EE XX OO MM AA RR SS

POCKOCMOC POCKOCMOC

Search for Life on Mars

Jorge L. Vago, F. Westall, F. Goesmann, F. Raulin, W. Brinckerhoff, H. Steininger, W. Goetz, C. Szopa, GeoPlanet Visit D. Loizeau, E. Sefton-Nash, H. Svedhem, D. Rodionov, ExoMars science working team and project team 9 January 2018, ESTEC (NL) 1 Early Terrestrial Planet Evolution EE XX OO MM AA RR SS

2 Early Terrestrial Planet Evolution EE XX OO MM AA RR SS

3 Early Terrestrial Planet Evolution EE XX OO MM AA RR SS

4 Early Terrestrial Planet Evolution EE XX OO MM AA RR SS

5 Early Terrestrial Planet Evolution EE XX OO MM AA RR SS

6 Early Terrestrial Planet Evolution EE XX OO MM AA RR SS

7 Early Terrestrial Planet Evolution EE XX OO MM AA RR SS

8 Early Terrestrial Planet Evolution EE XX OO MM AA RR SS

9 Early Earth EE XX OO MM AA RR SS

Start of conditions compatible with life 4.1 3.7 Pre-Noachian Noachian Hesperian Mars Subaerial environment

Standing bodies of water

Early heavy Late heavy bombardment bombardment Magma ocean Hydrothermal environment Earth atmosphere Supercritical Hadean Archaean Ga 4.568 4.4 3.9 3.5

Beginning of terrestrial Oldest preserved planetary accretion traces of life

10 Credit: Kasei Valles, MEX/HRSC Early Mars EE XX OO MM AA RR SS

Start of conditions Surface conditions compatible with life become less habitable 4.1 3.7 Pre-Noachian Noachian Hesperian Mars Subaerial environment

Standing bodies of water

Early heavy Late heavy bombardment bombardment Magma ocean Hydrothermal environment Earth atmosphere Supercritical Hadean Archaean Ga 4.568 4.4 3.9 3.5

Beginning of terrestrial Oldest preserved planetary accretion traces of life

11 Credit: Kasei Valles, MEX/HRSC Early Crust EE XX OO MM AA RR SS

Early Earth and Mars hosted numerous reducing, nutrient-rich, hydrothermal submarine environments with conditions that would have allowed hosting life.

Desirable attributes: ‣ Low-energy water environments ‣ Settings known to preserve biosignatures ‣ Aqueous mineral variety

12 Credit: Champagne vent white smoker, NOAA Why Life on Mars ? EE XX OO MM AA RR SS

‣ Many processes considered important for the origin of life on Earth were also active on young Mars;

‣ Early in the history of Mars, liquid water was present on its surface;

‣ The absence of plate tectonics on Mars means we can study rocks from the period when life appeared on our planet.

13 Credit: NASA/MGS Potential to Host Life EE XX OO MM AA RR SS

HH AA BB II TT AA BB II LL II TT YY

14 Potential to Detect Life EE XX OO MM AA RR SS

PP RR EE SS EE RR VV AA TT II OO NN

15 Credit: Cape Verde, Opportunity 2020 Mission Objectives EE XX OO MM AA RR SS

SCIENTIFIC OBJECTIVES ‣ To search for signs of past and present life on Mars; 2020 ‣ To investigate the water/subsurface environment as a function of depth.

TECHNOLOGY OBJECTIVES ‣ Surface mobility with a rover (having several kilometres range); ‣ Access to the subsurface to collect samples (with a drill, down to 2-m depth); ‣ Sample acquisition, preparation, distribution, and analysis.

‣ To characterise the surface environment.

‣ Throttleable braking engines for planetary landing. ‣ Russian deep-space communications stations working in combination with ESA’s ESTRACK.

16 Credit: Mamers Valles, MEX/HRSC Launch EE XX OO MM AA RR SS

Launch date: 24 Jul – 13 Aug 2020 Mars Arrival: 19 Mar 2021 Landing Site: TBD, –2 km MOLA Ellipse: 120 km x 20 km

4000

17 Credit: Mamers Valles, MEX/HRSC Carrier and Descent Module EE XX OO MM AA RR SS

18 Credit: Mamers Valles, MEX/HRSC Entry, Descent, and Landing EE XX OO MM AA RR SS

19 Credit: Mamers Valles, MEX/HRSC Descent Module EE XX OO MM AA RR SS

20˚ max 3.127 m

20 Credit: Mamers Valles, MEX/HRSC Surface Platform EE XX OO MM AA RR SS

PK Dust properties and Dust suite E field monitoring

FAST Trace gases IR Fourier spectrometerT and aerosol monitoring

RAT-M Surface and atmospheric Microwave radiometer T monitoring

ADRON-EM Subsurface water content Neutron detector Radiation dosimetry

MAIGRET Magnetic field Magnetometer measurements

MGAK Atmospheric GCMS Analysis

SEM Internal Mars structure Seismometer investigations

BIP Commands instruments M-DLS Atmospheric chemical and Science interface computer Collects data Diode laser spectrometer isotopic composition

TSPP-EM Color surface panoramas LaRa Radio science for internal Multi camera system Atmospheric dynamics Coherent transponder structure investigations

MTK T, P, wind, humidity, HABIT T, UV dose, humidity, Meteorological suite optical opacity Habitability studies salt deliquescence 21 Mobility + Subsurface Access EE XX OO MM AA RR SS

Nominal mission : 218 sols Nominal science : 6 Experiment Cycles + 2 Vertical Surveys EC length : 16–20 sols Rover mass : 300-kg class Mobility range : Several km

DRILLING TO REACH SAMPLING DEPTH DRILL UPLIFT CENTRAL PISTON IN CORE CUTTING SAMPLE UPPPER POSITION (closing shutter) DISCHARGE CORE FORMING

UV light

Oxidants 1 2 3 4 5 6

Ionising Radiation

Credit: ESA/Medialab 2-m depth 22 Credit: Argyre, MEX/HRSC Mobility + Subsurface Access EE XX OO MM AA RR SS

23 Integration of Service Module EE XX OO MM AA RR SS

24 Site Characterisation EE XX OO MM AA RR SS

WAC HRC WAC To establish the geological context ⇩ ⇩ ⇩ AT PANORAMIC SCALE: Two Wide Angle Cameras (WAC): Colour, stereo, 35° FOV; One High-Resolution Camera (HRC): Colour, 5° FOV One IR spectrometer (ISEM): 1° FOV.

ISEM ⇨ HRC ◉ ◉ ◉ ISEM

WAC

Neutron Detector AT DEPTH: To study the stratigraphy for drilling

0 0 Aeolian deposits

Ground Penetrating Radar Sedimentary filling (m) (ns) ~3-m penetration, with ~2-cm resolution (depends on subsurface EM properties)

10 100 0 Distance (m) 30 25 Heggy et al. 2007 Outcrop Characterisation EE XX OO MM AA RR SS

AT ROCK SCALE: To ascertain the past presence of water For a more detailed morphological examination

High-Resolution Camera Close-Up Imager Colour, 20–100-µm/pixel resolution, 19° FOV, Focusing range: 10 cm to ∞

Next step: ANALYSIS From an outcrop Use the drill to collect a sample From the subsurface

26 Close-Up Imager EE XX OO MM AA RR SS

Drill 10 cm

40 µm/px 7 cm CLUPI 21 cm @ 0.5 m 80 µm/px 14 cm

Wheel @ 1.0 m

Front imaging of outcrops, rocks, soils Image collected samples Mirror 1 CLUPI Mirror 2 CLUPI

FOV 2 FOV 3 FOV 1 Collected core

FOV 2 FOV 1 1768 FOV 3

Side imaging Image drilling area 640 1128 2652 pixels 2652 pixels Credit: Space Exploration Institute 27 Subsurface Drill EE XX OO MM AA RR SS

OBTAIN SAMPLES FOR ANALYSIS: From 0 down to 2-m depth

Subsurface drill includes a miniaturised IR spectrometer for borehole investigations.

28 Subsurface Drill EE XX OO MM AA RR SS

29 Sample Delivery EE XX OO MM AA RR SS

DRILL discharges sample into Core Sample Transport Mechanism (CSTM). PanCam HRC and CLUPI image the sample. Sample is delivered to Analytical Laboratory Drawer (ALD) —15 min.

30 Analytical Laboratory Drawer EE XX OO MM AA RR SS

31 Credit: TAS-I Analytical Laboratory Drawer EE XX OO MM AA RR SS

Ultra Clean Zone (UCZ)

32 Credit: TAS-I Analytical Laboratory Drawer EE XX OO MM AA RR SS

Ultra Clean Zone (UCZ)

33 Credit: TAS-I Analytical Laboratory Drawer EE XX OO MM AA RR SS

Blank Dispenser

Core Sample Transfer Mechanism (CSTM)

Alternative Transport Container (AC)

Carrousel with MOMA ovens Crushing Station (CS) and Refillable Container (RC)

Dosing Stations (DS)

Flattening Device

34 Credit: TAS-I Analytical Laboratory Drawer EE XX OO MM AA RR SS

35 Rock Crushing Station EE XX OO MM AA RR SS

36 Credit: OHB Powder Sample Dosing EE XX OO MM AA RR SS

37 Credit: OHB Sample Analysis EE XX OO MM AA RR SS

Use mineralogical + image information from μΩ Imaging VIS + IR spectrometer: 256 x 256 pixels, 20 µm/pixel resolution, to identify targets for Raman and MOMA-LDMS. 0.95–3.65 µm spectral range, 320 steps

Rock Crusher Sample

Powder

1) Survey 2) Detailed Analysis

Identify µΩ IR Targets • Gypsum • Kieserite • Jarosite Mineralogy Raman

MOMA

MOMA LDSM Detailed LDMS Survey & Pyr-Der GCMS μΩ = 20 μm Organics Raman = 50 μm LDMS = 400 μm

Raman: Spectral shift range 200–3800 cm–1 LDMS = Laser Desorption Mass Spectrometry Spectral resolution: 6 cm–1 GCMS = Gas Chromatograph Mass Spectrometer 38 Characterisation of Organic Molecules EE XX OO MM AA RR SS

Life Distribution

MOMA Organics Abundance Cosmic Distribution

Molecule Size

Broad identification range (50–1000 Da), including distribution, and chirality. High sensitivity (≤ 1 pmol/mol in TV-CGMS, ≤ 1 pmol/mol/mm2 in LDMS). Resolution ≤ 1 Da over 50–500 Da range, ≤ 2 Da thereafter. Ability to perform MS-MS analysis on trapped fragments. LDMS mode appears not to be disturbed by perchlorates.

39 Credit: Mamers Valles, MEX/HRSC ExoMars Biosignature Score EE XX OO MM AA RR SS

Morphological biosignatures: Σ points Multilayer organosedimentary structures (e.g. stromatolites) 20 Other candidate biomediated textures (e.g. MISS) 10 Features suggestive of (fossil) microorganisms 20

Result of first blank chemical check: Factor (prior to beginning sample analysis) No organics, clean background 1.0–0.9 OR Few, well known spacecraft organics in background 0.8–0.5 OR Background heavily compromised by contamination 0.2–0.0 Chemical biosignatures: Σ points × + Score Detection of primary biomolecules or their degradation products 20 Enantiomeric excess (or other isomer selectivity) 30 Molecular weight clustering of organic compounds 20 Evidence of repeating constitutional subunits 20 Systematic isotopic ordering at molecular (group) level 20 Bulk isotopic fractionation 10

Geological context: Σ points Long-lived water or hydrothermal setting (morphology) 15–10 Long-lived water or hydrothermal setting (mineralogy) 15–10

40 Credit: Mamers Valles, MEX/HRSC Pasteur Payload EE XX OO MM AA RR SS

ExoMars Rover Issue ‣ Astrobiology, June–July 2017 ‣ Introduction paper describing the ExoMars rover science and mission. ‣ A dedicated paper for each of the nine instruments.

41 Credit: Sand dunes near the north pole, MRO/HiRISE Rover Locomotion System EE XX OO MM AA RR SS

Locomotion formula: 6 x 6 x 6 + 6 6 supporting wheels 6 driven wheels 6 steered wheels 6 articulated knees

Back bogie

Side bogie

42 Flexible Wheels EE XX OO MM AA RR SS

Width 6 outer operating springs 12.0 cm Diameter 28.5 cm (Steel, 0.5 mm thick) 3 impact springs (Titanium, 1 mm thick)

Outer hub

Inner hub

Tire (Steel, 0.4 mm thick)

3 inner operating springs (Steel, 0.5 mm thick) 12 grousers

43 ES2 Soil - 21° Upslope - Back & Forth EE XX OO MM AA RR SS

Vivotec camera (GT-04-27) GoPro camera (GT-04-27)

video accelerated x25 video accelerated x25 Credit: RUAG, Airbus Defence & Space, ESA

Result: progress of 1.3 m in 94 min, excessive sinkage & slip

44 ES2 Soil - 21° Upslope - Wheel Walking EE XX OO MM AA RR SS

Vivotec camera (KBE-04-01) GoPro camera (KBE-04-01)

video accelerated x15 video accelerated x15 Credit: RUAG, Airbus Defence & Space, ESA

The tested WW gait respects all hardware kinematic constraints.

Result: progress of 3 m in 34 mins, low sinkage

45 Candidate Landing Sites EE XX OO MM AA RR SS

Start of conditions Surface conditions compatible with life become less habitable 4.1 3.7 Pre-Noachian Noachian Hesperian Mars Clays Oxia Planum Clays Mawrth Vallis

Early heavy Late heavy bombardment bombardment

Earth Hadean Archaean Ga 4.568 4.4 3.9 3.5

Beginning of terrestrial Oldest preserved planetary accretion traces of life

46 Credit: Kasei Valles, MEX/HRSC Mid- to Late-Noachian Settings EE XX OO MM AA RR SS

Detrital Snow or rain Detrital organics organics

Altered volcanics (phyllosilicates)

Chemotrophs near Lithotrophs Phyllosilicates Protocells hydrothermal on volcanic activity particles

47 Rover and Surface Platform EE XX OO MM AA RR SS

Credit: ESA/Medialab 48 Rover and Surface Platform EE XX OO MM AA RR SS

‣ 2020: ExoMars Rover and Surface Platform

• Travel back in time 4 billion years to explore the bottom of a Mars ocean. • Drill deep to penetrate below the organics degradation horizon. • Look for traces of life beyond Earth. • Study the surface geology and environment. • Obtain results that may make MSR and astronaut missions possible.

2-m depth

Credit: ESA/Medialab 49