Rover
Panoramic Camera (PanCam)
This instrument consists of a wide angle stereo camera and a high resolution channel. This will provide environmental information for operating the Rover's environment and will be critical in selecting targets for detailed examination. The narrow band filters allow the mineral composition of rocks and soils to be inferred and the concentration of water vapour and the dust optical properties to be measured. The instrument is led by the UK.
UK Contact Point: Dr Andrew Coates|, Mullard Space Science Laboratory: Tel: 01483 204145.
Other UK academic institution involvement:
Leicester University
University of Wales, Aberystwyth
Raman-LIBS (Laser-Induced Breakdown Spectrometer)
The powerful combination of the Raman and LIBS techniques will be used to determine the geochemistry, organic content and atomic composition of minerals for both the collected samples and remote analysis. It can detect the presence of extinct or extant life from the characteristic biochemicals produced by extremophilic organisms. The UK is a key player in the development of the CCD camera.
UK Contact Point: Dr Ian Hutchinson|, Brunel University
Tel: 01895 266518
Other UK academic institution involvement
Bradford University
Rutherford Appleton Laboratory, STFC
X-Ray Diffractometer (XRD)
The XRD is an essential tool in the mineralogical identification of rock samples. The interaction between hydrothermal fluids and rocks strongly alters the composition of both and may lead to the precipitation of hydrous minerals and carbonates. This instrument is therefore important in identifying areas that might have been cable of supporting life for further investigation. The UK is providing the X-ray CCD detectors, optimised for the instrument, with signal processing electronics.
UK Contact point: Dr Ian Hutchinson|, Brunel University
Tel: 01895 266518
Other UK academic institution involvement:
Leicester University
Mars Organics and Oxidents Detector (MOD)
The objective of MOD is to determine the chemical reactivity of oxidants and free radicals. It searches for trace levels of specific organic molecules, amino acids and polycyclic aromatic hydrocarbons. The compounds targeted by MOD span all likely organic assemblages. The UK is involved developing the techniques for sample extraction and analysis which will feed into the instrument design and optimisation.
UK Contact Dr Mark Sephton|, Imperial College London
Tel: 020 7594 6542.
Life Marker Chip
The LMC will be used to look for specific molecules that may be associate dwith life by detecting biomarkers through using techniques developed in the medical and biotechnology sectors. Detection of the molecular targets will use immuno-assay techniques. The UK is leading this instrument, responsible for the overall design, the assay and antibody development, detector and software.
UK Contact Point: Dr Mark Sims|
Tel: 0116 2523513.
Other UK academic institution involvement Cranfield
GEP
UV-VIS Spectrometer (UVIS)
This instrument measures the UV and Visible spectrum. This is an important measurement for astrobiology, as visible light is required for photosynthesis, but UV can be extremely damaging to biological structures. In addition solar irradiance is a key input parameter for atmospheric modelling and governs the photochemistry of planetary atmospheres. This instrument is lead by the UK
UK Contact Point:
Prof John Zarnecki|, The Open University, Tel: 01908 659599.
Meteorological Package (AEP)
This suite of instrument measures pressure, temperature, wind speed and direction, and sound. Understanding the Martian environment is crucial to understanding Mars' habitability. Furthermore, the near surface environment governs the exchange of heat, dust and water between the planetary surface and atmosphere and is key to unravelling the current atmospheric processes. The UK leads this instrument.
Contact Point:
Prof John Zarnecki|, The Open University, Tel: 01908 659599.
Dr Simon Calcutt| University of Oxford
Seismic System (SEIS)
This instrument will explore the internal structure of Mars. The location, depth and size of seismic activity and stress release on the planet. It will inform us about whether there is seismic activity with the large volcanic regions of Mars, Tharsis and Elysium. It will measure the size of the core of the planet and determine whether it is solid or liquid, and measure the thickness of the crust. It will address questions such as: are there deep marsquakes which would be associated with large scale mantle convection and is there evidence for upwelling beneath Tharsis. The UK would provide the microseismometer element of the system.
UK Contact Point: Dr T Pike|, Imperial College London, Tel: 020 7594 6207.
Magnetometer
Although Mars does not have an active magnetic dynamo, there are highly magnetised regions proving Mars had a dynamo in the past. Magnetic field measurements will provide information on the history of the planet's interior. Furthermore it will yield information about the solar wind interaction with the planet. The UK will provide the software for on-board analysis and event detection.
UK contact point: Professor Steve Schwartz|, Imperial College London, Tel: 020 7594 7660.
