Seasonal Comparison of Mars NIR Principal Components

Details Seasonal Comparison of Mars NIR Principal Components Seasonal Comparison of Mars NIR Principal Components

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003dps....35.1413k&link_type=abstract

American Astronomical Society, DPS meeting #35, #14.13; Bulletin of the American Astronomical Society, Vol. 35, p.936

Astronomy and Astrophysics

Astronomy

Scientific paper

We have gathered near-infrared spectral image sets from the NASA IRTF during the 1995, 1996--7, 1999, and 2001 oppositions which cover nearly three full Martian seasons (late northern spring through northern fall). The images were acquired using the NSFCAM over the spectral range from 1.5--2.5 μ m and 2.9--4.1 μ m. We have been able to show that the technique of principal components analysis (PCA) is able to map water ice coverage with less surface confusion than standard band-ratio maps [1]. We will present here our most complete set of such PCA maps showing the growth of the aphelion cloud belt and changes in the north polar hood.
PCA has also been used to analyze retrieved spectra from the Mars Global Surveyor Thermal Emission Spectrometer (MGS-TES) [2]. The most significant components are used to create spectral endmembers for the data set though a least-squares linear combination comparison to mineral spectral libraries. We present preliminary results of a similar study in the near-infrared in an effort to characterize the Martian surface and the Martian airborne dust over this spectral range.
References [1] Klassen, D. R., et al. (1999) Icarus, 138, 36.
[2] Bandfield, J. L., et al. (2000) J. Geophys. Res., 105, 9573.
Acknowledgements This work is supported by a grant from the NASA Mars Data Analysis Program.

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