Back نظام القياس الضوئي UBV Arabic Sistema fotomètric UBV Catalan UBV systém Czech UBV-System German Sistema fotométrico UBV Spanish Système photométrique UBV French Sistema fotometrico UBV Italian ジョンソンのUBVシステム Japanese UBV 측광계 Korean UBV-System LB

UBV photometric system

1P21 photomultiplier tube

The UBV photometric system (from Ultraviolet, Blue, Visual), also called the Johnson system (or Johnson-Morgan system), is a photometric system usually employed for classifying stars according to their colors. It was the first standardized photometric system. The apparent magnitudes of stars in the system are often used to determine the color indices B−V and U−B, the difference between the B and V magnitudes and the U and B magnitudes respectively.[1] The system is defined using a set of color optical filters in combination with an RMA 1P21 photomultiplier tube.[2]

The choice of colors on the blue end of the spectrum was assisted by the bias that photographic film has for those colors. It was introduced in the 1950s by American astronomers Harold Lester Johnson and William Wilson Morgan. A 13 in (330 mm) telescope and the 82 in (2,100 mm) telescope at McDonald Observatory were used to define the system.[1][3] The filters that Johnson and Morgan used were Corning 9 863 for U and 3 384 for V. The B filter used a combination of Corning 5 030 and Schott GG 13.[4]

Wavelengths

The filters are selected so that the mean wavelengths of response functions (at which magnitudes are measured to mean precision) are 364 nm for U, 442 nm for B, 540 nm for V. Zero-points were calibrated in the B−V (B minus V) and U−B (U minus B) color indices selecting such A0 main sequence stars which are not affected by interstellar reddening.[1] These stars correspond with a mean effective temperature (Teff (K)) of between 9727 and 9790 Kelvin, the latter being stars with class A0[a]V (V meaning five)[b].

The system has a key limit drawback. The short wavelength cutoff that is the shortest limit of the U filter is set by any given terrestrial atmosphere rather than the filter itself; thus, it (and observed magnitudes) varies chiefly with altitude and atmospheric water (humidity plus condensation into clouds).[5] However, many measurements have been made in this system, including thousands of the bright stars.[6]

  1. ^ a b c Johnson, H. L.; Morgan, W. W. (1953). "Fundamental stellar photometry for standards of spectral type on the revised system of the Yerkes spectral atlas". The Astrophysical Journal. 117 (3): 313–352. Bibcode:1953ApJ...117..313J. doi:10.1086/145697.
  2. ^ Johnson, H.L.; Morgan, W.W. (May 1953). "Fundamental stellar photometry for standards of spectral type on the Revised System of the Yerkes Spectral Atlas". Astrophysical Journal. 117 (3): 315. Bibcode:1953ApJ...117..313J. doi:10.1086/145697. Retrieved 22 July 2024.
  3. ^ Hearnshaw, J. B. (1996). The Measurement of Starlight: Two Centuries of Astronomical Photometry. Cambridge University Press. p. 421. ISBN 9780521403931. In the 1950–51 winter, Johnson had commenced photometry in three passbands (designated U, V, and Y) on the McDonald 13- and 82-inch reflectors [54].
  4. ^ Johnson, H.L. (January 1955). "A Photometric System". Annales d'Astrophysique. 18: 292–316. Bibcode:1953ApJ...117..313J. doi:10.1086/145697.
  5. ^ Hearnshaw, J. B. (1996). The Measurement of Starlight: Two Centuries of Astronomical Photometry. Cambridge University Press. p. 425. ISBN 9780521403931.
  6. ^ Iriarte, Braulio; Johnson, Harold L; Mitchell, Richard I; Wisniewski, Wieslaw K (1965). "Five-Color Photometry of Bright Stars". Sky and Telescope. 30: 21. Bibcode:1965S&T....30...21I.


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