The high-resolution stereo camera (HRSC) experiment on Mars Express: Instrument aspects and experiment conduct from interplanetary cruise through the nominal mission

Jaumann, R.; Neukum, G.; Behnke, Thomas; Duxbury, T.; Eichentopf, K.; Flohrer, J.; Gasselt, S. van; Giese, B.; Gwinner, K.; Hauber, Ernst; Hoffmann, H.; Hoffmeister, Angelika; Köhler, Ulrich; Matz, Klaus-Dieter; McCord, T. B.; Mertens, Volker; Oberst, J.; Pischel, R.; Reiss, D.; Ress, E.; Roatsch, Thomas; Saiger, Peter; Scholten, F.; Schwarz, Gottfried; Stephan, K.; Wählisch, Marita

doi:10.1016/j.pss.2006.12.003

Cited by 415 publications

(218 citation statements)

References 56 publications

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“…Gridded elevation data from the MOLA instrument (Smith et al, 2001) was used in the forms of contours, elevation cross sections, and colorized elevation to help identify unit contacts and perform other detailed analyses. Similarly, Digital Terrain Models (DTMs) from the HRSC (Jaumann et al, 2007) (~12.5 m/pixel) were useful in determining elevation differences for geologic mapping. All elevations discussed are based on gridded MOLA elevation values, and map coordinates use the IAU2000 reference system.…”

Section: Methodsmentioning

confidence: 99%

“…The first objective of this study is to map the Mangala Valles using Mars Reconnaissance Orbiter (MRO) Context Camera (CTX) images (Malin et al, 2007) to achieve a level of detail comparable to Basilevsky et al (2008), but over the outflow channel system in its entirety. CTX images provide a spatial resolution (~6 m/pixel) and coverage that was not available to previous authors, who relied on High-Resolution Stereo Camera (HRSC) onboard Mars Express (Jaumann et al, 2007), Mars Global Surveyor (MGS) Mars Orbiter Camera (MOC) (Malin and Edgett, 2001), MGS Mars Orbiter Laser Altimeter (MOLA) (Smith et al, 2001), and Viking data . The resolution of CTX images allows for the detection of small, but key surface features that lead to an improved understanding of the stratigraphic relations of larger geologic units.…”

Section: Introductionmentioning

confidence: 99%

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Episodes of fluvial and volcanic activity in Mangala Valles, Mars

Keske

Hamilton

McEwen

et al. 2015

Icarus

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A new mapping-based study of the 900-km-long Mangala Valles outflow system was motivated by the availability of new high-resolution images and continued debates about the roles of water and lava in outflow channels on Mars. This study uses photogeologic analysis, geomorphic surface mapping, cratering statistics, and relative stratigraphy. Results show that Mangala Valles underwent at least two episodes of fluvial activity and at least three episodes of volcanic activity during the Late Amazonian. The occurrence of scoured bedrock at the base of the mapped stratigraphy, in addition to evidence provided by crater retention ages, suggests that fluvial activity preceded the deposition of two of the volcanic units. Crater counts performed at 30 locations throughout the area have allowed us to construct the following timeline: (1) formation of Noachian Highlands and possible initial flooding event(s) before ~1 Ga, (2) emplacement of Tharsis lava flows in the valley from ~700 to 1000 Ma, (3) a megaflooding event at ~700-800 Ma sourced from Mangala Fossa, (4) valley fill by a sequence of lava flows sourced from Mangala Fossa ~400-500 Ma, (5) another megaflooding event from ~400 Ma, (6) a final phase of volcanism sourced from Mangala Fossa ~300-350 Ma, and (7) emplacement of eolian sedimentary deposits in the northern portion of the valley ~300 Ma. These results are consistent with alternating episodes of aqueous flooding and volcanism in the valles. This pattern of geologic activity is similar to that of other outflow systems, such as Kasei Valles, suggesting that there is a recurring, and perhaps coupled, nature of these processes on Mars.

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Section: Methodsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Episodes of fluvial and volcanic activity in Mangala Valles, Mars

Keske

Hamilton

McEwen

et al. 2015

Icarus

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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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“…While photogeology provides the qualitative interpretation of two-dimensional images, the third dimension is needed for quantitative geological analyses in terms of surface slopes, volumes, and mass balance of materials. with areas discussed by identified derived from HST images Detailed mapping of the topography is particularly important for understanding surface processes (Jaumann et al 2007) and is accomplished at Vesta through extensive stereoscopic mapping (Raymond et al 2011, this issue). FC multispectral imaging of the surface provides information on the spatial extent and character of compositional units.…”

Section: Introductionmentioning

confidence: 99%

Surface Composition of Vesta: Issues and Integrated Approach

et al. 2011

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The instruments on the Dawn spacecraft are exceptionally well suited to characterize and map the surface composition of Vesta in an integrated manner. These include a framing camera with multispectral capabilities, a high spectral resolution near-infrared imaging spectrometer, and a gamma-ray and neutron spectrometer. Three examples of issues addressed at Vesta are: (1) What is the composition of Vesta's interior and differentiation state as exposed by the Great South Crater? (2) How has space weathering affected Vesta, both globally and at a local scale? and (3) Are volatiles or hydrated material present on Vesta's surface? We predict that Dawn finds many surprises, such as an olivine-bearing mantle exposed near the south-pole, a weakly or un-weathered surface that has been rela- tively recently resurfaced, and a very thin layer of surficial volatiles derived from interaction with the solar wind.

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The high-resolution stereo camera (HRSC) experiment on Mars Express: Instrument aspects and experiment conduct from interplanetary cruise through the nominal mission

Cited by 415 publications

References 56 publications

Episodes of fluvial and volcanic activity in Mangala Valles, Mars

Episodes of fluvial and volcanic activity in Mangala Valles, Mars

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

Surface Composition of Vesta: Issues and Integrated Approach

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