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Paris Observatory, F Patrick Michel MarcoPolo-R Proposal core members Europe Maria Antonietta Barucci LESIA – Paris Observatory, F (Lead Proposer) Patrick Michel Univ. Nice, CNRS, OCA, F (Co-Lead Proposer) Philip A. Bland Imperial College, London, UK Hermann Böhnhardt MPS, Katlenburg-Lindau, D John R. Brucato INAF – Obs. of Arcetri, I Adriano Campo Bagatin Univ. Alicante, E Priscilla Cerroni INAF – IASF, Roma, I Elisabetta Dotto INAF – Obs. of Roma, I Alan Fitzsimmons QUB, Belfast, UK Ian A. Franchi Open Univ., Milton Keynes, UK Simon F. Green Open Univ., Milton Keynes, UK Luisa-M. Lara IAA – CSIC, Granada, E Javier Licandro IAC-CSIC, Tenerife, E Bernard Marty CRPG, Nancy, F Karri Muinonen Univ. Helsinki and FGI, FIN Andres Nathues MPS, Katlenburg-Lindau, D Jürgen Oberst DLR Berlin, D François Robert MNHN, Paris, F Raffaele Saladino Univ. of Tuscia, Viterbo, I Josep M. Trigo-Rodriguez CSIC – IEEC, Barcelona, E Stephan Ulamec DLR RB – MC, Cologne, D USA Andrew Cheng JHU – APL, Maryland (Lead U.S. Collaborator) Lance Benner JPL, California Richard P. Binzel MIT, Massachusetts Andrew Rivkin JHU – APL, Maryland Michael Zolensky NASA/JSC, Texas Science goals of the Marco Polo-R mission To return a sample from a near-Earth asteroid belonging to a primitive class to Earth. According to the Science Requirement Document, the sample must bring from cm to μm particles (few to hundreds, respectively). Total mass of several tens of grams. Key questions of the mission: 1) What were the processes occurring in the primitive Solar System and accompanying planet formation? 2) Do NEAs of primitive classes contain pre-solar material yet unknown in meteoritic samples? 3) What are the nature and the origin of the organics in primitive asteroids and how can they shed light on the origin of molecules necessary for life? 4) What are the physical properties and evolution of the building blocks of terrestrial planets? Do NEAs of primitive classes contain pre-solar material yet unknown in meteoritic samples? What are the physical properties and evolution of the building blocks of terrestrial planets? What are the nature and the origin of the organics in primitive asteroids and how can they shed light on the origin of molecules necessary for life? What were the processes occurring in the primitive Solar System and accompanying planet formation? Scientific objectives of the Marco Polo-R mission Characterize the chemical and physical environments in the early solar nebula Define the processes affecting the gas and the dust in the solar nebula Determine the timescales of solar nebula processes Determine the interstellar grain inventory Determine the stellar environment in which the grains formed Define the interstellar processes that created and formed the grains Determine the diversity and complexity of organic species in a primitive asteroid Understand the origin of organic species Provide insight into the role of organics in life formation Determine the global physical properties of a NEA Determine the physical processes and their chronology that shaped the surface structure Characterize the chemical processes that shaped the NEA composition (e.g. volatiles, water) Link the obtained characterization to meteorites and Interstellar Dust Particles (IDPs) and provide ground truth to the astronomical database What were the processes occurring in the primitive Solar System and accompanying planet formation? Do primitive class objects contain presolar What are the physical properties and evolution material yet unknown in meteoritic samples? of the building blocks of terrestrial planets? What are the nature and the origin of the organics in primitive asteroids and how can they shed light on the origin of molecules necessary for life ? Composition of primitive material Variation of composition with geological context Affect of space weathering and Interior collisions on NEA composition Elemental/Isotopic Nature of Mass, gravity Mineralogy Surface composition organics morphology density Laboratory study of returned sample Measurements at NEA • http://www.oca.eu/MarcoPolo-R/ European Community Supporters: – 564 scientists, 25 countries Marco Polo-R is an ESA-led mission with NASA participation. Official confirmation of NASA support: 1. Letter from the Director of Planetary Science Division of NASA on Sept. 19th 2011. 2. Interest reassured during the 2011 EPSC-DPS Joint meeting by Jim Green on behalf of NASA. MarcoPolo-R mission baseline 1996FG3 binary 1996FG3 Primary Secondary to primary Primary diameter: 1.4±0.2 km • diameter ratio: 0.28±0.02 km Primary geometric albedo: 0.035 • orbital semimajor axis: 3.1±0.5 km Primary spin period: 3.595±0.002 hrs • orbital eccentricity: 0.1±0.1 -3 Primary density: 1.4±0.3 g.cm • orbital period around p.: 16.14±0.01h Primary taxonomic type: C Advantages of a binary target The presence of a satellite of the target asteroid will allow us to know the mass of the primary Precise measurements of the mutual orbit and rotation state of both components can be used to probe higher-level harmonics of the gravitational potential, and therefore internal structure. A unique opportunity is offered to study the dynamical evolution driven by the YORP/Yarkovsky thermal effects. 1999 KW4 Possible migration of regolith on the (image Radar primary from poles to equator revealing fresh (previously subsurface) material on - maximize the scientific return of the mis the pole (good candidate site for - offer advantages for orbiter dynamics. unaltered sample collection) Onepossiblescenario Characterization before sampling: – Get the global/local context information. – Select safe and scientifically rewarding sites. Descent/sampling: 1m – Rehearsals, 3 sampling attempts. Courtesy of JAXA – Dedicated landing/touchdown system to ensure safe attitude during sampling operations. – Capability to cope with hazards up to 50 cm scale. – Safe sampling area & high landing accuracy (~ 3-5 m). – Fast “volumetric/mechanical” sampling and transfer technique (minutes). • Suitable and reliable to collect “up to tens of grams” given the considered soil properties • Verification technique as a “must”, backup methods to be investigated • Lowest development risk in Europe to achieve TRL 5 High-speed Earth re-entry: – Capsule design builds on existing architecture. Test with BWS (Brush Wheel Sampler) (APL-JPL- NASA) The BWS has been designed and tested to collect the sample (0.350-2.1 kg) in <1 sec ESA review: risk items (Nov. 2009) GNC development beyond ESA’s state-of-the-art: potential schedule driver + performance uncertainty – Landing accuracy can be relaxed to ~ tens of metres ~ 500 m Itokawa slope map Blue: Safe areas Red: Hazardous areas Close-up of Itokawa surface, Credit: JAXA Further consolidation of sample soil properties Higher risk associated to touch & go, early selection of short-term landing recommended NONO MAJORMAJOR RISKSRISKS ESA-led mission 2 coPolo-R at ESA and towards the scientific communit Study Manager – David Agnolon (ESA - Advanced Studies and Technology Preparation Division) Study Scientist – Detlef Koschny (ESA - Solar System Missions Division) Study Payload Manager – Jens Romstedt (ESA - Advanced Studies and Technology Preparation Division) Science Study Team (SST): • A. Barucci (F), J. Brucato (I), H. Böhnhardt (D), E. Dotto (I), P. Ehrenfreund (NL), I. Franchi (UK), S. Green (UK), L. M. Lara (E), B. Marty (F), P. Michel (F) Tasks of the SST: • To advise and to monitor the study from a scientific point of view Schedule Class M Missions: up to ca. 470 MEuro Advisory structure Selection of 4 missions 2011 ESA-internal studies in Concurrent Design Facility 2012 Industrial studies (2 competing for each mission) Final presentation; selection of two missions for 2013 definition study 2013 - 2015 Detailed definition study; selection of one mission 2015 - 2020 Implementation phase in industry, launch 2020 - 2022 MarcoPolo-R – current activities – Science Study Team was nominated in Apr 2011, first meeting 18/19 May 2011. – Science Study Team has just finished the Science Requirements Document (SciRD). – Internal mission analysis and proximity operations has started. – Concurrent Design Facility study is started on October 4, 2011. – Science Study Team will be informed about the outcome of the CDF on Nov. 8, 2011. Near future schedule A DOI (Declaration Of Interest) call for P/L related studies will be release – ESA Call for proposals 8th November 2011 – Submission deadline 6th January 2012 – Kick-off studies week 4 2012 – End of study spring 2013 non-member state contribution will be handled by ESA HQ Marco Polo-R baseline payload To fulfill the scientific requirements, the SciRD has identified th following payload on board the orbiter: Optical imaging system Visible and near-IR spectroscopy Mid-IR spectroscopy Neutral particle analysis Optional: Laser altimeter Penetrating radar Lander and touch down mechanism And in addition, the Sampling mechanism and the re-entry capsule. Technical goals of Marco Polo-R emonstrate: innovative capabilities such as: high-speed Earth re ntry capsule, sample collection, transfer and containment chniques, accurate planetary navigation and landing as well as mple return operational chain repare the next generation of curation and laboratory facilities f xtraterrestrial sample storage and analysis ave the way as pathfinder mission for future sample returns fro gh surface gravity bodies. Marco Polo-R Camera System Camera System In the current Science Requirement Document, a camera system is considered as one
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