RESULTS FROM THE MARS PATHFINDER CAMERA

Images of the martian surface returned by the Imager for Mars Pathfind er (IMP) show a complex surface of ridges and troughs covered by rocks that have been transported and modified by fluvial, aeolian, and impa ct processes. Analysis of the spectral signatures in the scene (at 440 - to 1000-nanometer wavelength) reveal three types of rock and four cl asses of soil. Upward-looking IMP images of the predawn sky show thin, bluish clouds that probably represent water ice forming on local atmo spheric haze (opacity similar to 0.5). Haze particles are about 1 micr ometer in radius and the water vapor column abundance is about 10 prec ipitable micrometers.