The Washington photometric system is a broadband photometric system, initially designed by G. Wallerstein and later developed by R. Canterna at the Kitt Peak National Observatory, aimed at obtaining accurate photometric temperatures, metal abundances, and a cyanogen blanketing index for G and K type giant stars. [1] It is composed of four main filters: C, M, T1 and T2 of effective wavelengths 3910, 5085, 6330 and 7885 Å respectively. Most of its colors can be well transformed into related colors in the Cousins BVRI system. [2]
See also
References
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^ R. Canterna (1976).
"Broad-band photometry of G and K stars - The C, M, T/1/, T/2/ photometric system". Astronomical Journal. 81: 228–244.
Bibcode:
1976AJ.....81..228C.
doi:
10.1086/111878.
{{ cite journal}}: Unknown parameter|month=ignored ( help) - ^ Michael S Bessell (2005). Standard Photometric Systems (PDF). Annual Review of Astronomy and Astrophysics.