Stereo topographic models of Mercury after three MESSENGER flybys

Preusker, Frank; Oberst, J.; Head, J. W.; Watters, T. R.; Robinson, M. S.; Zuber, M. T.; Solomon, Sean C.

doi:10.1016/j.pss.2011.07.005

Cited by 52 publications

(54 citation statements)

References 15 publications

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“…Topographic information for Mercury was gathered through two separate MESSENGER sources: (1) Mercury Laser Altimeter (MLA) data (Zuber et al, 2012) and (2) Deutsche Zentrum für Luft-und Raumfahrt, German Aerospace Center (DLR) stereo-mosaics (Preusker et al, 2011).…”

Section: Topographymentioning

confidence: 99%

“…However, the 665 m layer is affected by a decrease in quality towards the south of H02 because of the widening spacing between MLA tracks (up to ∼100 km at 22.5°N). The DLR stereo-topography is a product of three MESSENGER flybys (M1, M2 and M3) that covered 30% of the planet with a spatial resolution of 1000 m (Preusker et al, 2011). About 80% of the Victoria quadrangle is covered by the M2 stereo-mosaic as shown in Figure 2(c).…”

Section: Topographymentioning

confidence: 99%

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Geology of the Victoria quadrangle (H02), Mercury

et al. 2016

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Mercury's quadrangle H02 'Victoria' is located in the planet's northern hemisphere and lies between latitudes 22.5°N and 65°N, and between longitudes 270°E and 360°E. This quadrangle covers 6.5% of the planet's surface with a total area of almost 5 million km 2 . Our 1:3,000,000-scale geologic map of the quadrangle was produced by photo-interpretation of remotely sensed orbital images captured by the MESSENGER spacecraft. Geologic contacts were drawn between 1:300,000 and 1:600,000 mapping scale and constitute the boundaries of intercrater, intermediate and smooth plains units; in addition, three morpho-stratigraphic classes of craters larger than 20 km were mapped. The geologic map reveals that this area is dominated by Intercrater Plains encompassing some almost-coeval, probably younger, Intermediate Plains patches and interrupted to the north-west, north-east and east by the Calorian Northern Smooth Plains. This map represents the first complete geologic survey of the Victoria quadrangle at this scale, and an improvement of the existing 1:5,000,000 Mariner 10-based map, which covers only 36% of the quadrangle. ARTICLE HISTORY

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Section: Topographymentioning

confidence: 99%

Section: Topographymentioning

confidence: 99%

Geology of the Victoria quadrangle (H02), Mercury

et al. 2016

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“…(a) M1 portion of the stereo-derived DTM (Mancinelli et al, 2015;Preusker et al, 2011) with a resolution of 1 km/pixel. Due to systematic noise in the original portion M1 of the DTM from Preusker et al (2011), this was filtered with a 5×5 kernel low-pass filter (LPF) and fast Fourier (FFT), adding back 20% of the original value in order to preserve the spatial context (Mancinelli et al, 2015). (b) Portion of the northern hemisphere DTM at a resolution of 665 m/pixel (Zuber et al, 2012).…”

Section: Methodsmentioning

confidence: 99%

“…Despite that the northern hemisphere MLA DTM covers a larger portion of the quadrangle, it loses resolution at mid-and low latitudes (Figure 2(b)). Therefore, we used the M1 portion of the DTM (Preusker et al, 2011) as the main topographic support for the southern half of the map, the northern hemisphere DTM for the western boundary and the polar DTM for the northern part of the quadrangle. Scale values refer to the standard parallels.…”

Section: Methodsmentioning

confidence: 99%

Geology of the Raditladi quadrangle, Mercury (H04)

et al. 2016

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In this work, we present a 1:3,000,000-scale geologic map of the Raditladi quadrangle (H04) of Mercury. The area covers nearly 7% of the entire planet and encompasses several features of interest such as the Caloris basin, the Raditladi basin, hollow clusters and volcanic features. The mapping took advantage of the data produced during MESSENGER's orbital phase. The mapped deposits include impact-related units observed at several scales from the Caloris basin to the secondary crater chains. The Smooth Plains unit covers the majority of the area, mantling the older Intercrater Plains and Bright Intercrater Plains units. Results show that the emplacement of all the main units and the Caloris impact event, representing the main geologic events in the quadrangle, were concentrated between 3.96 and 3.72 Ga. After this intense phase, the geologic framework was modified only by local events such as impact craters and hollow formation. This map is among the first products for the detailed geologic characterization of Mercury at such a scale. It will contribute as a constraint and a support for both further local investigation and mapping, and targeting of the forthcoming BepiColombo ESA/JAXA joint exploration mission to Mercury. ARTICLE HISTORY

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“…During the orbital phases, the FC mapped the surface at image scales of $260 m/pixel (FC) in the survey phase, $60 m/pixel in HAMO and $20 m/pixel in the Low Altitude Mapping Orbit (LAMO). The stereo-photogrammetric processing of Dawn images is based on a software suite that has been applied successfully to several planetary stereo image data sets (Jaumann et al, 2007;Gwinner et al, 2009;Preusker et al, 2011). There are five steps to gain Dawn stereo-photogrammetry: photogrammetric block adjustment; multi-image matching; surface point triangulation; digital terrain model (DTM) generation; and base map generation .…”

Section: Data Base and Methodsmentioning

confidence: 99%

The geological nature of dark material on Vesta and implications for the subsurface structure

Jaumann

Naß

Otto

et al. 2014

Icarus

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a b s t r a c tDeposits of dark material appear on Vesta's surface as features of relatively low-albedo in the visible wavelength range of Dawn's camera and spectrometer. Mixed with the regolith and partially excavated by younger impacts, the material is exposed as individual layered outcrops in crater walls or ejecta patches, having been uncovered and broken up by the impact. Dark fans on crater walls and dark deposits on crater floors are the result of gravity-driven mass wasting triggered by steep slopes and impact seismicity. The fact that dark material is mixed with impact ejecta indicates that it has been processed together with the ejected material. Some small craters display continuous dark ejecta similar to lunar dark-halo impact craters, indicating that the impact excavated the material from beneath a higher-albedo surface. The asymmetric distribution of dark material in impact craters and ejecta suggests non-continuous distribution in the local subsurface. Some positive-relief dark edifices appear to be impact-sculpted hills with dark material distributed over the hill slopes. Dark features inside and outside of craters are in some places arranged as linear outcrops along scarps or as dark streaks perpendicular to the local topography. The spectral characteristics of the dark material resemble that of Vesta's regolith. Dark material is distributed unevenly across Vesta's surface with clusters of all types of dark material exposures. On a local scale, some craters expose or are associated with dark material, while others in the immediate vicinity do not show evidence for dark material. While the variety of surface exposures of dark material and their different geological correlations with surface features, as well as their uneven distribution, indicate a globally inhomogeneous distribution in the subsurface, the dark material seems to be correlated with the rim and ejecta of the older Veneneia south polar basin structure. The origin of the dark material is still being debated, however, the geological analysis suggests that it is exogenic, from carbon-rich low-velocity impactors, rather than endogenic, from freshly exposed mafic material or melt, exposed or created by impacts.

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Stereo topographic models of Mercury after three MESSENGER flybys

Cited by 52 publications

References 15 publications

Geology of the Victoria quadrangle (H02), Mercury

Geology of the Victoria quadrangle (H02), Mercury

Geology of the Raditladi quadrangle, Mercury (H04)

The geological nature of dark material on Vesta and implications for the subsurface structure

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