Mathematics – Logic
Scientific paper
Aug 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006iaujd..10e..26a&link_type=abstract
Progress in Planetary Exploration Missions, 26th meeting of the IAU, Joint Discussion 10, 21-22 August 2006, Prague, Czech Repub
Mathematics
Logic
Scientific paper
U. S. Geological Survey, Astrogeology Team, Flagstaff, AZ, United States Introduction: We have completed a new general unified lunar control network and lunar topographic model based on Clementine images. It includes the determination, in the lunar mean Earth/polar axis system, of the 3-D positions of 272,931 points on the lunar surface and the correction of the camera angles for 43,866 Clementine images, using 546,126 tie point measurements. The solution RMS is 0.9 pixels in the image plane, with the largest residual of 6.4 pixels. We are now documenting our solution and plan to release the solution results soon, initially as a USGS Open File report. ULCN 2005 Features: The new network is a combination of the Unified Lunar Control Network (ULCN), derived from the Apollo, Mariner 10, and Galileo missions, and Earth-based photographs, [1] and the Clementine Lunar Control Network (CLCN) [2], both derived from (mostly 750-nm) Clementine images, by M. Davies and T. Colvin at RAND. The primary difference between our new network and the previous ones is that we solve for the radii of the control points. This avoids (~7 km) distortion of horizontal positions present in the CLCN. The expected precision of such information is on the order of several hundred m, and compatible with Clementine LIDAR [3]. Thus, a by-product of this network is a global lunar topographic model that is denser than that provided by LIDAR and of similar accuracy, and denser than any other lunar topography information except that provided in limited areas ([4-7]). This is the only lunar topographic model positioning where both heights and horizontal positions are estimated in a globally-consistent system. Other features of the ULCN 2005 are that the camera angles to their values as measured during the mission, supposedly with an accuracy of 0.03º [8], and we have identified a majority of the original ULCN points on Clementine images. Future Work: The Lunar Orbiter (LO) digital mosaics now being generated [9] will be registered to the ULCN 2005. We will also further improve this network through the addition of Mariner 10, Galileo, and LO image measurements, and Clementine stereo [10], and by adding ties to the current absolute LLR and ALSEP network [11]. Although unfunded, the Clementine mosaics could also be regenerated in this system. It will be absolutely essential to further update and improve this network with data from future missions. This is necessary so that these new datasets can be compared to the prior data, particularly the LO and Clementine multispectral products. References: [1] Davies, M. E. et al. (1994) JGR, 99, E11, 23,211-23,214. [2] Edwards, et al. (1996), LPS XXVII, 335-336. [3] Smith, D. E. et al. (1997), JGR, 102, E1, 1591-1611. [4] Cook, A. C. et al. (2000), JGR, 105, E5, 12,023-12,033. [5] Rosiek, M. R. et al. (1998), LPS XXX, Abstract #1853. Rosiek, M. R., and Aeschliman, R. A. (2001) LPS XXXII, Abstract #1943. [6] Margot, J-L. C. (1999), PhD Thesis, Cornell University. [7] Wu, S. S. C. and Doyle, F. J. (1990), in Planetary Mapping, R. Greeley and R.M. Batson, eds., CUP, 169-207. [8] Nozette, S., et al. (1994), Science, 266, 1835-1839. [9] Weller, L., et al. (2006), LPS XXXVII, Abstract #2143. [10] Cook, A. C. et al. (2002), AGU Fall Meeting, Abstract #P22D-09. [11] Davies, M. E. and Colvin, T. R. (2000), JGR, 105, E8, 20,277-20,280.
Archinal Brent A.
Kirk Randolph L.
Redding Bonnie L.
Rosiek Mark R.
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