ExoMars 2016 and 2018 programmea very brief description(and LMD’s implication therein)
Ehouarn Millour for the LMD teamMay 14th 2015, Kobe

ExoMars 2016
• The 2016 mission will carry a 600 kg
Entry and descent Demonstration
Module (EDM) that shall allow Europe
to test and demonstrate its capability toland on Mars, and improve EDL
technologies for future missions.

• For this purpose, it will be equipped witha suite of sensors:

Trace Gas Orbiter

EDM– Front shield : pressure sensors + 7 thermalplugs– Back Shield sun sensors, 3 thermal plugs,Infrared radiometer– 2 Inertial measurement units– Near surface radar altimeter– Downward looking descent camera• LMD involved (as sub-contractor toTAS-I) in the characterization of theatmosphere for the preparation of EDLSurface
operation:
2-4 days

The science of the ExoMars 2016 EDM
The EDM will support two major scientific motivations:• Improve our knowledge of Mars atmospherewith in-situ observations (Entry-Descent-Landing phase)=> AMELIA experimentPI:
F. Ferri (Univ. Padova, It.)
co-PIs:F. Forget (Fr.), S. Lewis (UK), O. Katatekin (Bel.)+ 20 co-Is + 10 collaborators from 7 countries• Improve our knowledge of Mars environment
at times of high dust loading (Surface operations)=> DREAMS experimentPI:
F. Esposito (INAF, It.)
co-PI:
F. Montmessin (Fr.)+ 6 lead-CoIs + 40 co-Is from 9 countries

EDM Surface Payload (DREAMS)MicroAres
ODS
MetWind•Short lived: will only operate a few
days (2-4) on the surface of Mars

MarsTemDREAMS-H

DREAMS is an integrated andautonomous system which will perform:•First ever investigation of atmosphericelectric phenomena on Mars

P/L BatteryDREAMS-P•Characterization of thediurnal cycle during the dusty season.

ODS PECEU

Trace Gas Orbiter
Science instruments

ENOMAD

Atmospheric composition(CH4 ,O3 , trace species, isotopes)
High resolution occultation
dust, clouds, P&T profiles
and nadir spectrometers
UVIS (0.20 – 0.65 m) ~ 250

SO

Limb Nadir

IR (2.3 – 3.8 m) ~ 10,000

SO

Limb Nadir

IR (2.3 – 4.3 m) ~ 20,000

CaSSISSO

Mapping of sources;
landing site selection

High-resolution camera

5 m/px 3-colour imaging and panchromatic stereoACS
Suite of 3 high-resolution
spectrometersAtmospheric chemistry, aerosols,surface T,structure

Near IR (0.7 – 1.7 m) ~ 20,000

SOLimb Nadir

IR (Fourier, 2 – 25 m) ~ 4000 (SO)/500 (N)SO NadirMid IR (2.2 – 4.5 m) ~ 50,000

FREND
Collimated neutron detector

SO

Mapping of
subsurface water

All resolving power figures are calculated at mid-range

XO

M

ARS

TGO Science instruments

EXOM

ARMajor Scientific Products• Spatially-resolved inventory of trace gases and key isotopes– Monitoring and profiling of CO, H2O/HDO, organics, aerosols, ... (NOMAD, ACS)
– Mapping and profiling of isotopologues and O3 (NOMAD)– Monitor meteorology , and back-track trace gas sources=> Confirm/characterise CH4 presence on Mars
– mapping, profiling, image of sources and terrain• Higher resolution mapping of sub-surface water and hydratedminerals (FREND)• High resolution, colour and stereo coverage of extended areas(incl. future landing sites), with focus on trace gas sources anddynamic processes (CaSSIS)SLMD implication in ExoMars Trace Gas Orbiter• In performing retrievals using ACS (S. Guerlet).
• In performing data assimilation of ACS in near « real time » conditions tosupport retrievals for other instruments.
=> PhD work of T. Navarro: Using LETKF on Mars Climate Sounder data
Strategy: Temperature biases are also corrected by adding dust (and/or watervapor) based on dust-cloud-temperature correlations and/or direct aerosol
observations.
LETKF scheme from University of Maryland
Combined to the LMD GCM

ExoMars 2018 Candidates Landing sites• The four candidate sites lie around the Chryse basin.
• They all possess a record of ancient sediment deposition and alteration acting
over large scales (spatial and temporal), requiring a lot of water:– Mawrth Vallis and Oxia Planum are in extensive, finely layered
phyllosilicate-rich areas.
– Aram Dorsum and Hypanis Vallis are in alluvial settings: A sinuous river(Aram) and a delta/fan (Hypanis).
• The clays at Mawrth and Oxia, and the Aram Dorsum floodplains, date from thevery early, habitable epoch of Mars.
• The Hypanis Vallis deltaic deposits are more recent (early Hesperian).
• F. Forget is a member of the LLSWG (Landing Site Selection Working Group)EXOMARS 2018 ROVER AND LANDEDPLATFORM
A rover dedicated to thesearch for signs of life

Nominal mission:
Nominal science:
Cycles +220 sols
6 Experiment

2 VerticalSurveys
EC length:

16–20 sols

Rover mass:

300-kg class

Mobility range:

Several km

Rover Pasteur Payload
PanCamE

XOM

AR

Geological context
Rover traverse planning
Atmospheric studies

Wide-angle stereo camera pair
High-resolution camera
WAC 35° FOV, HRC 5° FOV

ISEM
IR spectrometer on mast

Bulk mineralogy of outcrops
Target selection

Analytical Laboratory DrawerMicrOmega

1.15 – 3.3 μm, 1° FOV

VIS + IR Spectrometer

CLUPI
Close-up imager

Geological deposition environment
Microtexture of rocks
Morphological biomarkers

0.9 – 3.5 μm, 256 x 256 pixels, 20-μm/pixel, 500 steps

RLS

20-μm resolution at 50-cm distance

Raman spectrometer

WISDOM

Mapping of subsurface
stratigraphy

Ground-penetrating radar3 – 5-m penetration, 2-cm resolution

FREND
Passive neutron detector

Mapping of subsurface
Water and hydrated minerals

Drill + Ma_MISS In-situ mineralogy information
IR borehole spectrometer
0.4 – 2.2 μm

Mineralogical characterizationof crushed sample material
Pointing for other instruments

Geochemical composition
Detection of organic pigments

spectral shift range 200–3800 cm–1, resolution ≤ 6 cm–1

MOMA

Broad-range organic molecule
detection at high sensitivity (ppb)
LDMS + Pyr-Dev GCMS
Chirality determination

Laser-desorption extraction and mass spectroscopy
Step-heating & Pyrolysis extraction in the presenceof derivatisation agents, coupled with chiral gas
chromatography and mass spectroscopy

SRover Pasteur PayloadE13X

OMARS

ExoMars 2018 Russian Surface platform:(European contributed payload currently under selection)
Lifetime ~1 Earth year