i:bul 2004 
rified. 
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ecked 
n, the 
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iduals 
25,590 
AND) 
. The 
asures 
pixels, 
s, and 
edone, 
cases 
not be 
lefined 
of an 
M 2.1 
imined 
» these 
IM 2.1 
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(at the 
s there 
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| point 
these 
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nosaic. 
tion of 
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ng the 
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kner, et 
will be 
etwork 
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ints on 
317 VO 
| 1.054 
RAND 
nerally 
image 
to add 
tion of 
total of 
it is the 
(to the 
The 
etwork, 
his new 
ly fixed 
d from 
ositions 
both the 
horizontal (7250 m) and vertical (^10 m). This network and the 
associated solved-for VO camera angles have been used to 
create the USGS MDIM 2.1 mosaic, thus assuring that the 
mosaic will have a similar level of accuracy, and that it can be 
used directly with MOLA derived products. A further product 
is camera angles in the TAU/IAG 2000 system for 1.054 
Mariner 9 and 5,317 VO images, which will also (e.g.) allow 
for their direct registration on MOLA topography. 
5. ACKNOWLEDGEMENTS 
We would like to particularly acknowledge Tim Colvin and 
the late Merton Davies of the RAND Corporation, who brought 
the RAND-USGS Mars control network to its state before our 
work began. This work was funded in part through the NASA 
Planetary Geology and Geophysics program. 
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