Space mid-IR detectors from DRS

Hogue, Henry H.; Guptill, Matthew L.; Reynolds, David; Atkins, Ernest W.; Stapelbroek, M. G.

doi:10.1117/12.461584

Cited by 10 publications

(2 citation statements)

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“…7 The relatively high background that WISE will see due to zodiacal emission implies that relatively relaxed requirements on dark current and read noise are acceptable. The Si:As array temperature of 7.8 K has been set to optimize dark current performance and linearity.…”

Section: Description Of Devicesmentioning

confidence: 99%

Characterization of flight detector arrays for the wide-field infrared survey explorer

et al. 2008

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The Wide-field Infrared Survey Explorer is a NASA Midex mission launching in late 2009 that will survey the entire sky at 3.3, 4.7, 12, and 23 microns (PI: Ned Wright, UCLA). Its primary scientific goals are to find the nearest stars (actually most likely to be brown dwarfs) and the most luminous galaxies in the universe. WISE uses three dichroic beamsplitters to take simultaneous images in all four bands using four 1024x1024 detector arrays. The 3.3 and 4.7 micron channels use HgCdTe arrays, and the 12 and 23 micron bands employ Si:As arrays. In order to make a 1024x1024 Si:As array, a new multiplexer had to be designed and produced. The HgCdTe arrays were developed by Teledyne Imaging Systems, and the Si:As array were made by DRS.All four flight arrays have been delivered to the WISE payload contractor, Space Dynamics Laboratory. We present initial ground-based characterization results for the WISE arrays, including measurements of read noise, dark current, flat field and latent image performance, etc. These characterization data will be useful in producing the final WISE data product, an all-sky image atlas and source catalog.

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Section: Description Of Devicesmentioning

confidence: 99%

Characterization of flight detector arrays for the wide-field infrared survey explorer

et al. 2008

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“…m  [6][7][8][9][10][11][12][13][14][15][16] 。图 1 列出了常用红外天文探测器的探测波长范围和工作温度 [17] [17] 。图片来自文献，并获得授权 Figure 1 The detection wavelength and working temperature of common infrared astronomical detectors [17] .…”

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Blocked impurity band very long wavelength infrared detector

Pan

Mou

Zhang

et al. 2021

Sci. Sin.-Phys. Mech. Astron.

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Blocked impurity band (BIB) detector is a derivative of the impurity band conduction (IBC) detector. It can detect low-energy photons whose energy is much smaller than the band gap of the semiconductor through the electronic transition on the impurity band. The detection wavelength of the BIB detector is mainly determined by the substrate and doped impurities which can cover the range of 5-300 m . Owning to the advantages of long detection wavelength, high detection rate and good radiation resistance, BIB detectors have been extensively studied and are widely used in various large-scale astronomical infrared detection platforms. Presently, Si-based BIB detectors are developing rapidly, but the development of Ge-based and GaAs-based BIB detectors is relatively slow. BIB detectors play an irreplaceable role in promoting the development of astronomy and related sciences. Developed countries such as Europe and the United States have invested a lot in scientific research on BIB detectors. With the development of China's economy and technology, Chinese researchers hope eagerly that the domestic BIB detector can be put into use as soon as possible. Herein, in order to help the related researchers to quickly understand the BIB detector, the device physical model, preparation methods, testing methods and development status have been discussed, and the involved working mechanism and key device technology are also explored.

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