UK work on ExoMars for Aurora
PPARC is investing £1.7 million for R&D work for the ExoMars mission with UK
academia and industry to develop key systems and technology for ESA’s ExoMars
mission. In addition UK industry is also investing in several of these projects at a
value above the PPARC award.
Whilst this overall UK investment does not guarantee that a particular instrument or
technology will be selected by ESA when the final mission payload is decided in
2007, it does enable the UK to develop robust and highly competitive technology
proposals that will position it to win leading roles.
The potential for transferring the knowledge gained and technology developed out of
Aurora and into other sectors is being actively fostered within this work package.
In addition to the work funded by PPARC, several UK groups are also working on
other instruments and technology for ExoMars.
Rover - Meet Britain's Robotic Mars Explorer!
Institutions: EADS Astrium, SciSys Ltd, Roke Manor Research Ltd, University of
Wales Aberystwyth, University of Leicester, Cranfield University, Strathclyde
University, Surrey University,
Contact: Mark Roe at EADS Astrium: mark.roe@astrium.eads.net Tel 01438 773330
PPARC funding has been
targeted at developing novel
autonomous technology that can
enhance the science return from
the ExoMars mission. The
highest priority has been given to
the development of an
“autonomous robotic scientist”,
which will assist in the
identification and analysis of
scientifically interesting Martian
features. The "autonomous
scientist" will be led by team
member SciSys with support
from Aberystwyth, Leicester and
Strathclyde Universities.
To support this, improvements in Rover navigation and mobility will also be
addressed by Roke Manor Research and Surrey University. Improvements in the
odometry (measurement of distance traveled) are being addressed by Cranfield
University, applying scientific methods to an industrial application. EADS Astrium will
coordinate these Rover developments.
An “Autonomous Robotic Scientist”
The aim for the Mars Rover is to act as a surrogate for the science team back on
Earth by allowing it to autonomously detect scientific targets of interest and explore
these in greater detail without the need for detailed supervision from ground control.
This robotic scientist will be able to identify potential targets from sensors such as
cameras using advanced image processing techniques.
Once a target is detected it will choose an appropriate investigative response
compatible with the intent of the science team. For example it may simply be to take
a high resolution image or move closer to the target in order to carry out more
detailed analysis. Having selected a desired action the system will then be able to
decide whether or not it has sufficient resources or energy to carry out this unplanned
procedure and ensure that it does not jeopardise the pre-planned science activities
for the day.
The overall objective of the autonomous robotic scientist is to increase the amount of
productive "science time" on the surface of Mars. The concept will be demonstrated
on the Mars Yard facility at Aberystwyth (see later in document)
“Bridget”
In support of these investigations EADS Astrium has developed its own Mars Rover
test bed to prove and integrate the different technologies required for interplanetary
robotic missions. The Rover, nicknamed "Bridget", has six driven wheels, four of
which steer, and is therefore capable of conventional and on-the-spot turning to
negotiate the kinds of obstacles found on Mars. Bridget recently underwent
locomotion trials in the El Teide National Park in Tenerife where engineers evaluated
its climbing and traction capability. The next stage in the test bed development is to
provide an autonomous navigation system which will enable the rover to navigate a
rocky landscape without the need for human intervention. The Rover test bed
weighs approx 120kg and has an "all up" weight capability of 300kg.
Life Marker Chip - taking ‘pregnancy test’ technology to Mars
UK Institutes: University of Leicester, Cranfield University, EADS Astrium, SSTL,
SciSys (flight programme), Qinetiq, University of Aberdeen, Open University, Imperial
College London
Contact Mark Sims, mrs@star.le.ac.uk Tel 0116 252 3513
The Life Marker Chip (LMC) will be used to look for specific molecules that may be
associated with life. It will use the fact that proteins and other biological molecules
will only bond with other molecules of a particular shape, essentially a “lock and key”
approach. Target molecules will only bind with the correct molecular receptor just as
only the right shaped key will turn in a lock.
Target molecules will include amino-acids, long chain molecules which are
associated with life on Earth for example cell membranes and pigments. The
instrument will search for evidence of past or present life based around water based
carbon life chemistry. It will operate in conjunction with other instruments on the
ExoMars payload to search for life and organics on Mars (for example the MOD/MOI
package – see later in this document).
“Essentially we are using biological molecules (proteins) and biological principles to
look for biology,” said Dr. Mark Sims University of Leicester “It will provide not only an
instrument for space research but will we hope have many terrestrial applications”.
"In essence, we are proposing to send hi-tech "pregnancy test" type devices - in
other words, molecular receptor based devices that can look for multiple pieces of
molecular evidence of life" said Dr David Cullen of Cranfield University who went on
to clarify "... but the intention and expectation is not to find pregnant Martians!"
The study builds upon work undertaken within the UK by the team over the last few
years to develop and apply the Life Marker Chip to space and other applications in
areas such as forensic science, health and defence and security, all areas where in
situ detection of organic markers / molecules are required. Examples include
detection of trace forensic evidence in the form of body fluids, detection of biological
or chemical hazards along with detection of explosive residues. During the last 15
months, discussions have been held with the Forensic Science Service and the
Health Protection Agency regarding possible applications of LMC technology.
The international consortium behind the LMC is led by the UK. The PPARC funding
will be used to develop the system to demonstrate its viability as an instrument. For
more details on the Life Marker Chip see the additional information in the press pack.
X-Ray Diffractometer/Spectrometer – looking at the geology of Mars
UK Institutes: Brunel University, University of Leicester, E2V, Imperial College
London, Natural History Museum and Open University
Contact: Andrew Holland, Tel. 01895 266516, Andrew.holland@brunel.ac.uk
X-ray diffraction is an essential tool in the mineralogical identification of rock
samples. ExoMars will be the first time a diffractometer will be used in-situ on Mars
to assess the local geology. Of particular importance will be the identification of
carbonates, silicates and other minerals, to assess the effect of possible chemical
weathering on the surface sediments, and to attempt to identify possible geochemical
fingerprints of past life on Mars. Traditional laboratory XRD instruments are huge and
weigh ~100kg, the real challenge for this project will be to make an instrument which
will return useful scientific data within an 800g mass envelope. The combination of
XRD with X-Ray Fluorescence (XRF) provides highly complementary techniques;
knowing the chemistry helps interpret the mineralogy and vice versa. XRD and XRF
together can constrain the composition of individual minerals; which is not currently
obtained using existing Mars surface instruments.
The project is already developing a breadboard instrument funded by ESA to
investigate the sensitivity of the instrument and to investigate system concepts with
project leaders in Italy (IRSPS and Laben) and collaborators in the Netherlands (Delft
U.). The PPARC investment will fund activities which go beyond the breadboard
development to prototype flight-style components which advance the technical
readiness of the instrument ready for the mission. The work will be an essential
activity toward meeting the challenging instrument mass goal!
Microseismometer – searching for Marsquakes
UK Institute: Imperial College London
Contact Tom Pike, Tel (0)20 7594 6207, Email w.t.pike@imperial.ac.uk
Researchers are planning to look deep inside Mars with a microseismometer
developed at Imperial College London. As part of a seismic system produced in
collaboration with France, Switzerland, the Netherlands, Germany and the US, this
will be the first in-situ investigation of the internal structure of another planet. The first
task of the seismic system will be to
listen out for Marsquakes. By looking
at how the vibrations from any quakes
have travelled through the planet, the
microseismometer will help work out
what’s going on in the deep interior. It
may also give some first indications of
the presence of liquid water.
Dr Tom Pike is designing the core of
the sensor in the Electrical and
Electronic Engineering department of Imperial College. “We’re carving out a near
perfect spring and weight from a single piece of silicon. We expect this 2-cm-square
sensor will be able to detect Marsquakes when they cause the smallest shuddering
of the silicon suspension. It looks like this sensor is going to stay on the static lander
and so we should also be able to feel the vibrations as the ExoMars rover sets off.
This should give some clues as to what is sitting directly below the surface of the
landing site. Depending on where we land on Mars, there is the possibility of
detecting sub-surface water.” The seismic system is designed to be part of a longlived geophysical and environmental package which should be able to listen for
Marsquakes and record the Martian weather for up to two years. The
microseismometer will give some indication of the level of any local volcanicity on
Mars.
The PPARC grant is funding the initial development work for a highly advanced
silicon micro-seismometer.
Caption: The heart of the microseismometer, the 2-cm-square micromachined silicon
suspension.
Advanced Environmental Package (AEP+) – looking at the weather on Mars
UK Institutes: Oxford University, Open University
Contact Simon Calcutt, calcutt@atm.ox.ac.uk , John Zarnecki,
j.c.zarnecki@open.ac.uk Tel. +44 (0)1908 659599 Mobile: +44 (0)778 9900099
The investigation and understanding of the Martian surface environment is crucial for
a number of reasons: Firstly, it determines the habitability of the Martian surface, for
microbial life as well as for future human explorers. Secondly, the near-surface
environment governs the exchange of heat, dust and water between the planetary
surface and atmosphere and thus holds the key to unravelling current atmospheric
processes as well as climate evolution. Thirdly, a better understanding of the surface
environment in general, and turbulence and dust processes in particular, will be
necessary for safe landing and operation of any future missions.
The AEP+ package, already selected by ESA for inclusion in the ExoMars mission,
will measure atmospheric pressure, temperature and humidity, as well as wind speed
and direction, dust momentum and optical depth. The AEP+ package will be led
jointly by the Open University and Oxford University, drawing on their extensive
experience in Mars meteorological instrumentation from the Beagle 2 Environmental
Sensor Suite (ESS) as well as designs for the (now cancelled) NetLander
ATMospheric Instrument Suite (ATMIS) and other missions. The proposed
instrument suite has a modular design making it robust and flexible, minimising
sensitivity to programmatic and technical risk. The sensor suite will be based on
improved variants of instruments already deployed on previous missions resulting in
a powerful yet resource-efficient instrument package.
This experiment will help characterise the Martian environment and provide answers
to the following:

What's the weather like at the ExoMars landing site?

Could any living organisms survive in this environment?

How are global dust storms started?

How and where is water to be found on the planet?

How turbulent is the atmosphere of Mars?
Oxford University has a PPARC grant for evaluating prototype wind sensors, and to
upgrade their Mars wind tunnel.
UV-VIS Spectrometer
UK Institutes: Open University, SSTL
Contact John Zarnecki, j.c.zarnecki@open.ac.uk Tel. +44 (0)1908 659599 Mobile:
+44 (0)778 9900099
The OU are currently working on a one year ESA contract to develop the prototype,
and will shortly start work on a PPARC grant (in conjunction with the Space Optics
Group at SSTL) to develop the front end fibre-optic interface.
Ultraviolet (UV) and Visible (VIS) radiation play an important role in planetary
environments, ranging from the photochemistry of upper atmospheres to the study of
astrobiology. Visible light is required for photosynthesis, whilst UV can be extremely
damaging to biological structures. The accurate determination of the solar UV/VIS
flux reaching the surface of Mars is addressed by this proposal through the design,
development and delivery of a space-qualified spectroscopic instrument for ExoMars.
The UV flux reaching the Martian surface has never before been directly measured.
This instrument aims to achieve for the first time, high resolution spectra of the UV
and visible flux present at the Martian surface.
The UV-VIS spectrometer (UVIS) is a miniature high-resolution spectroscopic
instrument designed for inclusion on a Martian lander to address these unresolved
issues. With extremely low mass and low power requirements (<300 g and <100 mW
respectively), it provides an ideal candidate for any Martian science payload, giving a
very significant science return in the form of a spectrum covering the UV and visible
spectrum (200-650nm) at high resolution (1-2 nm).
Panoramic Camera – our eyes on Mars
Institutes: UCL, UWA, UCL/Birkbeck, University of Leicester, University of Surrey.
Contact Andrew Coates, ajc@mssl.ucl.ac.uk, Tel 01483 204145
This wide-angle panoramic camera (PanCam) is an essential element of the
ExoMars Rover, led by UCL’s Mullard Space Science Laboratory (Andrew Coates,
Andrew Griffiths). PanCam images will set the context for the ExoMars life detection
experiments. As well as mapping, in 3D, the rover's immediate surroundings it will
look at the distant scene to identify future targets of interest. PanCam will observe
the drilling activities, look at rock layering, structure and composition, and examine
the rover's traverse for newly exposed material. It will also look for any macroscopic
evidence for biological activity.
The wide-angle camera is a stereo pair based on Beagle heritage. Just like our eyes,
it senses depth and shape on the surface using 'machine vision' techniques, and
spectral information gives geology (composition) and atmospheric information.
PanCam will make the vital three dimensional models of the rover's surroundings.
The PPARC R&D investment will allow explore if hyperspectral techniques (imaging
over a range of wavelengths from 400-1000nm visible and near infrared) could
replace fixed filters. Possible terrestrial uses of the technology include hostile
environment robotics, e.g. the nuclear industry and bomb disposal.
Using attenuation of sunlight near sunrise and sunset, PanCam will measure the
height profile of water vapour in the atmosphere. This water vapour is then blown
away by the solar wind at the top of the atmosphere as Mars lacks a global magnetic
field. Over billions of years, Mars dehydrates.
The High Resolution Camera part of PanCam (DLR, Germany provided) gives
complementary images, effectively a zoom lens for detailed imagery of interesting
targets and for high resolution panoramas.
PanCam images will be used for planning the rover's route across the Martian
surface, in particular scientific site selection. Panoramas will be taken to examine the
geology at each stopping point.
Major international collaborators are DLR, Joanneum Research (Austria), and Space
X (Switzerland) and the Science Team includes a wider international team.
Robust EDLS (Entry, Descent and Landing Systems)
Institutions: LogicaCMG, Vorticity Ltd, Fluid Gravity, SSTL, University of Manchester,
Open University, INSYS, Analyticon, University of Dundee
Contact: Andrew Hide, LogicaCMG, Email: andrew.hide@logicacmg.com Tel +44
7866 560239
A team led by LogicaCMG is developing technology aimed at ensuring a successful
landing for ExoMars. The team combines the essential expertise to address the
most critical phase of the ExoMars mission; the deceleration from hypersonic
velocities at the top of the Martian atmosphere to a soft landing on the surface. This
works builds on a successful track record with the Huygen’s probe which landed on
Titan in January 2005.
The PPARC R&D investment will produce improved models of the Martian
atmosphere and develop novel ways to determine location and speed during the
descent through the atmosphere.
The research will focus on:

Entry point accuracy determination

Entry & Descent error propagation analysis

Transverse Velocity determination towards the end of the landing phase
Fluid Inertial Simulation – a gentle touchdown on Mars
Institution: Vorticity Ltd
Contact Steve Lingard steve.lingard@vorticity-systems.com Tel 01865 893 212
Mobile 07710 546654
Parachutes are an essential part of the ExoMars EDLS.
To land on Mars the parachute must be deployed at twice the
speed of sound in order to give it time to decelerate the probe and
be descending vertically by the time it reaches the surface.
Designing a successful parachute requires understanding of how
it is affected by supersonic flow. Simulating how parachutes work
is complicated even at low speeds since the parachute is flexible
and the airflow affects the shape of the parachute and in turn the
shape of the parachute affects the airflow. This is called fluid
structure interaction (FSI). At supersonic speeds the disturbance
to the flow caused by the probe strongly affects the parachute.
The drag efficiency of the parachute falls rapidly above the speed of sound and the
parachute can suffer rapid and repeated inflation and collapse. These oscillations
could overstress the parachute structure and cause failure. To design a reliable
parachute for ExoMars demands a full understanding of these phenomena.
Recent advances in computational power and techniques will enable Vorticity Ltd to
simulate and understand the airflow around a flexible parachute leading to an
improved parachute system with minimal instability risks.
The PPARC funding will enable the efficiency of different parachutes designs under
different landing conditions to be modelled and evaluated.
Other work with a UK involvement:
Mars Organic Detector & Mars Oxidant Instrument (MOD and MOI)
Institution: Imperial College London
Contact: Mark Sephton, Tel: +44 (0)20 7594 6542, m.a.sephton@imperial.ac.uk
The Mars Organic Detector (MOD) instrument package searches for trace levels of
specific organic molecules, amino acids and polycyclic aromatic hydrocarbons
(PAH). These compound classes span all likely organic assemblages that may be
detected on Mars. All life as we know it uses amino acids, while sedimentary (fossil)
organic matter almost invariably contains some PAH; meteoritic organic matter
contains both.
In MOD, mineral samples are heated to release the target compounds in gas form.
From this form, PAH samples examined with a near-UV laser will fluoresce (emit
light) naturally and can be examined with a spectroscope. To detect amino acids the
sample holder will be covered with a
chemical that reacts with them to
fluoresce.
MOD is integrated with the Mars
Oxidant Instrument (MOI), which is
designed to characterise the
chemical species and reactions
responsible for the highly reactive
nature of the Martian soil and
perhaps the alteration and depletion
of organic compounds that comprise
the evidence of putative Martian life.
In other words, if MOD does not
detect organic compounds on Mars,
MOI can tell us why.
The instrument, together with the
drill, will allow scientists to
understand the fate of organic
molecules on Mars, by studying the distribution of organics and oxidants in the
subsurface with unprecedented sensitivity. MOD/MOI is considered a fundamental
instrument to achieve the mission's scientific objectives.
Magnetometer
Institution: Imperial College London, University of Edinburgh, University of Liverpool,
British Geological Survey, University of Leicester,
Contact: Professor Steven Schwartz, Tel +44 20 7594 7660
s.schwartz@imperial.ac.uk
The magnetometer will make the first localised surface measurements of Mar’s
magnetic field. Mars does not have a magnetic dynamo generating a field that
protects the planets atmosphere from the solar wind, though it is thought to have had
one in the past. Understanding what happened to the dynamo is key to the history of
Mars. The magnetometer will contribute to our understanding of Martian history,
study how the solar wind interacts with the planet’s atmosphere and characterise the
environment for future missions. It will also add to our knowledge of re-surfacing
effects on Mars (impacts, volcanoes, tectonics) as they have a effect on the magnetic
surface field.
UK groups are working on pre-flight calibration, on-board software and scientific
modelling.
Raman/LIBS spectrometer
Institution: Brunel University, CCLRC RAL, e2V, Bradford University
Contact: Chris Castelli, chris.castelli@brunel.ac.uk , Tel +44 (0)1895 266517, Mobile
07919160723
The combined Raman/LIBS (laser induced breakdown spectrometer) instrument is
one of the ESA recommended instruments on the Pasteur Rover Exobiology
Payload. This instrument will carry out detailed analysis of collected samples of rock
within the rover analytical laboratory as well as remote sampling through the use of
an external optical sensing head on the rover robotic arm. The powerful combination
of the Raman & LIBS techniques will be used to determine the geochemistry, organic
content and atomic composition of minerals.
Current
design of the
spectrometer
from the EBB
study
Raman spectroscopy has been demonstrated to be a viable non-destructive
technique for the analytical interrogation of geological scenarios for life-detection
signatures based on the presence of characteristic biochemicals produced by
extremophilic organisms for their survival in hostile environments. Several
advantages of Raman spectroscopic techniques for the molecular characterisation of
extremophiles are easily translatable from terrestrial to extraterrestrial applications
including an extended wavenumber range that covers signatures from both organic
and inorganic molecular species and the identification of biogeological modifications
and relict biomolecules present in the host geological matrices. In the ExoMars
programme, this instrument will be seeking to record signatures of any organic
materials and biomolecules that may be present.
TNO Science and Industry (Netherlands) leads a consortium of several European
partners to develop the Elegant Bread Board model for the instrument under contract
from ESA. The UK teams in this collaboration are providing the high performance,
miniature CCD camera and front end electronics. This teaming arrangement builds
on key technologies developed through the PPARC programme, in particular, space
qualified low mass and power custom CCD readout ASICs development by RAL and
flight qualified scientific CCDs from e2v. The scientific exploitation of the results is
being led by Bradford University who are world leaders in the use of Raman spectra
for the study of extremophiles in Mars analogue sites and for many years and have
built up expertise in the recognition of biomolecular signatures obtained under a wide
range of experimental conditions. Importantly, the Bradford Group is also integrated
into the international Raman/LIBS instrument science working team led by Prof.
Fernando Rull (University of Valladoid, Spain)
Mars Yard – simulating Mars on Earth
Institution: University of Wales Aberystwyth
Contact: Dave Barnes, dpb@aber.ac.uk Tel +44 01970 621561
The University of Wales Aberystwyth is
constructing a Planetary Analogue Terrain
Laboratory, informally known as a ‘Mars
Yard’. They are equipping a 45 square metre
area with soil and rocks that have similar
mechanical properties to those found on
Mars. The Mars Yard will be used to develop
and test the movements of rovers for use on
Mars.
Diagram: The Mars Yard will be used to test the same rover chassis concept as is
being developed at EADS Astrium. The half scale model at Aberystwyth will be used
to test additional designs options.
Descent System Design
Institution: Analyticon
Contact: Helen Ratay, Tel: [+44] (0) 1438 749886, helen.ratay@analyticon.co.uk
Analyticon was sub-contracted by Deimos Space S.L. to support the design of the
descent system for the mission. The descent system will activate after entry to the
Martian atmosphere, and will include a heat shield, a one- or two-stage parachute
system, retro-rockets and a final airbag to cushion the impact.
Analyticon’s responsibilities include complex trade-off calculations to assess the
lightest design for the descent system, as well as highly accurate simulations of the
performance of the descent system in different atmospheric conditions. Several
different designs are possible, using various types of parachute and airbag. Dave
Dungate, Technical Director of Analyticon, said: “Our integrated design tools allow
the optimal descent system solutions to be determinedvery quickly”.
Dave Northey, technical consultant at Analyticon, explained the difficulty of identifying
the best solution: “With any lander mission, mass is at a premium. Finding the
lightest solution for the descent system is complicated by the fact that the mass of
each part affects all the others. For example, if the airbags get heavier, you then
need a larger parachute to slow down the descent module carrying those airbags.”
Analyticon has previous experience of Entry, Descent and Landing Systems (EDLS),
which includes earlier investigations into airbag design, and participation in phase A
work for ExoMars.
Alternative Descent and Landing Technologies
Institution: Vorticity Ltd. InSys
Contact: Steve Lingard steve.lingard@vorticity-systems.com Tel 01865 893 212
Mobile 07710 546654
For any planetary exploration mission to Mars, one of the
most challenging phases is landing on the planetary
surface.
Successful solutions to the problem of landing to date
have included soft-propulsive landing (as for Viking), and
harder, bouncing airbag assisted landing (as for
Pathfinder and the Mars Exploration Rovers).
Conventional airbag concepts to date have consisted of a ‘billiard-ball' type of
arrangement with a payload capsule entirely surrounded by airbags. When released
from the descent parachute, the payload and airbags bounce many times on the
surface before coming to rest. This setup also requires the payload to have some
form of self righting mechanism.
The alternative investigated in this activity consists of a hexagonal platform
surrounded by airbags containing vent valves. On landing, sensors send a signal to
open the vents which causes a rapid but predictable deflation. In this concept there
should be no bouncing and the payload should come to rest in a predictable, upright
orientation.
This project will model the entire descent and landing phase, from the end of the
entry phase, through the deployment of parachutes, the activation of propulsive
velocity control systems and finally the landing with a vented airbag system. In
addition to theoretical modelling, this project is developing and testing a prototype
vented airbag to prove the feasibility of the concept.