HRSC Data Browser

Click here to open the HRSC Data Browser.


To download the complete HRSC images go to the Planetary Science Archive (ESA) or Planetary Data System (NASA).

Overview: The High Resolution Stereo Camera (HRSC)

To download the HRSC fact sheet providing further detailed information, useful links, software suggestions, and many more please click here.

Figure 1: HRSC system configuration (top); overall length of the camera system including baffle and digital unit is approx. 75 cm. Operating principle and viewing geometry of the individual CCD sensors (bottom); ND-nadir channel; S1, S2- stereo 1 and stereo 2 (±18.9°); P1 and P2- photometry 1 and photometry 2 (±12.8°); IR- near-infrared channel (+15.9°); GR- green channel (+3.3°); BL- blue channel (-3.3°); RE- red channel (+15.9°). All nine line sensors have a cross track field of view of ±6°. SRC- super-resolution channel (panchromatic) (Jaumann et al., 2007).

HRSC is a High Resolution Stereo Camera onboard the ESA's Mars Express spacecraft in orbit around Mars. This instrument provides high spatial resolution images of the Martian surface in 3D, and in full color. It was developed by the German Aerospace Center (DLR) and built in cooperation with industrial partners (EADS Astrium, Lewicki Microelectronic GmbH and Jena-Optronik GmbH). An airborne version of the HRSC camera, the HRSC-AX, is used to investigate terrestrial analogues (see the DLR Svalbard Campaign theme). The HRSC experiment is led by the Principal Investigator (PI) Prof. Dr Ralf Jaumann (FU Berlin). The science team of the experiment consists of 51 Co-Investigators from 33 institutions and 11 nations. Since its first data acquirements in January 2004, the camera provided the basis for extensive studies of the surface structure and morphology on local, regional and global scales using the photogeologic information from the image, the topographic information from the digital terrain model and spectral terrain information from color images (Jaumann et al., 2007). HRSC made a major contribution to the topographic mapping of Mars.

The HRSC instrument

The HRSC is a multi-sensor push broom instrument composed of 9 CCD line sensors mounted in parallel for simultaneous high-resolution stereo, multicolor and multi-phase imaging by delivering 9 superimposed image swaths (Neukum, et al., 2004) (Figure 1).

The stereo imaging is produced by 3 to 5 panchromatic channels including a nadir-directed, forward and aft-looking (±18.9°), and 2 inner (±12.8°) stereo line sensors. Their spectral range covers 675±90 nm (width at half-maximum). The along-track acquisition of stereo imagery avoids changes in atmospheric and illumination conditions, which so far have caused problems in the photogrammetric evaluation of stereo images acquired at different observing times (Jaumann et al., 2007). The triple to quintuple stereo images permit robust stereo reconstruction, yielding digital terrain models (DTMs) at a vertical accuracy of up to one pixel. The 5 panchromatic images are also used for multi-phase imaging allowing the determination of photometric surface characteristics.

Multispectral imaging is realized by four line sensors in the blue, green, red and near-infrared color ranges (440±45 nm, 530±45 nm, 750±20 nm, 970±45nm).

The HRSC instrument is also equipped of a Super Resolution Channel (SRC) telescope imaging the surface at 2.35 m/pixel (at the nominal periapsis altitude of 250 km).

The HRSC spatial resolution is 10 m/pixel at the nominal periapsis altitude of 250 km, with an image swath of 53 km. Until April 2009, HRSC achieved about 50% coverage of the surface with resolutions better than 20 m/pixel. The following figures display different HRSC products acquired in the region of Hebes Chasma in Valles Marineris, which is the biggest canyon system in the solar system (Figure 2).





Figure 2: MOLA shaded relief map of a portion of Valles Marineris displaying the location of the HRSC orbit 2140 over Hebes Chasma (1° S, 282°E). This orbit was obtained on 16 September 2005 with a spatial resolution of ~15 m/pixel. Credits: FU Berlin/ MOLA.

Nadir panchromatic and color images

Figure 3: Nadir image of a portion of Hebes Chasma. Credits: ESA/ DLR/ FU Berlin (G. Neukum)
Figure 4: False-color nadir view of Hebes Chasma. Credits: ESA/ DLR/ FU Berlin (G. Neukum)

Digital Terrain Models (DTM),ortho-images, and anaglyphs

Figure 5: Perspective view of Hebes Chasma corresponding to a HRSC-derived DTM overlaid with a false-color HRSC image. Credits: ESA/ DLR/ FU Berlin (G. Neukum)

The HRSC DTMs derived by stereo-photogrammetry have a grid size of 200 m that can reach up to 50 m and a vertical accuracy up to 10 m. Ortho-images are high-level topographic data products derived from the differential rectification of the original imagery based on previously derived HRSC DTMs (Scholten et al., 2005).

Figure 6: HRSC ortho-image of Hebes Chasma overlaid with elevation data from a HRSC-derived DTM. Credits: ESA/ DLR/ FU Berlin (G. Neukum).
Figure 7: 3D (anaglyph) image of Hebes Chasma. The anaglyph image was calculated from the nadir and one stereo channel, stereoscopic glasses are required to view it. Credits: ESA/ DLR/ FU Berlin (G. Neukum)

Last update: 26/11/2014 09:26