Photometric-standard star

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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.[1]

A current set of photometric-standard stars for UBVRI photometry was published by Arlo U. Landolt in 1992 in the Astronomical Journal.

References[edit]

  1. Landolt, A.U. (1 July 1992). "UBVRI photometric standard stars in the magnitude range 11.5-16.0 around the celestial equator". The Astronomical Journal 104: 340–371. Bibcode 1992AJ....104..340L. doi:10.1086/116242.


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{{{1}}}
Observation data
Epoch {{{epoch}}}      Equinox
Constellation {{{3}}}
{{{component1}}}
Right ascension {{{ra1}}}
Declination {{{dec1}}}
Apparent magnitude (V) {{{appmag_v1}}}
{{{component2}}}
Right ascension {{{ra2}}}
Declination {{{dec2}}}
Apparent magnitude (V) {{{appmag_v2}}}
Characteristics
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Spectral type {{{7}}}
Astrometry
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Details
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Diameter{{{5}}} D
Luminosity (bolometric){{{11}}} L
Temperature{{{8}}} K
Other designations
{{{1}}}, {{{2}}}
{{{1}}}, also known as {{{2}}}, is a star located in the constellation {{{3}}}. It is located {{{4}}} light years away from the Earth. {{{1}}} has a diameter of {{{5}}} D, making it around the size of the orbit of {{{6}}}. {{{1}}} has a stellar class of {{{7}}} and a temperature of {{{8}}} degrees Kelvin; it is a {{{9}}} that is currently burning {{{10}}} within its core. {{{1}}} is around {{{11}}} times brighter than the Sun. {{{12}}}{{{13}}}

References[edit]

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