In infrared astronomy, the K band is an atmospheric transmission window centered on 2.2 μm (in the near-infrared 136 THz range).[1][2] HgCdTe-based detectors are typically preferred for observing in this band.[3]
Photometric systems used in astronomy are sets of filters or detectors that have well-defined windows of absorption, based around a central peak detection frequency and where the edges of the detection window are typically reported where sensitivity drops below 50% of peak. Various organizations have defined systems with various peak frequencies and cutoffs in the K band, including K′, and KS, and Kdark.[4]
See also
Absolute magnitude
References
^Tokunaga, Alan T. (September 10, 2001). "Specifications for Astronomical Infrared Filters". www.ifa.hawaii.edu. Institute for Astronomy, University of Hawaii. Retrieved 2021-11-05.
^Jahne, Bernd (March 15, 2004). Practical Handbook on Image Processing for Scientific and Technical Applications. RC Press. p. 109. ISBN 9780849390302.
^Sizov, Fedir F. (May 5, 2020). Detectors and Sources for THz and IR. Materials Research Forum LLC. p. 138. ISBN 9781644900758.
^Jun Zhang (June 2023). "Sky-brightness measurements in J, H, and Ks bands at DOME A with NISBM and early results". Monthly Notices of the Royal Astronomical Society. 521 (4): 5624–5635. doi:10.1093/mnras/stad775. Table 1., Filter sets used at Mauna Kea and the South Pole.
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