Astrogeologist Gene Shoemaker was born in Los Angeles, California and became chief scientist at the USGS Center of Astrogeology (Flagstaff) and professor of geology at CalTech. He worked with his wife Carolyn on cratering, both on the Moon and the Earth, by volcanoes and by meteor and cometary impact. He discovered, with Edward Chao, coesite, a type of silica produced in a violent impact and a si...
K. L. Edmundson; O. Alexandrov; Archinal, B. A.; Becker, K.J.; Becker, T. L.; Kirk, R L; Moratto, Z. M.; Nefian, A. V.; Richie, J. O.; Robinson, M S
The integrated photogrammetric mapping system flown on the last three Apollo lunar missions (15, 16, and 17) in the early 1970s incorporated a Metric (mapping) Camera, a high-resolution Panoramic Camera, and a star camera and laser altimeter to provide support data. In an ongoing collaboration, the U.S. Geological Survey’s Astrogeology Science Center, the Intelligent Robotics Group of the NASA Ames Research Center, and Arizona State University are working to achieve the most complete...
Edmundson, K. L.; Alexandrov, O.; Archinal, B. A.; Becker, K. J.; Becker, T. L.; Kirk, R. L.; Moratto, Z. M.; Nefian, A. V.; Richie, J. O.; Robinson, M. S.
The integrated photogrammetric mapping system flown on the last three Apollo lunar missions (15, 16, and 17) in the early 1970s incorporated a Metric (mapping) Camera, a high-resolution Panoramic Camera, and a star camera and laser altimeter to provide support data. In an ongoing collaboration, the U.S. Geological Survey's Astrogeology Science Center, the Intelligent Robotics Group of the NASA Ames Research Center, and Arizona State University are working to achieve the most complete cartographic development of Apollo mapping system data into versatile digital map products. These will enable a variety of scientific/engineering uses of the data including mission planning, geologic mapping, geophysical process modelling, slope dependent correction of spectral data, and change detection. Here we describe efforts to control the oblique images acquired from the Apollo 15 Metric Camera.
Head, J. W.; Huffman, J. N.; Forsberg, A. S.; Hurwitz, D. M.; Basilevsky, A. T.; Ivanov, M. A.; Dickson, J. L.; Senthil Kumar, P.
Traditional methods of planetary geological mapping have relied on photographic hard copy and light-table tracing and mapping. In the last several decades this has given way to the availability and analysis of multiple digital data sets, and programs and platforms that permit the viewing and manipulation of multiple annotated layers of relevant information. This has revolutionized the ability to incorporate important new data into the planetary mapping process at all scales. Information on these developments and approaches can be obtained at http://astrogeology.usgs. gov/ Technology/. The processes is aided by Geographic Information Systems (GIS) (see http://astrogeology. usgs.gov/Technology/) and excellent analysis packages (such as ArcGIS) that permit co-registration, rapid viewing, and analysis of multiple data sets on desktop displays (see http://astrogeology.usgs.gov/Projects/ webgis/). We are currently investigating new technological developments in computer visualization and analysis in order to assess their importance and utility in planetary geological analysis and mapping. Last year we reported on the range of technologies available and on our application of these to various problems in planetary mapping. In this contribution we focus on the application of these techniques and tools to Venus geological mapping at the 1:5M quadrangle scale. In our current Venus mapping projects we have utilized and tested the various platforms to understand their capabilities and assess their usefulness in defining units, establishing stratigraphic relationships, mapping structures, reaching consensus on interpretations and producing map products. We are specifically assessing how computer visualization display qualities (e.g., level of immersion, stereoscopic vs. monoscopic viewing, field of view, large vs. small display size, etc.) influence performance on scientific analysis and geological mapping. We have been exploring four different environments: 1) conventional
The color shaded relief image used as the base for this globe has a resolution of 32 pixels per degree (approximately 1850 m/pixel), and was produced and supplied by the MOLA Science Team (http://ltpwww.gsfc.nasa.gov/tharsis/mola.html). The image is shaded as if illuminated everywhere from the west. The elevations represented in color are with respect to a gravitational equipotential surface whose mean equatorial radius is that of the topography. The Astrogeology Team of the U.S. Geological Survey reprojected the image into the format displayed above.The images are presented in a projection that portrays the entire surface of Mars in a manner suitable for the production of a globe; the number, size, and placement of text annotations were chosen for a 12-inch globe. Prominent features are labeled with names approved by the International Astronomical Union. A specialized program was used to create the 'flower petal' appearance of the images; the area of each petal from 0 to 75 degrees latitude is in the Transverse Mercator projection, and the area from 75 to 90 degrees latitude is in the Lambert Azimuthal Equal-Area projection. The northern hemisphere of Mars is shown on the left, and the southern hemisphere on the right.
Perry, Eugene; Marin, Luis; McClain, Jana; Velazquez, Guadalupe
A 180-km-diameter semicircular band of abundant karst sinkholes (Ring of Cenotes) in northwest Yucatan, Mexico, coincides approximately with a concentric ring of the buried Chicxulub structure, a circular feature manifested in Cretaceous and older rocks, that has been identified as the product of the impact of a bolide. The ring, expressed in Tertiary rocks, marks a zone of high permeability as shown by (1) the sinkholes themselves, (2) breaks in the coastal dune system and high density of springs where the ring intersects the coast, and (3) water-level transects characterized by a decline in water level toward the ring. Any direct relation that exists between the Ring of Cenotes and the Chicxulub structure bears on regional hydrogeology. If the layer or zone responsible for the ring is deeply buried, it may act as a barrier to the movement of ground water across the main flow direction. Shallower zones of horizontal permeability could result in less complete diversion of ground water. Through its influence on Yucatan aquifer characteristics, the ring may provide a link between modern environmental problems and astrogeology. Possible origins for the Ring of Cenotes are (1) faulting, perhaps reactivated by post-Eocene mid-Miocene basin loading, (2) permeability in a buried reef complex developed in the shallow Paleocene sea around the crater rim, or (3) breccia collapse occasioned by consolidation or by solution of evaporite components. If the ring developed on ancient faults, it may outline hydrothermal systems and mineral deposits produced during Paleocene cooling of the Chicxulub melt sheet.
., 2008, LPSC XXXIX, Abstract#2419  Yershov, V. et al., 2015 EPSC 10, EPSC2015-343  Kim, J. R. et al., 2013 EPS 65, 799-809  https://isis.astrogeology.usgs.gov/index.html  http://naif.jpl.nasa.gov/naif/index.html  Gwinner et al., 2010, EPS 294, 543-540  Gwinner et al., 2015, PSS  Dumke, A. et al., 2008, ISPRS, 37, Part B4, 1037-1042
Gaddis, Lisa R.; Hare, Trent; Beyer, Ross
and missions were represented. Presentations (some in video format) and tutorials are posted on the meeting site (http://astrogeology.usgs.gov/groups/Planetary-Data-Workshop).
Shylaja, B. S.
The notion of life has always fascinated curious minds. From prehistoric days, fancy voyages to other colonies and visits from non-earthly beings have been creatively imagined. Apart from science fictions, the last few centuries saw many observational investigations of "cities of Moon", "colonies of Mars" and so on. However, the sophisticated tools of the modern era quickly put a full stop to these developments revealing that the other planets are not hospitable, and infact hostile for a life form like ours to exist there. That explains why in the last few decades the efforts shifted to observing the satellites of large planets. The anxiety grew with the knowledge of their atmospheric structure, chemical composition and volcanic activity. Detection of water, albeit frozen, was a welcome surprise. The flyby of Voyager and Pioneer provided ample evidence for the presence of water, one of the most important ingredients for the germination of the seed of life. The detection of the fossil of a microorganism on a stone believed to have fallen from Mars, boosted the scientists zeal to pursue the research, although the date for life on Mars (more than 3 billion years ago) is not very convincing. Last year, many scientists, from different branches like astrophysics, geology, oceanography, biology and astrogeology discussed the possibilities of life elsewhere in the universe. The focal point was not Mars, but Europa, one of the Galilean satellites of Jupiter. Their studies based on Voyager images supported the possibility of liquid water beneath the frozen sheets of ice. However, heat is also an essential parameter. Europa, being at a distance five times the sun-earth separation can have only 1/25th the warmth of the earth. Then, where does it get the necessary warmth from? There are other important sources of heat in many of these satellites that lie concealed from our view. They are the volcanoes. If present, can these keep the water warm below the ice sheets? The unmanned