Hall, A.; Dobke, B.; Lisle, M.; Shilton, M.; Allouis, E.; Waugh, L.; Carroll, J.; Doignon, G.; Azkarate, M.; van Winnendael, M.; Duvet, L.; Martin, D.; Delfa, J.; Vago, J.; Schwenzer, S. P.; Balme, M.; Fawdon, P.; Turner, S.; Bedford, C.; Sargeant, H.; Pegg, D.; Mirino, M.; Barrett, T.; Ladegaard, A.; Rull, F.; Veneranda, M.; Bontognali, T.; Josset, T.; Josset, J.-L.; Josset, M.; Ciarletti, V.; Plettemeier, D.; Le Gall, A.; Hervé, Y.; Corbel, C.; Vieau, A.-J.; Oudart, N. R.; Trainer, V.; Benedix, W.-S.; Hegler, S.; Lopez, G.; Saiz, J.; Preston, L.; Cousins, C.; Allender, E.; Banham, S.; Barnes, R.; Northwood-Smith, G.; Sangwan, K.; Grindrod, P.; Davis, J.; Motaghian, S.; Dickeson, Z.; Boazman, S.; Schroder, C.; Hauber, E.; Schmitz, N.; Parkes-Bowen, A.; Bahir, R.; Barcenilla, R.; Leff, C.; Persud, D.; Coates, A.; Griffiths, A.; Stabbins, R.; Bohacek, E.; Kuhn, N. and Westall, F. (2019). ExoFiT: ExoMars-Like Field Trials – a Mission Simulation. In: 15th Symposium on Advanced Space Technologies in Robotics and Automation, 27-28 May 2019, ESA-ESTEC, Noordwijk, the Netherlands.

Balme, M. R.; Curtis-Rouse, M. C.; Banham, S.; Barnes, D.; Barnes, R.; Bauer, A.; Bedford, C.; Bridges, J.; Butcher, F. E. G.; Caballo, P.; Caldwell, A.; Coates, A.; Cousins, C.; Davis, J.; Dequaire, J.; Edwards, P.; Fawdon, P.; Furuya, K.; Gadd, M.; Get, P.; Griffiths, A.; Grindrod, P. M.; Gunn, M.; Gupta, S.; Hansen, R.; Harris, J. K.; Holt, J.; Huber, B.; Huntly, C.; Hutchinson, I.; Jackson, L.; Kay, S.; Kybert, S.; Lerman, H. N.; McHugh, M.; McMahon, W.; Muller, J.-P.; Paar, G.; Preston, L. J.; Schwenzer, S.; Stabbins, R.; Tao, Y.; Traxler, C; Turner, S.; Tyler, L.; Venn, S.; Walker, H.; Wright, J. and Yeomans, B. (2017). UK Space Agency “Mars Utah Rover Field Investigation 2016” (MURFI 2016): overview of mission, aims and progress. In: 48th Lunar and Planetary Science Conference, 20-24 Mar 2017, Houston.

The 2016 Mars Utah Rover Field Investigation (MURFI) was a Mars rover field trial run by the UK Space Agency in association with the Canadian Space Agency's 2015/2016 Mars Sample Return Analogue Deployment mission. MURFI had over 50 participants from 15 different institutions around the UK and abroad. The objectives of MURFI were to develop experience and leadership within the UK in running future rover field trials; to prepare the UK planetary community for involvement in the European Space Agency/Roscosmos ExoMars 2020 rover mission; and to assess how ExoMars operations may differ from previous rover missions. Hence, the wider MURFI trial included a ten-day (or ten-'sol') ExoMars rover-like simulation. This comprised an operations team and control centre in the UK, and a rover platform in Utah, equipped with instruments to emulate the ExoMars rovers remote sensing and analytical suite. The operations team operated in 'blind mode', where the only available data came from the rover instruments, and daily tactical planning was performed under strict time constraints to simulate real communications windows. The designated science goal of the MURFI ExoMars rover-like simulation was to locate in-situ bedrock, at a site suitable for sub-surface coresampling, in order to detect signs of ancient life. Prior to "landing", the only information available to the operations team was Mars-equivalent satellite remote sensing data, which were used for both geologic and hazard (e.g., slopes, loose soil) characterisation of the area. During each sol of the mission, the operations team sent driving instructions and imaging/analysis targeting commands, which were then enacted by the field team and rover-controllers in Utah. During the ten-sol mission, the rover drove over 100 m and obtained hundreds of images and supporting observations, allowing the operations team to build up geologic hypotheses for the local area and select possible drilling locations. On sol 9, the team obtained a subsurface core sample that was then analyzed by the Raman spectrometer. Following the conclusion of the ExoMars-like component of MURFI, the operations and field team came together to evaluate the successes and failures of the mission, and discuss lessons learnt for ExoMars rover and future field trials. Key outcomes relevant to ExoMars rover included a key recognition of the importance of field trials for (i) understanding how to operate the ExoMars rover instruments as a suite, (ii) building an operations planning team that can work well together under strict time-limited pressure, (iii) developing new processes and workflows relevant to the ExoMars rover, (iv) understanding the limits and benefits of satellite mapping and (v) practicing efficient geological interpretation of outcrops and landscapes from rover-based data, by comparing the outcomes of the simulated mission with post-trial, in-situ field observations. In addition, MURFI was perceived by all who participated as a vital learning experience, especially for early and mid-career members of the team, and also demonstrated the UK capability of implementing a large rover field trial. The lessons learnt from MURFI are therefore relevant both to ExoMars rover, and to future rover field trials.

Balme, M. R.; Curtis-Rouse, M. C.; Banham, S.; Barnes, D.; Barnes, R.; Bauer, A.; Bedford, C.; Bridges, J.; Butcher, F. E. G.; Caballo, P.; Caldwell, A.; Coates, A.; Cousins, C.; Davis, J.; Dequaire, J.; Edwards, P.; Fawdon, P.; Furuya, K.; Gadd, M.; Get, P.; Griffiths, A.; Grindrod, P. M.; Gunn, M.; Gupta, S.; Hansen, R.; Harris, J. K.; Holt, J.; Huber, B.; Huntly, C.; Hutchinson, I.; Jackson, L.; Kay, S.; Kybert, S.; Lerman, H. N.; McHugh, M.; McMahon, W.; Muller, J.-P.; Paar, G.; Preston, L. J.; Schwenzer, S.; Stabbins, R.; Tao, Y.; Traxler, C; Turner, S.; Tyler, L.; Venn, S.; Walker, H.; Wright, J. and Yeomans, B. (2017). UK Space Agency “Mars Utah Rover Field Investigation 2016” (MURFI 2016): overview of mission, aims and progress. In: 48th Lunar and Planetary Science Conference, 20-24 Mar 2017, Houston.

Emplacement of four or more kinetic penetrators geographically distributed over the lunar surface can enable a broad range of scientific exploration objectives of high priority and provide significant synergy with planned orbital missions. Whilst past landed missions achieved a great deal, they have not included a far-side lander, or investigation of the lunar interior apart from a very small area on the near side. Though the LCROSS mission detected water from a permanently shadowed polar crater, there remains in-situ confirmation, knowledge of concentration levels, and detailed identification of potential organic chemistry of astrobiology interest. The planned investigations will also address issues relating to the origin and evolution of the Earth–Moon system and other Solar System planetary bodies. Manned missions would be enhanced with use of water as a potential in-situ resource; knowledge of potential risks from damaging surface Moonquakes, and exploitation of lunar regolith for radiation shielding. LunarNet is an evolution of the 2007 LunarEX proposal to ESA (European Space Agency) which draws on recent significant advances in mission definition and feasibility. In particular, the successful Pendine full-scale impact trials have proved impact survivability for many of the key technology items, and a penetrator system study has greatly improved the definition of descent systems, detailed penetrator designs, and required resources. LunarNet is hereby proposed as an exciting stand-alone mission, though is also well suited in whole or in-part to contribute to the jigsaw of upcoming lunar missions, including that of a significant element to the ILN (International Lunar Network).

Scientific objectives R. Jaumann1, 2, A. Coates3, E. Hauber1, H. Hoffmann1, N. Schmitz1, L. Le Deit1, D. Tirsch1, G. Paar3, A. Griffiths3, and the PanCam Team 1Institute of Planetary Research, German Aerospace Center (DLR), Rutherfordstr. 2, Berlin, Germany. 2Institute for Geological Sciences, Free University Berlin, Germany. 3Mullard Space Science Laboratory, Univ. College London, UK. mail to: ralf.jaumann@dlr.de

Analysis. R. Li, W. Wang, M. Tang, P. Tang, A. Coates, J. P. Muller, A. Griffiths, G. Paar, and J. Oberst. Mapping and GIS Laboratory, CEEGS, The Ohio State University, 470 Hitchcock Hall, 2070 Neil Avenue, Columbus, OH 43210-1275, li.282@osu,edu, Mullard Space Science Laboratory, Department of Space and Climate Physics, University College London, London, UK, Institute of Digital Image Processing, Joanneum Research, Graz, Austria 8010, Institute of Planetary Research, German Aerospace Center (DLR), Berlin, Germany.

Introduction: While the surface missions to the Moon of the 1960s and 1970s achieved a great deal, scientifically a great deal was also left unresolved. The recent plethora of lunar missions (flown or proposed) reflects resurgence in interest in the Moon, not only in its own right, but also as a record of the formation of the Earth-Moon System and the interplanetary environment at 1 AU. Results from orbiter missions have indicated the possible presense of ice within permanently shaded craters at the lunar poles [1] – a situation that, if confirmed, will have profound impacts on lunar exploration.

Beagle2 is the UK-led lander element on ESA’s Mars Express mission, which will reach Mars in late December 2003. After separation from the Mars Express orbiter 6 days before the atmospheric entry, Beagle2 will descend to the Martian surface by means of ablative heat shields and parachutes. The impact will be cushioned by a set of airbags. The selected landing site at 11.6 deg N / 90.75 deg E (IAU 2000 coordinates) is situated in the south-east of the center of Isidis Planitia, a sedimentary basin which is expected to meet the requirements of Beagle’s scientific mission, the lander operations, and the entry, descent and landing systems. The exact determination of the Beagle2 landing site is important not only for the Beagle2 and MEX orbiter science investigations, but also for the reconstruction of Beagle’s entry and descent trajectory. A precise determination of the Beagle2 position is not possible via the MELACOM radio link. Instead, a novel method based on celestial navigation is employed, which utilizes the Stereo Camera System on the lander for imaging the Martian night sky. The position data is then refined by comparing the landing site panorama images with high resolution orbiter images and laser altimeter data. This combination of celestial navigation with image data analysis for precision position determination will be applicable for many future missions as well.

The performance of the PAW instrumentation on the 60kg Beagle 2 lander for ESA’s 2003 Mars Express mission will be described. Beagle 2 will search for organic material on and below the surface of Mars in addition to a study of the inorganic chemistry and mineralogy of the landing site. The lander will utilize acquisition and preparation tools to obtain samples from below the surface, and both under and inside rocks. In situ analysis will include examination of samples with an optical microscope, Mossbauer and fluorescent X-ray spectrometers. Extracted samples will be returned to the lander for analysis, in particular a search for organics and a measurement of their isotopic composition. The PAW experiment performance data will be described along with the status of the project.

The instrumentation on the 60 kg Beagle 2 lander for ESA's 2003 Mars Express mission will be described. Beagle 2 will be search for organic material on and below the surface of Mars in addition to a study of the inorganic chemistry and mineralogy of the landing site. The lander will utilize acquisitions and preparation tools to obtain samples from below the surface, and both under and inside rocks. In situ analysis will include examination of samples with an optical microscope, Mossbauer and fluorescent X-ray spectrometers. Extracted samples will be returned to the lander for analysis, in particular a search for organics and a measurement of their isotopic composition. The experiment configuration and design will be described along with the status of the project.