Results from the Mars Pathfinder camera

P. H. Smith; J. F. Bell; N. T. Bridges; D.T. Britt; Lisa R. Gaddis; R. Greeley; H.U. Keller; Kenneth E. Herkenhoff; R. Jaumann; J. R. Johnson; Randolph L. Kirk; M. Lemmon; J.N. Maki; M.C. Malin; S.L. Murchie; J. Oberst; T. J. Parker; R.J. Reid; R.M. Sablotny; Laurence A. Soderblom; C. Stoker; R. Sullivan; N. Thomas; M.G. Tomasko; W. Ward; E. Wegryn

doi:10.1126/science.278.5344.1758

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Results from the Mars Pathfinder camera

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Abstract

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 ∼0.5). Haze particles are about 1 micrometer in radius and the water vapor column abundance is about 10 precipitable micrometers.

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P. H. Smith, J. F. Bell, N. T. Bridges, D.T. Britt, Lisa R. Gaddis, R. Greeley, H.U. Keller, Kenneth E. Herkenhoff, R. Jaumann, J. R. Johnson, Randolph L. Kirk, M. Lemmon, J.N. Maki, M.C. Malin, S.L. Murchie, J. Oberst, T. J. Parker, R.J. Reid, R.M. Sablotny, Laurence A. Soderblom, C. Stoker, R. Sullivan, N. Thomas, M.G. Tomasko, W. Ward, E. Wegryn. 1997. Results from the Mars Pathfinder camera. https://doi.org/10.1126/science.278.5344.1758

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