be of enormous benefit to scientists who wish to find out 
whether there are some publications which describe an area, 
or an image, that they are interested in. 
We plan to hold this infomation in SYBASE SQL, but for 
now we have been prototyping the database using Prolog. 
Here are the Prolog facts that we are currently using; these are 
all tied together by specific unique reference identifiers e.g. 
Ref_id= "batson_1986": 
This would form the main reference table 
general_ref(Ref_id,Author_list, Title, Year, 
Pub type,Page. start, Page end,Keyword. list). 
where "Pub type" is one of: journal, book, proceedings 
The following are sub-reference tables for specific types of 
publications 
journal_ref(Ref_id, Journal, Vol, No). 
book_ref(Ref_id, Title, Edition, Publisher,Isbn_no, City, 
Pages). 
proceedings ref(Ref id, Conference, Vol,Part). 
Finally, for specific examples of images, features, locations, 
and regions, that have been mentioned in publications: 
image ref(Ref id,Keyword list, Spacecraft,Image, 
Clock_count, Photo_no, Page). 
feature_ref(Ref_id,Keyword_list, Feature, Page). 
location, ref(Ref id,Keyword list, Lon,Lat,Page). 
region, ref(Ref id,Keyword list,Lon w,Lon. e, 
Lat n,Lat s,Page). 
4. APPLICATIONS 
4.1 Image Footprints 
Ge 
10°S 
20°S 
  
90*w 80°W 70° W 
Figure 6: Clementine UVVIS C filter image footprints with 
respect to control points, and named crater outlines on the 
north-east of the Mare Orientale region of the Moon. 
192 
In fig. 6 we present a plot of C-filter (900nm) Clementine 
spacecraft image footprints, where the UVVIS (ultraviolet. 
visible) camera was tilted more than 5° off-nadir, during the 
third month of operation. These overlap with nadir pointing 
images that were taken, to produce a global image mosaic 
during the previous two months. Although SOLIS has a more 
systematic method of determining good stereo pairs (Cook e 
al., 1996), this plot clearly illustrates where the user might 
expect to find areas with strong stereo coverage. 
Displacements between control points (stars) and crater 
centres, infer a systematic offset between the coordinate 
systems used for these two datasets (Anderson and Whitaker, 
1987; Davies et al., 1994). This illustrates one way in which 
SOLIS can be used for cartographic verification. The plot 
also shows that the region in the vicinity of Mare Orientale 
does not have good control point coverage. This may be due 
to the lack of former spacecraft stereo coverage in this area, 
4.2 Phase Angle Coverage 
For photometric studies of planetary surfaces (Hapke, 1993), 
it is important to have as many images as possible 
available, taken under different phase angle conditions. Here 
we present a map (Cook er al., 1996) of the region covering 
Reiner Gamma (left) and Kepler (right of centre) on the 
Moon's surface illustrating the variety of different phase 
angle images, by the number of 5? phase bins covered. These 
two features, indicated by dark grey, have been imaged at 
many different phase angles, and hence are suitable regions 
on which to perform photometric studies. 
    
No. of S° phase angie bins 
012 3-48 8 7 
  
“10° 
soow 30°W 
Figure 7: Multiple phase angle coverage map of the lunar 
region 60°W-30°W, 0°N-15°N. 
5. SUMMARY AND FUTURE WORK 
Although SOLIS is still under development, it has been 
applied successfully to tasks involving Clementine mission 
imagery (Oberst et al., 1996). In particular it has been used 
to produce minimum ground pixel size, stereo, minimum 
phase angle, and multiple phase angle coverage, maps of the 
Moon (Cook, et al., 1996), and for the location of image 
footprints with respect to craters and control points. 
Furthermore it has proven capable of handling datasets with 
up to 2 million image records. The design of our raster 
cartographic database is efficient, compact, and allows for 
the multi-scale retrieval of thematic maps. We have found 
that even greater compression can be achieved on a global 
Mars image mosaic using JPEG. 
It is planned to output raster data in four formats: VICAR, 
GIF, JPEG, and raw binary format (no header). Tabular data 
are currently output in ASCII format, though we are also 
considering JPL IBIS format. Graphical output, at the time of 
writing, is either written to the X11 screen or to a postscript 
International Archives of Photogrammetry and Remote Sensing. Vol. XXXI, Part B4. Vienna 1996 
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