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 es and evolution of the building m particles (few to hundreds, respectively).
μ Key questions of the mission: blocks of terrestrial planets? 1) What were the processes occurring in 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 origin of organics in primitive asteroids and how can they shed light on the origin of molecules necessary for life? 4) What are the physical properti To return a sample fromprimitive a near-Earth class asteroid to belonging Earth. to a According to the Science Requirementbring Document, the sample from must cm to Total massTotal of several tens of grams.
Science goals of the Marco Polo-R mission 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? st Particles (IDPs) ites and Interstellar Du aped the NEA composition (e.g. volatiles, r chronology that shaped the surface organic species in a primitive asteroid environments in the early solar nebula as and the dust in solar nebula at created and formed the grains the astronomical database the astronomical Characterize the chemical and physical Characterize the chemical Define the processes affecting g of solar nebula processes Determine the timescales Determine the interstellar grain inventory Determine the stellar environment in which the grains formed Define the interstellar processes th and provide ground truth to Determine the diversity and complexity of 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 thei structure processes that sh Characterize the chemical water) Link the obtained characterization to meteor Scientific objectives of the Marco Polo-R mission 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. 1996FG3 binary
MarcoPolo-R mission baseline 0.01h ± 0.5 km ± 0.1 ± 0.02 km ± diameter ratio: 0.28 orbital semimajor 3.1 axis: orbital eccentricity: 0.1 orbital period around p.: 16.14 Secondary to primary • • • • -3 0.2 km 0.3 g.cm ± ± 0.002 hrs ± Primary Primary diameter: 1.4 Primary density: 1.4 Primary taxonomic type: C Primary geometric albedo: 0.035 Primary spin period: 3.595 1996FG3 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) 1m Courtesy of JAXA of Courtesy the considered soil soil the considered ensure safe attitude during sampling tens of grams” given properties • technique as a “must”, backup methods to be investigated Verification • 5 TRL to achieve in Europe risk Lowest development • and reliable to collect “up Suitable operations. – the global/local context information. Get – rewarding sites. safe and scientifically Select – 3 sampling attempts. Rehearsals, – Dedicated landing/touchdown system to – with hazards up to 50 cm scale. to cope Capability – sampling area & high landing accuracy (~ 3-5 m). Safe – Fast “volumetric/mechanical” sampling and transfer technique (minutes). – design builds on existing architecture. Capsule Characterization before sampling: Characterization Descent/sampling: High-speed Earth re-entry:
Onepossiblescenario 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 : Safe areas : Safe Blue : Hazardous areas Red ~ 500 m ~ 500
(Nov. 2009) (Nov. Itokawa map slope go, early selection of short-term laxed to ~ tens of metres JAXA Credit:
Close-up of Itokawa NO MAJOR RISKS
surface, NO MAJOR RISKS – Landing accuracy can be re landing recommended GNC development beyond ESA’s state-of-the-art: potential schedule driver + performance uncertainty Further consolidation of sample soil properties Higher risk associated to touch & ESA review: risk items ESA-led mission 2 it y Division) Ehrenfreund (NL), I. Franchi (UK), S. Green (UK), L. M. Lara (E), B. Mart Division) -R at ESA and towards the scientific commun (F), P. Michel (F) To advise and to monitor the study from a scientific point of view o – Jens Romstedt (ESA - Advanced Studies and Technology Preparation • A. Barucci (F), J. Brucato H. Böhnhardt (I), (D), E. Dotto (I), P. – David Agnolon - (ESA Advanced Studies and Technology Preparation – Detlef Koschny (ESA - Solar System Missions Division) • Study Payload Manager Science Study Team (SST): Study Manager Study Scientist Tasks of the SST: Tasks
Pol co Class M Missions: up to ca. 470 MEuro 470 ca. to Missions: up Class M Selection of 4 missions Selection ESA-internal studies in Concurrent Design Facility Concurrent studies in ESA-internal for each mission) Industrial studies (2 competing Final presentation; selection of two missions for definition study Detailed definition study; selection of one mission Implementation phase in industry, launch 2020 - 2022 2011 2012 2013 Advisory structure 2013 - 2015 2015 - 2020
Schedule meeting 18/19 May 2011. meeting Requirements Document (SciRD). started. 2011. the CDF on Nov. 8, 2011. MarcoPolo-R – current activities – Science Study Team was nominated in Apr 2011, first – Science Study Team has just finished the Science – mission analysis and proximity operations has Internal – Design Facility study is started on October 4, Concurrent – Science Study Team will be informed about the outcome of related November 2011 January 2012 th th DOI (Declaration Of Interest) call for P/L – Call for proposals ESA – Submission deadline– 8 studies Kick-off – of study End 6 4 2012 week spring 2013 A studies will be release non-member state contribution will be handled by ESA HQ Near future schedule ry
Sampling mechanism and the re-ent payload on board the orbiter: g Laser altimeter Penetrating radar Lander and touch down mechanism Optical imaging system Visible and near-IR spectroscopy Mid-IR spectroscopy Neutral particle analysis
Marco Polo-R baseline payload ptional: nd in addition, the o fulfill the scientific requirements, the SciRD has identified th apsule. ollowin
T f O A c 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 ny, Finland, France, Italy, USA, m) μ to characterise the asteroid and the sampling site1.- at globally three (resolution scales: in the order of2.- dm) locally (resolution the order in of3.- mm) its in context (hundred The interest on this instrumentfrom (and therefore, the science the data acquired to by the cameras) is retrieved be large, notthanks only to in Spain the OSIRIS heritage (IAA fromAlicante, etc), but Rosetta also Mission, IAC, University world of wide (Germa UK, etc). A camera system is the “eyes” ofscientific the mission phase. during (cruise the and) In the current Science Requirement Document, a camera systemconsidered is as one of payload the elements. The scientific objectives of this camera system are: Camera System on the electronics such that mass a Wide Angle Camera + Close-up a Narrow Angle Camera The proposal will benefit fromin August the previous 2009 (as the result Study of Report the previous submittedone selection to of of ESA M-class the Marco Polo as missions) Improvements in the current version ofthe opticalCamera System MP-R the design rely of on WAC+CuC the and is saved and resources are shared among 3 cameras. the To this call ofSpain+Germany+Finland) will DoI respond studies proposing for a camera system related p/l principle) led (in studies, we Spain. by (i.e. This camera system is composed of: Marco Polo-R Camera System . m). This challenge is μ instrument cannot continue, the others will have to assume that. – mission The (i.e. ESA) will not– the camera system. descope If one of the countries in the Consortium responsible for the already partially overcome WAC+CuC as designed have as one been single camera. Risks if there is descoping: Technologically, the (low risk) challenge is the in optical design to fulfillfocusing the scientific range objectives is as long needed (dm to If a committment as PI is acquiredcamera system to to provide the Marco Polo-R mission, I do not the see a “descoping” how scenario can be contemplated
MP-R Camera System during this for Phase A. no cost of the cameras. We have (as stated and justified the in data processing and archiving PCM is 0.0€ represent 60000€ , IAA would need economical support for : Phase A mechanics • detectors, DPU and low Germany: level control s/w • high-level Finland: software, • PCM, frame Spain: housing and of and opto- electronics, the opto-mechanical design Germany, Finland and Spain have agreedConsortium. A kick-off to meeting has not form taken a place yet (awaiting outcome of this meeting hereResponsibilities at MICINN). For this the estimated cost a of Acción Complementaria submitted to in July MICINN 2011). The study for the Frame housing and Phase A study. Marco Polo-R Camera System Extracted from the 2009 Design Study Report :
This cost can be decreased if model philosphy the changes.
–Phase A: 0.0€ –Phase B (STM and EM): 426000€ –Phase C+D (EQM, FM, FS): 1.9M€ – The cost here listed to relates 2STM, 2EM, 2EQM (whose refurbishment will be the FS) and 2FM. Opto-mechanics: 1STM, 1EM, 1EQM (to be refurbished to FS), 1FM. The STM, EM and FM are deliverable to ESA. –Phase A: 60000€ –Phase B (STM and EM): 2.6M€ –Phase C+D (EQM, FM, FS): 10.4M€ PCM, and framing and housing of E-box the
Updates to cost the estimated in 2009