Surface units of MER landing sites as seen by Mars Express/HRSC color data

Details Surface units of MER landing sites as seen by Mars Express/HRSC color data Surface units of MER landing sites as seen by Mars Express/HRSC color data

Dec 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agufm.p53a1440c&link_type=abstract

American Geophysical Union, Fall Meeting 2008, abstract #P53A-1440

Other

0305 Aerosols And Particles (0345, 4801, 4906), 0540 Image Processing, 3255 Spectral Analysis (3205, 3280), 5464 Remote Sensing, 5470 Surface Materials And Properties

Scientific paper

Imaging spectrometry and color data of the High Resolution Stereo Camera (HRSC, [1]) onboard Mars Express complement each other for mapping outcrop types. The HRSC dataset is the only one that currently combines extensivee coverage of the planet (75% and more in the future), 200 m/pixel spatial resolution or better and 5-band radiation filtering. Our current work shows the potential and limitations of HRSC color data as a visual support and as multispectral images. The MER landing sites provide us the opportunity to compare HRSC image analysis to in-situ observations[2, 3]. HRSC has five color filters in the visible and near-infrared that are designed for visual interpretation and the mapping of various surface units [1]. HRSC is sensitive to materials with absorption features in the visible and near-infrared up to 1 μm. Thus, oxide- rich red dust and basalts (pyroxenes) can be mapped, as well as very bright components like water ice [4, 5]. All broadband channels are acquired by separated cameras oriented at varying anglea from the normal to the surface. This implies that a given spectrum results from different proportions of shade at each wavelength. Thus, shade affects the shape of HRSC spectra in a different way from pixel to pixel. This contribution has to be considered when analyzing HRSC spectra in order to provide compositional and surface property information. We perform Spectral Mixing Analysis (SMA, [6, 7]) of HRSC data by using the Multiple-Endmember Linear Spectral Unmixing Model (MELSUM) [8, 9, 10]. Results for shade and residuals are related to topography, surface roughness, aerosol scattering, the geometry of illumination/observation and instrumental noise [9]. Comparisons with surface roughness-specific studies [11,12, 13] are used to better discriminate the aforementionned effects. References [1] Neukum G. et al. (2004) ESA SP, 90, 1151-1154. [2] Johnson et al., (2006) JGR 112. [3] Johnson et al. (2007) GRL 34. [3].[4] McCord T. B. et al. (2007) JGR 112. [5] McCord T. B. et al. (2006) LPSC 1757. [6] Adams et al. (1986), JGR 91. [7] Adams and Gillespie, Cambridge Univ. Press. [8] Combe J.-Ph. et al. (2008) PSS, 54/7. [9] Combe et al. (2008), LPSC 2381. [10] Combe J.-Ph. et al., submitted to Earth and Planet. Sci. Let.[11]Mushkin and Gillespie (2006), GRL 33. [12] Pinet et al. (2006) LPSC 1120. [13] Jehl et al. (2008), JGR 113. Work supported by the HRSC team and the NASA Mars Data Analysis Program NN-X07AZ37G.

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