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ABSTRACT: A variety of sedimentary deposits is observed in Xanthe Terra, Mars, including Gilbert-type deltas, fan deltas dominated by resedimentation processes, and alluvial fans. Sediments were provided through deeply incised valleys, which were probably incised by both runoff and groundwater sapping. Mass balances based on High-Resolution Stereo Camera (HRSC) digital terrain models show that up to ~30% of the material that was eroded in the valleys is present as deltas or alluvial fan deposits. Stratigraphic relationships and crater counts indicate an ageof ~4.0 to ~3.8 Ga for the fluvial activity. Hydrologic modeling indicates that the deposits were probably formed in geologically very short time scales. Our
results point to episodes of a warmer and wetter climate on early Mars, followed by a long period of significantly reduced erosion rates.
Planetary and Space Science 02/2013; 57(2009):944-957. · 2.22 Impact Factor
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ABSTRACT: Using the new High Resolution Stereo Camera (HRSC) data and other Martian data sets, we reconstructed the hydrological history of an unnamed complex crater in the Xanthe Terra region. The crater hosted a lacustrine basin fed by a dense and centripetal drainage system, developed along its inner rim, and by the Tyras Vallis channel. Where the Tyras Vallis opens into the crater, a prominent delta-like feature is visible, characterized by a central terrace and two small longitudinal scarps. This deposit has been used as sedimentary recorder of the crater lake history and allowed assessment of the overall hydrological evolution. Two major stands of the water level have been inferred at 700 and 550 m above the crater floor, based on the correlation between the morphology and topography of the fan and the crater floor deposits. Our reconstruction reveals a complex sedimentary evolution of the fan, which underwent deltaic and alluvial sedimentation, as a result of the different lake water levels and Tyras Vallis supplies. A dominant erosional evolution of the fan-delta was determined by the interaction between the fluvial characteristics and basin wave regime. Wave height analysis and morphological comparison with terrestrial analogues support this hypothesis. The lacustrine activity could be chronologically placed between the Late Noachian and the Hesperian. The climatic conditions could have allowed the recharge of the regional groundwater system by precipitation and episodic fluvial activity. However, also heating effects of cratering could have affected the system, rejuvenating or accelerating the recharge of the local aquifer.
Journal of Geophysical Research 02/2013; 111(2006-04-08):E04003. · 3.02 Impact Factor
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ABSTRACT: We investigate a steep fan-like deposit in the Coprates Catena region, using the new High Resolution Stereo Camera (HRSC) data and other Martian data sets. Water flowing in a 45-km-long sapping valley entered a deep trough and formed a stepped fan 1100-m-high above the trough floor with a mean slope of 7.4°. The origin of the fan is uncertain. However, we favor an alluvial, sheetflood-dominated deposition for the sedimentary feature, though there is weak evidence for a possible stationary water level (∼500 m above the floor) and a fan-delta origin. Regional morphotectonics and previous geological mapping suggest that groundwater-related aqueous sedimentation could have been active from Hesperian to Early Amazonian implying favorable climatic conditions for the flow and possible ponding of water during that period.
Geophysical Research Letters 02/2013; 33(2006-04-15):L07204. · 3.79 Impact Factor
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Gerhard Neukum,
Ralf Jaumann,
Alexander T. Basilevsky,
Alexander Dumke,
Stephan Van Gasselt,
Bernd Giese,
Ernst Hauber,
James W. Head,
Christian Heipke,
Nick Hoekzema, [......],
Jan-Peter Muller,
John B. Murray,
Jürgen Oberst,
Patrick C. Pinet,
René Pischel,
Thomas Roatsch,
Frank Scholten,
Konrad Willner,
the HRSC Co-Investigator Team,
HRSC Associates
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ABSTRACT: The ESA special publication SP-1291, published in June 2009, is dedicated to the scientific investigations of Mars Express, the first European mission to another planet.
The Mars Express spacecraft has been orbiting Mars since December 2003, carrying a suite of instruments that are investigating many scientific aspects of this planet in unprecedented detail.
Following a thematic overview of the mission's scientific results so far, the next seven chapters of this publication explain the scientific investigations in detail, for each of the instruments separately. These individual chapters can be downloaded in PDF format by clicking on the links in the table below.
The complete ESA SP-1291 publication, but with reduced image resolution for distribution on the web, can be downloaded as a single PDF by clicking on the cover image on the right.
01/2009: pages 15-74; , ISBN: 978-92-9221-975-8
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ABSTRACT: This study is based on the analysis of images taken by MEX High Resolution Stereo Camera and in combination with MGS MOC images. 3-D imagery in the form of HRSC-based anaglyphs and DTMs were very helpful for the study. Our observation and analysis confirm the well-known interpretation of Olympus Mons as a giant shield volcano, but also show that this construct locally has probably partly been made of airborne dust (and/or ash) and ice layered deposits (Neukum et al, 2004; Basilevsky et al., 2005; this study). The deposits form mesas locally standing above the lava fields in the volcano western and eastern flanks as well as ridges locally observed at the top parts of the scarps rimming the Olympus construct on its western and northern flanks. The ridge tops stand a few hundred meters above the adjacent lava flows coming from the volcano top. Ice presence in these deposits was inferred from the presence of "collapse" features locally extending downslope as channel-like forms. The neutron-spectrometry measurements (Feldman et al., 2004) show a noticeable decrease in the neutron flux suggesting presence of up to 15-18 vol. % of equivalent water (ice) in the upper 1 m surface layer in the western part of the construct. The ice-rich deposits could have been emplaced during the epochs of high orbital inclination of Mars (Mishna et al., 2004) and could be partly preserved in the modern epoch due to protecting dust covers (Skorov et al., 2001). At the foot of the western slope of the volcano are seen flow-like features interpreted as remnants of rock glaciers (Lucchitta, 1981; Milkovich and Head, 2006). The dating by crater statistics shows that different areas of the Olympus Mons construct and lava fields at its foot have a spread of ages from >3.5 b.y. to 2 m.y. and glacier-like flows show a 0.5 b.y. to 4 m.y. age range. The eastern flank of the volcano shows a complex of morphologies caused by fluvial (channels), tectonic (wrinkle ridges) and volcanic (lava flows and dikes) processes, which occurred in very recent time (<30-40 m.y. ago). Taking in account that the Olympus construct shows signatures of volcanis activity from very ancient (>3.5 b.y.) until very recent time (e.g., Neukum and Hiller, 1981; Neukum et al., 2004; this study) and that it occurred in at least episodic presence of subsurface water/ice, this 1 area may be a candidate long-duration Martian life habitat (Basilevsky et al., 2006) (Source: http://adsabs.harvard.edu/abs/2006epsc.conf..394B).
EPSC Abstracts. 09/2006;
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Christian Heipke,
Jürgen Oberst,
Jörg Albertz,
Maria Attwenger,
Peter Dorninger,
Egon Dorrer,
Markus Ewe,
Stephan Gehrke, Klaus Gwinner,
Heiko Hirschmüller, [......],
Jan-Peter Muller,
R. Rengarajan,
Matthias Rentsch,
Ralph Schmidt,
Frank Scholten,
Ji Shan,
Michael Spiegel,
Marita Wählisch,
Gerhard Neukum,
HRSC CO-Investigator team
ISPRS, Commission IV;
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ABSTRACT: High Resolution Stereo Camera (HRSC) data , with their stereo capabilities, allow the investigation of Martian sedimentary features at unprecedented details. Using these new data, we reconstructed the hydrological history of an unnamed Noachian complex crater in the Xanthe Terra region. The crater hosted a lacustrine basin fed by a dense and centripetal drainage system, developed along its inner rim, and by the Tyras Vallis channel. Where the Tyras Vallis feeder channel opens into the crater, is visible a prominent fan-shaped distributary feature, characterized by a central terrace and two small longitudinal scarps. The delta-like deposit covers an area of about 83 km<sup>2</sup>, with a 13 km radial length and an average slope gradient of about 3.5 degrees. The apex of the fan lies ~900 m above the crater floor. To investigate the geology of the Tyras Vallis paleolacustrine system, we considered the geomorphologic characteristics of the mapped units and determined their relative ages based on stratigraphic relationships. Evidence of strandlines within the crater provided constraints about the past presence of a standing body of water with its wave-related processes. Topography derived by HRSC stereo data supported the analysis of the Tyras fan deposit and allowed to reconstruct the overall lacustrine depositional history from the parallel observations of the Tyras fan and crater floor deposits. Two major stands of the water level have been inferred at 700 m and 550 m above the crater floor. Our reconstruction reveals a complex sedimentary evolution of the fan, which underwent deltaic and alluvial sedimentation, passing from a river-dominated progradational regime to a wave-dominated erosional regime. Groundwater processes and intrinsic fluctuations of the sapping dynamics likely affected the transport capacity of the Tyras Vallis and the changes of the water level in the paleolake. Moreover, the heating effects of cratering might have affected the area, initiating, rejuvenating or accelerating the recharge of the aquifer and the basin evolution. This eventuality advised against any global paleoclimatic extrapolation.
GSA Annual Meeting 2005;
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Frank Scholten, Klaus Gwinner,
Thomas Roatsch,
Klaus-Dieter Matz,
Bernd Giese,
Marita Wählisch,
Jürgen Oberst,
Ernst Hauber,
Harald Hoffmann,
Volker Mertens,
Joachim Flohrer,
Ralf Jaumann,
Gerhard Neukum,
HRSC Co-I-Team
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ABSTRACT: Die High Resolution Stereo Kamera (HRSC) an Bord der Mars Express Mission liefert seit Januar 2004 hochauflösende Bilddaten der Marsoberfläche sowie der Monde Phobos und Deimos in verschiedenen Stereo- und Spektralkanälen. Eine weitgehend automatisierte Verarbeitung, deren Verfahren in den vergangenen Jahren entwickelt wurden, umfasst die folgenden Schritte: die Daten der einzelnen 9 Sensoren (4 multispektrale und 5 panchromatische Stereokanäle) werden zunächst radiometrisch kalibriert und alle an die Bilddaten zeitlich angebundenen Informationen, z.B. zu Position und Orientierung, sowie die Bilddaten des höchstauflösenden Super Resolution Channels (SRC) extrahiert. Auf der Basis dieser Daten werden anschließend photogrammetrische Verfahren der Stereoverarbeitung zur Ableitung von Digitalen Oberflächenmodellen und Orthobildern angewendet. Erste Datenprodukte dieser Art in Auflösungen von bis zu 10 m/Pixel für die HRSC und bis zu 2,3 m/Pixel für die SRC liegen innerhalb weniger Tage nach Aufnahme der Daten vor. Wir geben einen Überblick über die Verarbeitungsschritte und stellen Beispiele der erzielten Produkte vor.
AEF/EP Frühjahrstagung;
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ABSTRACT: Automated procedures for ground processing of Mars Express HRSC data have been developed and are applied systematically immediately after download in order to provide calibrated data sets as well as photogrammetric image and 3D data products within a short time frame. Multi-spectral orthoimages in scales of 10 - 50 m/pixel and digital terrain models of 200 m raster width are generated within days even for large orbits covering areas of several hundred thousand square kilometers. An even higher image resolution of up to 2.3 m/pixel provided by HRSC's Super Resolution Channel (SRC) extends the potential of the HRSC camera experiment.
Photogrammetric Engineering and Remote Sensing. 71(2005-10-10):1143-1152.
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Frank Scholten,
Thomas Roatsch,
Joachim Flohrer,
Bernd Giese, Klaus Gwinner,
Ernst Hauber,
Harald Hoffmann,
Ralf Jaumann,
Klaus-Dieter Matz,
Volker Mertens,
Gerhard Neukum,
Jürgen Oberst,
Marita Wählisch,
HRSC Co-I-Team
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ABSTRACT: The HRSC onboard Mars Express is a multi-line pushbroom scanner which provides image data from 5 panchromatic stereo channels and 4 spectral bands (Neukum et al, 2004). A completely automated ground data processing line has been developed in the past years and is being applied on a routine base for each MEX orbit. It comprises the conversion of the original data stream transmitted to ground to de-compressed data (Level-1 data), the radiometric correction of the image data based on calibration information (Level-2 data) combined with orbit and pointing information for each image line, and a first rectification to standard scales of up to 12.5 m/pixel (Level-3 data) using a-priori topography information as defined by the MGS MOLA instrument. Level-2 and Level-3 data of HRSC's Super Resolution Channel (SRC) in scales of up to 2.5 m/pixel complete the HRSC capabilities. Thus, Level-2 and Level-3 are ready for distribution to the HRSC Co-Investigator
team within one day after data acquisition.
A standard Level-4 generation is started after completion of Level-2 data in order to derive HRSC digital terrain models in a standard 200 m grid. These DTMs are finally used for the generation of orthoimages of all 4 spectral bands and the high-resolution nadir channel. This standardized processing provides 3D and image data products within a few days after data acquisition for first science analyses. Based on nominal pointing and reconstructed orbit information the standard Level-4 data products comprise a mean absolute accuracy of a few hundred meters for planimetry and of better than 100 m for height.
Reference:
Neukum, G., Jaumann, R. and the HRSC Co-Investigator Team, 2004. HRSC: The High
Resolution Stereo Camera of Mars Express. ESA Special Publications SP-1240.
1st Mars Express Science Conference;
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Frank Scholten,
Thomas Roatsch, Klaus Gwinner,
Klaus-Dieter Matz,
Volker Mertens,
Joachim Flohrer,
Marita Wählisch,
Bernd Giese,
Rene Pischel,
Jürgen Oberst,
Ralf Jaumann,
Gerhard Neukum,
HRSC Co-I-Team
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ABSTRACT: Mars Express HRSC-Daten werden im Rahmen eines standardisierten Verfahrens eines operationellen Bodendatensystems zeitnah zu Digitalen Oberflächenmodellen und Orthobildern verarbeitet. Die bildhaften und 3D-HRSC-Produkte erweitern die Kenntnis der Marsoberfläche. Eine Abdeckung von 40 % mit Bildauflösungen von bis zu 10 m und Oberflächenmodellen mit Rasterweiten von 200 m konnte bereits in den ersten 16 Monaten der Mission durch die automatisierten Verfahren erreicht werden.
Photogrammetrie - Fernerkundung - Geoinformation Jahrgang 2005(2005-10-5):365-372. · 0.38 Impact Factor
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38th Lunar and Planetary Science Conference;
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38th Lunar and Planetary Science Conference;
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38th Lunar and Planetary Science Conference;
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ABSTRACT: The Acheron Fossae region is an ancient crustal block exposed in the northwestern Tharsis province on Mars. It is named after the Acheron Fossae, a particularly well-developed system of extensional tectonic grabens. This study is the first to describe the tectonic inventory in detail, using topographic and image data from the Global Surveyor and Mars Express missions. We see the extensional tectonics along the east–west trending topographic high of Acheron Fossae as a surface expression of upwelling asthenospheric material that initiated regional uplift, crustal extension and breakup, and associated volcanic activity in Noachian time. The tectonic architecture and the dimensions of the extensional structures are comparable to those of terrestrial continental rifts. An area of elevated topography and strong erosion, which constitutes a regional landmark in the eastern Acheron Fossae region, is interpreted as a rift-related center of volcanism, caused by local magmatic uprise and involvement of the lithosphere. The extension across the Acheron Fossae reaches values between 1.2 km and 8.7 km, comparable to young continental rifts on Earth. Crater statistics indicate an absolute cratering model age between ∼3.9 Ga and 3.7 Ga for the rifting. The uplift observed on the flanks of the Acheron Fossae indicates a fairly thin and thus hot lithosphere. Using flexural analysis, we have constrained the elastic lithosphere thickness at the time of rifting to 8.9–11.3 km, corresponding to thermal gradients between 28 and 41 K km<sup>−1</sup>. These heat flows are substantially larger than Noachian heat flow values previously reported, but are consistent with the presence of rift-related volcanism and a magmatically very active environment.
Journal of Geophysical Research. 112(2007-04-E4):E04005.
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ABSTRACT: Zusammenfassung: Schwerpunkte der photogrammetrischen Verarbeitung von planetaren
Fernerkundungsdaten am Deutschen Zentrum für Luft- und Raumfahrt e.V. in Berlin-
Adlershof sind, soweit durch die Aufnahmegeometrie gegeben, die Stereo-Auswertung zur
Ableitung der Topographie der abgebildeten Oberflächen, die lagegenaue Orthorektifizierung
der Bilddaten der vorhandenen Spektralkanäle sowie die Darstellung der
Ergebnisse in kartographischer Form. Je nach Datenbestand erfolgen diese Arbeiten lokal,
regional oder global. Daneben werden im Rahmen der Auswertungen auch andere
wissenschaftliche Ziele im Bereich der Geodäsie und Geophysik verfolgt (Definition der
Planetenachsen, Bestimmung von Rotationsparametern, Aufbau und Verdichtung von
Kontrollpunktnetzen, astrometrische Bahnbestimmung, Erfassung von Atmosphärenphänomenen,
etc.).
Dreiländertagung;
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ABSTRACT: This contribution describes the experiences of more than 10 years of photogrammetric processing of multi-line scanner data. Automated procedures have originally been developed for processing of the different HRSC cameras, in operation on aircraft and since 4 years in space on the European Mars Express mission. Other types of airborne multi-line scanners can easily be integrated into the processing line, if interior orientation information is provided and continuous GPS/INS data have been measured. If a sensor comprises adequate stereo channels in matchable spectral bands, a 3D reconstruction of the visible surface can be performed by multi-image matching, multiple forward ray intersection, and surface model interpolation. Based on this surface model an ortho-rectification process can handle any channel in order to finally derive orthoimage mosaics (b/w or color) of overlapping image strips. A first integration of a Leica Geosystems ADS40 data set into the processing chain allowed for a precise photogrammetric restitution and the derivation of considerable 3D surface descriptions and orthoimage mosaics.
Optical 3-D Measurement Conference;
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ABSTRACT: Light-toned and layered deposits (LDs) are present throughout the whole Valles Marineris and adjacent chaotic terrains. They are supposed to be of sedimentary [1,2,3] or volcanic origin [4]. Using high-resolution image and elevation data, we study their morphology, elevation, thickness, layer geometry, and consolidation in order to ascertain how they formed.
LDs show differing morphologies. There are light-toned mounds with a flat top and steep slopes, flow-like structures where light-toned material flows around the chaotic-terrain material as well as terrace-like structures and razorblade-shaped morphologies that show massive cap rocks at their top and layering in lower parts. Often, there is a diffuse contact between LDs and chaotic terrain due to dust coverage. Many of the LDs exhibit yardangs, suggesting weakly consolidated and fine-grained material shaped by wind erosion. Wind activity is also indicated by dunes that occur in depressions (e.g., fractures) that are cut into the LD surfaces. Debris fans and a general lack of boulders at their base may indicate loose to partly consolidated sedimentary material. This is also confirmed by TES-derived thermal-inertia values of ~ 300 SI indicating rock materials [7].
Elevation data show that LDs are located in depressions at different elevations but far beneath the surrounding plateau rims (1000-4000 m in the chasmata, 200-1500 m in the chaotic terrains). LDs are superimposed on chaotic-terrain material and are therefore younger. Strike and dip measurements point towards sub-horizontal layering (in the range of lower than 10°) and NS- to NNE-SSW-strike for Iani Chaos. LD thicknesses vary in the range of 200-4000 m, assuming ILDs have horizontal to sub-horizontal stratification (Fig. 1.1, 1.2).
When looking at higher-resolution MOC images, deposits show varying surfaces (rough, fractured, grooved, cap rock). Different surfaces textures may be due to differences in consolidation and/or wind erosion; the mineralogical composition is however comparable. LDs are closely connected to sulphate- [5] and hematite rich materials [6]. A topographic trend is observed as some LDs show surfaces that are restricted to chaotic terrains and other to chasmata.
References:
[1] Peterson, C. (1981), Proc. Lunar Planet. Sci. Conf., 11th, 1459-1471. [2] Nedell et al. (1987), Icarus, 70, 409-441. [3] Malin M. C., and K. S. Edgett (2000), Science, 290, 1927-1937. [4] Chapman M. G. (2002), Geol. Soc. Spec. Publ., 202, 273-303. [5] Gendrin A. et al. (2005), Science, 307, 587-1591. [6] Glotch T.D., and P.R. Christensen (2005), JGR, 110, doi:10.1029/2004JE002389. [7] Putzig et al. (2005), Icarus, 173, 325-341.
European Mars Science and Exploration Conference: Mars Express & ExoMars;
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ABSTRACT: The High Resolution Stereo Camera (HRSC) onboard the Mars Express mission is the first photogrammetric stereo sensor system employed for planetary remote sensing. The derivation of high-quality digital terrain models is subject to a variety of parameters, some of which show a significant variability between and also within individual datasets. Therefore, adaptive processing techniques and the use of efficient quality parameters for controlling automated processing are considered to be key requirements for DTM generation. We present the general procedure for the derivation of HRSC high-resolution DTM, representing the core element of the systematic derivation of high-level data products by the Mars Express HRSC experiment team. We also analyze test series applying specific processing variations, including a new method for signal adaptive image preprocessing. The results are assessed based on internal quality measures and compared to external terrain data. Sub-pixel scale 3D point accuracy of better than 10 m and a DTM spatial resolution of up to 50 m can be achieved for large parts of the surface of Mars within a reasonable effort. This confirms the potentials of the applied along-track multiple stereo imaging principle and allows for a considerable improvement in our knowledge of the topography of Mars.
Photogrammetric Engineering and Remote Sensing 75(2009-9):1127-1142. · 1.05 Impact Factor
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AEF Frühjahrstagung/ DPG Jahrestagung;
