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These are planetary missions which will be contributing to during the coming years.
ExoMars is a joint endeavour between the European Space Agency and Russia's Roscomos agency, and consists of a 2016 Trace Gas Orbiter and Schiaparelli lander, and the 2018 Rover. MSSL is leading the PanCam team to provide the rover's scientific cameras.
ExoMars 2018 Mission Science objectives
The overall goals of the ExoMars 2018 rover are to search for signs of past and present life on Mars, and to characterise the water/geochemical environment as a function of depth in the shallow subsurface. The key new aspect of the mission as a whole is the retrieval and analysis of samples from up to 2m under the oxidised surface of Mars. The strategy of the mission is:
1. To land at, or to be able to reach, a location possessing high exobiological interest for past or present life signatures, i.e., the Rover must have access to the appropriate geological environment.
2. To collect scientific samples from different sites, using a rover carrying a drill capable of reaching well into the subsurface and into surface rocky outcrops.
3. At each site, to conduct an integral set of measurements at multiple scales: beginning with a panoramic assessment of the geological environment, progressing to smaller-scale investigations on surface outcrops, and culminating with the collection of well-selected subsurface (or surface) samples to be studied in the Rover's analytical laboratory.
PanCam Science Objectives
The PanCam instrument plays a key role in the mission by contributing to item 3 above. The main objectives of the ExoMars rover PanCam instrument are to:
1. Provide context information for the rover and its environment, including digital elevation models and their proper visualisation.
2. Geologically investigate and map the rover sites including drilling locations.
3. Study the properties of the atmosphere and variable phenomena, including water and dust content of the atmosphere.
4. Locate the landing site and the rover position with respect to local references, by comparison and data fusion with data from orbiters
5. Support rover track planning
6. Image the acquired sample
The PanCam science team has developed a detailed science traceability matrix which links the high level goals to instrument performance.
PanCam plays a key role as part of the lander payload in several ways associated with wide angle and high resolution imaging, as mentioned above. We now consider the hardware implementation and, in broad terms, how the instrument addresses the objectives.
PanCam sets the geological and morphological context for the rest of the payload. Geological and red/green/blue filters provide a powerful camera system for planetary science. A pair of Wide Angle Cameras (WACs) and a close-up High Resolution Camera (HRC) provide complementary imaging at different scales. PanCam can view the lander top surface and verify mechanism deployments and potentially landing pad interaction with the regolith. In the current ExoMars design, PanCam is the only instrument which can remotely sense the geological context of the landing site, provide detailed 3D terrain models and measure the surface Bidirectional Reflectance Distribution Function (BRDF).
The PanCam design for Mars includes the following major items:
(a) Wide Angle Camera (WAC) pair, for multi-spectral stereoscopic panoramic imaging, using a miniaturised filter wheel. The WAC camera units themselves are provided by RUAG and Space-X, Switzerland, and the filter wheels and drives are produced by Mullard Space Science Laboratory, University College London (MSSL-UCL).
(b) High Resolution Camera (HRC) for high resolution colour images. The HRC hardware is produced by Kayser-Threde, Munich and DLR Institute for Planetary Research, Berlin, Germany.
(c) Pancam Interface Unit (PIU) to provide a single electronic interface. The PIU is provided by MSSL-UCL.
(d) PanCam Optical Bench (OB) to house PanCam and provide planetary and dust protection. The OB is provided by MSSL-UCL.
The PanCam mechanical design is illustrated below. The optical bench is located on a rover-supplied pan-tilt mechanism at the top of the rover mast, at a height of ~1.7m above the surface.
PanCam layout (MSSL)
A summary of the main characteristics of the WACs and HRC is shown in Table 1.
Each of the WACs includes 11 filters comprising R,G and B colour bands, a geological filter set (optimised for use on Mars) and atmospheric filters to analyse the water and dust content in the Mars atmosphere. The filter wheel and WAC camera system is illustrated below.
Mechanical configuration of WAC filter wheel and cameras (C.Theobald/MDO, MSSL-UCL)
The HRC includes R, G and B filters bonded to the detector chips to provide colour information. The optical path is housed within the optical bench structure and comprises a baffle and mirror arrangement, a focus mechanism and a detector with associated readout electronics, shown below.
HRC subsystems : a) exploded view and b) accommodated into an Optical Bench prototype (DLR/KT/MSSL)
The PIU is the main interface between the ExoMars rover and the PanCam subsystems, and uses an FPGA implementation. The final system component is the Optical Bench, which provides a planetary protection barrier to the external environment (including HEPA filters), as well as mechanical positioning of the PanCam components. A view of the prototype is shown in below.
Painted prototype optical bench (MSSL)
In addition to the major four PanCam optical bench mounted components outlined above, three additional hardware components known as the ‘Small items’ are part of the PanCam design to improve the scientific return and provide useful engineering data, namely the PanCam calibration target (PCT), rover inspection mirror (RIM) and fiducial markers (FidMs), both provided by Aberystwyth University.
PanCam arrangement on the rover (schematic). The Optical bench is at the top of the mast, the PCT is at the front of the rover, the FidMs on the top deck and the RIM near the front bogey of the rover.
The PanCam calibration target (PCT) is implemented using coloured glass elements similar to ‘stained glass’ with a shadow post for relief. The calibration target is located on the rover deck. The design accommodates the ISEM calibration target.
PanCam and ISEM Calibration Target (PCT) design – Aberystwyth University
Radiometric and geometric calibration is overseen by MSSL with involvement from Aberystwyth, Joanneum Research and DLR.
In addition to the PanCam hardware components mentioned above, the ExoMars PanCam team includes a 3D vision team which provides key software and calibration support for the PanCam team.
The radiometric and colourimetric data flow and operations scenario as envisaged by the 3D vision team, for 3D vision and for colour image processing is illustrated in the two diagrams below. Some of the procedures have been tested in the field particularly during the Arctic Mars Analogue Svalbard Expeditions (AMASE) expeditions, as discussed in the next section.
Data flow and operations scenario for ExoMars PanCam 3D Vision processing
Data flow scenario for ExoMars PanCam radiometric and colourimetric image processing.
The two WACs each have a field of view of 38.3°. Their images will measure 1024x1024 pixels, and will use a multispectral filter wheel carrying 11 filters per camera. Each pixel will have a field of view of 627 µrad, so objects 2m from the camera will be imaged at a resolution of 1.2mm. The WAC focus will be fixed, at 1.0m-∞.
The HRC has a field of view of 5°, and will also return 1024x1024 pixel images. It uses RGB on chip filters. The 83 µrad/pixel scale corresponds to a resolution of 0.17 mm
at 2m distance. HRC will use a mechanical autofocus, from 0.98m-∞.
A number of ExoMars-related field trials and tests have been performed in the last few years (see Figure 7), including participation in recent Arctic Mars Analogue Svalbard Expeditions (AMASE) 2008-11. For these tests, a representative PanCam simulator was used, provided by Aberystwyth University. This simulator includes representative (though not the final) filter wavelengths from which spectral information may be used to study mineralogy. These campaigns have been used, in combination with teams from other ExoMars instruments, to develop working procedures representative of a mission to Mars, as well as to test instrument performance, develop calibration techniques and pursue scientific investigations of particular areas. These included e.g., the Bockfjord Volcanic Complex (BVC), and the Nordaustlandet/Palander Icecap.
The AUPE PanCam simulator at tests in a Hertfordshire, UK quarry and at the AMASE campaign, Svalbard
Other PanCam ground tests have included ‘blind’ geological identifications performed in the AU Mars analogue facility, tests in a quarry in Hertfordshire with the Astrium UK ‘Bridget’ prototype rover, tests as part of the SAFER campaign, tests in Iceland in 2013 and 2015, tests in Boulby mine and tests with the Raman team in Staffordshire, UK (2015).
PanCam Instrument Team
PI Institute UCL-MSSL (PI Andrew Coates, Project Manager Craig Leff, Instrument Scientist Andrew Griffiths, System Engineering Theo Theodorou and Barry Hancock, Mechanical/thermal engineers Tom Hunt and Jonathan Jones, Planetary protection Alex Rousseau and Vitor Botelho, Product Assurance Alan Spencer)
co-PI (HRC) DLR Berlin (co-PI Ralf Jaumann, lead engineer Nicole Schmitz, industrial contractor OHB (lead Herbert Mosebach)
co-PI (WAC camera module) Space-X Switzerland (lead co-I Jean-Luc Josset)
Industrial contractor WAC camera module RUAG, Zurich (lead Martin Mosberger)
Lead co-I (small items) Aberystwyth University (lead Matt Gunn)
Lead co-I (3D vision) Joanneum Research, Austria (lead Gerhard Paar)
PanCam Science Team
Andrew Coates, Ralf Jaumann, Jean-Luc Josset, Andrew Griffiths, Jörg Albertz, Matt Balme, Jean-Pierre Bibring, John Bridges, Claire Cousins, Ian Crawford, Nadezda Evdokimova, Anna Fedorova, Bernard Foing, François Forget, Vittorio Formisano, Yang Gao, Stephan van Gasselt, Matt Golombek, John Grant, Peter Grindrod, Matt Gunn, Sanjeev Gupta, Ernst Hauber, Harald Hoffmann, Pat Irwin, Geraint Jones, Beda Anton Hofmann, Marie Josset, Ruslan Kuzmin, Mark Leese, Ron Li, Wojciech Markiewicz, Philippe Masson, Diedrich Möhlmann, Stefano Mottola, Peter Muller, Jürgen Oberst, Gordon (‘Oz’) Osinski, Gerhard Paar, Tim Parker, Manish Patel, Derek Pullan, Peter Rueffer, Caroline Smith, Tilman Spohn, Nicole Schmitz, Nick Thomas, Roland Trautner, Frances Westall, Colin Wilson
The Jupiter Icy Moons Explorer (JUICE) is an ambitious European Space Agency mission to Ganymede and the Jupiter system.
JUICE is scheduled to be launched in 2022, and to arrive at Jupiter in
2030. It will then orbit the planet, during which time it will study
Jupiter itself and its magnetosphere, and will encounter the active icy
moon Europa, and Callisto, before entering orbit around Ganymede in
2032. Ganymede is the largest moon in the solar system, and is the only
moon known to possess a global magnetic field.
MSSL is providing hardware for the mission's Particle Environment Package (PEP), led by the Stas Barabash of the Swedish Institute of Space Physics in Kiruna. We also have science co-investigator roles on the spacecraft's J-MAG magnetometer instrument, led by Prof. Michele Dougherty, Imperial College London, and the JANUS camera, led by P. Palumbo of Università degli Studi di Napoli, Italy.
Page last modified on 22 nov 15 22:59