"snapshops" in which the high apogee and the wide field of view of EUV provide in a single exposure a map of the entire plasmasphere. EUV consists of three identical sensor heads, each having a field of view of 30° in diameter. These sensors are tilted relative to one another to cover a fan-shaped field of 84° by 30°, which is swept across the plasmasphere by the spin of the satellite. EUV's spatial resolution is 0.6° of 0.1 RE in the equatorial plane seen from apogee. The sensitivity is 1.9 count/second-Rayleigh, sufficient to map the position of the plasmapause with a time resolution of 10 minutes. Far Ultraviolet Imager (FUV) The IMAGE satellite instrument complement includes three Far Ultraviolet (FUV) instruments. In the wavelength region 120-190 nm, a downward-viewing auroral imager is only minimally contaminated by sunlight, scattered from clouds and ground, and radiance of the aurora observed in a nadir viewing geometry can be observed in the presence of the high-latitude dayglow. The Wideband Imaging Camera (WIC) provides broadband ultraviolet images of the aurora for maximum spatial and temporal resolution by imaging the LBH N2 bands of the aurora. The Spectrographic Imager (SI), a monochromatic imager, images different types of aurora, filtered by wavelength. By measuring the Doppler-shifted Lyman-a, the proton-induced component of the aurora can be imaged separately. Finally, the GEO instrument observes the distribution of the geocoronal emission, which is a measure of the neutral background density source for charge exchange in the magnetosphere. The FUV instrument complement looks radially outward from the rotating IMAGE satellite and, therefore, it spends only a short time observing the aurora and the Earth during each spin (120-seconds period). Detailed descriptions of the WIC, SI, GEO, and their individual performance validations can be found in the January 2000 issue of the Space Science Reviews. One primary requirement of the FUV instrument is to maximize photon collection efficiency and use efficiently the short time available for exposures. The FUV auroral imagers WIC and SI both have wide fields of view and take data continuously as the auroral region proceeds through the field of view. To minimize data volume, multiple images are taken and electronically co-added by suitably shifting each image to compensate for the spacecraft rotation. In order to minimize resolution loss, the images have to be distortion -corrected in real time for both WIC and SI prior to co-adding. The distortion