
Proceedings Paper
Near-field calibration of an objective spectrophotometer to NIST radiometric standards for the creation and maintenance of standard stars for ground- and space-based applicationsFormat | Member Price | Non-Member Price |
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Paper Abstract
NIST-calibrated detectors will be used by the ground-based 100mm diameter Astronomical Extinction
Spectrophotometer (AESoP) to calibrate the spectral energy distributions of bright stars to sub-1% per 1nm spectral
resolution element accuracy. AESoP will produce about a hundred spectroradiometrically calibrated stars for use by
ground- and space-based sensors. This will require accurate and near-continuous NIST calibration of AESoP, an
equatorially mounted objective spectrophotometer operating over the wavelength range 350nm – 1050nm using a CCD
detector.
To provide continuous NIST calibration of AESoP in the field a near-identical, removable 100mm diameter transfer
standard telescope (CAL) is mounted physically parallel to AESoP. The CAL transfer standard is calibrated by NIST
end-to-end, wavelength-by-wavelength at ~ 1nm spectral resolution. In the field, CAL is used in a near-field
configuration to calibrate AESoP. Between AESoP science observations, AESoP and CAL simultaneously observe clear
sub-apertures of a 400mm diameter calibration collimator. Monochromatic light measured simultaneously by AESoP and
CAL is dispersed by the objective grating onto the AESoP pixels measuring the same wavelength of starlight, thus
calibrating both wavelength and instrumental throughput, and simultaneously onto a unique low-noise CAL detector
providing the required throughput measurement. System sensitivity variations are measured by vertically translating the
AESoP/CAL pair so that CAL can observe the AESoP sub-aperture.
Details of this system fundamental to the calibration of the spectral energy distributions of stars are discussed and its
operation is described. System performance will be demonstrated, and a plan of action to extend these techniques firstly
into the near infrared, then to fainter stars will be described.
Paper Details
Date Published: 13 September 2012
PDF: 11 pages
Proc. SPIE 8450, Modern Technologies in Space- and Ground-based Telescopes and Instrumentation II, 84501S (13 September 2012); doi: 10.1117/12.927296
Published in SPIE Proceedings Vol. 8450:
Modern Technologies in Space- and Ground-based Telescopes and Instrumentation II
Ramón Navarro; Colin R. Cunningham; Eric Prieto, Editor(s)
PDF: 11 pages
Proc. SPIE 8450, Modern Technologies in Space- and Ground-based Telescopes and Instrumentation II, 84501S (13 September 2012); doi: 10.1117/12.927296
Show Author Affiliations
John T. McGraw, The Univ. of New Mexico (United States)
Peter C. Zimmer, The Univ. of New Mexico (United States)
Daniel C. Zirzow, The Univ. of New Mexico (United States)
John T. Woodward, National Institute of Standards and Technology (United States)
Peter C. Zimmer, The Univ. of New Mexico (United States)
Daniel C. Zirzow, The Univ. of New Mexico (United States)
John T. Woodward, National Institute of Standards and Technology (United States)
Keith R. Lykke, National Institute of Standards and Technology (United States)
Claire E. Cramer, National Institute of Standards and Technology (United States)
Susana E. Deustua, Space Telescope Science Institute (United States)
Dean C. Hines, The Univ. of New Mexico (United States)
Space Telescope Science Institute (United States)
Claire E. Cramer, National Institute of Standards and Technology (United States)
Susana E. Deustua, Space Telescope Science Institute (United States)
Dean C. Hines, The Univ. of New Mexico (United States)
Space Telescope Science Institute (United States)
Published in SPIE Proceedings Vol. 8450:
Modern Technologies in Space- and Ground-based Telescopes and Instrumentation II
Ramón Navarro; Colin R. Cunningham; Eric Prieto, Editor(s)
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