Ultraviolet imaging spectrometer (UVIS) for monitoring high-latitude precipitating patterns

Details Ultraviolet imaging spectrometer (UVIS) for monitoring high-latitude precipitating patterns Ultraviolet imaging spectrometer (UVIS) for monitoring high-latitude precipitating patterns

Jul 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993spie.2008..173m&link_type=abstract

Proc. SPIE Vol. 2008, p. 173-182, Instrumentation for Magnetospheric Imagery II, Supriya Chakrabarti; Ed.

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Scientific paper

Previously flown satellite imaging experiments have demonstrated the suitability of the vacuum ultraviolet region for remote sensing observations of auroral particle precipitation. In the wavelength region 120 - 145 nm, a downward viewing imager is uncontaminated by the earth albedo and the intensity of the auroral emissions in most cases is competitive with the rescattered light even during daylit conditions. These features permit the quantitative imaging of the auroral regions during day and night conditions. An instrument suitable for such observation which has adequate wavelength resolution to separate key spectral features and simultaneously observe the Doppler profile of the auroral Lyman alpha line was designed. This instrument, in its simplest form, consists of an F3.8 Rowland circle spectrography with an FUV intensified CCD at the focal region. The entrance slit is perpendicular to the orbit plane and parallel to the spin axis of the satellite. The field of view of the instantaneous slit image is 50 degrees in the direction perpendicular to the rotational axis and 1 degree parallel to the spin axis [i.e. in the direction parallel to the orbital plane]. The spectrography produces a two dimensional spectral image where one dimension represents luminosity distribution and the other wavelength dependence. The UV intensified CCD is programmed to pick up the luminosity distribution of various key spectral regions. During the 360 degree rotation, a complete luminosity map of the 50 degree wide region under the satellite is recorded. Depending on the satellite rotation rate and the wavelength of interest, more than one complete rotation will be needed to achieve the desired signal to noise ratio.

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