The AXAF CCD imaging spectrometer

G. P. Garmire, G. R. Ricker, M. W. Bautz, B. Burke, David Nelson Burrows, S. A. Collins, J. P. Doty, K. Gendreau, D. H. Lumb, John Andrew Nousek

Research output: Chapter in Book/Report/Conference proceedingConference contribution

8 Citations (Scopus)

Abstract

The Advanced X–ray Astrophysics Facility (AXAF) CCD Imaging Spectrometer (ACIS) is being developed as a core focal plane instrument for AXAF, the third of NASA’s Great Observatories which is scheduled for launch late in this decade. The instrument consists of an image recording array of charge coupled devices (CCD’s) and a linear arrangement of CCD’s to record the spectra formed by the objective grating spectrometer. Both arrays employ CCD’s with pixel dimensions which correspond to about 0.5 arc second samples of the image. The CCD’s provide moderate spectral resolution (E/ΔE ≈ 45(E(keV/5.9))1/2) and good detection efficiency over the energy range 0.5 to 10 keV. Spectral resolution of 200 or more is achievable using the objective grating with the grating array. Special clocking modes are planned for the CCD operation which will permit timing of temporal variations for point sources intensities down to 60 µ sec. The detection sensitivity for point sources exceeds 10-15 ergs/cm2/sec for exposures of 105 seconds. Radiation damage effects have been shown to degrade the energy resolution of CCD’s. Specially designed CCD pixel architecture has been employed together with shielding and low temperature operation to slow the effects of radiation damage. A heater has been included in the focal plane system design to anneal the CCD’s after radiation damage exceeds an acceptable level. The annealing will regain most of the lost performance.

Original languageEnglish (US)
Title of host publicationAIAA Space Programs and Technologies Conference, 1992
PublisherAmerican Institute of Aeronautics and Astronautics Inc, AIAA
StatePublished - 1992
EventAIAA Space Programs and Technologies Conference, 1992 - Huntsville, United States
Duration: Mar 24 1992Mar 27 1992

Other

OtherAIAA Space Programs and Technologies Conference, 1992
CountryUnited States
CityHuntsville
Period3/24/923/27/92

Fingerprint

radiation damage
Astrophysics
astrophysics
imaging spectrometers
Charge coupled devices
Spectrometers
charge coupled devices
spectrometer
spectral resolution
Imaging techniques
point source
pixel
Radiation damage
annealing
erg
energy
temporal variation
observatory
Spectral resolution
gratings

All Science Journal Classification (ASJC) codes

  • Aerospace Engineering
  • Space and Planetary Science

Cite this

Garmire, G. P., Ricker, G. R., Bautz, M. W., Burke, B., Burrows, D. N., Collins, S. A., ... Nousek, J. A. (1992). The AXAF CCD imaging spectrometer. In AIAA Space Programs and Technologies Conference, 1992 [AIAA-92-1473] American Institute of Aeronautics and Astronautics Inc, AIAA.
Garmire, G. P. ; Ricker, G. R. ; Bautz, M. W. ; Burke, B. ; Burrows, David Nelson ; Collins, S. A. ; Doty, J. P. ; Gendreau, K. ; Lumb, D. H. ; Nousek, John Andrew. / The AXAF CCD imaging spectrometer. AIAA Space Programs and Technologies Conference, 1992. American Institute of Aeronautics and Astronautics Inc, AIAA, 1992.
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title = "The AXAF CCD imaging spectrometer",
abstract = "The Advanced X–ray Astrophysics Facility (AXAF) CCD Imaging Spectrometer (ACIS) is being developed as a core focal plane instrument for AXAF, the third of NASA’s Great Observatories which is scheduled for launch late in this decade. The instrument consists of an image recording array of charge coupled devices (CCD’s) and a linear arrangement of CCD’s to record the spectra formed by the objective grating spectrometer. Both arrays employ CCD’s with pixel dimensions which correspond to about 0.5 arc second samples of the image. The CCD’s provide moderate spectral resolution (E/ΔE ≈ 45(E(keV/5.9))1/2) and good detection efficiency over the energy range 0.5 to 10 keV. Spectral resolution of 200 or more is achievable using the objective grating with the grating array. Special clocking modes are planned for the CCD operation which will permit timing of temporal variations for point sources intensities down to 60 µ sec. The detection sensitivity for point sources exceeds 10-15 ergs/cm2/sec for exposures of 105 seconds. Radiation damage effects have been shown to degrade the energy resolution of CCD’s. Specially designed CCD pixel architecture has been employed together with shielding and low temperature operation to slow the effects of radiation damage. A heater has been included in the focal plane system design to anneal the CCD’s after radiation damage exceeds an acceptable level. The annealing will regain most of the lost performance.",
author = "Garmire, {G. P.} and Ricker, {G. R.} and Bautz, {M. W.} and B. Burke and Burrows, {David Nelson} and Collins, {S. A.} and Doty, {J. P.} and K. Gendreau and Lumb, {D. H.} and Nousek, {John Andrew}",
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Garmire, GP, Ricker, GR, Bautz, MW, Burke, B, Burrows, DN, Collins, SA, Doty, JP, Gendreau, K, Lumb, DH & Nousek, JA 1992, The AXAF CCD imaging spectrometer. in AIAA Space Programs and Technologies Conference, 1992., AIAA-92-1473, American Institute of Aeronautics and Astronautics Inc, AIAA, AIAA Space Programs and Technologies Conference, 1992, Huntsville, United States, 3/24/92.

The AXAF CCD imaging spectrometer. / Garmire, G. P.; Ricker, G. R.; Bautz, M. W.; Burke, B.; Burrows, David Nelson; Collins, S. A.; Doty, J. P.; Gendreau, K.; Lumb, D. H.; Nousek, John Andrew.

AIAA Space Programs and Technologies Conference, 1992. American Institute of Aeronautics and Astronautics Inc, AIAA, 1992. AIAA-92-1473.

Research output: Chapter in Book/Report/Conference proceedingConference contribution

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T1 - The AXAF CCD imaging spectrometer

AU - Garmire, G. P.

AU - Ricker, G. R.

AU - Bautz, M. W.

AU - Burke, B.

AU - Burrows, David Nelson

AU - Collins, S. A.

AU - Doty, J. P.

AU - Gendreau, K.

AU - Lumb, D. H.

AU - Nousek, John Andrew

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N2 - The Advanced X–ray Astrophysics Facility (AXAF) CCD Imaging Spectrometer (ACIS) is being developed as a core focal plane instrument for AXAF, the third of NASA’s Great Observatories which is scheduled for launch late in this decade. The instrument consists of an image recording array of charge coupled devices (CCD’s) and a linear arrangement of CCD’s to record the spectra formed by the objective grating spectrometer. Both arrays employ CCD’s with pixel dimensions which correspond to about 0.5 arc second samples of the image. The CCD’s provide moderate spectral resolution (E/ΔE ≈ 45(E(keV/5.9))1/2) and good detection efficiency over the energy range 0.5 to 10 keV. Spectral resolution of 200 or more is achievable using the objective grating with the grating array. Special clocking modes are planned for the CCD operation which will permit timing of temporal variations for point sources intensities down to 60 µ sec. The detection sensitivity for point sources exceeds 10-15 ergs/cm2/sec for exposures of 105 seconds. Radiation damage effects have been shown to degrade the energy resolution of CCD’s. Specially designed CCD pixel architecture has been employed together with shielding and low temperature operation to slow the effects of radiation damage. A heater has been included in the focal plane system design to anneal the CCD’s after radiation damage exceeds an acceptable level. The annealing will regain most of the lost performance.

AB - The Advanced X–ray Astrophysics Facility (AXAF) CCD Imaging Spectrometer (ACIS) is being developed as a core focal plane instrument for AXAF, the third of NASA’s Great Observatories which is scheduled for launch late in this decade. The instrument consists of an image recording array of charge coupled devices (CCD’s) and a linear arrangement of CCD’s to record the spectra formed by the objective grating spectrometer. Both arrays employ CCD’s with pixel dimensions which correspond to about 0.5 arc second samples of the image. The CCD’s provide moderate spectral resolution (E/ΔE ≈ 45(E(keV/5.9))1/2) and good detection efficiency over the energy range 0.5 to 10 keV. Spectral resolution of 200 or more is achievable using the objective grating with the grating array. Special clocking modes are planned for the CCD operation which will permit timing of temporal variations for point sources intensities down to 60 µ sec. The detection sensitivity for point sources exceeds 10-15 ergs/cm2/sec for exposures of 105 seconds. Radiation damage effects have been shown to degrade the energy resolution of CCD’s. Specially designed CCD pixel architecture has been employed together with shielding and low temperature operation to slow the effects of radiation damage. A heater has been included in the focal plane system design to anneal the CCD’s after radiation damage exceeds an acceptable level. The annealing will regain most of the lost performance.

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M3 - Conference contribution

BT - AIAA Space Programs and Technologies Conference, 1992

PB - American Institute of Aeronautics and Astronautics Inc, AIAA

ER -

Garmire GP, Ricker GR, Bautz MW, Burke B, Burrows DN, Collins SA et al. The AXAF CCD imaging spectrometer. In AIAA Space Programs and Technologies Conference, 1992. American Institute of Aeronautics and Astronautics Inc, AIAA. 1992. AIAA-92-1473