Smith P H, Bell J F, Bridges N T, Britt D T, Gaddis L, Greeley R, Keller H U, Herkenhoff K E, Jaumann R, Johnson J R, Kirk R L, Lemmon M, Maki J N, Malin M C, Murchie S L, Oberst J, Parker T J, Reid R J, Sablotny R, Soderblom L A, Stoker C, Sullivan R, Thomas N, Tomasko M G, Wegryn E
Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ 85721, USA.
Science. 1997 Dec 5;278(5344):1758-65. doi: 10.1126/science.278.5344.1758.
Images of the martian surface returned by the Imager for Mars Pathfinder (IMP) show a complex surface of ridges and troughs covered by rocks that have been transported and modified by fluvial, aeolian, and impact processes. Analysis of the spectral signatures in the scene (at 440- to 1000-nanometer wavelength) reveal three types of rock and four classes of soil. Upward-looking IMP images of the predawn sky show thin, bluish clouds that probably represent water ice forming on local atmospheric haze (opacity approximately 0.5). Haze particles are about 1 micrometer in radius and the water vapor column abundance is about 10 precipitable micrometers.
火星探路者成像仪（IMP）传回的火星表面图像显示，其表面复杂，布满了山脊和沟槽，上面覆盖着因河流、风成和撞击作用而搬运和改变的岩石。对该场景光谱特征（波长在440至1000纳米之间）的分析揭示了三种岩石类型和四类土壤。黎明前天空的IMP向上拍摄图像显示出稀薄的蓝色云层，这可能代表在当地大气阴霾（不透明度约为0.5）上形成的水冰。阴霾颗粒半径约为1微米，水汽柱丰度约为10可沉淀微米。
