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High resolution flat crystal spectrometer for the Shanghai EBIT
We report on a high resolution flat crystal spectrometer designed for the Shanghai EBIT. Its energy range is from 0.5 to 10 keV. Three crystals can be installed in the vacuum chamber simultaneously, a...

Invited Article: Deep Impact instrument calibration

Rev. Sci. Instrum. 79, 091301 (2008); doi:10.1063/1.2972112

Published 25 September 2008

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Kenneth P. Klaasen,1 Michael F. A'Hearn,2 Michael Baca,3 Alan Delamere,4 Mark Desnoyer,5 Tony Farnham,2 Olivier Groussin,2 Donald Hampton,6 Sergei Ipatov,2 Jianyang Li,2 Carey Lisse,7 Nickolaos Mastrodemos,1 Stephanie McLaughlin,2 Jessica Sunshine,2 Peter Thomas,5 and Dennis Wellnitz2
1Jet Propulsion Laboratory, California Institute of Technology, Mail Stop 306-392, 4800 Oak Grove Dr., Pasadena, California 91109, USA
2Department of Astronomy, University of Maryland, College Park, Maryland 20742-2421, USA
3Science Applications International Corporation, 5180 Parkstone Drive, Suite 100, Chantilly, Virginia 20151, USA
4Delamere Support Services, 525 Mapleton Ave., Boulder, Colorado 80304, USA
5Cornell University, Space Science Building, Ithaca, New York 14853, USA
6Ball Aerospace and Technologies, 1600 Commerce St., Boulder, Colorado 80301, USA
7Johns Hopkins University Applied Physics Laboratory, SD/SRE, MP3/W-155, 7707 Montpelier Road, Laurel, Maryland 20723, USA
Calibration of NASA's Deep Impact spacecraft instruments allows reliable scientific interpretation of the images and spectra returned from comet Tempel 1. Calibrations of the four onboard remote sensing imaging instruments have been performed in the areas of geometric calibration, spatial resolution, spectral resolution, and radiometric response. Error sources such as noise (random, coherent, encoding, data compression), detector readout artifacts, scattered light, and radiation interactions have been quantified. The point spread functions (PSFs) of the medium resolution instrument and its twin impactor targeting sensor are near the theoretical minimum [~1.7  pixels full width at half maximum (FWHM)]. However, the high resolution instrument camera was found to be out of focus with a PSF FWHM of ~9  pixels. The charge coupled device (CCD) read noise is ~1 DN. Electrical cross-talk between the CCD detector quadrants is correctable to <2 DN. The IR spectrometer response nonlinearity is correctable to ~1%. Spectrometer read noise is ~2 DN. The variation in zero-exposure signal level with time and spectrometer temperature is not fully characterized; currently corrections are good to ~10 DN at best. Wavelength mapping onto the detector is known within 1  pixel; spectral lines have a FWHM of ~2  pixels. About 1% of the IR detector pixels behave badly and remain uncalibrated. The spectrometer exhibits a faint ghost image from reflection off a beamsplitter. Instrument absolute radiometric calibration accuracies were determined generally to <10% using star imaging. Flat-field calibration reduces pixel-to-pixel response differences to ~0.5% for the cameras and <2% for the spectrometer. A standard calibration image processing pipeline is used to produce archival image files for analysis by researchers. ©2008 American Institute of Physics
History: Received 9 August 2007; accepted 18 July 2008; published 25 September 2008
Permalink: http://link.aip.org/link/?RSINAK/79/091301/1
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KEYWORDS and PACS

Keywords
PACS
  • 95.55.Fw
    Space-based ultraviolet, optical, and infrared telescopes
  • 95.55.Qf
    Photometric, polarimetric, and spectroscopic instrumentation for astronomy
  • 95.55.Pe
    Lunar, planetary, and deep-space probes
  • 96.30.Cw
    Comets
  • 07.57.Ty
    Infrared spectrometers, auxiliary equipment, and techniques
  • 07.57.Kp
    Bolometers; infrared, submillimeter wave, microwave, and radiowave receivers and detectors
  • 06.20.fb
    Measurement standards and calibration
  • YEAR: 2008

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PUBLICATION DATA

ISSN:
0034-6748 (print)   1089-7623 (online)
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