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ISPRS Abstract Book.Pdf ISPRS Working Group IV/7 Extraterrestrial Mapping Advances in Planetary Mapping 2007 Lunar and Planetary Institute, Houston, Tx, March 17, 2007 08:30 Registration 09:00 Welcome / Logistics Oral Presentations Moon Chair persons: J. Oberst and J. Haruyama 09:05 – 09:20 Report on the final completion of the unified Lunar control network 2005 and Lunar topographic model B.A. Archinal, M.R. Rosiek, R.L. Kirk, T.L. Hare, and B.L. Reddin 09:20 – 09:35 Global mapping of the Moon with the Lunar Imager/Spectrometer on SELENE J. Haruyama, M. Ohtake, T. Matunaga, T. Morota, C. Honda, M. Torii, Y. Yokota, H. Kawasaki, and LISM working group 09:35 – 09:50 Lunar orbiter laser altimeter on Lunar Reconnaissance Orbiter G. A. Neumann, D. E. Smith, and M. T. Zuber 09:50 – 10:05 LROC – Lunar Reconnaissance Orbiter Camera M.S. Robinson, E.M. Eliason, H.Hiesinger, B.L. Jolliff, A.S. McEwen, M.C. Malin, M.A. Ravine, D. Roberts, P.C. Thomas, and E.P. Turtle Coffee and Poster Viewing Methods in Planetary Mapping Chair persons: J. Haruyama and J. Oberst 10:35 – 10:50 Toward machine geomorphic mapping of planetary surfaces T.F. Stepinski 10:50 – 11:05 MR PRISM - an Image analysis tool and GIS for CRISM A.J. Brown, J. L. Bishop, and M.C. Storrie-Lombardi 11:05 – 11:20 Description of the JPL planetary web mapping server L. Plesea, T.M. Hare, E. Dobinson, and D. Curkendall 11:20 – 11:35 Do we really need to put stereo cameras on landers? A.C. Cook 11:35 – 11:50 Restoration of degraded planetary imagery R. Schmidt, G. Neukum, and the HRSC Co-Investigator Team 11:50 – 12:05 Applying the constant-scale natural boundary mapping technique P.E. Clark, C.S. Clark, and P.D. Lowman 12:05 – 12:10 World maps with Constant-Scale Natural Boundaries: CSNB 2007 (poster introduction) C. S. Clark 12:10 – 12:15 A prototype of Online Conference system for collaborative mapping (poster introduction) Works H. Demura, M. Kanzawa, N. Hirata, and N. Asada Lunch Break and Poster Viewing Mars Chair persons: T. Roatsch and P. Schenk 13:15 – 13:30 The HRSC DTM test C. Heipke, J. Oberst, J. Albertz, M. Attwenger, P. Dorninger, E. Dorrer, M. Ewe, S. Gehrke, K. Gwinner, H. Hirschmüller, J.R.Kim, R.L.Kirk, H. Mayer, J.-P. Muller, R. Rengarajan, M.Rentsch, R. Schmidt, F. Scholten, J. Shan, M. Spiegel, M. Wählisch, G. Neukum, and the HRSC Co-Investigator Team 13:30 – 13:45 Global Mapping of Mars by Systematic Derivation of Mars Express HRSC High-Resolution Digital Elevation Models and Orthoimages K. Gwinner, F. Scholten, R. Jaumann, T. Roatsch, J. Oberst, and G. Neukum 13:45 – 14:00 Simultaneous adjustment of interior and exterior orientation of HRSC on MARS EXPRESS M. Spiegel and G. Neukum 14:00 – 14:15 HRSC Data Proccessing by Matching in Object Space, II. Effects of Image and DTM Filtering S. Gehrke and C. Bischoff 14:15 – 14:30 Where is Viking Lander 2? Recovered Landing Site in MRO Images Not in Agreement with Earlier Predictions J. Oberst, M. Wählisch, and K.-D. Matz 14:30 – 14:45 A new astrometric measurement technique for Phobos using background stars and surface control points K. Willner, J. Oberst, K-D. Matz, T. Roatsch, and H. Hoffmann Coffee Break and Poster Viewing Asteroids Chair persons: P. Schenk and T. Roatsch 15:15 – 15:30 Mapping small bodies with stereophotoclinometry R. W. Gaskell 15:30 – 15:45 Integrated tool for analysis of irregular shaped small bodies N. Hirata, Y. Fujii, H. Demura, and N. Asada 15:45 – 16:00 Global mapping of asteroid CERES with HST/ACS J.-Y. Li, L. A. McFadden, J. Wm. Parker, E. F. Young, and P. C. Thomas Outer Planet Satellites 16:00 – 16:15 Global geologic mapping of Io: data and techniques D. A. Williams, L. P. Keszthelyi, P. E. Geissler, W. L. Jaeger, T. L. Becker, D. A. Crown, P. M. Schenk, and J. A. Rathbun 16.15 – 16:30 Combining Galileo SSI, NIMS, and PPR DATA into GIS to study volcanic centers on Io J.A. Rathbun and S. E. Barrett 16:30 – 16:45 Resolution effects in radarclinometry R. L. Kirk and J. Radebaugh 16:45 – 17:00 High resolution Enceladus atlas derived from CASSINI-ISS images T. Roatsch, M. Wählisch, B. Giese, A. Hoffmeister, A. Kuhn, F. Scholten, K.- D. Matz, G. Neukum, P. Helfenstein, and C. Porco 17:00 Adjourn Posters First stereoscopic RADAR images of Titan R.L. Kirk, E. Howington-Kraus, K.L. Mitchell, S. Hensley, B.W. Stiles, and the Cassini RADAR Team Ultrahigh resolution topografic mapping of Mars with HiRISE stereo images: methods and first results R.L. Kirk, E. Howington-Kraus, M.R. Rosiek, D. Cook, J. Anderson, K. Becker, B.A. Archinal, L. Keszthelyi, R. King, A.S. McEwen, and the HiRISE Team The evolution of Ares Vallis A. Pacifici, G.G. Ori, G. Komatsu, and M. Pondrelli CASSINI-VIMS multiwavelength mapping of Titan J.W. Barnes, J. Ivens, and R.H. Brown Venus on two world maps with constant-scale natural boundaries B.S. Clark and P.E. Clark HRSC data processing by matching in object space, I. joint derivation of DTM and orthoimage S. Gehrke and I. Haase Combining HRSC imagery and MOLA DTM: the first north-polar sheets of the "Topographic image map Mars 1:200,000" S. Gehrke, D. Bornemann, M. Wählisch, and J. Albertz Geological map of the Holden and Eberswalde craters area M. Pondrelli, A.P. Rossi, L. Marinangeli, E. Hauber, G.G. Ori, and G. Neukum Calibration of MOLA pulse spread for interpretation of surface roughness P. Saiger, J. Oberst, and M. Wählisch World maps with Constant-Scale Natural Boundaries: CSNB 2007 C.S. Clark A prototype of Online Conference system for collaborative mapping Works H. Demura, M. Kanzawa, N. Hirata, and N. Asada Report on the final completion of the unified Lunar control network 2005 and Lunar topographic model B.A. Archinal, M.R. Rosiek, R.L. Kirk, T.L. Hare, and B.L. Redding Asteroids and Map Projections: Choices and Compromises P.J. Stooke REPORT ON THE FINAL COMPLETION OF THE UNIFIED LUNAR CONTROL NETWORK 2005 AND LUNAR TOPOGRAPHIC MODEL. B. A. Archinal, M. R. Rosiek, R. L. Kirk, T. L. Hare, and B. L. Redding, U. S. Geological Survey, Astrogeology Team, 2255 N. Gemini Drive, Flagstaff, AZ 86001, USA, [email protected]. Introduction: In order to highlight this project to the average. When the ULCN 2005 solution radii of all 272,931 extraterrestrial mapping community, we repeat here our ear- control points are compared to the a priori radii derived from lier abstract [1], with a corrected Figure 2. A report describ- an interpolation of a combination of Clementine LIDAR and ing the Unified Lunar Control Network 2005 and the files polar Clementine stereo data [6], the differences are not sig- associated with that network is now available as an on-line nificant so the radii must therefore be of similar accuracy. USGS Open-File Report [2] at the location The mean absolute difference of the solution radii from their http://pubs.usgs.gov/of/2006/1367/. A “Readme” file de- a priori values is 137 m, with a standard deviation of 219 m. scribes the available files, including the report text, the Uses of the ULCN 2005: The original reason for doing a original photogrammetric solution input and output files, solution that combined the ULCN (1994) and CLCN was derived files such as information on all the control point primarily to remove the large horizontal errors known to be positions, the expected vertical precision (EVP) of the points present in the CLCN, and thus allow for the possible option and the solution residuals, and a directory containing global of generating an improved Clementine Basemap Mosaic DEMs derived from the point positions. While a paper pro- (CBM)[8] and other Clementine mosaics[9,10]. Indeed, that viding further details about the solution is in preparation, we option still exists, although we have been unable to obtain provide some useful additional information about the solu- funding to carry it out. However, as part of a funded PG&G tion and possible uses for it here. task to generate an initial Lunar GIS, we are creating an The Solution: The ULCN 2005 includes the determina- improved version of the CBM by warping the mosaic based tion of the 3-D positions of 272,931 points on the lunar sur- on the change in point coordinates from the CLCN to the face and the correction of the camera angles for 43,866 ULCN 2005. We are excited to report initial tests show Clementine images, using 546,126 tie point measurements. better results than we hoped for. We tested 3, 6, and 12 pa- The solution RMS is 20 µm (= 0.9 pixels) in the image rameter polynomial warps and have settled on a 6 parameter plane, with the largest residual of 6.4 pixels. The 7 iteration warp. Using a 30°x30° test area and more that 7400 vectors, solution took ~40 hours for completion on a ~2 GHz system. we successfully obtained RMS errors of <110 meters. But There is an average of 46 km2/point and therefore ~6.8 km more importantly, a visual inspection of the registration is between points. This photogrammetric network solution is also impressive (Figure 2 – corrected from reference [1]). the largest planetary control network ever completed. Other We will continue to use 30°x30° tiles for entire global data- details of the solution are given in Table 1.
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