MARCO POLO Near Earth Asteroid Sample Return Mission

Near Earth Asteroid Sample Return MARCO POLO Near Earth Asteroid Sample Return Mission

Science Study Team: M.A. Barucci (F), H. Boehnhardt (D), J.R. Brucato (I), E. Dotto (I), I.A. Franchi (UK), S.F. Green (UK), J.-L. Josset (CH), P. Michel (F), K. Muinonen (FIN), J. Oberst (D), R. Binzel (MIT, USA), M. Yoshikawa, J. Kawaguchi, H. Yano (JSPEC/JAXA, J) ESA study team: D. Koschny, D. Agnolon, J. Romstedt Near Earth Asteroid Sample Return International collaborations:

Community supporters: 658 scientists, 25 countries, and counting

JAXA junior participation (from Hayabusa heritage): • GNC (Guidance, Navigation, and Control): Engineering supports by providing real data from Hayabusa for navigation training Hardware (e.g. LIDAR) From operations: determination of mass, shape, density, etc. • Tracking support (e.g. ranging and telemetry) • Heat shield of the Earth ReEntry Capsule • Outcomes of testing of sampling devices • Science instruments

NASA junior participation: SALMON (Stand Alone Missions of Opportunity): hardware & software components Near Earth Asteroid Sample Return Marco Polo will rendezvous with a primitive NEA: scientifically characterize it at multiple scales, and return a sample to Earth unaffected by the atmospheric entry process or terrestrial contamination.

Marco Polo is the first sample return mission to a primitive low albedo asteroid

Marco Polo will return a sample (10s of grams) for laboratory analyses of organic-rich material

Marco Polo will determine the geological context of the returned sample Near Earth Asteroid Marco Polo addresses a wide range of objectives Sample Return

Stars Stellar nucleosynthesis Nature of stellar condensate grains The Interstellar Medium IS grains, mantles & organics

The protosolar nebula Accretion disk environment, processes and timescales Planetary formation Inner Solar System Disk & planetesimal properties at the time of planet formation Asteroids Accretion history, Life alteration processes, Nature of impact events, organics in NEOs regolith

The Earth Impact hazard Evolution of life on Earth Near Earth Asteroid Sample Return

Animation Near Earth Asteroid Sample Return We need to return samples from space Original material Formation processes Chronology

Ios N A S A

Genesis Apollo & Luna Stardust A pristine sample from a primitive asteroid is required to study the precursors of terrestrial planets Near Earth Asteroid Sample Return

Look different, but common origin Near Earth Asteroid Minor Bodies: Asteroids and Comets Visited So Far Sample Return （（（Not to scale! ））） Steins

Eros 2.7 g/cm 3

Ida & Dactyl Itokawa

Braille Mathilde 1.3 g/cm 3

Annefrank

P/Halley Look different, but common origin. Gaspra Only primitive P/Wild2types retainP/Tempel1 a memory of the origin. P/Borrelly Near Earth Asteroid Sample Return Marco Polo target: dark primitive classes: C, P, D

1.50

E 3103 Eger 100 1.25

1.00 D REFLECTIVITY

80 A=0.53 2.0 S 0.75 0.4 0.6 0.8 1.0 1.2 1.4 1.6 1.8 433 Eros WAVELENGTH (micron) S E 1.5 60 P 1.0 C REFLECTIVITY A=0.25 0.5 2100 RaShalom 0.4 0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.0 40 1.1 C WAVELENGTH (micron)

1.0

0.9 20 M REFLECTIVITY 0.8 A=0.10 B,T 0.4 0.6 0.8 1.0 1.2 1.4 1.6 1.8 WAVELENGTH (micron) 3.0 D 3552 Don Quixote 0 2.5

2.0 PERCENT OF TOTALPOPULATION PERCENT OF

1.5 REFLECTIVITY 2 3 4 5 1.0 A=0.03 0.5 DISTANCE FROM SUN (astronomical units) 0.4 0.6 0.8 1.0 1.2 1.4 1.6 1.8 WAVELENGTH (micron) Near Earth Asteroid NearSample Earth Return Asteroid Sample Return

? D ? C CAIs

Chondrule s Eucrites HED differentiation Differentiation Planetesimal accretion Angrites Pallasites Mesosiderites Planetary Mars Formation Earth Near Earth Asteroid Sample Return Asteroid population Near Earth Asteroids

Mars

Jupiter Near Earth Asteroid More than 6000 known NEOs Sample Return

NEO

SOURCE IEO Fast resonances: Main Belt Asteroids become rapidly NEAs by dynamical transport from a source region (in a few million years)

Mars Venus Earth Earth

Mars Animation showing evolution of asteroidQuickTime™ orbitset un décompresseur codec YUV420 sont requis pour visionner cette image.

Venus

Numerical simulations: Several 1000 particles Near Earth Asteroid Sample Return Why an NEA? NEAs offer many advantages:

• Accessibility

• Identified links to the origin population

Eros

2001SK162 2001SG286 • Great diversity of physical properties 1999JU3 composition 1999UQ Itokawa

NEA Population (H<21) • Hazard mitigation NEAs visited

Marco Polo targets

1999 JU3: C class, 0.92 km Near Earth Asteroid Sample Return Marco Polo will provide crucial elements to answer the following key questions:

1) What were the processes occurring in the primitive solar system and accompanying planet formation?

2) What are the physical properties and evolution of the building blocks of terrestrial planets?

3) Do NEAs of primitive classes contain pre-solar material yet unknown in meteoritic samples?

4) 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? Near Earth Asteroid Sample Return What were the processes occurring in the early solar system and accompanying planet formation? Measurements A. Characterise the chemical and physical Bulk chemistry environments in the early Mineralogy, solar nebula Petrology Isotopic chemistry in inclusions, B. Define the processes matrix, presolar affecting the gas and the grains and dust in the solar nebula volatiles, water

C. Determine the timescales of solar nebula processes Near Earth Asteroid Sample Return What are the physical properties and evolution of the building blocks of terrestrial planets? Measurements D. Determine the global physical properties of an NEA Volume, shape, mass Surface morphology E. Determine the physical and geology processes, and their chronology, Mineralogy & that shaped the surface structure Petrology Isotope F. Characterise the chemical geochemistry & processes that shaped the NEA chronology composition ( e.g. volatiles, water) Weathering effects Thermal properties G. Link the detailed orbital and laboratory characterisation to meteorites and IDPs and provide ground truth for the astronomical database Near Earth Asteroid Sample Return Do NEAs of primitive classes contain presolar material yet unknown in meteoritic samples?

Meteorites contain 1 light yr refractory pre-solar grains from supernovae, H. Determine the novae, AGB stars interstellar grain inventory

I. Determine the stellar environment in which the grains formed Croat et al 2003 J. Define the interstellar processes that have affected the grains

Measurements

Bulk chemistry Grain mineralogy and composition, Isotope chemistry of grains Near Earth Asteroid Sample Return 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? Current exobiological scenarios for the origin of life invoke the exogenous delivery of organic matter to the early Earth

The planets of the inner solar system experienced an intense influx of organicrich material for several hundred million years after they formed. Animation showing transport The earliest evidence for of organics to Earth life on Earth coincides with the decline of this bombardment. Many biologically important molecules are present in the organic materials. Near Earth Asteroid Sample Return 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?

K. Determine the diversity and complexity of organic species Measurements in a primitive asteroid Abundances and L. Understand the origin of distribution of insoluble organic organic species species Soluble organics M. Provide insight into the role Global surface of organics in life formation distribution and identification of organics Near Earth Asteroid From stars to meteorites Sample Return

after Davidson 2009 Near Earth Asteroid From stars to meteorites Sample Return Mantle formation Nucleosynthesis Chemical reaction Condensation Shock Implantation Irradiation

Accretion Thermal/aqueous alteration Impacts Weathering Evaporation Atmospheric entry Condensation Contamination Shock weathering Irradiation after Davidson 2009 Chemical reaction Near Earth Asteroid From stars to meteorites Sample Return Mantle formation Nucleosynthesis Chemical reaction Condensation Shock Implantation Irradiation

Accretion Thermal/aqueous alteration Impacts Weathering Evaporation Atmospheric entry Condensation Contamination Shock Weathering Irradiation after Davidson 2009 Chemical reaction Near Earth Asteroid From stars to meteorites Sample Return Mantle formation Nucleosynthesis Chemical reaction Condensation Shock Implantation Irradiation

Accretion Thermal/aqueous alteration Impacts Weathering Evaporation Condensation Shock Irradiation after Davidson 2009 Chemical reaction Near Earth Asteroid Sample Return

“Why do you need to return samples?” Near Earth Asteroid Sample Return Superior instruments…

“Miranda” GC-IRMS Laboratory Isotope ratio ± 0.01%

Rosetta Ptolemy In situ Isotope ratio ± 1%

In-situ instruments limited (mass/volume/power/reliability) Near Earth Asteroid Sample Return Superior instruments…

Diamond synchrotron source Near Earth Asteroid Sample Return Superior instruments… In-situ measurements provide insufficient precision

Whole-rock measurements 150 Meteorites

100 CI,CM 50 CO,CV,CK

Enstatite 0

N N (‰) Ordinary

15 -50 SNC δ

-100 Basaltic Achondrites Ureilite -150 -40 -30 -20 -10 0 10 20 30 Grady, 2004 δ13 C (‰) Near Earth Asteroid Sample Return

In-situ measurements provide little or no sample discrimination

100 m Courtesy: Kita, U. Wisconsin Near Earth Asteroid Sample Return Complexity… • Same sample analysed by many instruments • Complex sample selection and preparation

Initial selection Process characterisation

Krot Split Example: isotope dating of Isotope dating chondritic components - Dissolution - Purification Context (mm–µm) – check secondary effects - Analysis - Calibration Zega et al 2007

Fehr Near Earth Asteroid Sample Return

“Why do you need to return samples when we have meteorites?” Near Earth Asteroid Sample Return Going beyond meteorites

Re-distributes elements & isotopes, Modifies minerals Accreted & organics material? CM Chondrites CM

Compressive strength Atmospheric Entry Filter?

To survive atmospheric entry requires major processing Near Earth Asteroid Sample Return Presolar grains

Many sources, and stellar environments After Davidson 2009 unpublished

Aqueous Alteration

SiC x l

Silicate xx x Pre-solar Silicate Abundance

nDiamond

Spinel

Davidson 2009 Graphite Near Earth Asteroid Sample Return Aqueous alteration Brearley 2006 Mixed regolith provides range of alteration Free of terrestrial contamination find low alteration materials study alteration process

Water Carbonaceous chondrites exhibit aqueous alteration - How much water was there initially? - What was the fate of the water? - Implications for terrestrial planets.

Is D/H in primitive asteroids similar to that on Earth? Near Earth Asteroid Sample Return Avoid contamination…

Tagish Lake Most perfectly collected sample?

Collected within 5 days from frozen lake and kept at -20°C

terrestrial contamination Terrestrial hydrocarbons … any result obtained for organics in

meteorites may be questioned Abundance

Tagish Lake hydrocarbons Abundance Near Earth Asteroid Sample Return Organics Over 80 ET amino acids

Many different synthesis mechanisms Strecker

Hydrolysis

Ammonia addition

Requires precise abundances of molecules and precursors Near Earth Asteroid Sample Return Context 50 km Marco Polo payload: Structure (shape, density) Collisional history cratering record Geological context Compositional heterogeneity Space weathering 1 km 500 m

Meteorite/NEA spectra/ground truth 10 cm 40 m

Laboratory data: Petrology, composition, chronology

Courtesy: Krot Near Earth Asteroid Sample Return

NEA sample return will use a combination of in situ and laboratory measurements to Returned primitive NEA sample provide a unique window into distant past provideallowing ascientists unique to window unravel mysteries into the surroundin distantg pastbirth and evolution of Solar System allow scientists to unravel mysteries surrounding the birth Legacyand - evolution Retention of ofsamples the solar for future system advances Curation and distribution facility involveLarge community a large community,– range of disciplines in a wide range of disciplines Planetology- direct involvement Astrobiology Nucleosynthesis Cosmochemistry

retain samples for future advances through a Curation and Distribution Facility

demonstrate key capabilities for any sample return mission generate tremendous public interest Near Earth Asteroid Sample Return Mission profile

6 year mission to 1999 JU 3 (17 months at the asteroid) Direct escape, single spacecraft (chemical) + Earth reentry capsule

Launch mass: ~1450 – 1560kg Backup launch

. 1 Total deltaV ~ 1600 m s Dec. 2020 Earth flyby . 1 Dec. 2019 Reentry velocity ~ 12 km s Earth flyby Arrival : EarthSpacecraft: 2.4 AU max. Feb. 2022 Launch : Dec. 2018 SunSpacecraft: 0.85 – 1.55 AU

Asteroid properties Reentry : Dec. 2024 • Diameter ~ 1 km

• Rotation period: 7.7 hours Departure : Jul. 2023 Near Earth Asteroid Sample Return Baseline payload

Wide angle camera Narrow angle camera Closeup camera Vis/NIR imaging spectrometer (0.4–3.3 m) MIR spectrometer (5–25 m) Coloured image of Eros, Credit: NASA Radio science Possible camera Laser altimeter concept, Credit: Neutral particle analyser MPI Complementary instruments/lander possible

Total Development Mass [kg] 30 compatible with Power [W] 90 overall schedule Data volume [Gbit] 280 Near Earth Asteroid Sample Return Descent/Sampling

3 sampling attempt capability Landing/touchdown Clearance: ~ 50 cm hazards Landing accuracy ~ 5 m

Dust to cm-sized fragments Sampling Contamination-avoidance strategy

1 2 5

3 4

Asteroid descent and sampling sequence Near Earth Asteroid Sample Return Descent/Sampling

1. Asteroid characterization 2. Hovering at 200 – 400 m altitude, “go-decision” 3. Autonomous terrain-relative descent • Navigation camera + multi-beam laser/radar altimeter 4. Touchdown/sampling 5. Ascent to safe position

Animation

1 2 5

3 4

Asteroid descent and sampling sequence Example of touchdown operation Near Earth Asteroid Sample Return Descent/Sampling

Sampling option 1: Short-term landing (~ 10 min.), “energy-absorbing” landing legs, down-thrust, rotating corer (sample canister) Sampling option 2: Touch & go (< 3 sec.), “elastic” legs, fast sampler (sample canister)

Rotating corer designs Animation Fast sampler

Example of sampling operation Near Earth Asteroid Sample Return Main spacecraft

Concept 1 : Corer, top-mounted capsule, one articulated arm inside central cylinder Span: 8m Height: ~ 2.5m

Concept 2 : Corer, bottom-mounted capsule, two articulated arms

Concept 3 : Fast sampler, top-mounted capsule, transfer via landing pads/legs + elevator in central cone Near Earth Asteroid Sample Return Earth reentry

Altitude (km) 2 120 1

3 10 0 Stardust capsule recovery operations, Credit: NASA 4 5

1. T 0 – 4 hours: Separation with main spacecraft . -2 2. T 0: Re-entry (heat flux ~ 15 MW m ) 3. T 0 + 200 s: Parachute opening (~ 10 km, subsonic) 4. T 0 + 1800 s: Soft landing in Woomera, Australia 5. Landing + few min/hrs: Search & Recovery Near Earth Asteroid Sample Return Earth reentry capsule

45 o half-cone angle front shield In-development lightweight ablative material or classical carbon phenolic Capsule mass: 25 – 69 kg

Front shield

Antenna

Beacons, batteries

Back shield Parachute

Sample container Near Earth Asteroid Sample Return Development

ProtoFlight Model + dedicated qualification models No specific planetary protection measures required Predevelopment • Sample acquisition, transfer and containment system Navigation camera • Guidance, Navigation & Control (GNC) – descent/sampling Astrium • Further development of ablative material • Low-gravity landing/touchdown system All testing facilities available

Navigation landmarks TAS

High heat flux test of heat shield material, IRS Sampling test results Sampling test results SENER SELEX Galileo Near Earth Asteroid Sample Return ESA review: risk items

GNC development beyond ESA’s stateoftheart: 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 Closeup of Itokawa surface, Credit: JAXA Further consolidation of sample soil properties Higher risk associated to touch & go, early selection of shortterm landing recommended Near Earth Asteroid Conclusions Sample Return

Technically feasible mission

Contractor 1 Contractor 2 Contractor 3 Total dry mass 745 744 812 Launch mass 1448 1462 1557 Launch vehicle performance 1629 1719 1629 Launch mass margins (%) 11 15 4 Marco Polo spacecraft mass budget (kg) Maximal use of ongoing/past activities allows an effective and robust development plan Safe landing/touchdown (including “relaxed” GNC) Sample collection, transfer and sealing Earth re-entry High heritage and no predevelopment needed for: Mission and science operations “Standard” platform equipment (e.g. power, thermal, propulsion)