3 edition of Performance of multiplexed GE:GA detector arrays in the far infrared found in the catalog.
Performance of multiplexed GE:GA detector arrays in the far infrared
by National Aeronautics and Space Administration, Ames Research Center, National Technical Information Service, distributor in Moffett Field, Calif, [Springfield, Va
Written in English
|Statement||Jam Farhoomand, Craig McCreight.|
|Series||NASA technical memorandum -- 102275.|
|Contributions||McCreight, Craig R., Ames Research Center.|
|The Physical Object|
We present initial test results for far-infrared arrays built at the University of Arizona using Ge:Ga photoconductors and low temperature readouts operating at a temperature of 2 K. We also present separate test results for the Hughes CRC multiplexer used in this by: 7. Among the direct detectors, low-temperature bolometers currently offer the highest sensitivity from the far-infrared to millimetre-wave region of the electromagnetic spectrum providing background limited performance with NEP up to ∼(–3)×10 −19 W/Hz 1/2 at operation temperature ∼– mK.
We have constructed and used two dimensional arrays of both unstressed and stressed Ge:GA photoconductive detectors for far-infrared astronomy from the Kuiper Airborne Observatory (KAO). The 25 element (5 x 5) arrays are designed for a new cryogenically cooled spectrometer, the MPE/UCB Far-Infrared Imaging Fabry-Perot Interferometer (FIFI).Cited by: "In-flight Far-Infrared Performance of the CIRS Instrument on Cassini." Brasunas, J., B. Lakew, and R. Fettig. "A comment on the reported detectivity of a new uncooled thermal infrared detector." Sensors and Actuators A,
Submillimeter cameras now have up to 10^4 pixels (SCUBA 2). The proposed CCAT meter submillimeter telescope will feature a 1 degree field-of-view. Populating the focal plane at microns would require more than 10^6 photon-noise limited pixels. To ultimately achieve this scaling, simple detectors and high-density multiplexing are essential. Agnese P, Cigna C, Pornin J-L (plus ten authors) () Filled bolometer arrays for Herschel/PACS in millimeter and submillimeter detectors for astronomy. Proc SPIE – Google Scholar Boggess NW, Mather JC, Weiss R (plus 15 authors) () The COBE Mission: Its design and performance two years after the by: 2.
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PERFORMANCE OF MULTIPLEXED GE:GA DETECTOR ARRAYS IN THE FAR INFRARED Jam Farhoomand* and Craig McCreight Ames Research Center SUMMARY The performance of two multielement, multiplexed Ge:Ga linear arrays under low-background conditions has been investigated. The on-focal-plane switching is accomplished by MOSFET.
The performance of two multi-element, multiplexed Ge:Ga linear arrays under low-background conditions was investigated. The on-focal switching is accomplished by MOSFET switches, and the integrated charge is made available through MOSFET source followers. Get this from a library.
Performance of multiplexed GE:GA detector arrays in the far infrared. [Jam Farhoomand; Craig McCreight; Ames Research Center.].
The performance of two multi-element, multiplexed Ge:Ga linear arrays under low-background conditions was investigated. The on-focal switching is accomplished by MOSFET switches, and the integrated charge is made available through MOSFET source : Craig Mccreight and Jam Farhoomand. The performance of a multielement Ge:Ga linear array under low-background conditions is investigated.
On-focal plane switching is accomplished by MOSFET switches and the integrated charge is made available through MOSFET source : Jam Farhoomand, Craig R. McCreight. The performance of a multielement Ge:Ga linear array under low-background conditions is investigated.
On-focal plane switching is accomplished by MOSFET switches and the integrated charge is made available through MOSFET source followers. Evaluation of a far infrared Ge:Ga multiplexed detector array. The performance of a multielement Ge:Ga linear array under low-background conditions is investigated.
On-focal plane switching is accomplished by MOSFET switches and the integrated charge is made available through MOSFET source followers.
The tests were conducted at microns Author: Jam Farhoomand and Craig Mccreight. Stratospheric Observatory for Infrared Astronomy (SOFIA). Arrays of slightly stressed Ge:Ga detectors cover a wavelength range from 55 to micron for PACS and from 40 to micron for FIFI LS, whereas arrays of highly stressed Ge:Ga detectors cover a wavelength range from to micron for PACS and to micron for FIFI LS.
The unstressed Ge:Ga detector array will cover the wavelength range from 40 to microns, and the stressed Ge:Ga detector array from to microns.
Due to advanced detector materials and microelectronics, large scanning and staring focal plane arrays (FPA) with few defects are now readily available in the short wave- length infrared (SWIR; 1 to 3 μm), medium wavelength infrared (MWIR; ≈3 to 5 μm), and long wavelength infrared (LWIR; ≈8 to File Size: 1MB.
The arrays, based on earlier 5 X 5 detector arrays used on the KAO, will be for our new instrument, the Far Infrared Field Imaging Line Spectrometer (FIFI LS). The unstressed Ge:Ga detector array will cover the wavelength range from 40 to micrometers, and the stressed Ge:Ga detector array from to by: 6.
We are developing a far-infrared Ge:Ga monolithic array detector for the future space telescope SPICA. We demonstrate the performance of our detector by showing the test results of 5×5 pixel prototype detectors. These detectors worked properly and they showed the expected performance.
This banner text can have markup. web; books; video; audio; software; images; Toggle navigation. Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy V. Editor(s): Wayne S. Holland; Jonas Zmuidzinas. Development of a far-infrared Ge:Ga monolithic array for a possible application to SPICA First implementation of TES bolometer arrays with SQUID-based multiplexed readout on a balloon-borne platform.
SAFARI's aggressive science goals drive the development of a unique detector system combining large-format Transition Edge Sensor arrays and frequency division multiplexed SQUID readout with a.
32 Ge:Ga array (Young et al. ) operates between 50 and m, while a 2; 20 stressed Ge:Ga device (Schnurr et al. ) operates at m. These detectors have multiple time constants of response: a rapid one associated with tra-ditional photoconductivity in the bulk of the detector andCited by: The detection of far-infrared (far-IR) and sub-mm-wave radiation is resistant to the commonly employed techniques in the neighbouring microwave and IR frequency bands.
In this wavelength detection range the use of solid state detectors has been hampered for the reasons of transit time of charge carriers being larger than the time of one Cited by: Such arrays are highly demanded for upcoming far-infrared astronomy missions with space and airborne telescopes.
However, bulk GaAs photoconductors have only limited sensitivity, due to low absorption and high dark currents. Considerable improvement of the detector performance can be expected from the development of GaAs blocked impurity band. The Ge:Ga arrays were manufactured by hand: individual Ge:Ga pixels or linear strips of pixels are typically mounted next to one another to form far-infrared photoconductor arrays.
Recent developments have enabled the fabrication of monolithic 2D arrays, with pixels formed using lithographic and wet-etching by: 1 Institute of Applied Physics, Military University of Technology, 2 Kaliskiego Str.,Warsaw, Poland ; 2 Institute of Semiconductor Physics of the Ukrainian National Academy of Sciences, Kiev,41 Nauki Ave, Ukraine.
Key elements in attaining this level of performance are the Ge:Ga detectors materials and the cryogenic CRC readout electronics.
We present laboratory data for a 16 X 32 prototype of the array, and describe the plans for the construction of the qualification and flight by: current noise in photon detectors, by contrast, decreases exponentially with decreasing temperature.
Both bolometers and Ge:Ga photoconductors are used in the µm range. The photoconductors operate at higher temperatures, and multiplexed element arrays have been built for SIRTF6. However, quantum.SLAC Microresonator Radio Frequency (SMuRF) Electronics for Future CMB and Sub-millimeter Surveys Shawn W.
Henderson a,b, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy VIII, Proc. SPIEp. S, July\Development of a Microwave SQUID-Multiplexed TES Array for MUSTANG-2," Journal of Cited by: