometry is performed over broad wavelength bands of radiation, where not only the amount of radiation but also its spectral distribution is measured, the term ''spectrophotometry'' is used.
The word is composed of the Greek affixes ''photo-'' ("light") and ''-metry'' ("measure").
==Methods==
The methods used to perform photometry depend on the wavelength regime under study. At its most basic, photometry is conducted by gathering light in a telescope, sometimes passing it through specialized photometric optical bandpass filters, and then capturing and recording the light energy with a photosensitive instrument. Standard sets of passbands (called a photometric system) are defined to allow accurate comparison of observations.〔Warner, Brian (2006). ''A Practical Guide to Lightcurve Photometry and Analysis'', Springer, ISBN 0-3872-9365-5〕
Historically, photometry in the near-infrared through long-wavelength ultra-violet was done with a photoelectric photometer, an instrument that measured the light intensity of a single object by directing its light onto a photosensitive cell. These have largely been replaced with CCD cameras that can simultaneously image multiple objects, although photoelectric photometers are still used in special situations, such as where fine time resolution is required.
抄文引用元・出典: フリー百科事典『 ウィキペディア（Wikipedia）』
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