Astrobiological Signatures with Penetrators on Europa

Biosignatures on Exoplanets Workshop – Mulhouse, France. June 25 2009 MSSL/UCL UK

Astrobiological Signatures Astrobiological Signatures with Penetrators on Europawith Penetrators on Europa

Rob Gowen (MSSL/UCL, UK)on behalf of Penetrator Consortium

Alan Smith1, Richard Ambrosi6, Olga Prieto Ballesteros16, Simeon Barber2, Dave Barnes11, Chris Braithwaite9, John Bridges6, Patrick Brown5, Phillip Church10, Glyn Collinson1, Andrew Coates1, Gareth Collins5, Ian Crawford3, Veronique Dehant21, Michele Dougherty5,

Julian Chela-Flores17, Dominic Fortes7, George Fraser6, Yang Gao4, Manuel Grande11, Andrew Griffiths1, Peter Grindrod7, Leonid Gurvits19, Axel Hagermann2, Tim van Hoolst21, Hauke Hussmann13, Ralf Jaumann13, Adrian Jones7, Geraint Jones1, Katherine Joy3,

Ozgur Karatekin21, Günter Kargl20, Antonella Macagnano14, Katarina Miljkovic 7,Anisha Mukherjee5, Peter Muller1, Ernesto Palomba12,Tom Pike5, Bill Proud9, Derek Pullan6, Francois Raulin15, Lutz Richter18, Keith Ryden2, Simon Sheridan2, Mark Sims6,

Frank Sohl13, Joshua Snape7, Paul Stevens10, Jon Sykes6, Vincent Tong3, Tim Stevenson6, Werner Karl5, Lionel Wilson8, Ian Wright2, John Zarnecki2.

1: Mullard Space Science Laboratory, University College London, 2: Planetary and Space Sciences Research Institute, Open University, UK. 3:Birkbeck College, University of London, UK. 4: Surrey Space Centre, Guildford, UK. 5: Imperial College, London,

UK, 6: University of Leicester, UK. 7: University College London, UK. 8: Lancaster University, UK. 9: Cavendish Laboratory, Cambridge, UK. 11: University of Aberystwyth, UK. 12: Istituto di Fisica dello Spazio Interplanetario-INAF, Roma, Italy. 13: DLR,

Berlin, Germany. 14: Institute of Microelectronics and Microsystem-CNR, Roma, Italy. 15: Université Paris, France. 16: Centro de Astrobiologia-INTA-CSIC, España. 17: Abdus Salam International Centre for Theoretical Physics (ICTP), Trieste, Italy. 18:

DLR, Bremen, Germany. 19: Joint Institute for VLBI in Europe (JIVE), Dwingeloo, The Netherlands. 20: IWF, Space Research Institute, Graz, Austria. 21: Royal Observatory, Belgium


ContentsContents

Mission to EuropaMission to Europa EuropaEuropa PenetratorsPenetrators InstrumentsInstruments AstrobiologyAstrobiology ConclusionsConclusions


Mission to EuropaMission to Europa EuropaEuropa PenetratorsPenetrators InstrumentsInstruments AstrobiologyAstrobiology ConclusionsConclusions

ContentsContents



Mission to Europa

EJSM – joint ESA/NASA mission to Jovian system. JEO – Jupiter/Europa Orbiter (NASA element) launch nominally 2020 arrive Europa 2028 observe 9 months (heavy radiation)

may include penetrators…



Descent Module release from Orbiter

Reorient

Spin-up & Decelerate

Penetrator Separation

Penetrator & PDS Penetrator & PDS surface Impactsurface Impact

Spin-Down

Penetrator deliveryPenetrator delivery

Delivery sequence courtesy SSTL Operate from Operate from

below surfacebelow surface


Europa

•

Astrobiology potential ? • atmosphere – trace Oxygen (10-12 Earth)• surface material - water ice• strong tidal forces• subsurface ocean ? subsurface ocean ? • rocky ocean floor bottomrocky ocean floor bottom • habitable ?habitable ?• life ?life ?

Basic parameters• mass : 0.7 Moon• surface gravity : 0.8 Moon• radius : 0.9 Moon• orbital period : 3.5 day• surface temp : 40-120K• surface radiation : Mrads


Japanese Lunar-AContinuous launch delays

Several paper studies

surface features


10Km

high resolution


Accessing Astrobiological Material

upwelled material available in striations from ocean beneath (may contain astrobiological material)

evidence of sulphates in striations.

young surface: 5-60 Ma(minimise radiation and meteroid damage)

but surface mostly very rough

Image from Proctor (JHU), Patterson (APL) & Senske (JPL) (2009, Europa Lander Workshop, Moscow)

Biosignatures on Exoplanets Workshop – Mulhouse, France. June 25 2009 MSSL/UCL UKFrom Proctor (JHU), Patterson (APL) & Senske (JPL) (2009, Europa Lander Workshop, Moscow)


Impact Site Characteristics

Feature TypeYoung

?Upwelled material ?

Flat /

smooth ?

Ridges & troughsyes

many? no

Bands no yes no

Chaos & Lenticulae yes yessome areas

Impact features yes yes no

Based on Proctor (JHU), Patterson (APL) & Senske (JPL) (2009, Europa Lander Workshop, Moscow)


Vertical exagguration x20.Vertical height ~ 1km.Landing ellipse ~5km into smooth area, equatorial

From Proctor (JHU), Patterson (APL) & Senske (JPL) (2009, Europa Lander Workshop, Moscow)


Penetrators


Micropenetrator & InstrumentsMicropenetrator & Instruments

• Low mass [~5-15Kg] • Very tough [~100-500m/s, impact ~10-50kgee]• Perform science from below surface [~0.5-few m]

Example Payload (~2kg)Example Payload (~2kg) Science Capability Science Capability

Micro seismometers(radio beacon, magnetometer)

sub-surface ocean, inner body structuretectonics, cryovulcanism

Chemistry package (mass spect.) organics and inorganics

Soil/environment package (accel, magnetometer,therm,...)

soil mechanical properties, thermal & electrical properties

Sample imager/astrobiology camera

Mineralogy, UV DNA flouresence

Descent camera impact site context & PR

~20-60cms


Post ImpactPost Impact

Target area of upwelled material (astrobiology)Target area of upwelled material (astrobiology) ~0.5 to few metres below surface (reduced radiation)~0.5 to few metres below surface (reduced radiation) 2 penetrators - derisk/improve performance2 penetrators - derisk/improve performance Lifetime: few hours (geochemistry/astrobiology, soil Lifetime: few hours (geochemistry/astrobiology, soil

properties) to few orbits (seismic measurements)properties) to few orbits (seismic measurements)


Instruments and TRLInstruments and TRL Previous Mars96, DS2, Lunar-A developmentsPrevious Mars96, DS2, Lunar-A developments UK currently developing technology for lunar UK currently developing technology for lunar

missionmission Most instruments have existing space heritage.Most instruments have existing space heritage. + successful full scale impact trial in UK.+ successful full scale impact trial in UK.

Micro-seismometer Imperial College(ExoMars)

Prototype,

ruggedized ion trap

mass-spectrometer

Open University

(Rosetta)


Impact trial – internal architectureImpact trial – internal architecture

Radiation sensor

MagnetometersBatteries

Mass spectrometer

Micro-seismometers

Drill assembly

AccelerometersPowerInterconnectionProcessing

Accelerometers, ThermometerBatteries,Data logger


Trial Hardware Trial Hardware

Inners Stack


Impact Trial - ConfigurationImpact Trial - Configuration

Rocket sledRocket sled PenetratorPenetrator


TargetTarget

Dry sandDry sand 2m x2m x6m2m x2m x6m Small front entrance aperture (polythene)Small front entrance aperture (polythene)


Real-Time Impact Video


FiringFiring


Astrobiology


Any life on Europa??

Comets deliver organicsRadiation from Jupiter’s

magnetosphere forms oxidants at surface that

could be used as food source

10cm radiation danger

Clinging life forms could use food brought by current

Photosynthetic plants could take advantage of sunlight

Floating forms could move up and down with the tides

Strong daily tidal currents

Warm ocean

Habitable zone

Image: University of Arizona, Lunar and Planetary Laboratory

Adapted from ‘Biogeochemistry of the Europa icy surface’, by Katarina Miljkovic, OU Feb’07


Another model…Adapted from K.Hand et. al. Moscow’09, who adapted it from Figueredo et al. 2003

1. habital zone on ocean floor adjacent to nutrients

2. communication of life forms to surface

3. astrobiological spectral signatures


Astrobiology Signatures ?

Presence of habitat Body image and motion Organic chemical inventory and proportions Isotopic ratios (sulphur) (weak spectral component )

Spectral signatures (complex)


Astrobiology Investigations

Microseismometers/Radio beacon/Magnetometer - Determine existence and characterise potentially habitable subsurface ocean.

Chemical sensing – via sample acquisition or e.g. stand-off laser ablation (mass spectrometer, quartz micro-balance and electronic noses, etc…)– mass spec can determine presence of organic molecules and their relative

abundances. – mass spec can determine 32S/34S isotopic ratio which is expected to have

quite different value whether origin is biological or geological.(very difficult to detectable spectrally)

Spectral sensing – remote (but close) chemical determination.(don’t yet have candidate instrument for spectral signal !) Raman.

Astrobiology imager – view either remote or acquired sample. Image life forms but more likely look for uv fluorescence (RNA/DNA)


Questions ?Questions ?

What does discovery of a rejected grant application What does discovery of a rejected grant application form mean ?form mean ?

How many different measurements to prove life ?How many different measurements to prove life ? What are best measurements to make to prove life ?What are best measurements to make to prove life ? 2 penetrators better than 1 ?2 penetrators better than 1 ?


Conclusions Earth is only body currently known to contain life... Detection of biosignatures on Europa or exoplanet could

inform other field. Detection of life on Europa or exoplanet could inform other

field. Heavy surface radiation is not necessarily an impediment to

life. Penetrators may also detect biosignatures on other planetary

bodies (e.g. Moon, Mars). Are there any other commonalities/useful connections with in-

situ search for astrobiological signals ? Good luck with hunting astrobiology signals from exoplanets !


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Astrobiological Signatures with Penetrators on Europa