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Fig. 1: Digital Terrain Model from Galileo stereo images showing of parts of the nearside northern
hemisphere including the Humboldtianum Basin (82?E, 57?N) and Mare Crisium (58?E, 18?N).
Heights vary from -4500 to +2000m. The DTM is represented in a sinusoidal map projection with 5
km/pixel scale. Note the gaps in the terrain data near the lunar limb and near the terminator, and in
areas of high sun elevation angles, where the digital image matching failed.
In the case of Galileo, control points were used exclusively.
The adjustment involved 49 images, 212 control points, and a
total of 1004 individual image coordinate measurements.
Control points were taken from the "Unified lunar control
network" (Davies et al., 1994), which involves more than 1000
control points located mostly on the nearside hemisphere. In
the case of Clementine, the adjustment involved 417 conjugate
points and 1403 individual line/sample measurements in a total
of 96 images. 6 control points from an earlier photogrammetric
study of Clementine data (Oberst et al., 1996) were used to
support the adjustment.
Next, we performed several parallel image matching runs
Involving one reference image and up.to six target images,
respectively, using an automatic area-based least- squares
matching technique in image space (Ackermann, 1984; Oberst
et al, 1996). The matched data were converted to object
coordinates using the spacecraft position and camera pointing
data determined in the bundle adjustment using ray intersection
methods. Finally, the object coordinates were converted to
line/sample coordinates in an appropriate map projection
followed by interpolation to form a regular DTM grid. The
DTMs are normally presented in a sinusoidal map projection.
4. RESULTS
Analysis of the Galileo images resulted in a terrain model
covering much of the nearside northern hemisphere at 2000 m
grid spacing and 500 m height resolution (see Fig. 1).
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International Archives of Photogrammetry and Remote Sensing. Vol. XXXI, Part B4. Vienna 1996