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  • 1
    Electronic Resource
    Electronic Resource
    Observing and Calibration Strategies for FIR Imaging with SIRTF (2000)
    Springer
    Experimental astronomy 10 (2000), S. 403-413 
    Details
    ISSN: 1572-9508
    Keywords: FIR detectors ; MIPS ; SIRTF ; space instrumentation
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract We present data from a 16×32 array of unstressed Ge:Gadetectors, showing the long time constant responses and hook effectcharacteristic of these devices. This array is half the size of the70 μm imaging array planned for MIPS, the Multiband ImagingPhotometer for SIRTF. We present simulations of the FIR (farinfrared) sky as viewed by a MIPS array, including realistic noiseeffects and extraction of point sources with a standard photometrypackage, showing that the photometric goals of MIPS are attainablewith the current array performance and using standard analysistechniques. Previous calculations by Heim et al. (1998) haddetermined that MIPS would achieve 5-σ detections of ≤1 mJy at 70 μm in 2000 s; the simulations presented hereobtain results consistent with those calculations.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1023/A:1008027931585
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    Paper (German National Licenses)
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  • 2
    Electronic Resource
    Electronic Resource
    The MPE/UCB far-infrared imaging Fabry-Perot interferometer (FIFI) (1991)
    Springer
    International journal of infrared and millimeter waves 12 (1991), S. 859-884 
    Details
    ISSN: 1572-9559
    Keywords: Spectrometer ; Infrared Astronomy ; Infrared Techniques ; Detector Array ; Cryogenic Electronics ; Fabry-Perot ; Cryogenic ; Imaging ; Instrument Function
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract FIFI is an imaging spectrometer with two or three Fabry-Perot interferometers (FPI) in series for airborne astronomical observations in the far-infrared range (λ=40...200μm). It employs 5×5 arrays of photoconducting detectors and offers spectral resolutions as small as 2km/s. Resolution and bandwidth can be set over a wide range to match a variety of astronomical sources. Cryogenic optics minimizes thermal background radiation and provides for in-flight step tunable spatial resolution. At 158 μm wavelength the background-limited NEP is 3 × 10-15W/ℚHz at 40 km/s resolution and with two FPI's; with three FPI's the expected NEP is ≤10-15W√Hz at 5 km/s resolution. The frequency-chopping mode of the high-resolution Fabry-Perot allows for line detection in extended objects. Absolute internal flux calibration ensures adequate “flat fielding” of the array elements.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF01009647
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  • 3
    Electronic Resource
    Electronic Resource
    Stressed and unstressed Ge:Ga detector arrays for airborne astronomy (1992)
    Springer
    International journal of infrared and millimeter waves 13 (1992), S. 1689-1707 
    Details
    ISSN: 1572-9559
    Keywords: Infrared Astronomy ; Infrared Techniques ; Photoconductive Detector Array ; Cryogenic Electronics
    Source: Springer Online Journal Archives 1860-2000
    Topics: Physics
    Notes: Abstract 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 (5×5) arrays are designed for a new cryogenically cooled spectrometer, the MPE/UCB Far-Infrared Imaging Fabry-Perot Interferometer (FIFI). All of the pixels for the stressed array performed well on the first flights with FIFI; 25% of the detectors in the array are more sensitive than our best single element detector, with background limited noise equivalent powers (NEPs)≲3.0×10−15 W Hz−1/2 at 158 μm and 40 km s−1 spectral resolution. The average array element performs within±15% of this value. With a bias field of 0.1 V/cm, the average detector response is 20±6 Amp/Watt at 158 μm. The cutoff wavelength and response also compare well with our single element detectors. The unstressed array delivers significantly better performance than our single element detector due to the lower thermal background in the new spectrometer. The average background limited NEp at 88 μm and 35 km s−1 spectral resolution is ∼7×10−15 W Hz−1/2. The least sensitive pixel is only 40% less sensitive. The unstressed array response at 88 μm with a bias field of 1 V/cm is 5±1 Amp/Watt. Twenty four of the 25 elements worked on the first flights-on subsequent flights all channels have worked. Some of the exciting new science possible with far-infrared detector arrays is also discussed.
    Type of Medium: Electronic Resource
    URL: http://dx.doi.org/10.1007/BF01010739
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  • 4
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    Stressed detector arrays for airborne astronomy (1989)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: The development of stressed Ge:Ga detector arrays for far-infrared astronomy from the Kuiper Airborne Observatory (KAO) is discussed. Researchers successfully constructed and used a three channel detector array on five flights from the KAO, and have conducted laboratory tests of a two-dimensional, 25 elements (5x5) detector array. Each element of the three element array performs as well as the researchers' best single channel detector, as do the tested elements of the 25 channel system. Some of the exciting new science possible with far-infrared detector arrays is also discussed.
    Keywords: ASTRONOMY
    Type: NASA, Ames Research Center, Proceedings of the Third Infrared Detector Technology Workshop; p 247-258
    Format: application/pdf
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    NASA TECHNICAL REPORTS
  • 5
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    Improved low frequency stability of bolometric detectors (1990)
    In:  Other Sources
    Details
    Publication Date: 2019-07-12
    Description: An ac bridge readout system has been developed that greatly improves the low-frequency stability of bolometric detectors. The readout can be implemented with a simple circuit appropriate for use in space applications. A matched pair of detectors was used in the readout to achieve system noise within a factor of two of the fundamental noise limit of the detectors at frequencies as low as 10 mHz. The low-frequency stability of the readout system allows slower, more sensitive detectors to be used in many applications, and it facilitates observing strategies that are well suited to spaceborne observations.
    Keywords: ASTRONOMY
    Type: IEEE Transactions on Nuclear Science (ISSN 0018-9499); 37; 566-572
    Format: text
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    NASA TECHNICAL REPORTS
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