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Fig. 3: Radial distances and errors for the control points of Dione 
3. DIGITAL IMAGE MOSAICS 
Image mosaics and maps were produced for the five largest 
Satellites (excluding the cloud-shrouded satellite Titan) 
Mimas, Enceladus, Tethys, Dione, and Rhea. The images were 
first reprojected to digital maps, using orbit and pointing 
data derived by Davies and Katayama (1983a,b,c; 1984). 
However, for Dione images, improved pointing data were 
taken from limb-fitting procedures mentioned above. 
For comparison and interpretation of the maps, a 3-axial 
ellipsoid was used for the calculation of the ray intersection 
point; however, the map projections were done on a sphere, 
with all satellite shape parameters taken from IAU 
recommendations (Seidelmann et al., 2003, see Table 1). A 
photometric correction using the Minnaert function was 
applied to every image during map projection. 
The final step of the image processing was the combination 
of all map-projected images (14, 9, 8. 13, and 37 Voyager-1 
images, for Mimas, Enceladus, Tethys, Dione, and Rhea, 
respectively) to a homogeneous mosaic. Special care had to 
be taken to the different ground resolution of the input 
881