Abstract
The near-UV (190 to 270 nm) coronal emission lines present a unique opportunity to observe heliospheric plasmas between one and two solar radii. The near-UV coronagraph was specifically designed to obtain observations in these lines from a sounding rocket platform. The design demonstrates that high-resolution, two-dimensional coronal observations in the near-UV are readily achievable within the practical constraints of a sounding rocket. The near-UV coronagraph consists of a reflective, coronagraph telescope followed by an imaging channeled spectrograph. The telescope includes a Lyot stop and an occulter to minimize instrumentally scattered disk radiation. The choice of a mirror objective gives rise to a compact, achromatic telescope with excellent off-axis rejection and good imaging properties. The focal plane package combines a Fabry-Pérot interferometer with a tandem Wadsworth spectrograph to produce a channeled spectrum consisting of a series of two-dimensional (25 x 500 arcsec), narrow-bandpass (~0.1 Å) images at the instrument focal plane. The instrument will produce a number of high-spatial-resolution (< 1 arcsec) coronal images in a single flight.
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