Spectral energy distribution
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A spectral energy distribution (SED) is a plot of energy versus frequency or wavelength of light (not to be confused with a 'spectrum' of flux density vs frequency or wavelength).[1] It is used in many branches of astronomy to characterize astronomical sources. For example, in radio astronomy they are used to show the emission from synchrotron radiation, free-free emission and other emission mechanisms. In infrared astronomy, SEDs can be used to classify young stellar objects.
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Detector for spectral energy distribution
The count rates observed from a given astronomical radiation source have no simple relationship to the flux from that source, such as might be incident at the top of the Earth's atmosphere.[2] This lack of a simple relationship is due in no small part to the complex properties of radiation detectors.[2]
These detector properties can be divided into
- those that merely attenuate the beam, including
- residual atmosphere between source and detector,
- absorption in the detector window when present,
- quantum efficiency of the detecting medium,[2]
- those that redistribute the beam in detected energy, such as
- fluorescent photon escape phenomena,
- inherent energy resolution of the detector.[2]
See also
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