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Proceedings Paper

Flat field of UVCS detectors for early part of SOHO mission
Author(s): Mario L. Cosmo; Peter L. Smith; Nigel Atkins; R. M. Suleiman; Larry D. Gardner; John L. Kohl
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Paper Abstract

The Ultraviolet Coronagraph Spectrometer (UVCS) on the Solar and Heliospheric Observatory (SOHO) comprises two telescopes and two spectrometer channels for spatially resolved ultraviolet spectral diagnostics of the solar corona. The principal lines for which the two channels are optimized are the H I 'Lyman-(alpha) ' line at 121.5 nm and the O VI (O5+) doublet at 103.2 and 103.7 nm. An 'in-flight' method, using observations of stars and scattered solar disk light, has been devised to determine the flat field function, i.e., the relative detection efficiency of the detector pixels. We present the details and results of this process. Local pixel-to-pixel efficiency variation is found to be, typically, about plus or minus 9% to plus or minus 17% (1 (sigma) ) for the H I Lyman-(alpha) channel and plus or minus 9% for the O VI channel.

Paper Details

Date Published: 25 November 1999
PDF: 7 pages
Proc. SPIE 3764, Ultraviolet and X-Ray Detection, Spectroscopy, and Polarimetry III, (25 November 1999); doi: 10.1117/12.371094
Show Author Affiliations
Mario L. Cosmo, Harvard-Smithsonian Ctr. for Astrophysics (United States)
Peter L. Smith, Harvard-Smithsonian Ctr. for Astrophysics (United States)
Nigel Atkins, Harvard-Smithsonian Ctr. for Astrophysics (United States)
R. M. Suleiman, Harvard-Smithsonian Ctr. for Astrophysics (United States)
Larry D. Gardner, Harvard-Smithsonian Ctr. for Astrophysics (United States)
John L. Kohl, Harvard-Smithsonian Ctr. for Astrophysics (United States)


Published in SPIE Proceedings Vol. 3764:
Ultraviolet and X-Ray Detection, Spectroscopy, and Polarimetry III
Silvano Fineschi; Bruce E. Woodgate; Randy A. Kimble, Editor(s)

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