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topography data (Smith et al.
2001
) and Thermal Emission Imaging System
(THEMIS, on board the NASA Mars Odyssey orbiter) 100 m/pixel InfraRed (IR)
day-time mosaics (Christensen et al.
2004
) were used, both provided by the United
States Geological Survey (USGS) MeRCaToR Lab (Hare et al.
2012
). MOLA data
were added to rasdaman and THEMIS data were converted to GeoTIFF in order to
be accessed using MapServer. High Resolution Stereo Camera (HRSC, on board
the ESA Mars Express orbiter) ortho-recti
ed (Level 4) visual imagery and stereo-
derived DTMs (Neukum et al.
2004
; Gwinner et al.
2010
) were provided by the
Freie Universitaet Berlin.
On the client side a quick-view web client has been developed, based on
OpenLayers. The web client provides access to the CRISM and MOLA data using
the WCPS protocol and CTX, THEMIS and color-coded MOLA data using the
WMS protocol. ESRI ArcGIS 10.2, on the other hand, was used for advanced
analysis of the CTX and CRISM data. The CTX could be added to ArcGIS, as a
WMS service or as a JP2 raster. ArcGIS, however, does not have a standard
capability to analyze hyperspectral data, such as CRISM. Typically a planetary
scientist would use spectral analysis software such as IDL/ENVI instead. To enable
CRISM analysis directly inside ArcGIS a python add-in toolbox was developed
which uses the WCPS protocol to access the CRISM data the same way as the
PlanetServer web client does. It also allows for the loading of the various Planet-
Server WMS layers directly into ArcGIS.
A wiki system hosted at Jacobs University Bremen was used to collaboratively
share the results of the Noachis Terra Case Study among participating researchers.
3 Noachis Terra Case Study
The Noachis Terra region is situated in the heavily cratered southern highlands of
Mars. The region is the type location of the Noachian System in the Martian
chronostratigraphy (Tanaka et al.
2013
; Tanaka
1986
), which ended around 3.57
-
3.74 Ga (Werner and Tanaka
2011
). Enigmatic graben systems occur in the region,
immediately to the west of the 2,300 km in diameter Hellas impact basin. They
have been interpreted by Wichman and Schultz (
1989
) as distant-concentric
“
systems, related to the Hellas impact event (Fig.
2
). Rogers and Nazarian
(
2013
) detected olivine signatures in deposits which they interpreted to be effusive
volcanic plains, spatially associated with the graben structures (Fig.
2
). Carter et al.
(
2013b
) and Ehlmann et al. (
2012
) observed various types of hydrated minerals,
mostly associated with impact craters.
TheCase Study involved a 2,000
canyon
”
1,000 km
2
area inNoachis Terra, centered around
×
°
°
30
S(Figs.
2
and
3
). It encompassed (structural) geological mapping using,
among others, CTX data and a mineralogical investigation using CRISM data. The
relation between the tectonics, volcanism and hydrated minerals was investigated.
The (structural) geological mapping was started regional scale using semi-
transparent THEMIS mosaic data on top of color-coded MOLA data in ArcGIS.
E, 30
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