Editing Infrared astronomy (section)

== Infrared technology ==
One of the most common infrared detector arrays used at research telescopes is [[HgCdTe]] arrays. These operate well between 0.6 and 5 micrometre wavelengths. For longer wavelength observations or higher sensitivity other detectors may be used, including other [[narrow gap semiconductor]] detectors, low temperature [[bolometer]] arrays or photon-counting [[Superconducting]] Tunnel Junction arrays.

Special requirements for infrared astronomy include: very low dark currents to allow long integration times, associated low noise [[Readout integrated circuit|readout circuits]] and sometimes very high [[pixel]] counts.

Low temperature is often achieved by a coolant, which can run out.<ref name=werner>{{cite web | url = http://www.spacenews.com/civil/101005-last-minute-reprieve.html | archive-url = https://archive.today/20121209065100/http://www.spacenews.com/civil/101005-last-minute-reprieve.html | url-status = dead | archive-date = 9 December 2012 | title = Last-minute Reprieve Extends WISE Mission | publisher = [[Space News]] | date = 5 October 2010 | access-date = 14 January 2014 | first = Debra | last = Werner}}</ref> Space missions have either ended or shifted to "warm" observations when the coolant supply used up.<ref name=werner/> For example, [[Wide-field Infrared Survey Explorer|WISE]] ran out of coolant in October 2010, about ten months after being launched.<ref name=werner/> (See also [[NICMOS]], Spitzer Space Telescope)