Preliminary Analysis of the Absolute Cartographic Accuracy of the Clementine UVVIS Mosaics

Details Preliminary Analysis of the Absolute Cartographic Accuracy of the Clementine UVVIS Mosaics Preliminary Analysis of the Absolute Cartographic Accuracy of the Clementine UVVIS Mosaics

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002agufm.p22d..09c&link_type=abstract

American Geophysical Union, Fall Meeting 2002, abstract #P22D-09

Other

5464 Remote Sensing, 5494 Instruments And Techniques, 6250 Moon (1221), 6297 Instruments And Techniques

Scientific paper

Our analysis reveals that the UVVIS basemap absolute cartographic accuracy may be in the range of +/-1 km to +/- 10 km locally. No absolute ground control points exist on the lunar farside making assessment of any lunar control network problematic. Bore sighted centers for Clementine UVVIS images derived from mission produced NAIF archived spacecraft position and orientation data were compared with image centers derived from the USGS/RAND photogrammetrically adjusted pointing (using an assumed lunar radius of 1737.4 km). Offsets are typically < 1 km within the USGS/RAND absolute control net region (enclosed within +/-40 deg E/W and N/S region on the nearside), worsening up to approximately 10 km in the vicinity of the 90W and 90E longitude lines (albeit smaller near the poles), and then reducing to <1 km towards the center of the farside. The USGS 750 nm basemap (upon which all other UVVIS and NIR mosaics are registered) shows several km discrepancies in absolute spatial position with respect to an earlier "Unified Control Net"; these differences are being measured and a comparison will be made with the mission produced NAIF archived position and pointing data. We propose that when the RAND control net was constructed from the Clementine images, the fact that a constant radius of the Moon was used, and that the images were relatively small (requiring approximately 140 thousand images to cover the Moon), may have resulted in poorly constrained fits in regions where no absolute control was available i.e the entire farside and the nearside beyond the absolute control area. Compounding this problem is the fact that the Moon exhibits +/- 8 km of relief on the farside thus resulting in +/-2% scale errors for a significant portion of the images that compose the basemap. The lack of control, and the scaling problems on the farside, must negatively affect the control network solution in complex ways due to the large number of uncontrolled frames. At this time a definitive resolution of the discrepancies is not possible. However, we can make progress by generating synthetic images of the Moon using the UVVIS mosaic and a planet-wide 1 km/pixel Digital Elevation Model and then compare these to large area lunar images taken from Earth or from spacecraft. Obtaining an accurate cartographic solution of the entire Moon is required before future sample return missions are attempted for the farside or nearside limb areas.

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