page_title: Spectral energy distribution
hierarchical_section_title: Spectral energy distribution
caption_attribution_description: English: An example of the data that is processed by theSkyNet POGS distributed computing project. Three different images of the same galaxy are shown, at Ultraviolet, Optical and Infrared wavlengths, taken by the GALEX, Pan-STARRS1 and WISE telescopes respectively. The far right image then shows the process used by theSkyNet POGS to determine different characteristics of the galaxy in question using the three images in a process called Spectral Energy Distribution (SED) fitting.
context_page_description: A spectral energy distribution is a plot of energy versus frequency or wavelength of light. 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.
context_section_description: 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).  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.
caption: The SED of M51 (upper right) obtained by combining data at many different wavelengths, e.g. UV, visible, and infrared (left)
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