Results from the Mars Pathfinder camera

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

Research output: Contribution to journalReview articlepeer-review

206 Scopus citations

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.

Original languageEnglish (US)
Pages (from-to)1758-1765
Number of pages8
JournalScience
Volume278
Issue number5344
DOIs
StatePublished - Dec 5 1997

ASJC Scopus subject areas

  • General

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