K band (infrared)

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 K_S, and K_dark.^[4]

^ Cite error: The named reference ifa was invoked but never defined (see the help page).
^ Cite error: The named reference Bernd2004 was invoked but never defined (see the help page).
^ Cite error: The named reference Sizov2020 was invoked but never defined (see the help page).
^ 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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[Bernd2004-2] Cite error: The named reference Bernd2004 was invoked but never defined (see the help page).

[Sizov2020-3] Cite error: The named reference Sizov2020 was invoked but never defined (see the help page).

[4] 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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K band (infrared)

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