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Automated Crater Detection and Counting Using the Hough Transform (Decoding the Geology of Mars). Monty Galloway University of Western Australia. Supervisors: G.K. Benedix 1 , P.A. Bland 1 , J. Paxman 2 , M.C. Towner 1 , T. Tan 2. 1 Department of Applied Geology, Curtin University
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Automated Crater Detection and Counting Using the Hough Transform (Decoding the Geology of Mars) Monty Galloway University of Western Australia Supervisors: G.K. Benedix1, P.A. Bland1, J. Paxman2, M.C. Towner1, T. Tan2 1Department of Applied Geology, Curtin University 2Department of Mechanical Engineering, Curtin University
Overview • Why count craters? Why automate? • Method • Edge Detection • Hough Transform • Performance Analysis • Results and Future Work 6 km HiRISE Crater Image: https://hirise.lpl.arizona.edu/ESP_034809_1655
Martian Meteorites Crater: http://static.uahirise.org/images/wallpaper/800/ESP_034285_1835.jpg Earth: http://eoimages.gsfc.nasa.gov/images/imagerecords/57000/57723/globe_east_540.jpg MartianMeteorite LA001: http://www2.jpl.nasa.gov/snc/la001.jpg
Surface Age-Dating Older Surface Younger Surface Mars: http://hubblesite.org/newscenter/archive/releases/2001/24/image/a/ HRSC Surface Images: http://pds-geosciences.wustl.edu/mex/mex-m-hrsc-5-refdr-mapprojected-v2/mexhrsc_1001/data/ Superposed Craters
Method Image Canny Edge Detection OpenCV Edge Pixels Hough Transform Circles Performance Analysis
Canny Edge Detection High Threshold Gradient Low
Hough Transform Image Detection Edges Voting
Performance Analysis 1 True Positive False True Negative False
Performance Analysis 2 (Windows) Positive Negative
Performance Analysis 3 (Results) ROC for three Canny threshold settings. TPR TPR = TP / (FN + TP) FPR = FP / (TN + FP) FPR
Summary and Future Work • Tested influence of edge detection on Hough Transform. • Results suggest refinement of edge detection will improve. • Sun direction edge data. • Integrate with Urbach& Stepinski1 crater candidate method. • Parallelization. 1E.R. Urbach and T.F. Stepinski, “Automatic detection of sub-km craters in high resolution planetary images,” Planetary and Space Science, vol. 57, pp. 880–887, 2009.
Acknowledgements Thank you to iVEC for supporting this work through the 2013-2014 Summer Internship program. Thank you to Tele, Jonathan, Gretchen, Phil and Martin for their support and technical advice.