Statistics – Computation
Scientific paper
May 2004
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004agusm.p33d..18n&link_type=abstract
American Geophysical Union, Spring Meeting 2004, abstract #P33D-18
Statistics
Computation
0910 Data Processing, 0933 Remote Sensing, 6225 Mars, 6297 Instruments And Techniques
Scientific paper
It is well known within the planetary science community that a considerable amount of time can be dedicated to Mars data preparation before one is able to actually conduct remote sensing analyses. A prototype system developed at the Center for Nuclear Waste Regulatory Analyses (CNWRA) reduces such time by optimizing the process of locating, preparing, and retrieving MOLA PEDR, MOLA MEGDR and Themis VIS/IR datasets. A graphical user interface allows for searching data spatially, temporally, or by keywords. Spatial searches are done either by drawing a box around a map location or by entering coordinate values in planetographic/planetocentric latitude and west/east longitude coordinate systems. Temporal searches may be conducted by searching for specific Themis IR and VIS release dates. Key word searches may be conducted by searching for a particular MOLA PEDR orbit number. The retrieved data is provided in either a native format (such as ASCII for MOLA PEDR datasets) or in a format selected by the user and based on the chosen value-added product. In the case of MOLA PEDR datasets, the user can choose between two interpolation methods (Delaunay-based or natural neighbor) and may receive data in a TIFF or raster grid format. Natural neighbor interpolation produces fewer artifacts, but it is computationally intensive. The time required (minutes or tens of minutes compared with fractions of seconds used by the first method) makes it necessary to provide the user with an email notification once the interpolated dataset becomes available. The interpolated data provide effective resolution that approaches ~150 m compared to the PEDR resolution of ~300 m. In the case of Themis IR and VIS, data may be provided as one B/W single band image or as three-band color composite image in several raster formats. This system was successfully used to analyze Walla Walla Vallis (approximately 305.3 to 305.6E, 9.4S to 9.9S) and Aromatum Chaos/Ravi Vallis (approximately 315E to 322E, 1N to 2S) outflow channels. For Walla Walla Vallis (name provisionally approved by the International Astronomical Union), a small outflow channel, the integrated datasets helped resolve the locations of reaches that were indistinct in visible light images. For Ravi Vallis, the composite data system enhanced our understanding of how some chaotic terrain forms. As presented by Coleman, N.M. (2004 Lunar and Planetary Science Conference, Abstract #1299), thinning of the cryosphere by deep fluvial incision spawned secondary breakouts of groundwater, forming new chaos zones. The systems flexible design allows for incorporation of additional remote sensing datasets, such as those provided by MOC, TES, and MARSIS instruments. In summary, our integrated data-access system will make the wealth of new Martian data more readily available to planetary researchers enabling scientists to focus more time on analyses or algorithm development rather than on finding data and format conversions. Disclaimer: An employee of the U.S. Nuclear Regulatory Commission (NRC) made contributions to this work on his own time apart from regular duties. NRC has neither approved nor disapproved the technical context of this abstract.
Coleman Neil M.
Colton S.
Dinwiddie Cynthia L.
Necsoiu M.
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