Imaging the Aurora in the Far Ultraviolet from the IMAGE Spacecraft S. B. Mende, H. U. Frey, M. Lampton, J. Gerard, B. Hubert, S. Habraken, E. Renotte, C. Jamar, J. Spann, S. Fuselier, R. Gladstone, J. L. Burch Direct imaging of the magnetosphere by instruments on the IMAGE spacecraft are supplemented by observation of the global aurora, the footprint of magnetospheric particles. To assure the simultaneity of these observations and the measurement of the magnetospheric neutral hydrogen density three Far Ultraviolet (FUV) instruments are flown on IMAGE. The wavelength region 120-170 nm is most suitable for a downward-viewing auroral imager because it is only minimally contaminated by scattered sun light and the aurora can be observed even in the presence of high-latitude dayglow. The Wide-Band Imaging Camera (WIC) provides broad band ultraviolet images of the aurora for maximum spatial resolution by imaging the LBH N2 bands of the aurora. The Spectrographic Imager (SI), a dual wavelength channel monochromatic imager, images the Doppler-shifted Lyman alpha, the proton-induced aurora component in one channel and auroral 135.6 nm OI in the other. The GEO instrument observes the spatial distribution of the geocoronal emission, which is a measure of the neutral background 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 (few seconds) observing the aurora and the earth during each (2 min) spin. The first three month of data was analyzed mostly for validating the instrument performance. Images show that all instruments are capable of making sensitive measurements with high spatial resolution in the presence of summer sunlit conditions. The SI12 channel is capable to "see" the energetic protons through the detection of Doppler shifted Lyman-alpha, the WIC observes the aurora primarily in emissions of N2 and N while the SI13 channel is mostly sensitive to oxygen emission at O 135.6 nm. _______________ Presented at the Fall American Geophysical Union Meeting, San Francisco, CA., December 15-19, 2000