Abstract
The main objective of this study is to develop a Hapke photometric model that is suited for Chang’E-1 (CE-1) Interference Imaging Spectrometer (IIM) data. We first divided the moon into three areas including ‘maria’, ‘new highland’ and old ‘highland’ with similar photometry characteristic based on the Hapke parameters of the moon derived from Lunar Reconnaissance Orbiter Camera (LROC) Wide Angle Camera (WAC) multispectral data. Then, we selected the sample data in the ‘maria’ area and obtained a new set of Hapke model’s parameters that can best fit these data. Result shows that photometric correction using Hapke model with these new derived parameters can eliminate the effect of variations in viewing and luminating geometry, especially ‘opposition surge’, more efficiently than the empirical model. The corrected mosaic shows no significant artifacts along the tile boundaries and more detailed information of the image can be exhibited due to a better correction of ‘opposition surge’ at small phase angle (g < 15°).
Highlights
Visible and infrared spectroscopy is sensitive to the mineralogy of the Moon
We divided the moon into three areas based on the Hapke model parameters and each area should approximately have the similar photometric characteristic
USGS made a global false color image mosaic with Clementine UV/VIS spectral data at 415 nm, 750 nm and 1000 nm. 750/415 nm band ratio was set as R representing low titanium area or high glass content; 750/1000 nm band ratio was set as G, which is sensitive to the content of iron; 415/750 nm was set as B which indicates the presence of the high titanium content
Summary
Visible and infrared spectroscopy is sensitive to the mineralogy of the Moon. Abundance of these minerals can be estimated according to their hyperspectral reflectance data and characteristic absorption features. Most of the spectrometers used in the remote sensing exploration of the moon are multi-spectral cameras, which only cover the limited range of wavelengths. The inversion of mineral abundance on the lunar surface mainly depends on ‘band ratio’ [1], which are strongly affected by the extreme differences in the measured spectral reflectance resulting from the variation in viewing geometry of different orbits. The viewing geometry can be defined by three angles: incidence angle i, emission angle e and phase angle g. The viewing geometry varies in different orbits and at different location of the Lunar surface. Much details of the image obtained at small phase angle (phase angle < 20◦) can be lost because of ‘opposition surge’ effect and obvious brightness difference can be observed at the boundary between two adjacent orbits images
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