Physics
Scientific paper
Dec 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003agufm.p11a..02s&link_type=abstract
American Geophysical Union, Fall Meeting 2003, abstract #P11A-02
Physics
5464 Remote Sensing, 5470 Surface Materials And Properties, 5494 Instruments And Techniques
Scientific paper
The SELENE mission to the Moon in 2005 includes the Multiband Imager (MI) [1], a visible/near-infrared imaging spectrometer, and the Terrain Camera (TC), a 10m panchromatic stereoimager for global topography. The ˜1TB of TC data will take years to reduce; initial photometric correction of MI data will not include the effect of topography. We present a method for prioritizing analysis of TC data so topography can be included in photometric correction of MI data at the earliest time to regions of the lunar surface where the effects of topography are most significant. We have calculated the general quantified dependence of photometric correction on incidence angle, emission angle, phase angle, and local topographic slopes. To calculate photometric correction we use the method used for Clementine [2,3] with the following corrections: The factor of 2 is included in the XL function (see [3]), P(α ,g) = (1-g2)/(1+g2+2gcos(α ))1.5, and g1 = D*R30 + E. In order to predict the topography of the Moon to determine the regional distribution of local slopes at the resolution of MI (20m and 62m), we performed a fractal analysis on existing topographic data derived from Clementine LIDAR [4], Earth-based radar of Tycho crater [5], and Apollo surface-based stereoimagery [6]. The fractal parameter H, which describes the relationship between scale and roughness, is 0.65+/-0.02, 0.64+/-0.01, and 0.69+/-0.06 [6] at the 20-75km, 150m-1.5km, and 0.1-10mm scales, respectively. Based on the consistency of H at these disparate scales, we interpolate H=0.65+/-0.03 (a weighted average) at the 20m and 62m scales of the MI cameras. The second fractal parameter, σ (L0), is calculated from Clementine LIDAR data for overlapping 3x3 degree segments over the lunar surface. From this, we predict local topographic slopes for all regions on the Moon -60° to +60° at the 20m and 62m scales based on H=0.65 and σ (L0) as determined for each pixel. These results allow us to prioritize TC data analysis to maximize the scientific return from MI data during the first years of data analysis. This work was supported by the Japan Society for the Promotion of Science and the National Science Foundation's East Asia Summer Institutes. References: [1] Ohtake, M. LPSC XXXIV, abs 1976, 2003. [2] McEwen, A.S. LPSC XXVII, 841-842, 1996. [3] McEwen, A. et al. LPSC XXIX, abs 1466, 1998. [4] Smith, D.E. et al., JGR, 102(E1), 1591-1611, 1997. [5] Margot, J.-L. et al. JGR, 104(E5), 11875-11882, 1999. [6] Helfenstein, P. & M.K. Shepard. Icarus, 141, 107-131, 1999.
Ohtake Makiko
Steutel Donovan
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