Applied Coherent Technology Corporation

Herndon, VA, United States

Applied Coherent Technology Corporation

Herndon, VA, United States
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Domingue D.L.,Planetary Science Institute | Hash C.D.,Applied Coherent Technology Corporation | Denevi B.W.,Johns Hopkins University | Murchie S.L.,Johns Hopkins University
Icarus | Year: 2017

The photometric standardization model derived from the Mercury Dual Imaging System's (MDIS) eight-color photometric observations has been extrapolated to provide photometric parameters for the remaining three colors, such that images acquired through each of the eleven narrow-band filters can be photometrically standardized using a consistent model. The resulting photometric standardization parameters for the three filters not included in the original eight-color analysis display spectral variations commensurate with those observed within the original eight-color photometry. Some caution should be exercised on spectral interpretations based strongly on the behavior in the 698.8-nm filter. © 2017 The Authors

Ensor S.L.,Johns Hopkins University | Reid M.R.,Johns Hopkins University | Mick A.A.,Johns Hopkins University | Turner Jr. F.S.,Johns Hopkins University | And 4 more authors.
AIAA SPACE Conference and Exposition 2012 | Year: 2012

This paper presents lessons learned for NASA missions charged with the delivery of data to the Planetary Data System (PDS). These lessons are drawn from experiences on the MErcury Surface, Space ENvironment, GEochemistry, and Ranging (MESSENGER) and Near Earth Asteroid Rendezvous (NEAR) missions and the Miniature Radio Frequency (Mini-RF) instruments. NASA's Science Mission Directorate sponsors the PDS in order to "ensure the long-term usability of NASA data and to stimulate advanced research."* The general science community benefits when missions collaborate with the PDS to make their data available. These lessons focus on good practices that facilitate on-time delivery of highquality products within budget. They relate to management practices, team organization, coordination within the project team and with PDS personnel, technical understanding of the data products, and knowledge of PDS standards by the archiving staff. © 2012 by the American Institute of Aeronautics and Astronautics, Inc.

Pieters C.M.,Brown University | Besse S.,University of Maryland University College | Boardman J.,Analytical Imaging and Geophysics LLC | Buratti B.,Jet Propulsion Laboratory | And 23 more authors.
Journal of Geophysical Research E: Planets | Year: 2011

High-resolution compositional data from Moon Mineralogy Mapper (M 3) for the Moscoviense region on the lunar farside reveal three unusual, but distinctive, rock types along the inner basin ring. These are designated "OOS" since they are dominated by high concentrations of orthopyroxene, olivine, and Mg-rich spinel, respectively. The OOS occur as small areas, each a few kilometers in size, that are widely separated within the highly feldspathic setting of the basin rim. Although the abundance of plagioclase is not well constrained within the OOS, the mafic mineral content is exceptionally high, and two of the rock types could approach pyroxenite and harzburgite in composition. The third is a new rock type identified on the Moon that is dominated by Mg-rich spinel with no other mafic minerals detectable (<5% pyroxene, olivine). All OOS surfaces are old and undisturbed since basin formation. They are effectively invisible in image data and are only recognized by their distinctive composition identified spectroscopically. The origin of these unusual lithologies appears to be linked to one or more magmatic intrusions into the lower crust, perhaps near the crust-mantle interface. Processes such as fractional crystallization and gravity settling within such intrusions may provide a mechanism for concentrating the mafic components within zones several kilometers in dimension. The OOS are embedded within highly anorthositic material from the lunar crust; they may thus be near contemporaneous with crustal products from the cooling magma ocean. Copyright © 2011 by the American Geophysical Union.

Murchie S.L.,Johns Hopkins University | Klima R.L.,Johns Hopkins University | Denevi B.W.,Johns Hopkins University | Ernst C.M.,Johns Hopkins University | And 13 more authors.
Icarus | Year: 2015

A principal data product from MESSENGER's primary orbital mission at Mercury is a global multispectral map in eight visible to near-infrared colors, at an average pixel scale of 1km, acquired by the Mercury Dual Imaging System. The constituent images have been calibrated, photometrically corrected to a standard geometry, and map projected. Global analysis reveals no spectral units not seen during MESSENGER's Mercury flybys and supports previous conclusions that most spectral variation is related to changes in spectral slope and reflectance between spectral end-member high-reflectance red plains (HRP) and low-reflectance material (LRM). Comparison of color properties of plains units mapped on the basis of morphology shows that the two largest unambiguously volcanic smooth plains deposits (the interior plains of Caloris and the northern plains) are close to HRP end members and have average color properties distinct from those of most other smooth plains and intercrater plains. In contrast, smaller deposits of smooth plains are nearly indistinguishable from intercrater plains on the basis of their range of color properties, consistent with the interpretation that intercrater plains are older equivalents of smooth plains. LRM having nearly the same reflectance is exposed in crater and basin ejecta of all ages, suggesting impact excavation from depth of material that is intrinsically dark or darkens very rapidly, rather than gradual darkening of exposed material purely by space weathering. A global search reveals no definitive absorptions attributable to Fe2+-containing silicates or to sulfides over regions 20km or more in horizontal extent, consistent with results from MESSENGER's Mercury Atmospheric and Surface Composition Spectrometer. The only absorption-like feature identified is broad upward curvature of the spectrum centered near 600nm wavelength. The feature is strongest in freshly exposed LRM and weak or absent in older exposures of LRM. We modeled spectra of LRM as intimate mixtures of HRP with candidate low-reflectance phases having a similar 600-nm spectral feature, under the assumption that the grain size is 1μm or larger. Sulfides measured to date in the laboratory and coarse-grained iron are both too bright to produce LRM from HRP. Ilmenite is sufficiently dark but would require Ti abundances too high to be consistent with MESSENGER X-Ray Spectrometer measurements. Three phases or mixtures of phases that could be responsible for the low reflectance of LRM are consistent with our analyses. Graphite, in amounts consistent with upper limits from the Gamma-Ray Spectrometer, may be consistent with geochemical models of Mercury's differentiation calling for a graphite-enriched primary flotation crust from an early magma ocean and impact mixing of that early crust before or during the late heavy bombardment (LHB) into material underlying the volcanic plains. The grain size of preexisting iron or iron sulfide could have been altered to a mix of nanophase and microphase grains by shock during those impacts, lowering reflectance. Alternatively, iron-bearing phases and carbon in a late-accreting carbonaceous veneer may have been stirred into the lower crust or upper mantle. Decoupling of variations in color from abundances of major elements probably results from the very low content and variation of Fe2+ in crustal silicates, such that reflectance is controlled instead by one or more minor opaque phases and the extent of space weathering. © 2015 Elsevier Inc.

Domingue D.L.,Planetary Science Institute | Denevi B.W.,Johns Hopkins University | Murchie S.L.,Johns Hopkins University | Hash C.D.,Applied Coherent Technology Corporation
Icarus | Year: 2016

Photometric analyses are used to standardize images obtained at a variety of illumination and viewing conditions to a common geometry for the construction of maps or mosaics and for comparison with spectral measurements acquired in the laboratory. Many models exist that can be used to model photometric behavior. Two of the most commonly use models, those of Hapke and Kaasalainen-Shkuratov, are compared for their ability to standardize MESSENGER images of Mercury. Analysis of the modeling results shows that photometric corrections using the Kaasalainen-Shkuratov model provides significantly less contrast between images acquired at large differences in emission angle. The contrast seen between images acquired at large differences in either incidence and phase angle is smaller with the Hapke model based corrections, but not significantly better than that provided by the Kaasalainen-Shkuratov model. Photometric studies are also used to infer scattering properties of the surface regolith. The quantitative correlation between photometric model parameters and surface properties is questionable, but laboratory studies do indicate general correlations and trends between parameters and sample properties that allow for comparisons between surfaces based on photometric modeling. Based on comparisons with the Moon and several asteroids that have been observed by spacecraft, the photometric analyses presented here are interpreted to indicate that Mercury's regolith is smoother on micrometer scales and has a narrower particle size distribution with a lower mean particle size than lunar regolith. Grain structures of regolith particles from Mercury are inferred to be different than those of the Moon or those asteroids observed to date. Mercury's regolith may contain a component compositionally distinct from lunar regolith. © 2016 The Authors.

Izenberg N.R.,Johns Hopkins University | Klima R.L.,Johns Hopkins University | Murchie S.L.,Johns Hopkins University | Blewett D.T.,Johns Hopkins University | And 14 more authors.
Icarus | Year: 2014

The MESSENGER spacecraft's Mercury Atmospheric and Surface Composition Spectrometer (MASCS) obtained more than 1.6. million reflectance spectra of Mercury's surface from near-ultraviolet to near-infrared wavelengths during the first year of orbital operations. A global analysis of spectra in the wavelength range 300-1450. nm shows little regional variation in absolute reflectance or spectral slopes and a lack of mineralogically diagnostic absorptions. In particular, reflectance spectra show no clear evidence for an absorption band centered near 1. μm that would be associated with the presence of ferrous iron in silicates. There is, however, evidence for an ultraviolet absorption possibly consistent with a very low iron content (2-3. wt% FeO or less) in surface silicates and for the presence of small amounts of metallic iron or other opaque minerals in the form of nano- or micrometer-sized particles. These findings are consistent with MESSENGER X-ray and gamma-ray measurements of Mercury's surface iron abundance. Although X-ray and gamma-ray observations indicate higher than expected quantities of sulfur on the surface, reflectance spectra show no absorption bands diagnostic of sulfide minerals. Whereas there is strong evidence of water ice in permanently shadowed craters near Mercury's poles, MASCS spectra provide no evidence for hydroxylated materials near permanently shadowed craters. © 2013 Elsevier Inc.

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