HRSC: the High Resolution Stereo Camera of Mars Express

By Gerhard Neukum, Ralf Jaumann, Hrsc Co-Investigator, Experiment Team. 2004

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Fluid lava flows in Gusev crater, Mars (2005, unknown): “For example, Figure 2 shows the floor of Gusev crater imaged by the High Resolution Stereo Camera (HRSC) [ Neukum et al. , 2004] on board the Mars Express orbiter compared with Grimaldi crater on the Moon, which was flooded with basaltic lavas but has no indication of the source vents.”
Radar evidence for ice in lobate debris aprons in the mid‐northern latitudes of Mars (2009, methodology): “However, in most cases, inspection of MOLA topography and higher resolution imagery from the High Resolution Stereo Camera [Neukum et al., 2004] and Thermal Emission Imaging System [Christensen et al., 2004] indicates that surface clutter cannot be responsible for the later echoes, and we thus…”
Mars Express HRSC Data Processing - Methods and Operational Aspects (2005, methodology): “The full exploitation of the HRSC potential for systematic and stereo-photogrammetric processing requires methods which take into account the specific geometric characteristics of the applied multi-line pushbroom sensor type and the imaging conditions during the mission.”
Mars Reconnaissance Orbiter's High Resolution Imaging Science Experiment (HiRISE) (2007, methodology): “[27] HiRISE color data will be complementary to that from the Thermal Emission Imaging System (THEMIS) [Christensen et al., 2004] and High Resolution Stereo Camera (HRSC) [Neukum and Jaumann, 2004].”
Gusev crater: Wind‐related features and processes observed by the Mars Exploration Rover Spirit (2006, methodology): “In addition, Thermal Emission Imaging System (THEMIS) [Christensen et al., 2004b] data from Mars Odyssey and High Resolution Stereo Camera (HRSC) [Neukum et al., 2004] images from Mars Express were analyzed to identify potential changes on the surface just before and during Spirit operations…”
The High Resolution Stereo Camera (HRSC) of Mars Express and its approach to science analysis and mapping for Mars and its satellites (2016, background): “Finally, we note that the horizontal strip offsets even in the single-strip case amount to a fraction of the MOLA grid size and are on the order of the estimated lateral position uncertainty of individual MOLA profiles (about 100 m; Neumann et al., 2003).”
Large-scale spring deposits on Mars? (2008, methodology): “Indeed, Tharsis activity dates back to the Noachian and developed during Hesperian and Amazonian [Scott and Tanaka, 1986], but the volcanic, and likely hydrothermal and enhanced hydrologic activity, has persisted possibly up to recent times [Neukum et al., 2004b, 2007].”
The timing of martian valley network activity : Constraints from buffered crater counting (2008, background): “Valley networks appear to have had less influence on modifying the characteristics of drainage basin topography than is typical on Earth (Stepinski and Collier, 2004), and low-order tributaries appear less commonly on Mars than on Earth, suggesting a less mature drainage system on Mars.”