Blocked impurity band hybrid infrared focal plane arrays for astronomy

Reynolds, David; Seib, D. H.; Stetson, S.; Herter, T.; Rowlands, Neil; Schoenwald, Justin

doi:10.1109/23.34565

Cited by 31 publications

(12 citation statements)

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“…The main changes on the instrument hardware side are a replacement of the midinfrared Si:Ga detectors of the center telescope spectrometers (SCS and SCL) by Si:As BIB detectors [ Reynolds et al , 1989]. This increased the signal‐to‐noise ratio for most channels.…”

Section: The Crista‐2 Experimentsmentioning

confidence: 99%

The CRISTA‐2 mission

et al. 2002

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The second mission of the CRyogenic Infrared Spectrometers and Telescopes for the Atmosphere (CRISTA) experiment took place in August 1997. The experiment was flown aboard the ASTROnomical Shuttle PAllet Satellite (ASTRO‐SPAS) free‐flying platform launched by the NASA space shuttle. CRISTA analyzes the infrared radiation emitted by trace gases from the Earth limb in the altitude regime from the upper troposphere to the lower thermosphere. The main aim of CRISTA is to detect small‐scale dynamically induced structures in the distribution of trace constituents in the middle atmosphere. The instrument is therefore equipped with three telescopes that simultaneously collect the infrared radiation from three different air volumes. The high spatial density of the measurement grid obtained during the first CRISTA mission in November 1994, as well as the latitudinal coverage, was considerably improved by making use of newly developed satellite pointing and maneuvering capabilities. The altitude coverage was extended to include the upper troposphere where water vapor distributions are analyzed. Dynamically induced features are observed in practically all trace gases and at various spatial scales. The smallest scales that could be analyzed on the basis of the CRISTA data set are well below 100 km. Compared to the first mission, much more emphasis was laid on measurements in the upper mesosphere and lower thermosphere—this was possible because of higher radiometric sensitivities in some channels. Atomic oxygen, carbon dioxide, and ozone densities are derived in the upper mesosphere and lower thermosphere. The mission conditions allowed the study of polar stratospheric clouds (PSC) over the Antarctic and of polar mesospheric clouds (PMC) at high northern latitudes. For the first time, summer high latitude mesopause temperatures were retrieved from CO2 15‐μm spectra using a nonlocal thermodynamic equilibrium model. The derived temperatures compare well with a temperature climatology based on rocket soundings.

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Section: The Crista‐2 Experimentsmentioning

confidence: 99%

The CRISTA‐2 mission

et al. 2002

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“…Because BIB detector physics, models, and performance have been previously documented , Petroff et al 1985, Reynolds et al 1989), only the salient features of these devices are summarized here. BIB detectors effectively use the hopping conductivity phenomenon associated with "impurity banding" in relatively-heavily-doped semiconductors (specifically single-crystalline Si:As or Si:Sb for this discussion).…”

Section: Blocked Impurity Band Detectorsmentioning

confidence: 99%

A new large-well 1024×1024 Si:As detector for the mid-infrared

et al. 2005

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We present a description of a new 1024x1024 Si:As array designed for ground-based use from 5 -28 microns. With a maximum well depth of 5e6 electrons, this device brings large-format array technology to bear on ground-based midinfrared programs, allowing entry to the megapixel realm previously only accessible to the near-IR. The multiplexer design features switchable gain, a 256x256 windowing mode for extremely bright sources, and it is two-edge buttable. The device is currently in its final design phase at DRS in Cypress, CA. We anticipate completion of the foundry run in the beginning of 2006. This new array will enable wide field, high angular resolution ground-based follow up of targets found by space-based missions such as the Spitzer Space Telescope and the Widefield Infrared Survey Explorer (WISE).

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“…1 As & Sb have been successhlly developed using CVD. (Reynolds, et al 1992;Huffman, et al 1992) 1.3.3 Ge Blocked Impurity Band Detectors…”

Section: State Of the Art Of Silicon Blocked Impurity Band Detectorsmentioning

confidence: 99%

Advanced far infrared blocked impurity band detectors based on germanium liquid phase epitaxy

Olsen

1998

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is an equal opportunity employer. DISCLAIMERPortions of this document may be illegible in electronic image products. Images are produced from the best available original document. Germanium Blocked Impurity Band (BIB) detectors have been fabricated using Liquid Phase Epitaxy (LPE) to grow the high purity blocking layer and the heavily doped infrared absorbing layer, the major components of these devices. To achieve the necessary properties of both epilayers, very low structural and electrical defect concentrations are required. We have developed a high purity LPE process which can be used for the growth of high purity as well as purely doped Ge epilayers. We chose the low melting point, high purity metal lead (Pb) which has a negligible solubility in. solid Ge and does not form electronic levels in the band gap of Ge. We have identified the residual impurities Bi, P, LBNL-4 18

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Blocked impurity band hybrid infrared focal plane arrays for astronomy

Cited by 31 publications

References 1 publication

The CRISTA‐2 mission

The CRISTA‐2 mission

A new large-well 1024×1024 Si:As detector for the mid-infrared

Advanced far infrared blocked impurity band detectors based on germanium liquid phase epitaxy

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