foing (sloppy): 585 papers, Hirsch index 28, Hirsch ratio 0.048.
adsauthor "Foing, B." abstract sloppy
@--------------------------------------------------------------------
Title: Toward a global space exploration program: A
stepping stone approach
Authors: Ehrenfreund, Pascale; McKay, Chris; Rummel, John D.;
Foing, Bernard H.; Neal, Clive R.;
Masson-Zwaan, Tanja; Ansdell, Megan; Peter, Nicolas;
Zarnecki, John; Mackwell, Steve;
Perino, Maria Antionetta; Billings, Linda;
Mankins, John; Race, Margaret
Bibliographic Code: 2012AdSpR..49....2E
Abstract
In response to the growing importance of space exploration in future
planning, the Committee on Space Research (COSPAR) Panel on Exploration
(PEX) was chartered to provide independent scientific advice to support
the development of exploration programs and to safeguard the potential
scientific assets of solar system objects. In this report, PEX
elaborates a stepwise approach to achieve a new level of space
cooperation that can help develop world-wide capabilities in space
science and exploration and support a transition that will lead to a
global space exploration program. The proposed stepping stones are
intended to transcend cross-cultural barriers, leading to the
development of technical interfaces and shared legal frameworks and
fostering coordination and cooperation on a broad front. Input for this
report was drawn from expertise provided by COSPAR Associates within the
international community and via the contacts they maintain in various
scientific entities. The report provides a summary and synthesis of
science roadmaps and recommendations for planetary exploration produced
by many national and international working groups, aiming to encourage
and exploit synergies among similar programs. While science and
technology represent the core and, often, the drivers for space
exploration, several other disciplines and their stakeholders (Earth
science, space law, and others) should be more robustly interlinked and
involved than they have been to date. The report argues that a shared
vision is crucial to this linkage, and to providing a direction that
enables new countries and stakeholders to join and engage in the overall
space exploration effort. Building a basic space technology capacity
within a wider range of countries, ensuring new actors in space act
responsibly, and increasing public awareness and engagement are concrete
steps that can provide a broader interest in space exploration,
worldwide, and build a solid basis for program sustainability. By
engaging developing countries and emerging space nations in an
international space exploration program, it will be possible to create a
critical bottom-up support structure to support program continuity in
the development and execution of future global space exploration
frameworks. With a focus on stepping stones, COSPAR can support a global
space exploration program that stimulates scientists in current and
emerging spacefaring nations, and that will invite those in developing
countries to participate---pursuing research aimed at answering
outstanding questions about the origins and evolution of our solar
system and life on Earth (and possibly elsewhere). COSPAR, in
cooperation with national and international science foundations and
space-related organizations, will advocate this stepping stone approach
to enhance future cooperative space exploration efforts.
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Title: The ORGANIC experiment on EXPOSE-R on the ISS:
Flight sample preparation and ground control
spectroscopy
Authors: Bryson, K. L.; Peeters, Z.; Salama, F.; Foing, B.;
Ehrenfreund, P.; Ricco, A. J.; Jessberger, E.;
Bischoff, A.; Breitfellner, M.; Schmidt, W.;
Robert, F.
Bibliographic Code: 2011AdSpR..48.1980B
Abstract
In March of 2009, the ORGANIC experiment integrated into the European
multi-user facility EXPOSE-R, containing experiments dedicated to
Astrobiology, was mounted through Extra Vehicular Activity (EVA)
externally on the International Space Station (ISS). The experiment
exposed organic samples of astronomical interest for a duration of 97
weeks (˜22 months) to the space environment. The samples that were
returned to Earth in spring 2011, received a total UV radiation dose
during their exposure including direct solar irradiation of >2500 h,
exceeding the limits of laboratory simulations. We report flight sample
preparation and pre-flight ultraviolet-visible (UV-Vis) characterization
of the ORGANIC samples, which include 11 polycyclic aromatic
hydrocarbons (PAHs) and three fullerenes. The corresponding
time-dependent ground control monitoring experiments for ORGANIC
measured over ˜19 months are presented and the results anticipated
upon return of the samples are discussed. We present the first UV-Vis
spectrum of solid circobiphenyl (C38H16). Further,
we present the first published UV-Vis spectra of
diphenanthro[9,10-b',10'-d]thiophene
(C28H16S),
dinaphtho[8,1,2-abc,2',1',8'-klm]coronene
(C36H16),
tetrabenzo[de,no,st,c'd']heptacene
(C42H22), and dibenzo[jk,a'b']octacene
(C40H22) in solid phase and in solution. The
results of the ORGANIC experiment are expected to enhance our knowledge
of the evolution and degradation of large carbon-containing molecules in
space environments.
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Title: Microbiological contamination assessment from
drilling activities - recognition and design of
prevention strategy
Authors: Rodrigues, L.; Davies, G. R.; Foing, B.; Correia, A.;
Alves, A.; Valdivia-Silva, J.; Zavaleta, J.;
Stoker, C.; Wilson, D.; Clarke, J.
Bibliographic Code: 2011epsc.conf.1370R
Abstract
The search for traces of extinct and extant life combined with
sub-surface sampling on Mars will be investigated for the first time in
ExoMars Exploration Mission. Sub-surface sampling will be addressed
using a robotic drill that will minimize the risk of forward
contamination. Hence the risks associated with drill contamination must
be addressed. This paper describes contamination assessment related to
dry drilling activities in Terrestrial Martian analogues.
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Title: Analysis of organic compounds, minerals and biota:
Preparation for future Mars life detection missions
Authors: Martins, Z.; Kotler, J. M.; Direito, S. O. L.;
Sephton, M. A.; Stoker, C.; Foing, B. H.;
Ehrenfreund, P.
Bibliographic Code: 2011epsc.conf..709M
Abstract
In the present study we have measured the amino acid content of Mars
analogue soil samples, and related those results to the microbial and
mineralogical data of the soil samples. These were performed on soils
collected near the Mars Desert Research Station (MDRS) in the Utah
desert (Figure 1), during the EuroGeoMars 2009 campaign [2,3]. The Utah
soil displays mineralogies similar to Mars, with sedimentary deposits of
sands, evaporites, clays and gypsum [4].
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Title: On the polarisation of the Red Rectangle optical
emission bands
Authors: Cox, N. L. J.; Foing, B. H.; Cami, J.; Sarre, P. J.
Bibliographic Code: 2011A&A...532A..46C, eprint = 1105.4795
Abstract
Context. The origin of the narrow optical emission bands seen towards
the Red Rectangle is not yet understood. We investigate the proposal
that these are caused by luminescence of large carbonaceous molecules.
Aims: We aim to measure the polarisation of the optical narrow
Red Rectangle bands (RRBs). Polarised signals of several percent could
be expected from certain asymmetric molecular rotators.
Methods:
The ESPaDOnS échelle spectrograph mounted at the CFHT was used to
obtain high-resolution optical spectropolarimetric data of the Red
Rectangle nebular emission.
Results: The RRBs at 5800, 5850, and
6615 Å are detected in spectra of the nebular emission 7"
and 13" north-east from the central star. The 5826 Å and
6635 Å RRB are detected only at the position nearest to the
central star. For both positions the Stokes Q and U spectra show no
unambiguous polarisation signal in any of the RRBs. We derive an upper
limit of 0.02% line polarisation for these RRBs. A tentative feature
with peak polarisation of 0.05% is seen for the 5800 Å RRB at
7" offset. However, the null spectra suggest that this may be an
instrumental artefact.
Conclusions: The lack of a clear
polarisation signal for the five detected RRBs implies that if the
emission is caused by luminescence of complex organics, these gas-phase
molecular carriers are likely to have a high degree of symmetry because
they do not exhibit a Q-branch in their rotational profile, although
this may be modified by statistical effects.
Based on observations obtained at the Canada-France-Hawaii Telescope
(CFHT) which is operated by the National Research Council of Canada, the
Institut National des Sciences de l'Univers of the Centre National de la
Recherche Scientique of France, and the University of Hawaii.
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Title: Multidisciplinary integrated field campaign to an
acidic Martian Earth analogue with astrobiological
interest: Rio Tinto
Authors: Gómez, F.; Walter, N.; Amils, R.; Rull, F.;
Klingelhöfer, A. K.; Kviderova, J.; Sarrazin, P.;
Foing, B.; Behar, A.; Fleischer, I.; Parro, V.;
Garcia-Villadangos, M.; Blake, D.;
Martin Ramos, J. D.; Direito, S.; Mahapatra, P.;
Stam, C.; Venkateswaran, K.; Voytek, M.
Bibliographic Code: 2011IJAsB..10..291G
Abstract
Recently reported results from latest Mars Orbiters and Rovers missions
are transforming our opinion about the red planet. That dry and
inhospitable planet reported in the past is becoming a wetter planet
with high probabilities of water existence in the past. Nowadays, some
results seem to indicate the presence of water beneath the Mars surface.
But also mineralogy studies by NASA Opportunity Rover report iron oxides
and hydroxides precipitates on Endurance Crater. Sedimentary deposits
have been identified at Meridiani Planum. These deposits must have
generated in a dune aqueous acidic and oxidizing environment.
Similarities appear when we study Rio Tinto, and acidic river under the
control of iron.
The discovery of extremophiles on Earth widened the window of
possibilities for life to develop in the Universe, and as a consequence
on Mars and other planetary bodies with astrobiological interest. The
compilation of data produced by the ongoing missions offers an
interested view for life possibilities to exist: signs of an early wet
Mars and rather recent volcanic activity as well as ground morphological
characteristics that seem to be promoted by liquid water. The discovery
of important accumulations of sulfates and the existence of iron
minerals such as jarosite in rocks of sedimentary origin has allowed
specific terrestrial models to come into focus. Río Tinto
(Southwestern Spain, Iberian Pyritic Belt) is an extreme acidic
environment, product of the chemolithotrophic activity of
micro-organisms that thrive in the massive pyrite-rich deposits of the
Iberian Pyritic Belt. Some particular protective environments should
house the organic molecules and bacterial life forms in harsh
environments such as Mars surface supporting microniches inside
precipitated minerals or inside rocks. Terrestrial analogues could help
us to afford the comprehension of habitability (on other planetary
bodies).
We are reporting here the multidisciplinary study of some endolithic
niches inside salt deposits used by phototrophs for taking advantage of
sheltering particular light wavelengths. These acidic salts deposits
located in Río Tinto shelter life forms that are difficult to
visualize by eye. This interdisciplinary field analogue campaign was
conducted in the framework of the CAREX FP7 EC programme.
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Title: Mineralogical, chemical, organic and microbial
properties of subsurface soil cores from Mars Desert
Research Station (Utah, USA): Phyllosilicate and
sulfate analogues to Mars mission landing sites
Authors: Stoker, Carol R.; Clarke, Jonathan;
Direito, Susana O. L.; Blake, David;
Martin, Kevin R.; Zavaleta, Jhony; Foing, Bernard
Bibliographic Code: 2011IJAsB..10..269S
Abstract
We collected and analysed soil cores from four geologic units
surrounding Mars Desert Research Station (MDRS) Utah, USA, including
Mancos Shale, Dakota Sandstone, Morrison formation (Brushy Basin member)
and Summerville formation. The area is an important geochemical and
morphological analogue to terrains on Mars. Soils were analysed for
mineralogy by a Terra X-ray diffractometer (XRD), a field version of the
CheMin instrument on the Mars Science Laboratory (MSL) mission (2012
landing). Soluble ion chemistry, total organic content and identity and
distribution of microbial populations were also determined. The Terra
data reveal that Mancos and Morrison soils are rich in phyllosilicates
similar to those observed on Mars from orbital measurements
(montmorillonite, nontronite and illite). Evaporite minerals observed
include gypsum, thenardite, polyhalite and calcite. Soil chemical
analysis shows sulfate the dominant anion in all soils and
SO4>>CO3, as on Mars. The cation pattern
Na>Ca>Mg is seen in all soils except for the Summerville where
Ca>Na. In all soils, SO4 correlates with Na, suggesting
sodium sulfates are the dominant phase. Oxidizable organics are low in
all soils and range from a high of 0.7% in the Mancos samples to
undetectable at a detection limit of 0.1% in the Morrison soils.
Minerals rich in chromium and vanadium were identified in Morrison soils
that result from diagenetic replacement of organic compounds.
Depositional environment, geologic history and mineralogy all affect the
ability to preserve and detect organic compounds. Subsurface biosphere
populations were revealed to contain organisms from all three domains
(Archaea, Bacteria and Eukarya) with cell density between
3.0×106 and 1.8×107 cells
ml-1 at the deepest depth. These measurements are
analogous to data that could be obtained on future robotic or human Mars
missions and results are relevant to the MSL mission that will
investigate phyllosilicates on Mars.
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Title: Human crew-related aspects for astrobiology research
Authors: Thiel, Cora S.; Pletser, Vladimir; Foing, Bernard
Bibliographic Code: 2011IJAsB..10..255T
Abstract
Several space agencies and exploration stakeholders have a strong
interest in obtaining information on technical and human aspects to
prepare for future extra-terrestrial planetary exploration. In this
context, the EuroGeoMars campaign, organized with support from the
International Lunar Exploration Working Group (ILEWG), the European
Space Agency (ESA), the National Aeronautics and Space Administration
(NASA) Ames Research Center and partner institutes, was conducted by the
crews 76 and 77 in February 2009 in The Mars Society's `Mars
Desert Research Station' (MDRS) in Utah.
The EuroGeoMars encompasses two groups of experiments: (1) a series of
field science experiments that can be conducted from an
extra-terrestrial planetary surface in geology, biology,
astronomy/astrophysics and the necessary technology and networks to
support these field investigations; (2) a series of human crew-related
investigations on crew time organization in a planetary habitat, on the
different functions and interfaces of this habitat, and on
man-machine interfaces of science and technical equipment.
This paper recalls the objective of the EuroGeoMars project and presents
the MDRS and its habitat layout. Social and operational aspects during
simulations are described. Technical and operational aspects of biology
investigations in the field and in the habitat laboratory are discussed
in detail with the focus point set on the polymerase chain reaction
(PCR)-based detection of microbial DNA in soil samples.
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Title: Astrobiology and habitability studies in preparation
for future Mars missions: trends from investigating
minerals, organics and biota
Authors: Ehrenfreund, P.; Röling, W. F. M.; Thiel, C. S.;
Quinn, R.; Sephton, M. A.; Stoker, C.; Kotler, J. M.;
Direito, S. O. L.; Martins, Z.; Orzechowska, G. E.;
Kidd, R. D.; van Sluis, C. A.; Foing, B. H.
Bibliographic Code: 2011IJAsB..10..239E
Abstract
Several robotic exploration missions will travel to Mars during this
decade to investigate habitability and the possible presence of life.
Field research at Mars analogue sites such as desert environments can
provide important constraints for instrument calibration, landing site
strategies and expected life detection targets. We have characterized
the mineralogy, organic chemistry and microbiology of ten selected
sample sites from the Utah desert in close vicinity to the Mars Desert
Research Station (MDRS) during the EuroGeoMars 2009 campaign (organized
by International Lunar Exploration Working Group (ILEWG), NASA Ames and
ESA ESTEC). Compared with extremely arid deserts (such as the Atacama),
organic and biological materials can be identified in a larger number of
samples and subsequently be used to perform correlation studies. Among
the important findings of this field research campaign are the diversity
in the mineralogical composition of soil samples even when collected in
close proximity, the low abundances of detectable polycyclic aromatic
hydrocarbons (PAHs) and amino acids and the presence of biota of all
three domains of life with significant heterogeneity. An extraordinary
variety of putative extremophiles, mainly Bacteria and also Archaea and
Eukarya was observed. The dominant factor in measurable bacterial
abundance seems to be soil porosity and lower small (clay-sized)
particle content. However, correlations between many measured parameters
are difficult to establish. Field research conducted during the
EuroGeoMars 2009 campaign shows that the geological history and
depositional environment of the region, as well as the mineralogy
influence the ability to detect compounds such as amino acids and DNA.
Clays are known to strongly absorb and bind organic molecules often
preventing extraction by even sophisticated laboratory methods. Our
results indicate the need for further development and optimization of
extraction procedures that release biological compounds from host
matrices to enable the effective detection of biomarkers during future
sampling campaigns on Earth and Mars.
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Title: Extraction of amino acids from soils close to the
Mars Desert Research Station (MDRS), Utah
Authors: Martins, Z.; Sephton, M. A.; Foing, B. H.;
Ehrenfreund, P.
Bibliographic Code: 2011IJAsB..10..231M
Abstract
Future space missions that aim to detect life should search for
molecules that are vital to all living organisms. Although the Viking
landers did not find any signs of organic molecules on Mars, signatures
of past and/or present life may still exist in the Martian regolith. In
this paper, we describe amino acid analyses performed in several Martian
analogue soil samples collected close to the Mars Desert Research
Station (MDRS), Utah, during the International Lunar Exploration Working
Group (ILEWG) EuroGeoMars campaign in February 2009. The Utah desert
around Hanksville is characterized as shale desert and is cold and arid
with an average annual temperature of 12°C. It is subjected to wind
erosion and was shaped by fluvial erosion. The data show large
differences in the total amino acid abundances between all the collected
soil samples, with values ranging from non-detectable to 100 000
parts per billion (ppb). These results are explained in the context of
mineralogical differences (namely different clay content) among the soil
samples. The data have implications for future life-detection missions
and the target mineralogy that may host biological signatures.
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Title: Analysis of mineral matrices of planetary soil
analogues from the Utah Desert
Authors: Kotler, J. M.; Quinn, R. C.; Foing, B. H.;
Martins, Z.; Ehrenfreund, P.
Bibliographic Code: 2011IJAsB..10..221K
Abstract
Phyllosilicate minerals and hydrated sulphate minerals have been
positively identified on the surface of Mars. Studies conducted on Earth
indicate that micro-organisms influence various geochemical and
mineralogical transitions for the sulphate and phyllosilicate minerals.
These minerals in turn provide key nutrients to micro-organisms and
influence microbial ecology. Therefore, the presence of these minerals
in astrobiology studies of Earth-Mars analogue environments could
help scientists better understand the types and potential abundance of
micro-organisms and/or biosignatures that may be encountered on Mars.
Bulk X-ray diffraction of samples collected during the EuroGeoMars 2009
campaign from the Mancos Shale, the Morrison and the Dakota formations
near the Mars Desert Research Station in Utah show variable but common
sedimentary mineralogy with all samples containing quantities of
hydrated sulphate minerals and/or phyllosilicates. Analysis of the clay
fractions indicate that the phyllosilicates are interstratified
illite-smectites with all samples showing marked changes in the
diffraction pattern after ethylene glycol treatment and the
characteristic appearance of a solvated peak at ˜17 Å. The
smectite phases were identified as montmorillonite and nontronite using
a combination of the X-ray diffraction data and Fourier-Transform
Infrared Spectroscopy. The most common sulphate mineral in the samples
is hydrated calcium sulphate (gypsum), although one sample contained
detectable amounts of strontium sulphate (celestine). Carbonates
detected in the samples are variable in composition and include pure
calcium carbonate (calcite), magnesium-bearing calcium carbonate
(dolomite), magnesium, iron and manganese-bearing calcium carbonate
(ankerite) and iron carbonate (siderite). The results of these analyses
when combined with organic extractions and biological analysis should
help astrobiologists and planetary geologists better understand the
potential relationships between mineralogy and microbiology for
planetary missions.
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Title: Analysis of Mars analogue soil samples using
solid-phase microextraction, organic solvent
extraction and gas chromatography/mass spectrometry
Authors: Orzechowska, G. E.; Kidd, R. D.; Foing, B. H.;
Kanik, I.; Stoker, C.; Ehrenfreund, P.
Bibliographic Code: 2011IJAsB..10..209O
Abstract
Polycyclic aromatic hydrocarbons (PAHs) are robust and abundant
molecules in extraterrestrial environments. They are found ubiquitously
in the interstellar medium and have been identified in extracts of
meteorites collected on Earth. PAHs are important target molecules for
planetary exploration missions that investigate the organic inventory of
planets, moons and small bodies. This study is part of an
interdisciplinary preparation phase to search for organic molecules and
life on Mars. We have investigated PAH compounds in desert soils to
determine their composition, distribution and stability. Soil samples
(Mars analogue soils) were collected at desert areas of Utah in the
vicinity of the Mars Desert Research Station (MDRS), in the Arequipa
region in Peru and from the Jutland region of Denmark. The aim of this
study was to optimize the solid-phase microextraction (SPME) method for
fast screening and determination of PAHs in soil samples. This method
minimizes sample handling and preserves the chemical integrity of the
sample. Complementary liquid extraction was used to obtain information
on five- and six-ring PAH compounds. The measured concentrations of PAHs
are, in general, very low, ranging from 1 to 60 ng g-1.
The texture of soils is mostly sandy loam with few samples being 100 %
silt. Collected soils are moderately basic with pH values of 8-9
except for the Salten Skov soil, which is slightly acidic. Although the
diverse and variable microbial populations of the samples at the sample
sites might have affected the levels and variety of PAHs detected, SPME
appears to be a rapid, viable field sampling technique with implications
for use on planetary missions.
@--------------------------------------------------------------------
Title: A wide variety of putative extremophiles and large
beta-diversity at the Mars Desert Research Station
(Utah)
Authors: Direito, Susana O. L.; Ehrenfreund, Pascale;
Marees, Andries; Staats, Martijn; Foing, Bernard;
Röling, Wilfred F. M.
Bibliographic Code: 2011IJAsB..10..191D
Abstract
Humankind's innate curiosity makes us wonder whether life is or was
present on other planetary bodies such as Mars. The EuroGeoMars 2009
campaign was organized at the Mars Desert Research Station (MDRS) to
perform multidisciplinary astrobiology research. MDRS in southeast Utah
is situated in a cold arid desert with mineralogy and erosion processes
comparable to those on Mars. Insight into the microbial community
composition of this terrestrial Mars analogue provides essential
information for the search for life on Mars: including sampling and life
detection methodology optimization and what kind of organisms to expect.
Soil samples were collected from different locations.
Culture-independent molecular analyses directed at ribosomal RNA genes
revealed the presence of all three domains of life (Archaea, Bacteria
and Eukarya), but these were not detected in all samples. Spiking
experiments revealed that this appears to relate to low DNA recovery,
due to adsorption or degradation. Bacteria were most frequently detected
and showed high alpha- and beta-diversity. Members of the
Actinobacteria, Proteobacteria, Bacteroidetes and Gemmatimonadetes phyla
were found in the majority of samples. Archaea alpha- and beta-diversity
was very low. For Eukarya, a diverse range of organisms was identified,
such as fungi, green algae and several phyla of Protozoa. Phylogenetic
analysis revealed an extraordinary variety of putative extremophiles,
mainly Bacteria but also Archaea and Eukarya. These comprised
radioresistant, endolithic, chasmolithic, xerophilic, hypolithic,
thermophilic, thermoacidophilic, psychrophilic, halophilic,
haloalkaliphilic and alkaliphilic micro-organisms. Overall, our data
revealed large difference in occurrence and diversity over short
distances, indicating the need for high-sampling frequency at similar
sites. DNA extraction methods need to be optimized to improve extraction
efficiencies.
@--------------------------------------------------------------------
Title: PCR-based analysis of microbial communities during
the EuroGeoMars campaign at Mars Desert Research
Station, Utah
Authors: Thiel, Cora S.; Ehrenfreund, Pascale; Foing, Bernard;
Pletser, Vladimir; Ullrich, Oliver
Bibliographic Code: 2011IJAsB..10..177T
Abstract
The search for evidence of past or present life on Mars will require the
detection of markers that indicate the presence of life. Because
deoxyribonucleic acid (DNA) is found in all known living organisms, it
is considered to be a `biosignature' of life. The main
function of DNA is the long-term storage of genetic information, which
is passed on from generation to generation as hereditary material. The
Polymerase Chain Reaction (PCR) is a revolutionary technique which
allows a single fragment or a small number of fragments of a DNA
molecule to be amplified millions of times, making it possible to detect
minimal traces of DNA. The compactness of the contemporary PCR
instruments makes routine sample analysis possible with a minimum amount
of laboratory space. Furthermore the technique is effective, robust and
straightforward. Our goal was to establish a routine for the detection
of DNA from micro-organisms using the PCR technique during the
EuroGeoMars simulation campaign. This took place at the Mars Society's
Mars Desert Research Station (MDRS) in Utah in February 2009 (organized
with the support of the International Lunar Exploration Working Group
(ILEWG), NASA Ames and the European Space Research and Technology Centre
(ESTEC)). During the MDRS simulation, we showed that it is possible to
establish a minimal molecular biology lab in the habitat for the
immediate on-site analysis of samples by PCR after sample collection.
Soil and water samples were taken at different locations and soil
depths. The sample analysis was started immediately after the crew
returned to the habitat laboratory. DNA was isolated from
micro-organisms and used as a template for PCR analysis of the highly
conserved ribosomal DNA to identify representatives of the different
groups of micro-organisms (bacteria, archaea and eukarya). The PCR
products were visualized by agarose gel electrophoresis and documented
by transillumination and digital imaging. The microbial diversity in the
collected samples was analysed with respect to sampling depth and the
presence or absence of vegetation. For the first time, we have
demonstrated that it is possible to perform direct on-site DNA analysis
by PCR at MDRS, a simulated planetary habitat in an extreme environment
that serves as a model for preparation and optimization of techniques to
be used for future Mars exploration.
@--------------------------------------------------------------------
Title: Field astrobiology research in Moon-Mars analogue
environments: instruments and methods
Authors: Foing, B. H.; Stoker, C.; Zavaleta, J.;
Ehrenfreund, P.; Thiel, C.; Sarrazin, P.; Blake, D.;
Page, J.; Pletser, V.; Hendrikse, J.; Direito, S.;
Kotler, J. M.; Martins, Z.; Orzechowska, G.;
Gross, C.; Wendt, L.; Clarke, J.; Borst, A. M.;
Peters, S. T. M.; Wilhelm, M.-B.; Davies, G. R.;
Davies
Bibliographic Code: 2011IJAsB..10..141F
Abstract
We describe the field demonstration of astrobiology instruments and
research methods conducted in and from the Mars Desert Research Station
(MDRS) in Utah during the EuroGeoMars campaign 2009 coordinated by
ILEWG, ESA/ESTEC and NASA Ames, with the contribution of academic
partners. We discuss the entire experimental approach from determining
the geological context using remote sensing, in situ measurements,
sorties with sample collection and characterization, analysis in the
field laboratory, to the post sample analysis using advanced laboratory
facilities.
We present the rationale for terrestrial field campaigns to strengthen
astrobiology research and the link between in situ and orbital remote
sensing data. These campaigns are supporting the preparation for future
missions such as Mars Science Laboratory, ExoMars or Mars Sample Return.
We describe the EuroGeoMars 2009 campaign conducted by MDRS crew 76 and
77, focused on the investigation of surface processes in their
geological context. Special emphasis was placed on sample collection and
pre-screening using in-situ portable instruments. Science investigations
included geological and geochemical measurements as well as detection
and diagnostic of water, oxidants, organic matter, minerals, volatiles
and biota.
EuroGeoMars 2009 was an example of a Moon-Mars field research campaign
dedicated to the demonstration of astrobiology instruments and a
specific methodology of comprehensive measurements from selected
sampling sites. We discuss in sequence: the campaign objectives and
trade-off based on science, technical or operational constraints. This
includes remote sensing data and maps, and geological context; the
monitoring of environmental parameters; the geophysical context and
mineralogy studies; geology and geomorphology investigations;
geochemistry characterization and subsurface studies.
We describe sample handling (extraction and collection) methods, and the
sample analysis of soils and rocks performed in the MDRS laboratory
using close inspection, initial petrological characterization,
microscopy, Visible-NIR spectrometry, Raman spectrometry, X-ray
diffraction/X-ray fluorescence spectrometry, soil analysis,
electrochemical and biological measurements.
The results from post-mission analysis of returned samples using
advanced facilities in collaborator institutes are described in
companion papers in this issue. We present examples of in-situ analysis,
and describe an example investigation on the exploration and analysis of
endolithic microbial mats (from reconnaissance, in-situ imaging,
sampling, local analysis to post-mission sample analysis).
@--------------------------------------------------------------------
Title: Astrobiology field research in Moon/Mars analogue
environments
Authors: Foing, B. H.; Stoker, C.; Ehrenfreund, P.
Bibliographic Code: 2011IJAsB..10..137F
Abstract
Extreme environments on Earth often provide similar terrain conditions
to landing/operation sites on Moon and Mars. Several field campaigns
(EuroGeoMars2009 and DOMMEX/ILEWG EuroMoonMars from November 2009 to
March 2010) were conducted at the Mars Desert Research Station (MDRS) in
Utah. Some of the key astrobiology results are presented in this special
issue on `Astrobiology field research in Moon/Mars analogue
environments' relevant to investigate the link between geology,
minerals, organics and biota. Preliminary results from a
multidisciplinary field campaign at Rio Tinto in Spain are presented.
@--------------------------------------------------------------------
Title: Lunar mare single-scattering, porosity, and
surface-roughness properties with SMART-1 AMIE
Authors: Muinonen, K.; Parviainen, H.; Näränen, J.;
Josset, J.-L.; Beauvivre, S.; Pinet, P.; Chevrel, S.;
Koschny, D.; Grieger, B.;
Foing, B. AMIE SMART-1 Team
Bibliographic Code: 2011A&A...531A.150M
Abstract
A novel shadowing and coherent-backscattering model is utilized in the
analysis of the single-scattering albedos and phase functions, local
surface roughness, and regolith porosity of specific lunar mare regions
imaged by the AMIE camera (Advanced Moon micro-Imager Experiment)
onboard ESA SMART-1 mission. Shadowing due to the regolith particles is
accounted via ray-tracing computations for densely-packed particulate
media with a fractional-Brownian-motion interface with free space. The
shadowing modeling allows us to derive the scattering phase function for
a ~100-mum volume element of the lunar mare regolith. The
volume-element phase function is explained by coherent-backscattering
modeling, where the fundamental single scatterers are the
wavelength-scale particle inhomogeneities or the smallest fraction of
the particles on the lunar surface. The phase function of the
fundamental scatterers is expressed as a sum of two Henyey-Greenstein
terms, accounting for increased backward scattering as well as increased
forward scattering. Based on the modeling of the AMIE lunar photometry,
we conclude that most of the lunar mare opposition effect is caused by
coherent backscattering within volume elements comparable in size to
typical lunar particles, with only a small contribution from shadowing
effects.
@--------------------------------------------------------------------
Title: Linear and circular spectropolarimetry of diffuse
interstellar bands
Authors: Cox, N. L. J.; Ehrenfreund, P.; Foing, B. H.;
D'Hendecourt, L.; Salama, F.; Sarre, P. J.
Bibliographic Code: 2011A&A...531A..25C, eprint = 1104.4581
Abstract
Context. The identification of the carriers of diffuse interstellar
bands (DIBs) remains one of the long-standing mysteries in astronomy.
The detection of a polarisation signal in a DIB profile can be used to
distinguish between a dust or gas-phase carrier. The polarisation
profile can give additional information on the grain or molecular
properties of the absorber.
Aims: To measure the polarisation
efficiency of the carriers of the diffuse interstellar bands.
Methods: In order to detect and measure the linear and circular
polarisation of the DIBs we observed reddened lines of sight showing
continuum polarisation. For this study we selected two stars HD
197770 and HD 194279. We used
high-resolution (R ~ 64 000) spectropolarimetry in the wavelength range
from 3700 to 10 480 Å with the ESPaDOnS échelle
spectrograph mounted at the CFHT.
Results: High S/N and high
resolution Stokes V (circular), Q and U (linear) spectra were obtained.
We constrained upper limits by a factor of 10 for previously observed
DIBs. Furthermore, we analysed ~30 additional DIBs for which no
spectropolarimetry data has been obtained before. This included the 9577
Å DIB and the 8621 Å DIB. The former is attributed to the
C60^+ fullerene, which could become aligned in a magnetic
field. The latter shows a tight correlation with the amount of dust in
the line-of-sight and therefore most likely may show a polarisation
signal related the aligned grains.
Conclusions: The lack of
polarisation in 45 DIB profiles suggests that none of the absorption
lines is induced by a grain-type carrier. The strict upper limits, less
than ~0.01%, derived for the observed lines-of-sight imply that if DIBs
are due to gas-phase molecules these carriers have polarisation
efficiencies which are at least 6 times, and up to 300 times, smaller
than those predicted for grain-related carriers.
Based on observations obtained at the Canada-France-Hawaii Telescope
(CFHT) which is operated by the National Research Council of Canada, the
Institut National des Sciences de l'Univers of the Centre National de la
Recherche Scientique of France, and the University of Hawaii.Appendices
are available in electronic form at http://www.aanda.orgIntensity and
polarisation spectra are only available at the CDS via anonymous ftp to
cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/531/A25
@--------------------------------------------------------------------
Title: The ORGANIC Experiment on the ISS EXPOSE-R
Authors: Bryson, K.; Peeters, Z.; Salama, F.; Foing, B.;
Ehrenfreund, P.; Jessberger, E.; Bischoff, A.;
Breitfellner, M.; Schmidt, W.
Bibliographic Code: 2011IAUS..280P.401B
Abstract
Polycyclic aromatic hydrocarbons (PAHs) and aromatic networks are among
the most abundant organic material in space. PAHs and fullerenes have
been identified in meteorites and are proposed as carriers for numerous
astronomical absorption and emission features. Recently the fullerenes
C60 and C70 have been discovered in a young planetary nebula, Tc 1 and
in other astronomical environments. Thin films of selected PAHs and
fullerenes have been subjected to the low Earth orbit environment as
part of the ORGANIC experiment on the multi-user facility EXPOSE-R,
which was deployed onboard the International Space Station (ISS) in
March 2009 and retrieved by extra-vehicular activity (EVA) in January
2011. The ORGANIC experiment monitors the chemical evolution, survival,
destruction, and chemical modification of PAHs and fullerenes exposed to
solar illumination and cosmic radiation. The radiation dose that is
collected on the ISS by the samples cannot be accurately simulated in
Earth laboratories. Dark samples are shielded from the UV photons and
will enable us to differentiate between the effects of exposure to
photons and cosmic rays. The samples are monitored before and after
space exposure; ground control samples were continuously monitored. We
describe the ORGANIC experiment on the Space Station and report on
laboratory ground-control measurements in the UV-Vis-NIR at NASA-Ames.
Extended space exposure allows us to collect data on multiple samples
which can be extrapolated to other astrophysical environments and thus
greatly enhance our knowledge on the evolution of organic compounds in
space environment.
@--------------------------------------------------------------------
Title: Astrobiology and Habitability Studies Supporting
Mars Research and Missions
Authors: Foing, B. H.; Thiel, C.; Direito, S.;
Ehrenfreund, P.; Roling, W.; Martins, Z.;
Sephton, M.; Stoker, C.; Zhavaleta, J.;
Orzechowska, G.; Kidd, R.; Quinn, R.; Kotler, M.;
Eurogeomars Mdrs Team
Bibliographic Code: 2011LPI....42.1762F
Abstract
During EuroGeoMars 2009 campaign, we characterized the mineralogy,
organic compounds and microbiology of selected samples from different
geological sites, and established correlations (Special Issue:
``Astrobiology field research in Moon/Mars analog
environments'': IJA 2011).
@--------------------------------------------------------------------
Title: Properties of Subsurface Soil Cores from Four
Geologic Provinces Surrounding Mars Desert Research
Station, Utah: Characterizing Analog Martian Soil in
a Human Exploration Scenario
Authors: Stoker, C. R.; Clarke, J. D. A.; Direito, S.;
Foing, B.
Bibliographic Code: 2011LPI....42.1231S
Abstract
We present results of analysis of sulfate-rich soil cores from Mars
analog site in Utah.
@--------------------------------------------------------------------
Title: Bioaugmentation in growing plants for lunar bases
Authors: Zaets, I.; Burlak, O.; Rogutskyy, I.; Vasilenko, A.;
Mytrokhyn, O.; Lukashov, D.; Foing, B.;
Kozyrovska, N.
Bibliographic Code: 2011AdSpR..47.1071Z
Abstract
Microorganisms may be a key element in a precursory scenario of growing
pioneer plants for extraterrestrial exploration. They can be used for
plant inoculation to leach nutritional elements from regolith, to
alleviate lunar stressors, as well as to decompose both lunar rocks and
the plant straw in order to form a protosoil. Bioleaching capacities of
both French marigold (Tagetes patula L.) and the associated bacteria in
contact with a lunar rock simulant (terrestrial anorthosite) were
examined using the model plant-bacteria microcosms under controlled
conditions. Marigold accumulated K, Na, Fe, Zn, Ni, and Cr at higher
concentrations in anorthosite compared to the podzol soil. Plants
inoculated with the consortium of well-defined species of bacteria
accumulated higher levels of K, Mg, and Mn, but lower levels of Ni, Cr,
Zn, Na, Ca, Fe, which exist at higher levels in anorthosite. Bacteria
also affected the &\#1057;&\#1072;/Mg and Fe/Mn ratios in the biomass of
marigold grown on anorthosite. Despite their growth retardation, the
inoculated plants had 15% higher weight on anorthosite than
noninoculated plants. The data suggest that the bacteria supplied basic
macro-and microelements to the model plant.
@--------------------------------------------------------------------
Title: Linear and circular polarisation of diffuse
interstellar bands.
Authors: Cox, N. L. J.; Ehrenfreund, P.; Foing, B. H.;
D'Hendecourt, L.; Salama, F.; Sarre, P. J.
Bibliographic Code: 2011yCat..35319025C
Abstract
Linear and circular polarisation and total intensity spectra obtained
with ESPaDOnS at the CFHT for the two lines-of-sight towards HD197770
and HD194279. For each line-of-sight we give the average (globally
normalised) Stokes I, Q, U, and V spectra. The spectra cover the
wavelength range from 376nm to 1000nm.
(2 data files).
@--------------------------------------------------------------------
Title: Fullerenes and Cosmic Carbon
Authors: Ehrenfreund, P.; Foing, B. H.
Bibliographic Code: 2010Sci...329.1159E
Abstract
@--------------------------------------------------------------------
Title: Beijing Lunar Declaration 2010: B) Technology and
Resources; Infrastructures and Human Aspects; Moon,
Space and Society
Authors: Arvidson, R.; Foing, B. H.; Blamont, J. E.;
Plescia, J.; Cohen, B.; Gluc-Iceum1 Participants
Bibliographic Code: 2010LPICo1595....4A
Abstract
@--------------------------------------------------------------------
Title: Beijing Lunar Declaration 2010: A) GLUC-ICEUM11
Report and Recommendations on Science and
Exploration
Authors: Arvidson, R.; Foing, B. H.; Cohen, B.; Plescia, J.;
Blamont, J. E.; Gluc-Iceum1 Participants
Bibliographic Code: 2010LPICo1595....3A
Abstract
@--------------------------------------------------------------------
Title: Investigation in Mars analogue habitats of the
Transantarctic Mountains of Victoria Land
Authors: de Vera, J.-P. P.; Foing, B.; Ullrich, E.; Ott, S.
Bibliographic Code: 2010epsc.conf..145D
Abstract
@--------------------------------------------------------------------
Title: Lunar single-scattering, porosity, and
surface-roughness characteristics with SMART-1/AMIE
Authors: Näränen, J.; Parviainen, H.; Muinonen, K.;
Josset, J.-L.; Beauvivre, S.; Pinet, P.; Chevrel, S.;
Koschny, D.; Grieger, B.; Foing, B.
Bibliographic Code: 2010els..conf..202N
Abstract
@--------------------------------------------------------------------
Title: 3D structure of the Gusev Crater region
Authors: Parker, Mirjam Van Kan; Zegers, Tanja;
Kneissl, Thomas; Ivanov, Boris; Foing, Bernard;
Neukum, Gerhard
Bibliographic Code: 2010E&PSL.294..411P
Abstract
Gusev Crater lies within the Aeolis Quadrangle of Mars at the boundary
between the northern lowlands and southern highlands. The ancient valley
Ma'adim Vallis dissects the highlands south of Gusev Crater and is
thought to have fed the crater with sediments. High Resolution Stereo
Camera data and Digital Elevation Models were used to construct a
geologic-geomorphic map (173.5-178.5° E, 10-18° S) and
cross-sections, complemented by data from Mars Orbiter Camera, Mars
Orbiter Laser Altimeter and Thermal Emission Imaging System. Three
geologic domains are recognised: the highlands in the south, Gusev
Crater and lowlands in the north. Twelve units are mapped, with
thicknesses ranging from hundred meters to several kilometres.
Thicknesses of units, and their bedding attitude, are estimated
combining the geologic map and topographic information. Relative ages
are determined from crater counts, ranging from Early Noachian for
highland units to Middle Amazonian for units in Gusev Crater and in
lowlands. Episodes of intense geologic activity (deposition, volcanism,
deformation) occur at around 4.0 Ga, 3.7 Ga, and 3.5 Ga. Comparing the
geometry of the Gusev Crater with similar sized, filled and un-filled,
Martian craters, suggests that the Columbia Hills are relics of the
original central peak of Gusev Crater.
@--------------------------------------------------------------------
Title: The SMART-1 lunar impact
Authors: Burchell, M. J.; Robin-Williams, R.; Foing, B. H.
Bibliographic Code: 2010Icar..207...28B
Abstract
The SMART-1 spacecraft impacted the Moon on 3rd September 2006 at a
speed of 2 km s-1 and at a very shallow angle of
incidence (˜1°). The resulting impact crater is too small to
be viewed from the Earth; accordingly, the general crater size and shape
have been determined here by laboratory impact experiments at the same
speed and angle of incidence combined with extrapolating to the correct
size scale to match the SMART-1 impact. This predicts a highly
asymmetric crater approximately 5.5-26 m long, 1.9-9 m wide,
0.23-1.5 m deep and 0.71-6.9 m3 volume. Some of
the excavated mass will have gone into crater rim walls, but
0.64-6.3 m3 would have been ejecta on ballistic
trajectories corresponding to a cloud of 2200-21,800 kg of lunar
material moving away from the impact site. The shallow Messier crater on
the Moon is similarly asymmetric and is usually taken as arising from a
highly oblique impact. The light flash from the impact and the
associated ejecta plume were observed from Earth, but the flash
magnitude was not obtained, so it is not possible to obtain the luminous
efficiency of the impact event.
@--------------------------------------------------------------------
Title: SMART-1 New Results from 2009-2010
Authors: Foing, Bernard
Bibliographic Code: 2010EGUGA..1213886F
Abstract
We present highlights and new SMART-1 results published or obtained in
2009-2010 that are relevant for lunar science and future exploration, in
relation with subsequent missions and future landers. SMART-1 is the
first of ESA's Small Missions for Advanced Research and Technology
[1,2,3]. Its prime objective has been achieved to demonstrate Solar
Electric missions (such as Bepi-Colombo) and to test new technologies
for spacecraft and instruments. The SMART-1 spacecraft was launched in
2003, as Ariane-5 auxiliary passenger, and reached on 15 March 2005 a
lunar orbit 400-3000 km for a nominal science period of six months, with
1 year extension until impact on 3 September 2006. New SMART-1 lunar
science and exploration results since 2009 include: - Multiangular
photometry of Mare regions allowing to model scattering in planetary
regoliths - The study of specific regions at different phase angles
allowed to detect variations in regolith roughness - Lunar North and
South polar maps and repeated high resolution images have been obtained,
giving a monitoring of illumination to study potential sites relevant
for future exploration. This permitted to identify SMART-1 peaks of
quasi-eternal light and to derive their topography. - The SMART-1
archive observations have been used to support Kaguya, Chandrayaan-1,
Chang'E 1, the US Lunar Reconnaissance Orbiter, the LCROSS impact, and
to prepare subsequent landers and future human activities and lunar
bases. References: [1] Foing, B. et al (2001) Earth Moon Planets, 85,
523 . [2] Racca, G.D. et al. (2002) Earth Moon Planets, 85, 379. [3]
Racca, G.D. et al. (2002) PSS, 50, 1323. [4] Grande, M. et al. (2003)
PSS, 51, 427. [5] Dunkin, S. et al. (2003) PSS, 51, 435. [6] Huovelin,
J. et al. (2002) PSS, 50, 1345. [7] Shkuratov, Y. et al (2003) JGRE 108,
E4, 1. [8] Foing, B.H. et al (2003) Adv. Space Res., 31, 2323. [9]
Grande, M. et al (2007) PSS 55, 494. [10] Pinet, P. et al (2005) PSS,
53, 1309. [11] Josset J.L. et al (2006) Adv Space Res, 37, 14. [12]
Foing B.H. et al (2006) Adv Space Res, 37, 6. Co-authors: B.H. Foing,
B. Grieger, D. Koschny, J.-L. Josset, S. Beauvivre, V. Kaydash, Y.
Shkuratov, K. Muinonen, U. Mall, A. Nathues, B. Kellett, P. Pinet, S.
Chevrel, P. Cerroni, M.C. de Sanctis, M.A. Barucci, S. Erard, D. Despan,
V. Shevchenko, S. Peters, A. Borst, F. Bexkens, M. Almeida, D. Frew,
J.Volp, D. Heather, SMART1 Science Technology Working Team, ESTEC/SRE-S,
postbus 299, 2200 AG Noordwijk, NL, Europe
@--------------------------------------------------------------------
Title: ExoGeoLab Pilot Project for Landers, Rovers and
Instruments
Authors: Foing, Bernard
Bibliographic Code: 2010EGUGA..1213779F
Abstract
We have developed a pilot facility with a Robotic Test Bench (ExoGeoLab)
and a Mobile Lab Habitat (ExoHab). They can be used to validate concepts
and external instruments from partner institutes. The ExoGeoLab research
incubator project, has started in the frame of a collaboration between
ILEWG (International Lunar Exploration working Group
http://sci.esa.int/ilewg), ESTEC, NASA and academic partners, supported
by a design and control desk in the European Space Incubator (ESI), as
well as infrastructure. ExoGeoLab includes a sequence of technology and
research pilot project activities: - Data analysis and interpretation
of remote sensing and in-situ data, and merging of multi-scale data sets
- Procurement and integration of geophysical, geo-chemical and
astrobiological breadboard instruments on a surface station and rovers -
Integration of cameras, environment and solar sensors, Visible and near
IR spectrometer, Raman spectrometer, sample handling, cooperative rovers
- Delivery of a generic small planetary lander demonstrator (ExoGeoLab
lander, Sept 2009) as a platform for multi-instruments tests - Research
operations and exploitation of ExoGeoLab test bench for various
conceptual configurations, and support for definition and design of
science surface packages (Moon, Mars, NEOs, outer moons) - Field tests
of lander, rovers and instruments in analogue sites (Utah MDRS 2009
& 2010, Eifel volcanic park in Sept 2009, and future campaigns).
Co-authors, ILEWG ExoGeoLab & ExoHab Team: B.H. Foing(1,11)*\#, C.
Stoker(2,11)*, P. Ehrenfreund(10,11), L. Boche-Sauvan(1,11)*, L.
Wendt(8)*, C. Gross(8, 11)*, C. Thiel(9)*, S. Peters(1,6)*, A.
Borst(1,6)*, J. Zavaleta(2)*, P. Sarrazin(2)*, D. Blake(2), J.
Page(1,4,11), V. Pletser(5,11)*, E. Monaghan(1)*, P. Mahapatra(1)\#, A.
Noroozi(3), P. Giannopoulos(1,11) , A. Calzada(1,6,11), R. Walker(7), T.
Zegers(1, 15) \#, G. Groemer(12)\# , W. Stumptner(12)\#, B. Foing(2,5), J.
K. Blom(3)\#, A. Perrin(14)\#, M. Mikolajczak(14)\#, S. Chevrier(14)\#, S.
Direito(6)\#, S. Voute (15)\#, A. Olmedo-Soler(17)\#, T. E. Zegers(1,
15)\#, D. Scheer(12)\#, K. Bickert(12)\#, D. Schildhammer(12)\#, B.
Jantscher(1, 11, 12)\#, MECA Team(6)\#, ExoGeoLab ILEWG ExoHab
teams(1,4,11) EuroGeoMars team(1,4,5); 1)ESTEC/SRE-S Postbus 299, 2200
AG Noordwijk, NL, 2)NASA Ames, 3)Delft TU, 4)ESTEC TEC Technology
Dir., 5)ESTEC HSF Human Spaceflight, 6)VU Amsterdam, 7)ESTEC Education
Office, 8)FU Berlin, 9)Max Planck Goettingen, 10)Leiden/GWU, 11)ILEWG
ExoHab Team, 12)Austrian Space Forum (OEWF Innsbruck); 14) Ecole de
l'Air, Salons de Provence, 15) Utrecht U., 16) MECA Team, 17) Olmedo
Knowledge Systems S.L.; * EuroGeoMars Utah crew, \# ILEWG Eifel crew,
EuroMoonMars/DOMMEX Utah crew.
@--------------------------------------------------------------------
Title: ExoHab Pilot Project & Field Tests for Moon-Mars
Human Laboratories
Authors: Foing, Bernard
Bibliographic Code: 2010EGUGA..1213688F
Abstract
We studied concepts for a minimal Moon-Mars habitat, in focussing on the
system aspects and coordinating every different part as part an evolving
architecture. We validated experimentally the Habitat and Laboratory
ExoHab concept constraints during EuroGeoMars campaign in Utah desert
research station (from 24 Jan. to 28 Feb. 2009) and EuroMoonMars/DOMMEX
campaigns in Nov 2009 and February-April 2010. We discuss from the ILEWG
ExoHab concept studies and field simulations the specifics of human
exploration, with focus on habitability and human performance. In the
ExoHab pilot concept project (supported by ILEWG, ESA NASA), we justify
the case for a scientific and exploration outpost allowing experiments,
sample analysis in laboratory (relevant to the origin and evolution of
planets and life, geophysical and geo-chemical studies, astrobiology and
life sciences, observation sciences, technology demonstration, resource
utilisation, human exploration and settlement). In this modular concept,
we consider various infra structure elements: core habitat, Extra
Vehicular activity (EVA), crew mobility, energy supply, recycling
module, communication, green house and food production, operations. We
review some studies space agencies' architecture proposals, with
landers, orbiters, rovers, habitats, surface operations and protocols.
We focus on the easiest and the soonest way in settling a minimal base
immediately operational in scientific experimentation and exploration,
but not immediately autonomous. Through a modular concept, this outpost
will be possibly evolved into a long duration or permanent base. We will
analyse the possibilities of settling such a minimal base by means of
the current and near term propulsion technology, as a full Ariane 5 ME
carrying 1.7 T of gross payload to the surface of the Moon (Integrated
Exploration Study, ESA ESTEC [1,2]). The low solar rays incidence may
permit having ice in deep craters, which will be beneficial for the
evolution of the outpost into an autonomous base. After a robotic sample
return mission, a human presence will allow deeper research through well
chosen geological samples. A polar lunar outpost can serve to prepare
for a Mars outpost: system and crew safety aspects, use of local
resources, operations on farside with limited communication to Earth,
planetary protection protocol, astrobiology and life sciences.
References: [1] Exploration Architecture Trade Report", ESA 2008. [2]
Integrated Exploration Architecture", ESA, 2008. [3] 9th ILEWG
International Conference on Exploration Utilization of the moon, 2007,
sci.esa.int/ilewg [4] Schrunk et al, The Moon: Resources, Future
Development and Colonization", 1999. [5] The Moon as a Platform for
Astronomy and Space Science", B.H. Foing, ASR 14 (6), 1994. [6]
Boche-Sauvan L., Foing B (2008) MSc/ESTEC report. Co-authors, ILEWG
ExoGeoLab & ExoHab Team: B.H. Foing(1,11)*\#, C. Stoker(2,11)*, P.
Ehrenfreund(10,11), L. Boche-Sauvan(1,11)*, L. Wendt(8)*, C. Gross(8,
11)*, C. Thiel(9)*, S. Peters(1,6)*, A. Borst(1,6)*, J. Zavaleta(2)*, P.
Sarrazin(2)*, D. Blake(2), J. Page(1,4,11), V. Pletser(5,11)*, E.
Monaghan(1)*, P. Mahapatra(1)\#, A. Noroozi(3), P. Giannopoulos(1,11) ,
A. Calzada(1,6,11), R. Walker(7), T. Zegers(1, 15) \#, G. Groemer(12)\# ,
W. Stumptner(12)\#, B. Foing(2,5), J. K. Blom(3)\#, A. Perrin(14)\#, M.
Mikolajczak(14)\#, S. Chevrier(14)\#, S. Direito(6)\#, S. Voute (18)\#, A.
Olmedo-Soler(17)\#, T. E. Zegers(1, 18)\#, D. Scheer(12)\#, K.
Bickert(12)\#, D. Schildhammer(12)\#, B. Jantscher(1, 11, 12)\#, MECA
Team(6)\#, ExoGeoLab ILEWG ExoHab teams(1,4,11) EuroGeoMars team(1,4,5);
1)ESTEC/SRE-S Postbus 299, 2200 AG Noordwijk, NL, 2)NASA Ames, 3)Delft
TU, 4)ESTEC TEC Technology Dir., 5)ESTEC HSF Human Spaceflight, 6)VU
Amsterdam, 7)ESTEC Education Office, 8)FU Berlin, 9)Max Planck
Goettingen, 10)Leiden/GWU, 11)ILEWG ExoHab Team, 12)Austrian Space
Forum (OEWF Innsbruck); 14) Ecole de l'Air, Salons de Provence, 15)
Utrecht U., 16) MECA Team, 17) Olmedo Knowledge Systems S.L.; *
EuroGeoMars Utah crew, \# ILEWG Eifel crew, EuroMoonMars/DOMMEX Utah
crew.
@--------------------------------------------------------------------
Title: UV and Space Exposure of Aromatic Compounds on the
EXPOSE-R Facility Onboard the International Space
Station
Authors: Bryson, Kathryn; Salama, F.; Ehrenfreund, P.;
Ricco, A. J.; Peeters, Z.; Foing, B.; Jessberger, E.;
Robert, F.; Mumma, M.
Bibliographic Code: 2010AAS...21641106B
Abstract
Aromatic networks are likely the most abundant organic material in
space. Specifically, polycyclic aromatic hydrocarbons (PAHs) and
fullerenes have been identified in meteorites and are thought to be
among the carriers for numerous astronomical absorption and emission
features. Thin films of selected PAHs and fullerenes are being subjected
to the low Earth orbit environment as part of the Organics experiment on
the multi-user facility EXPOSE-R, which has been deployed onboard the
International Space Station since March 2009 and will be retrieved in
Fall 2010. The Organics experiment monitors the chemical evolution,
survival, destruction, and chemical modification of PAHs and fullerenes
exposed to solar illumination and cosmic radiation. The radiation dose
that is collected by the samples during flight exceeds the limits of
simulations in the laboratory and will greatly enhance our knowledge on
the evolution of large molecules in space environments. Dark samples are
shielded from the UV photons and will enable us to differentiate between
the effects of exposure to photons and cosmic rays. The samples are
monitored before and after space exposure. We present spectra measured
in the UV-Vis-NIR range of ground control samples and flight samples.
@--------------------------------------------------------------------
Title: Eurogeomars Field Campaingn: Sample Analysis of
Organic Matter and Minerals
Authors: Foing, B. H.; Stoker, C.; Zhavaleta, J.;
Ehrenfreund, P.; Quinn, R.; Blake, D.; Martins, Z.;
Sephton, M.; Becker, L.; Orzechowska, G.;
van Sluis, C.; Boche-Sauban, L.; Gross, C.;
Thiel, C.; Wendt, L.; Sarrazin, P.; Mahapatra, P.;
Direito, S.; Roling, W.; Eurogeomars Mdrs Team
Bibliographic Code: 2010LPICo1538.5656F
Abstract
A strategic search for life on Mars requires a thorough
interdisciplinary preparation phase that include the optimization of
sample analysis techniques, instrument development and calibration and
extensive terrestrial field test at Mars analog sites.
@--------------------------------------------------------------------
Title: Sample Collection and Analysis from CAREX Field
Workshop at Rio Tinto
Authors: Direito, S.; Foing, B. H.; Mahapatra, P.; Gomez, F.;
Rull, F.; Carex Rio Tinto 2009 Workshop
Bibliographic Code: 2010LPICo1538.5648D
Abstract
We described the sample collection protocol, multi- measurements
techniques and selected results (using Ramand and visible NIR
spectrometer) and interpretation from a CAREX field workshop at Rio
Tinto in september 2009.
@--------------------------------------------------------------------
Title: ExoHab and EuroGeoMars Campaigns: Human Exploration
and Astrobiology
Authors: Foing, B. H.; Boche-Sauvan, L.; Stoker, C.;
Ehrenfreund, P.; Wendt, L.; Gross, C.; Thiel, C.;
Peters, S.; Borst, A.; Zhavaleta, J.; Sarrazin, P.;
Blake, D.; Page, J.; Pletser, V.; Monaghan, E.;
Mahapatra, P.; Wills, D.; Noroozi, A.; Walker, R.;
Zegers, T.; Exogeolab; Exohab Team; Eurogeomars Team
Bibliographic Code: 2010LPICo1538.5625F
Abstract
We studied concepts for a minimal ExoHab habitat, in focussing on the
system aspects and as part of an evolving architecture. We validated
experimentally the ExoHab concept during EuroGeoMars campaign in Utah
desert research station (24 Jan. to 28 Feb. 2009).
@--------------------------------------------------------------------
Title: The Organics Experiment on EXPOSE-R
Authors: Bryson, K. L.; Peeters, Z.; Salama, F.;
Ehrenfreund, P.; Foing, B.; Ricco, A. J.;
Monaghan, E.; Willis, D.; Breitfellner, M.;
Jessberger, E.; Robert, F.; Mumma, M.
Bibliographic Code: 2010LPICo1538.5513B
Abstract
Thin films of selected PAHs and fullerenes are being subjected to the
low Earth orbit environment as part of the Organics experiment on the
multi-user facility EXPOSE-R onboard the International Space Station.
@--------------------------------------------------------------------
Title: ExoGeoLab Test Bench for Landers, Rovers and
Astrobiology Instruments
Authors: Foing, B. H.; Mahapatra, P.; Boche-Sauvan, L.;
Som, S.; Page, J.; Stoker, C.; Zhavaleta, J.;
Sarrazin, P.; Blake, D.; Poulakis, P.; Visentin, G.;
Noroozi, A.; Ehrenfreund, P.; Barton, A.;
Lebreton, J. P.; Zegers, T.; Koschny, D.; Peters, S.;
Borst, A.; Monaghan, E.; Wills, D.; Thiel, C.;
Wendt, L.; Gross, C.; Nijman, F.; Pletser, V.;
McKay, C.; Davies, G.; van Westrenen, W.;
Batenburg, P.; Drijkoningen, G.; Slob, E.; Gill, E.;
Guglielmi, M.; Freire, M.; Walker, R.;
Exogeolab Team
Bibliographic Code: 2010LPICo1538.5477F
Abstract
ExoGeoLab is a Robotic Test Bench used to validate concepts and
instruments packages that could help in the technical research and
science preparation of lander and rover missions for astrobiology.
@--------------------------------------------------------------------
Title: Photosynthesis and Its Implications for Space
Research
Authors: de Vera, J. P. P.; Leya, T.; Lorek, A.; Koncz, A.;
de La Torre Noetzel, R.; Kozyrovska, N.; Burlak, O.;
Foing, B.
Bibliographic Code: 2010LPICo1538.5139D
Abstract
Photosynthesis is useful for biosignature definition, for the definition
of the habitability of a planet, for research on the likelihood of
Panspermia and for use in manned space flight missions by integration
into life supporting systems.
@--------------------------------------------------------------------
Title: Testing Portable Raman Spectrometry for Astrobiology
Authors: Som, S. M.; Foing, B. H.; Exogeolab Team
Bibliographic Code: 2010LPICo1538.5085S
Abstract
We report on results of mineralogical, petrological and biological
samples using a 785nm DeltaNu Rockhound portable Raman spectrometer.
@--------------------------------------------------------------------
Title: Geochemical Results from EuroGeoMars MDRS Utah 2009
Campaign
Authors: Borst, A.; Peters, S.; Foing, B. H.; Stoker, C.;
Wendt, L.; Gross, C.; Zavaleta, J.; Sarrazin, P.;
Blake, D.; Ehrenfreund, P.; Boche-Sauvan, L.;
Page, J.; McKay, C.; Batenburg, P.; Drijkoningen, G.;
Slob, E.; Poulakis, P.; Visentin, G.; Noroozi, A.;
Gill, E.; Guglielmi, M.; Freire, M.; Walker, R.;
Sabbatini, M.; Pletser, V.; Monaghan, E.; Ernst, R.;
Oosthoek, J.; Mahapatra, P.; Wills, D.; Thiel, C.;
Lebreton, J. P.; Zegers, T.; Chicarro, A.;
Koschny, D.; Vago, J.; Svedhem, H.; Davies, G.;
Westenberg, A.; Edwards, J.; Exogeolab Team;
Eurogeomars Team
Bibliographic Code: 2010LPI....41.2744B
Abstract
We report on the geochemistry investigations during the EuroGeoMars
Campaign at the MDRS station in Utah. A total of ~150 samples from
different lithologies were analyzed using advanced and miniaturized
instruments (XRF, Raman and spectrometers).
@--------------------------------------------------------------------
Title: Drilling on the Moon and Mars: Developing the
Science Approach for Subsurface Exploration with
Human Crews
Authors: Stoker, C. R.; Zavaleta, J.; Bell, M.; Direto, S.;
Foing, B.; Blake, D.; Kim, S.
Bibliographic Code: 2010LPI....41.2697S
Abstract
The paper describes first results from DOMEX, an analog mission to
develop the approach for using human crews to perform science activities
on the Moon and Mars involving exploration and sampling of the
subsurface.
@--------------------------------------------------------------------
Title: The Cyborg Astrobiologist: Testing a Novelty
Detection Algorithm at the Mars Desert Research
Station (MDRS), Utah
Authors: Gross, C.; Wendt, L.; McGuire, P. C.; Bonnici, A.;
Foing, B. H.; Souza-Egipsy, V.; Bose, R.; Walter, S.;
Ormö, J.; Díaz-Martínez, E.; Oesker, M.; Ontrup, J.;
Haschke, R.; Ritter, H.
Bibliographic Code: 2010LPI....41.2457G
Abstract
Herein we present a computer vision algorithm, based in part on an
artificial neural network capable of identifying novel, previously
unseen areas of geological or astrobiological scenery.
@--------------------------------------------------------------------
Title: Highlights from Remote Controlled Rover for
EuroGeoMars MDRS Campaign
Authors: Hendrikse, J.; Foing, B. H.; Monaghan, E.;
Stoker, C.; Zavaleta, J.; Selch, F.; Ehrenfreund, P.;
Wendt, L.; Gross, C.; Thiel, C.; Peters, S.;
Borst, A.; Sarrazin, P.; Blake, D.; Boche-Sauvan, L.;
Page, J.; Pletser, V.; Mahapatra, P.; Wills, D.;
McKay, C.; Davies, G.; van Westrenen, W.;
Batenburg, P.; Drijkoningen, G.; Slob, E.;
Poulakis, P.; Visentin, G.; Noroozi, A.; Gill, E.;
Guglielmi, M.; Freire, M.; Walker, R.;
Exogeolab Team; Eurogeomars Team
Bibliographic Code: 2010LPI....41.2435H
Abstract
The goal of the EuroGeoMars mission (from January 24 through February
28, 2009) was to validate a remote controlled rover for surface
reconnaissance and extravehicular activity support and evaluate rover
technical requirement for remote controlled reconnaissance from a
habitat and in situ support.
@--------------------------------------------------------------------
Title: ILEWG ExoHab & EuroGeoMars Campaigns: Habitability &
Human Operations
Authors: Boche-Sauvan, L.; Foing, B. H.; Stoker, C.;
Ehrenfreund, P.; Wendt, L.; Gross, C.; Thiel, C.;
Peters, S.; Borst, A.; Zavaleta, J.; Sarrazin, P.;
Blake, D.; Page, J.; Pletser, V.; Monaghan, E.;
Mahapatra, P.; Noroozi, A.; Giannopoulos, P.;
Calzada, A.; Walker, R.; Zegers, T.; Exogeolab;
ILEWG Exohab Team; Eurogeomars Team
Bibliographic Code: 2010LPI....41.1759B
Abstract
We studied concepts for a minimal Moon-Mars habitat, focussing on the
system aspects and as an evolving architecture. We validated
experimentally the Habitat and Laboratory ExoHab concept constraints
during EuroGeoMars campaign in Utah desert research station.
@--------------------------------------------------------------------
Title: EuroGeoMars Field Campaign: Sample Analysis of
Organic Matter and Minerals
Authors: Ehrenfreund, P.; Foing, B. H.; Stoker, C.;
Zavaleta, J.; Quinn, R.; Blake, D.; Martins, Z.;
Sephton, M.; Becker, L.; Orzechowska, G.;
van Sluis, C.; Boche-Sauvan, L.; Gross, C.;
Thiel, C.; Wendt, L.; Sarrazin, P.; Mahapatra, P.;
Direito, S.; Roling, W.; Eurogeomars Mdrs Team
Bibliographic Code: 2010LPI....41.1723E
Abstract
We report on the results of chemical, physical and astrobiological
measurements of samples collected during the EuroGeoMars campaign at
Utah Mars Desert Research Station (MDRS) in February 2009, as
interdisciplinary preparation for a strategic search for life on Mars.
@--------------------------------------------------------------------
Title: ExoGeoLab Lander, Rovers and Instruments: Tests at
ESTEC & Eifel Volcanic Field
Authors: Foing, B. H.; Barton, A.; Blom, J. K.; Mahapatra, P.;
Som, S.; Jantscher, B.; Page, J.; Zegers, T.;
Stoker, C.; Zavaleta, J.; Poulakis, P.; Visentin, G.;
Noroozi, A.; Ehrenfreund, P.; Mickolacjzak, M.;
Perrin, A.; Chevrier, S.; Direito, S.; Dene, A.;
Voute, S.; Olmedo, A.; Groemer, G.; Stumptner, W.;
Davies, G.; van Westrenen, W.; Koschny, D.;
Lebreton, J. P.; Guglielmi, M.; Freire, M.;
Walker, R.; ILEWG Exogeolab Team;
ILEWG Eifel Field Test Team
Bibliographic Code: 2010LPI....41.1701F
Abstract
We have built an ExoGeoLab lander demonstrator for future planetary
missions, equipped with remotely operated instruments. We tested them at
ESTEC and at an ILEWG field campaign at Eifel volcanic park in Germany
in September 2009.
@--------------------------------------------------------------------
Title: ILEWG Eifel 2009 Campaign: Astronaut Extravehicular
Surface/Subsurface Activities and Human Aspects
Authors: Groemer, G.; Stumptner, W.; Foing, B.; Blom, J. K.;
Perrin, A.; Mikolajczak, M.; Chevrier, S.;
Direito, S.; Olmedo-Soler, A.; Zegers, T. E.;
Scheer, D.; Bickert, K.; Schildhammer, D.;
Jantscher, B.; Mahapatra, P.; Meca Team
Bibliographic Code: 2010LPI....41.1680G
Abstract
The ILEWG organised a field campaign on 26-30 Sep 2009 with
partners in Mendig, Germany, in the volcanic Eifel region. They tested
their systems as simulation of lunar or planetary human and robotic
mission operations, and for the first time in a subterranean lavadome.
@--------------------------------------------------------------------
Title: CAREX Rio Tinto Field Workshop: Instruments, Sample
Collection and Analysis
Authors: Mahapatra, P.; Foing, B.; Direito, S.; Gomez, F.;
Rull, F.
Bibliographic Code: 2010LPI....41.1374M
Abstract
At Rio Tinto, a Mars analogue site, Raman and fibre-optic spectrometers
were successfully used to select appropriate rock and soil samples, and
detect minerals for which it is interesting to study the associated
microorganisms for innovative molecular biology techniques.
@--------------------------------------------------------------------
Title: The Cyborg Astrobiologist: testing a novelty
detection algorithm on two mobile exploration
systems at Rivas Vaciamadrid in Spain and at the
Mars Desert Research Station in Utah
Authors: McGuire, P. C.; Gross, C.; Wendt, L.; Bonnici, A.;
Souza-Egipsy, V.; Ormö, J.; Díaz-Martínez, E.;
Foing, B. H.; Bose, R.; Walter, S.; Oesker, M.;
Ontrup, J.; Haschke, R.; Ritter, H.
Bibliographic Code: 2010IJAsB...9...11M, eprint = 0910.5454
Abstract
In previous work, a platform was developed for testing computer-vision
algorithms for robotic planetary exploration. This platform consisted of
a digital video camera connected to a wearable computer for real-time
processing of images at geological and astrobiological field sites. The
real-time processing included image segmentation and the generation of
interest points based upon uncommonness in the segmentation maps. Also
in previous work, this platform for testing computer-vision algorithms
has been ported to a more ergonomic alternative platform, consisting of
a phone camera connected via the Global System for Mobile Communications
(GSM) network to a remote-server computer. The wearable-computer
platform has been tested at geological and astrobiological field sites
in Spain (Rivas Vaciamadrid and Riba de Santiuste), and the phone camera
has been tested at a geological field site in Malta. In this work, we
(i) apply a Hopfield neural-network algorithm for novelty detection
based upon colour, (ii) integrate a field-capable digital microscope on
the wearable computer platform, (iii) test this novelty detection with
the digital microscope at Rivas Vaciamadrid, (iv) develop a Bluetooth
communication mode for the phone-camera platform, in order to allow
access to a mobile processing computer at the field sites, and (v) test
the novelty detection on the Bluetooth-enabled phone camera connected to
a netbook computer at the Mars Desert Research Station in Utah. This
systems engineering and field testing have together allowed us to
develop a real-time computer-vision system that is capable, for example,
of identifying lichens as novel within a series of images acquired in
semi-arid desert environments. We acquired sequences of images of
geologic outcrops in Utah and Spain consisting of various rock types and
colours to test this algorithm. The algorithm robustly recognized
previously observed units by their colour, while requiring only a single
image or a few images to learn colours as familiar, demonstrating its
fast learning capability.
@--------------------------------------------------------------------
Title: Reflections and proposals on robotic and human
exploration of Moon; Mars, and near-Earth asteroids
Authors: Ehrenfreund, Pascale; Zarnecki, John; Mc Kay, Chris;
Foing, Bernard; Peter, Nicolas; Rummel, John;
Masson-Zwaan, Tanja; Perino, Maria A.;
Macwell, Steve; Worms, Jean Claude; Billings, Linda
Bibliographic Code: 2010cosp...38.3969E
Abstract
The objective of the COSPAR Panel on Exploration (PEX) is to provide the
best, independent, input to support the development of worldwide space
exploration programs and to safeguard the scientific assets of solar
system objects. In recent years, there has been ample study activity
concerning space exploration and overall international cooperation has
increased strongly. For lunar exploration, the International Lunar
Exploration Working Group (ILEWG) and the Lu-nar Exploration Analysis
Group (LEAG)---as well as other committees---represent important
foci for an even broader base of expertise. The Mars Exploration
Planning and Analysis Group (MEPAG) continues to be an excellent
community forum providing analysis for NASA and international Mars
programs represented cross-agency by the International Mars Exploration
Working Group (IMEWG). The PEX report 2010 provides a summary and
outlines synergies of existing documents and roadmaps of each of these
bodies. Additonal expertise is provided via the contacts maintained by
COSPAR's various Associates within the international community and
scientific entities. PEX also offers a stepwise approach to foster a
future international plan-etary exploration program, a system-of-systems
approach with small exploration missions that serves as preparation for
future large-scale endeavors. The PEX document is aimed to foster
transnational alliances, support joint research and educate and inspire
a new space generation.
@--------------------------------------------------------------------
Title: Protecting the Moon for research: ILEWG report
Authors: Foing, Bernard H.
Bibliographic Code: 2010cosp...38.3956F
Abstract
We give a report on recommendations with emphasis on environment
protection, and since last COSPAR from ILEWG International conferences
Exploration and Utilisation of the Moon on held at Cape Canaveral in
2008 (ICEUM10), and in Beijing in May 2010 with IAF (GLUC -ICEUM11). We
discuss the different rationale for Moon exploration, as debated at
ILEWG. ILEWG Science task group has listed priorities for scientific
investigations: clues on the formation and evolution of rocky planets,
accretion and bombardment in the inner solar system, comparative
planetology processes (tectonic, volcanic, impact cratering, volatile
delivery), records astrobiology, survival of organics; past, present and
future life; sciences from a biology lunar laboratory. We discuss how to
preserve Moon research potential in these areas while operating with
instruments, landers, rover during a cooperative robotic village, and
during the transition form lunar human outpost to permanent sustainable
human base. We discuss how Moon-Mars Exploration can inspire solutions
to global Earth sustained development with the trade-off of In-Situ
Utilisation of resources; Establishment of permanent robotic
infrastructures, Environmental and planetary protection aspects and
lessons for Mars; Life sciences laboratories, and support to human
exploration. Co-authors: ILEWG Task Groups on Science, Technology and
Human Lunar Bases ILEWG Reference documents: http://sci.esa.int/ilewg
-10th ILEWG Conference on Exploration and Utilisation of the Moon, NASA
Lunar Ex-ploration Analysis Group-PSace Resources Roundtable, Cape
Canaveral October 2008, pro-gramme online at http://sci.esa.int/ilewg/
-9th ILEWG Conference on Exploration and Utilisation of the Moon, ICEUM9
Sorrento 2007, programme online at http://sci.esa.int/ilewg/ -8th ILEWG
Conference on Exploration and Utilisation of the Moon, Beijing July
2006, programme online at http://sci.esa.int/ilewg/ -The Moon and Near
Earth Objects (P. Ehrenfreund, B.H. Foing, A. Cellino Editors),
Ad-vances in Space Research, Volume 37, Issue 1, pp 1-192, 2006 -7th
ILEWG Conference on Exploration and Utilisation of the Moon, Toronto
Sept 2005, Programme and Proceedings on line at www.ilewg.org, R.
Richards et al Editors -6th ILEWG Conference on Exploration and
Utilisation of the Moon, Udaipur Nov. 2004, Proceedings ( N. Bhandari
Editor), Journal Earth System Science, India, 114, No6, Dec 2005, pp.
573-841 -5th ILEWG Conference on Exploration and Utilisation of the
Moon, Hawaii Nov 2003, Pro-ceedings ILC2005/ICEUM5 (S.M. Durst et al
Editors), Vol 108, 1-576 pp, Science and Tech-nology Series, American
Astronautical Society, 2004 -'The next steps in exploring deep space -A
cosmic study by the IAA', W. Huntress, D. Stetson, R. Farquhar, J.
Zimmerman, B. Clark, W. O'Neil, R. Bourke and B. Foing, Acta
Astronautica, Vol 58, Issues 6-7, March-April 2006, p302-377 -IAA/ESA
workshop on "Next Steps in Exploring Deep Space", ESTEC 22-23 sept. 2003
(B.H. Foing W. Huntress, conveners) Lunar Exploration, Planetary and
Space Science, Vol 50, issue 14-15, Dec 2002 (B.H. Foing al) -ESLAB36
symposium on "Earth-like Planets and Moons", 2002, ESA-SP514, pp. 1-356,
(B.H.Foing B. Battrick, editors) -'Lunar Exploration 2000', (B.H. Foing,
D. Heather, Editors), Adv. Space Research Vol 30, Nr 8, 2002
-'Earth-Moon Relationships', Proceedings of the Conference held in
Padova, Italy at the Ac-cademia Galileiana di Scienze Lettere ed Arti,
Nov. 2000, (C. Barbieri and F. Rampazzi, Editors), in Earth, Moon,
Planets Vol. 85-86, Nos 1-3, pp 1-575, 2001 -4th International
Conference on Exploration and Utilisation of the Moon, ESTEC, 2000, ESA
SP-462 (B.H. Foing M. Perry, editors) -Investing in Space: The Challenge
for Europe. Long-Term Space Policy Committee, Second Report, May 1999.
ESA-SP-2000 -2nd International Lunar Workshop, held at Kyoto in October
1996, Proceedings, H. Mizutani, editor, Japan Space Forum Publisher,
1997 International Lunar Workshop, 1994 May 31-June 3, Beatenberg,
Switzerland. Proceedings. Ed. Balsiger, H. et al. European Space Agency,
1994. ESA-SP-1170 -Astronomy and Space Science from the Moon',
Proceedings of COSPAR/IAF session at World Congress, Washington, (B.H.
Foing et al editors), Advances in Space Research, Volume 14, Issue 6,
1994 -Mission to the Moon, Europe's Priorities for Scientific
Exploration and Utilisation of the Moon', R.M. Bonnet et al, European
Space Agency, ESA SP-1150, June 1992
@--------------------------------------------------------------------
Title: Outreach and education from EuroGeoMoonMars2009
Field Campaign in Utah
Authors: Foing, Bernard H.
Bibliographic Code: 2010cosp...38.3893F
Abstract
The goal of the EuroGeoMoonMars mission at Utah Desert Research
station(from 24 January to 28 February 2009) was to demonstrate
instruments from ExoGeoLab pilot project, to support the interpretation
of ongoing lunar and planetary missions, to validate a procedure for
surface in-situ and return science, to study human performance aspects,
and perform outreach and education projects. The EuroGeoMoonMars
campaign included four sets of objectives: 1) Technology demonstration
aspects: a set of instruments were deployed, tested, assessed, and
training was provided to scientists using them in subsequent rotations
2) Research aspects: a series of field science and exploration
investigations were conducted in geology, geochemistry, biology,
astronomy, with synergies with space missions and research from
planetary surfaces and Earth extreme environments. 3) Human crew related
aspects, i.e. (a) evaluation of the different functions and interfaces
of a planetary habitat, (b) crew time organization in this habitat, (c)
evaluation of man-machine interfaces of science and technical equipment;
4) Education, outreach, communications, multi-cultural public relations
Outreach, education and inspiration: We produced written, pictures, and
video materials that can be used for education, outreach and public
relations. Daily reports were posted on the MDRS website. We had during
the Technical crew preparation, the visit of film producer Mark Arabella
and film crew for a Moon related National Geographics documentary "Earth
without the Moon". Two media crew visitors stayed also in the Hab to
film our activities documenting the operational, research, human,
simulation, imaginative and fantasy aspects of Moon-Mars-extreme Earth
exploration. They contributed a journalist report, and even performed an
EVA outreach filming a sortie to Hanksville village on Earth. Other film
and journalists visited the EuroGeoMars crew for interviews and
exchange. Specific crew reports were also prepared for some national and
international communication channels, including Plan`te Mars, RTBF,
ILEWG, COSPAR, IAF, IAA. We thank ILEWG, NASA Ames, ESA, the Mars
society, VU Amsterdam and collaborating institutes for supporting the
campaign.
@--------------------------------------------------------------------
Title: Automatic rock detection for in situ spectroscopy
applications on Mars
Authors: Mahapatra, Pooja; Foing, Bernard H.
Bibliographic Code: 2010cosp...38.3504M
Abstract
A novel algorithm for rock detection has been developed for effectively
utilising Mars rovers, and enabling autonomous selection of target rocks
that require close-contact spectroscopic measurements. The algorithm
demarcates small rocks in terrain images as seen by cameras on a Mars
rover during traverse. This information may be used by the rover for
selection of geologically relevant sample rocks, and (in conjunction
with a rangefinder) to pick up target samples using a robotic arm for
automatic in situ determination of rock composition and mineralogy
using, for example, a Raman spectrometer. Determining rock samples
within the region that are of specific interest without physically
approaching them significantly reduces time, power and risk. Input
images in colour are converted to greyscale for intensity analysis.
Bilateral filtering is used for texture removal while preserving rock
boundaries. Unsharp masking is used for contrast enhance-ment. Sharp
contrasts in intensities are detected using Canny edge detection, with
thresholds that are calculated from the image obtained after
contrast-limited adaptive histogram equalisation of the unsharp masked
image. Scale-space representations are then generated by convolving this
image with a Gaussian kernel. A scale-invariant blob detector (Laplacian
of the Gaussian, LoG) detects blobs independently of their sizes, and
therefore requires a multi-scale approach with automatic scale
se-lection. The scale-space blob detector consists of convolution of the
Canny edge-detected image with a scale-normalised LoG at several scales,
and finding the maxima of squared LoG response in scale-space. After the
extraction of local intensity extrema, the intensity profiles along rays
going out of the local extremum are investigated. An ellipse is fitted
to the region determined by significant changes in the intensity
profiles. The fitted ellipses are overlaid on the original Mars terrain
image for a visual estimation of the rock detection accuracy, and the
number of ellipses are counted. Since geometry and illumination have the
least effect on small rocks, the proposed algorithm is effective in
detecting small rocks (or bigger rocks at larger distances from the
camera) that consist of a small fraction of image pixels.
Acknowledgements: The first author would like to express her gratitude
to the European Space Agency (ESA/ESTEC) and the International Lunar
Exploration Working Group (ILEWG) for their support of this work.
@--------------------------------------------------------------------
Title: A dual bacterial culture augments Kalanchoe spp.
photosynthesis under extreme conditions
Authors: Burlak, Olexii; Rogutskyy, Ivan; Danilchenko, Boris;
Mikheev, Olexander; Zaetz, Iryna; Lorek, Andreas;
Koncz, Alexander; de Vera, Jean-Pierre;
Foing, Bernard H.; Kozyrovska, Natalia
Bibliographic Code: 2010cosp...38.3470B
Abstract
In consistence with conception of using microbial technology for plant
growing/protosoil for-mation for Lunar/Martian greenhouses (Kozyrovska
et al., 2004-2010), we anticipate microbes to alleviate impact of the
environmental stressors on plant development. Bacteria can augment
physiological processes in plants, for example, photosynthesis, by
regulating a hormone level and decreasing glucose sensing in planta
(Zhang et al., 2008). The study aimed to examine impact of consortium of
well-defined bacteria Klebsiella oxytoca IMBG26 and Paenibacillus sp.
IMBG150 on the CAM-plantlets Kalanhoe diagramontiana and Kalanhoe
tubiflora pho-tosynthetic activity after acute action of gamma radiation
(60Co), Near Martian ultraviolet radiation, low pressure (100 mbar), and
high concentrations of CO2 (95Plantlets of K. tubi-flora were exposed to
harmful doses of Near Martian UV radiation for 3 hours (26.53 J/cm2). A
week before experiment kalanchoe plantlets were subjected to acute
effects of ionizing radiation at doses of 30 and 70 Gy. In noninoculated
plantlets after 30 Gy the photosynthetic activity fell to 71
@--------------------------------------------------------------------
Title: Investigation of microbial diversity in a desert
Mars-like environment: Mars Desert Research Station
(MDRS), Utah
Authors: Direito, Maria Susana; Staats, Martijn;
Foing, Bernard H.; Ehrenfreund, Pascale;
Roling, Wilfred
Bibliographic Code: 2010cosp...38.3327D
Abstract
The Utah Mars Desert Research Station (MDRS) harbours geo-morphology and
geo-processes analogues to the planet Mars. Soil samples were collected
during the EuroGeoMars campaign (from 24 January to 1 March 2009) from
different locations and depths [1]. Samples were distributed among
scientific collaborator institutes for analysis of microbial diversity,
amino acid content and degradation, content of PAH or larger organic
molecules, and respective soil properties. Our sample analysis had the
objective of characterizing the microbial communities in this Mars
analogue: DNA isolation, PCR (Polymerase Chain Reaction) using primers
for DNA amplification of Bacteria, Archaea and Eukarya ribosomal RNA
(rRNA) gene fragments, DGGE (Denaturing Gradient Gel Electrophoresis)
and clone library construction with the final aim of sequencing. Results
indicate that life is present in all the three domains of life (Archaea,
Bacteria and Eukarya), while the most diversity was found in the domain
Bacteria. Microorgan-isms are heterogeneously present and their
identities are currently investigated. The obtained information will be
later related to the other scientific analysis in order to obtain a
better understanding of this Mars analogue site, which in turn will
provide important information for the search for life on Mars. [1]
Foing, B.H. et al. (2009). Exogeolab lander/rover instruments and
EuroGeoMars MDRS campaign. LPI, 40, 2567.
@--------------------------------------------------------------------
Title: EuroGeoMars Field Campaign: habitability studies in
preparation for future Mars missions
Authors: Ehrenfreund, Pascale; Foing, B. H.; Stoker, C.;
Zhavaleta, J.; Orzechowska, G.; Kotler, M.;
Martins, Z.; Sephton, M.; Becker, L.; Quinn, R.;
van Sluis, C.; Boche-Sauvan, L.; Gross, C.;
Thiel, C.; Wendt, L.; Sarrazin, P.; Mahapatra, P.;
Direito, S.; Roling, W.
Bibliographic Code: 2010cosp...38.3299E
Abstract
The goal of the EuroGeoMars field campaign sponsored by ESA, NASA and
the international lunar exploration working group (ILEWG) was to
demonstrate instrument capabilities in sup-port of current and future
planetary missions, to validate a procedure for Martian surface in-situ
and return science, and to study human performance aspects. The Mars
Desert Re-search Station (MDRS) represents an ideal basis to simulate
aspects of robotic and human exploration in support of future missions
to planetary bodies. During the campaign, MDRS Crew 77 tested X-ray
diffraction and Raman instruments, and assessed habitat and operations.
Special emphasis was given to sample collection in the geologically rich
vicinity of MDRS and subsequent analysis of organic molecules in the
soil to simulate the search for bio-signatures with field
instrumentation. We describe the results of in-situ and posterior
analysis of the physical and chemical properties including elemental
composition, salt concentrations as well as carbon and amino acid
abundances. The analyses of organics and minerals show that the
subsurface mineral matrix represents a key to our understanding of the
survival of organics on Mars.
@--------------------------------------------------------------------
Title: Challenges from new lunar data: ILEWG report
Authors: Foing, Bernard H.
Bibliographic Code: 2010cosp...38..812F
Abstract
Recent lunar missions including Clementine, Lunar Prospector, SMART-1,
Selene Kaguya, Chang'E 1 , Chandrayaan-1 have been producing new data in
large volumes. We shall discuss the challenges in data calibration and
intercalibration, integration, the defin ition of an accurate coordinate
systems and geodesic grid, incorporation of latest altimetry and
gravimetry data. LRO Lunar Reconnaissance Orbiter and subsequent
missions will go even futher in data volume and diversity of
instruments. We shall discuss the upcoming challenges in data archiving,
management and interpretative tools, to merge orbital remote sensing
with surface data from landers and rovers for the various elements of
ILEWG lunar robotic village. Co-authors: ILEWG Task Groups on Science,
Data and Outreach Relevant ILEWG Reference documents:
http://sci.esa.int/ilewg -10th ILEWG Conference on Exploration and
Utilisation of the Moon, NASA Lunar Ex-ploration Analysis Group-Space
Resources Roundtable, Cape Canaveral October 2008, pro-gramme online at
http://sci.esa.int/ilewg/ -9th ILEWG Conference on Exploration and
Utilisation of the Moon, ICEUM9 Sorrento 2007, programme online at
http://sci.esa.int/ilewg/ -8th ILEWG Conference on Exploration and
Utilisation of the Moon, Beijing July 2006, programme online at
http://sci.esa.int/ilewg/ -7th ILEWG Conference on Exploration and
Utilisation of the Moon, Toronto Sept 2005, Programme and Proceedings on
line at www.ilewg.org, R. Richards et al Editors -6th ILEWG Conference
on Exploration and Utilisation of the Moon, Udaipur Nov. 2004,
Proceedings ( N. Bhandari Editor), Journal Earth System Science, India,
114, No6, Dec 2005, pp. 573-841 -5th ILEWG Conference on Exploration and
Utilisation of the Moon, Hawaii Nov 2003, Pro-ceedings ILC2005/ICEUM5
(S.M. Durst et al Editors), Vol 108, 1-576 pp, Science and Tech-nology
Series, American Astronautical Society, 2004 -4th International
Conference on Exploration and Utilisation of the Moon, ESTEC, 2000, ESA
SP-462 (B.H. Foing M. Perry, editors)
@--------------------------------------------------------------------
Title: EuroMoonMars Dommex (EMMD 2010): Geology results
from EMMD3 in a desert Mars-like environment, Utah
Authors: van Vynckt, Delphine; Voute, Sara;
Calzada, Mss Abigail; Le Maire, Victor; Jago, Alban;
de Crombrugghe, Guerric; Denies, Jonathan;
Reydam, Marc; van Vynckt, D.; Voute, Sara;
Calzada, Abigail; de Crombrugghe, G.; Denies, J.;
Jago, A.; Le Maire, V.; de Lobkowicz, I.;
Mertens, A.; Reydams, M.; Foing, Bernard H.;
Stoker, C.
Bibliographic Code: 2010cosp...38..537V
Abstract
EMMD3 Geology results: Delphine Van Vynckt Introduction: EMMD3 is part
of the JUMP Martian mission simulation conducted by stu-dents in the
Mars Desert Research Station (MDRS), a habitat installed by the Mars
Society (MS) in the Utah desert. The campaign was supported by ILEWG
International Lunar Explo-ration Working Group, ESTEC, NASA Ames, and
partners. The geology objectives of EMMD 2010 are to study the surface
and subsurface of the Jurassic-Cretaceous Earth in Utah, to mea-sure
mineral composition and to analyse the various rocks after a sampling in
EVA suit. The geological EMMD3 research is divided in three main parts.
The first one consists of developing a sampling procedure for Martian
missions; the second one concerns the exact determination of the
durations of the different steps of this sampling procedure; the last
one will study the possi-bility to work with a rover, and the
interactions human-machine. The project is in line with the ILEWG
EuroMoonMars project which coordinates several MDRS missions, and
contributes to the preparation of future Mars sample return missions.
Procedure validation: During a previous crew rotation at the MDRS, Sara
Voute (EDMM1) will finalize and test a procedure she developed for
geological missions. During our crew rotation we will test the sampling
part of that procedure into more details. One of the objectives is to
determine whether it is understandable and usable for astronauts that
are not specialized in geology. Rover monitoring: A rover will be lent
by NASA Ames to our crew. We will study the different ways to work with
such tool in geological missions. The rover can be used as a technical
support for astronauts in outside missions. The astronauts could
communicate information (images, spectrometer scans, etc.) to the base
through the rover in order to sample efficiently. The scientists located
in the base have access to treatment tools that an astronauts in outside
mission have not and so this allows a pre-selection of the sampling
carried back. We will study also the interaction rover-astronauts in a
general way in order to determine the benefits both for the rover and
the astronauts. Moreover, we will perform exploration missions with
rover monitored remotely from the base and see the limitations of this
approach. We shall report on the science and technical results, and
implications for Earth-Mars compar-ative studies.
@--------------------------------------------------------------------
Title: Search for Mars climatic signal in periglacial
deposits
Authors: Foing, Bernard H.
Bibliographic Code: 2010cosp...38..503F
Abstract
Mars has experienced large variations in its orbital parameters
throughout its history, with periodicity of 120 000 years for its
obliquity, 95 to 100,000 years for its eccentricity, and 51,000 years
for its precession (Laskar et al) . At high obliquity, signicant amount
of ice can be deposited from snow at low latitudes. This can be relevant
for understanding features from the modern Polar Layered Deposits, the
Elysium frozen sea (Murray et al 2005), or Ellas hourglass (Head et al
2005). General circulation models predict an annual net accumulation
rate of ice on the west of Tharsis volcanoes. We analysed Mars Express
images on Pavonis Mons and other periglacial deposits. By texture
analysis we could distinguish ridges, knobbies from various episodes and
relate them with geological studies. Using a glacier progression model
under different snow fall conditions according to obliquity, we find
oscillations of the glacier extents and ridges that can constrain the
past history of Martian climate. We acknowledge discussions with A.
Orsi, T. Zegers, F. Forget, J. Head, J. Laskar, S. van Gasselt, G.
Neukum Mars Express HRSC team
@--------------------------------------------------------------------
Title: Moon-Mars Analogue Mission (EuroMoonMars 1 at the
Mars Desert Research Station)
Authors: Lia Schlacht, Irene; Voute, Sara; Irwin, Stacy;
Foing, Bernard H.; Stoker, Carol R.;
Westenberg, Artemis
Bibliographic Code: 2010cosp...38..475L
Abstract
The Mars Desert Research Station (MDRS) is situated in an analogue
habitat-based Martian environment, designed for missions to determine
the knowledge and equipment necessary for successful future planetary
exploration. For this purpose, a crew of six people worked and lived
together in a closed-system environment. They performed habitability
experiments within the dwelling and conducted Extra-Vehicular Activities
(EVAs) for two weeks (20 Feb to 6 Mar 2010) and were guided externally
by mission support, called "Earth" within the simulation. Crew 91, an
international, mixed-gender, and multidisciplinary group, has completed
several studies during the first mission of the EuroMoonMars campaign.
The crew is composed of an Italian designer and human factors
specialist, a Dutch geologist, an American physicist, and three French
aerospace engineering students from Ecole de l'Air, all with ages
between 21 and 31. Each crewmember worked on personal research and
fulfilled a unique role within the group: commander, executive officer,
engineer, health and safety officer, scientist, and journalist. The
expedition focused on human factors, performance, communication, health
and safety pro-tocols, and EVA procedures. The engineers' projects aimed
to improve rover manoeuvrability, far-field communication, and data
exchanges between the base and the rover or astronaut. The crew
physicist evaluated dust control methods inside and outside the habitat.
The geologist tested planetary geological sampling procedures. The crew
designer investigated performance and overall habitability in the
context of the Mars Habitability Experiment from the Extreme-Design
group. During the mission the crew also participated in the Food Study
and in the Ethospace study, managed by external groups. The poster will
present crew dynamics, scientific results and daily schedule from a
Human Factors perspective. Main co-sponsors and collaborators: ILEWG,
ESA ESTEC, NASA Ames, Ecole de l'Air, SKOR, Extreme-Design, Universit`
di Torino, MMS TU-Berlin, Space Florida, DAAD, Uni-a versity of Utrecht,
The Mars Society.
@--------------------------------------------------------------------
Title: From Apollo Traverses to Future Exploration
Authors: Calzada, Mss Abigail; Voute, Sara;
van Vynckt, Delphine; Foing, Bernard H.
Bibliographic Code: 2010cosp...38..443C
Abstract
Historically, Apollo program is known as the first time that human could
land in other space object, in this case Earth's moon, and come back
safely to the Earth. It was the first time that humans had to adapt
geological field work to extreme conditions in space. We can summarize
the field work in a few steps: -Planning of the mission and field
training of the astronauts. -Development of instrumental packages and
reconnaissance of the area. -Geophysical measure-ments in situ and some
sampling near the Lunar Module (LM). -Various EVA's of an average of six
hours, from Apollo 15 with Lunar Rover Vehicle (LRV) support, collecting
samples and taking measurements of various geophysical experiments. From
now to future exploration we have to focus on apply all the knowledge we
have from Apollo traverses and adapt it to the new technologies we are
developing. The use of robotic rovers can save us hours of human EVA's
in the way that we can predict the possible sites of interest before
send human there. Also, the development of a field laboratory and
habitat can provide us of the intruments necessary to do experiments
without the need of a sample return mission. We validate these traverses
in EuroMoonMars campaign.
@--------------------------------------------------------------------
Title: The inducible CAM plants in putative lunar lander
experiments
Authors: Burlak, Olexii; Zaetz, Iryna; Soldatkin, Olexii;
Rogutskyy, Ivan; Danilchenko, Boris;
Mikheev, Olexander; de Vera, Jean-Pierre;
Vidmachenko, Anatolii; Foing, Bernard H.;
Kozyrovska, Natalia
Bibliographic Code: 2010cosp...38..442B
Abstract
Precursory lunar lander experiments on growing plants in locker-based
chambers will increase our understanding of effect of lunar conditions
on plant physiology. The inducible CAM (Cras-sulacean Acid
Metabolism)-plants are reasonable model for a study of relationships
between environmental challenges and changes in plant/bacteria gene
expression. In inducible CAM-plants the enzymatic machinery for the
environmentally activated CAM switches on from a C3-to a full-CAM mode
of photosynthesis in response to any stresses (Winter et al., 2008). In
our study, Kalanchoe spp. are shown to be promising candidates for
putative lunar experiments as resistant to irradiation and desiccation,
especially after inoculation with a bacterial consortium (Boorlak et
al., 2010). Within frames of the experiment we expect to get information
about the functional activity of CAM-plants, in particular, its
organogenesis, photosystem, the circadian regulation of plant metabolism
on the base of data gaining with instrumental indications from
expression of the reporter genes fused to any genes involved in vital
functions of the plant (Kozyrovska et al., 2009). References 1. Winter
K., Garcia M., Holtum J. (2008) J. Exp. Bot. 59(7):1829-1840 2. Bourlak
O., Lar O., Rogutskyy I., Mikheev A., Zaets I., Chervatyuk N., de Vera
J.-P., Danilchenko A.B. Foing B.H., zyrovska N. (2010) Space Sci.
Technol. 3. Kozyrovska N.O., Vidmachenko A.P., Foing B.H. et al.
Exploration/call/estec/ESA. 2009.
@--------------------------------------------------------------------
Title: Kombucha might be promising probiotics for
consumption on the Moon
Authors: Kozyrovska, Natalia; Foing, Bernard H.
Bibliographic Code: 2010cosp...38..434K
Abstract
The sanitization at permanently manned lunar bases and consuming
germ-free food in a concert with effect of lunar stressors may result in
crews disorders, including inflammatory and atopic states and decrease
of resistance to indigenous pathogens which present in human organism in
suppressed state. The administration of live microbial supplements with
presumptive health benefits on human physiology might be reasonable
solution to prevent disbacteriosis. Many of microbial species are
associated with the fermentation of dairy products, however, they have a
short self-life and so far unpractical to be used at lunar habitation.
The popular "Tea mushroom" or "Kombucha Tea" is a probiotics proven by
FDA that many people are now taking in health promoting diets to
detoxify and revitalize the organism (Danielian, 1993; Sreeramulu et
al., 2001). Kombucha is composed by symbiotic bacteria and yeasts,
surrounded by a permeable membrane. The Kombucha culture is a tiny
biochemical factory, producing organic acids, amino acids, enzymes,
polyphenols, antibiotic substances, vitamins, enzymes as well as some
other products beneficial for human health. Within the ages the Kombucha
Tea has been consumed by practically all nations in Far East and now in
Eastern Europe and America due to probiotic properties, and within this
period the Kombucha microbial ecosystem has been selected to be
remarkably adaptive to culturing conditions and resistant to adverse
factors. Metagenomic approaches in a study of microbial ecosystems will
allow to reconstruct the Kombucha microbiome and to elucidate unknown
species and genes on the base of bioinformatics programs. Compared with
Kombucha wild type, metabolically engineered strains, expected to
exhibit broader substrate specificity, utilizing sugars from waste
material which will be used for Kombucha fermentation. References 1.
Danielian L.T. (1993) Tea fungus. Publ. House "Armenia", 112 pp. 2.
Palmer C., Bik E.M., DiGiulio D.B., Relman D.A., Brown P.O. (2007)
Development of the Human Infant Intestinal Microbiota. PLoS Biol 5(7):
e177. 3. Sreeramulu G., Zhu Y., Knol W. (2001) Characterization of
antimicrobial activity in Kom-bucha fermentation. Acta Biotechnol.
21:49-56. 4. Versalovic J., Relman R. (2006) How bacterial communities
expand functional repertoires. PLoS Biol 4(12): e430.
@--------------------------------------------------------------------
Title: 3min. poster presentations of B01
Authors: Foing, Bernard H.
Bibliographic Code: 2010cosp...38..433F
Abstract
We give a report on recommendations from ILEWG International conferences
held at Cape Canaveral in 2008 (ICEUM10), and in Beijing in May 2010
with IAF (GLUC -ICEUM11). We discuss the different rationale for Moon
exploration. Priorities for scientific investigations include: clues on
the formation and evolution of rocky planets, accretion and bombardment
in the inner solar system, comparative planetology processes (tectonic,
volcanic, impact cratering, volatile delivery), historical records,
astrobiology, survival of organics; past, present and future life. The
ILEWG technology task group set priorities for the advancement of
instrumenta-tion: Remote sensing miniaturised instruments; Surface
geophysical and geochemistry package; Instrument deployment and robotic
arm, nano-rover, sampling, drilling; Sample finder and collector.
Regional mobility rover; Autonomy and Navigation; Artificially
intelligent robots, Complex systems. The ILEWG ExogeoLab pilot project
was developed as support for instru-ments, landers, rovers,and
preparation for cooperative robotic village. The ILEWG lunar base task
group looked at minimal design concepts, technologies in robotic and
human exploration with Tele control, telepresence, virtual reality;
Man-Machine interface and performances. The ILEWG ExoHab pilot project
has been started with support from agencies and partners. We discuss
ILEWG terrestrial Moon-Mars campaigns for validation of technologies,
research and human operations. We indicate how Moon-Mars Exploration can
inspire solutions to global Earth sustained development: In-Situ
Utilisation of resources; Establishment of permanent robotic
infrastructures, Environmental protection aspects; Life sciences
laboratories; Support to human exploration. Co-Authors: ILEWG Task
Groups on: Science, Technology, Robotic village, Lunar Bases,
Commercial and Societal aspects, Roadmap synergies with other
programmes, Public en-gagemnet and Outreach, Young Lunar Explorers.
@--------------------------------------------------------------------
Title: SMART-1 recent results and lessons for future
exploration
Authors: Foing, Bernard H.
Bibliographic Code: 2010cosp...38..417F
Abstract
We present recent results from SMART-1 ESA mission to the Moon published
or obtained since last COSPAR. We discuss the technology demonstration,
science and exploration results, and lessons learned for the future. We
describe SMART-1 lunar science investigations including studies of the
chemical composition of the Moon, of geophysical processes (volcanism,
tectonics, cratering, soil roughness from multi-angular photometry ) for
comparative planetology. We also show high resolution studies of recent
impact sites (Kaguya, LCROSS), and of polar regions in preparation for
future exploration.
@--------------------------------------------------------------------
Title: Transiting exoplanets from the CoRoT space mission.
VIII. CoRoT-7b: the first super-Earth with measured
radius
Authors: Léger, A.; Rouan, D.; Schneider, J.; Barge, P.;
Fridlund, M.; Samuel, B.; Ollivier, M.; Guenther, E.;
Deleuil, M.; Deeg, H. J.; Auvergne, M.; Alonso, R.;
Aigrain, S.; Alapini, A.; Almenara, J. M.;
Baglin, A.; Barbieri, M.; Bruntt, H.; Bordé, P.;
Bouchy, F.; Cabrera, J.; Catala, C.; Carone, L.;
Carpano, S.; Csizmadia, Sz.; Dvorak, R.; Erikson, A.;
Ferraz-Mello, S.; Foing, B.; Fressin, F.;
Gandolfi, D.; Gillon, M.; Gondoin, Ph.; Grasset, O.;
Guillot, T.; Hatzes, A.; Hébrard, G.; Jorda, L.;
Lammer, H.; Llebaria, A.; Loeillet, B.; Mayor, M.;
Mazeh, T.; Moutou, C.; Pätzold, M.; Pont, F.;
Queloz, D.; Rauer, H.; Renner, S.; Samadi, R.;
Shporer, A.; Sotin, Ch.; Tingley, B.; Wuchterl, G.;
Adda, M.; Agogu, P.; Appourchaux, T.; Ballans, H.;
Baron, P.; Beaufort, T.; Bellenger, R.; Berlin, R.;
Bernardi, P.; Blouin, D.; Baudin, F.; Bodin, P.;
Boisnard, L.; Boit, L.; Bonneau, F.; Borzeix, S.;
Briet, R.; Buey, J.-T.; Butler, B.; Cailleau, D.;
Cautain, R.; Chabaud, P.-Y.; Chaintreuil, S.;
Chiavassa, F.; Costes, V.; Cuna Parrho, V.;
de Oliveira Fialho, F.; Decaudin, M.; Defise, J.-M.;
Djalal, S.; Epstein, G.; Exil, G.-E.; Fauré, C.;
Fenouillet, T.; Gaboriaud, A.; Gallic, A.; Gamet, P.;
Gavalda, P.; Grolleau, E.; Gruneisen, R.;
Gueguen, L.; Guis, V.; Guivarc'h, V.; Guterman, P.;
Hallouard, D.; Hasiba, J.; Heuripeau, F.;
Huntzinger, G.; Hustaix, H.; Imad, C.; Imbert, C.;
Johlander, B.; Jouret, M.; Journoud, P.; Karioty, F.;
Kerjean, L.; Lafaille, V.; Lafond, L.; Lam-Trong, T.;
Landiech, P.; Lapeyrere, V.; Larqué, T.; Laudet, P.;
Lautier, N.; Lecann, H.; Lefevre, L.; Leruyet, B.;
Levacher, P.; Magnan, A.; Mazy, E.; Mertens, F.;
Mesnager, J.-M.; Meunier, J.-C.; Michel, J.-P.;
Monjoin, W.; Naudet, D.; Nguyen-Kim, K.;
Orcesi, J.-L.; Ottacher, H.; Perez, R.; Peter, G.;
Plasson, P.; Plesseria, J.-Y.; Pontet, B.;
Pradines, A.; Quentin, C.; Reynaud, J.-L.;
Rolland, G.; Rollenhagen, F.; Romagnan, R.; Russ, N.;
Schmidt, R.; Schwartz, N.; Sebbag, I.; Sedes, G.;
Smit, H.; Steller, M. B.; Sunter, W.; Surace, C.;
Tello, M.; Tiphène, D.; Toulouse, P.; Ulmer, B.;
Vandermarcq, O.; Vergnault, E.; Vuillemin, A.;
Zanatta, P.
Bibliographic Code: 2009A&A...506..287L
Abstract
Aims: We report the discovery of very shallow (Delta F/F ≈
3.4× 10-4), periodic dips in the light curve of an
active V = 11.7 G9V star observed by the CoRoT satellite, which we
interpret as caused by a transiting companion. We describe the 3-colour
CoRoT data and complementary ground-based observations that support the
planetary nature of the companion.
Methods: We used CoRoT colours
information, good angular resolution ground-based photometric
observations in- and out- of transit, adaptive optics imaging,
near-infrared spectroscopy, and preliminary results from radial velocity
measurements, to test the diluted eclipsing binary scenarios. The
parameters of the host star were derived from optical spectra, which
were then combined with the CoRoT light curve to derive parameters of
the companion.
Results: We examined all conceivable cases of
false positives carefully, and all the tests support the planetary
hypothesis. Blends with separation >0.40´´or triple
systems are almost excluded with a 8 × 10-4 risk left.
We conclude that, inasmuch we have been exhaustive, we have discovered a
planetary companion, named CoRoT-7b, for which we derive a period of
0.853 59 ± 3 × 10-5 day and a radius of
Rp = 1.68 ± 0.09 R_Earth. Analysis of preliminary
radial velocity data yields an upper limit of 21 M_Earth for the
companion mass, supporting the finding.
Conclusions: CoRoT-7b is
very likely the first Super-Earth with a measured radius. This object
illustrates what will probably become a common situation with missions
such as Kepler, namely the need to establish the planetary origin of
transits in the absence of a firm radial velocity detection and mass
measurement. The composition of CoRoT-7b remains loosely constrained
without a precise mass. A very high surface temperature on its
irradiated face, ≈1800-2600 K at the substellar point, and a very low
one, ≈50 K, on its dark face assuming no atmosphere, have been
derived.
The CoRoT space mission, launched on 27 December 2006, has been
developed and is operated by CNES, with the contribution of Austria,
Belgium, Brazil, ESA, Germany, and Spain. First CoRoT data are
available to the public from the CoRoT archive:
http://idoc-corot.ias.u-psud.fr. The complementary observations were
obtained with MegaPrime/MegaCam, a joint project of CFHT and CEA/DAPNIA,
at the Canada-France-Hawaii Telescope (CFHT) which is operated by NRC in
Canada, INSU-CNRS in France, and the University of Hawaii; ESO
Telescopes at the La Silla and Paranal Observatories under programme ID
081.C-0413(C), DDT 282.C-5015; the IAC80 telescope operated by the
Instituto de Astrofísica de Tenerife at the Observatorio del
Teide; the Isaac Newton Telescope (INT), operated on the island of La
Palma by the Isaac Newton group in the Spanish Observatorio del Roque de
Los Muchachos of the Instituto de Astrofisica de Canarias; and at the
Anglo-Australian Telescope that have been funded by the Optical Infrared
Coordination network (OPTICON), a major international collaboration
supported by the Research Infrastructures Programme of the European
Commissions Sixth Framework Programme; Radial-velocity observations were
obtained with the SOPHIE spectrograph at the 1.93m telescope of
Observatoire de Haute Provence, France.
@--------------------------------------------------------------------
Title: Photospheric activity and rotation of the
planet-hosting star CoRoT-4a
Authors: Lanza, A. F.; Aigrain, S.; Messina, S.; Leto, G.;
Pagano, I.; Auvergne, M.; Baglin, A.; Barge, P.;
Bonomo, A. S.; Collier Cameron, A.; Cutispoto, G.;
Deleuil, M.; de Medeiros, J. R.; Foing, B.;
Moutou, C.
Bibliographic Code: 2009A&A...506..255L
Abstract
Aims: The space experiment CoRoT has recently detected a transiting hot
Jupiter in orbit around a moderately active F-type main-sequence star
(CoRoT-4a). This planetary system is of particular interest because it
has an orbital period of 9.202 days, the second longest one among the
transiting planets known to date. We study the surface rotation and the
activity of the host star during an uninterrupted sequence of optical
observations of 58 days.
Methods: Our approach is based on a
maximum entropy spot modelling technique extensively tested by modelling
the variation in the total solar irradiance. It has been successfully
applied to model the light curve of another active star with a
transiting planet observed by CoRoT, i.e., CoRoT-2a. It assumes that
stellar active regions consist of cool spots and bright faculae,
analogous to sunspots and solar photospheric faculae, whose visibility
is modulated by stellar rotation.
Results: The modelling of the
light curve of CoRoT-4a reveals three main active longitudes with
lifetimes between {˜ }30 and {˜ }60 days that rotate
quasi-synchronously with the orbital motion of the planet. The different
rotation rates of the active longitudes are interpreted in terms of
surface differential rotation, and a lower limit of 0.057 ± 0.015
is derived for its relative amplitude. The enhancement of activity
observed close to the subplanetary longitude suggests a magnetic
star-planet interaction, although the short duration of the time series
prevents us from drawing definite conclusions.
Conclusions: The
present work confirms the quasi-synchronicity between stellar rotation
and planetary orbital motion in the CoRoT-4 system and provides a lower
limit for the surface differential rotation of the star. This
information can be important in trying to understand the formation and
evolution of this highly interesting planetary system. Moreover, there
is an indication of a possible star-planet magnetic interaction that
needs to be confirmed by future studies.
Based on observations obtained with CoRoT, a space project operated by
the French Space Agency, CNES, with partecipation of the Science
Programme of ESA, ESTEC/RSSD, Austria, Belgium, Brazil, Germany, and
Spain.
@--------------------------------------------------------------------
Title: Search for radio flashes caused by collisions of
meteoroids with the moon
Authors: Volvach, A. E.; Berezhnoy, A. A.; Foing, B.;
Erenfroyd, P.; Havroshkin, O. B.; Volvach, L. N.
Bibliographic Code: 2009KPCB...25..194V
Abstract
@--------------------------------------------------------------------
Title: PCR-based Detection of Microbial Communities during
the EuroGeoMars MDRS Campaign
Authors: Thiel, C.; Wills, D.; Foing, B. H.
Bibliographic Code: 2009epsc.conf..660T
Abstract
@--------------------------------------------------------------------
Title: Drilling on the Moon and Mars: Human Exploration
Simulation Experiments
Authors: Stoker, C.; Foing, B.; Zavaleta, J.; Clark, J.
Bibliographic Code: 2009epsc.conf..659S
Abstract
@--------------------------------------------------------------------
Title: From Robotic to Human Exploration of the Moon: ILEWG
roadmap
Authors: Foing, B. H.
Bibliographic Code: 2009epsc.conf..657F
Abstract
@--------------------------------------------------------------------
Title: From SMART-1 to Global Robotic Village and
International Lunar Bases
Authors: Foing, B. H.
Bibliographic Code: 2009epsc.conf..655F
Abstract
@--------------------------------------------------------------------
Title: Synthesis of SMART-1 lunar results
Authors: Foing, B. H.
Bibliographic Code: 2009epsc.conf..654F
Abstract
@--------------------------------------------------------------------
Title: Validation of Instruments and Robotics from
EuroGeoMars&Moon Campaign
Authors: Foing, B. H.
Bibliographic Code: 2009epsc.conf..643F
Abstract
@--------------------------------------------------------------------
Title: Outreach and education from EuroGeoMars Campaign
Authors: Foing, B. H.
Bibliographic Code: 2009epsc.conf..641F
Abstract
@--------------------------------------------------------------------
Title: ExoGeoLab Test Bench for Landers, Rovers and
Instruments
Authors: Foing, B. H.
Bibliographic Code: 2009epsc.conf..639F
Abstract
@--------------------------------------------------------------------
Title: ExoGeoLab Test Bench for Landers, Rovers and
Instruments
Authors: Foing, B. H.
Bibliographic Code: 2009epsc.conf..637F
Abstract
@--------------------------------------------------------------------
Title: Highlights from Remote Controlled Rover for
EuroGeoMars MDRS Campaign
Authors: Hendrikse, J.; Foing, B. H.; Monaghan, E.
Bibliographic Code: 2009epsc.conf..588H
Abstract
@--------------------------------------------------------------------
Title: Testing the Cyborg Astrobiologist at the Mars Desert
Research Station (MDRS), Utah
Authors: Gross, C.; Wendt, L.; McGuire, P. C.; Bonnici, A.;
Foing, B. H.; Souza-Egipsy, V.; Bose, R.; Walter, S.;
Ormö, J.; Diaz-Martinez, E.
Bibliographic Code: 2009epsc.conf..548G
Abstract
@--------------------------------------------------------------------
Title: Raman investigations of the EuroGeoMars Campaign
Authors: Wendt, L.; Mahapatra, P.; Gross, C.; Borst, A.;
Foing, B. H.; Exogeolab Team; Eurogeomars Team
Bibliographic Code: 2009epsc.conf..457W
Abstract
@--------------------------------------------------------------------
Title: A Prototype Instrumentation System for Rover-Based
Planetary Geology
Authors: Mahapatra, P.; Foing, B.; Nijman, F.; Page, J.;
Noroozi, A.
Bibliographic Code: 2009epsc.conf..364M
Abstract
@--------------------------------------------------------------------
Title: The Polar Maps of the Moon with AMIE/SMART-1
Authors: Despan, Daniela; Erard, S.; Barucci, A.;
Josset, J. L.; Beauvivre, S.; Koschny, D.;
Almeida, M.; Grieger, B.; Foing, B.; AMIE team
Bibliographic Code: 2009DPS....41.3506D
Abstract
The AMIE camera on SMART-1, the first European lunar mission, provided a
large data set, including the north and the south pole regions. SMART-1
was in a 300 x 3000 km elliptical orbit, with perilune over the south
pole.
The Moon surface displays two major types of terrain: the bright and
rugged highlands and darker, smoother plains. The lunar north pole is in
a highland region and spread out in between three large impact craters:
Peary, 88,6° N, 33° E, Hermite, 86° N, 89,9° W and
Rozhdestvensky, 85,2° N, 155,4° W. The quantitative map around
the north pole shows news details of surface topography. The floor of
the Peary crater is smooth and presents only few meteoritic bombardment
formations most of them being near the rim. Similar technics were
applied to construct maps of the South pole region. The southern
highlands of the Moon are rugged and heavily cratered terrains with
geology dominated by the South pole -Aitken (SPA) basin. Abundant basin
secondary craters are scattered across the area, mostly created by the
Orientale basin impact to the west and north. A particular interest has
been carried to the topography surrounding the Shackleton crater, which
is nearly coincident with the South pole, at 89.9° latitude and
0° longitude, with 19 km diameter, according to USGS coordinates.
The AMIE mosaic of Shackleton crater spreads among 88,80 ° and 90
° S in latitude. The high resolution mosaic give details about the
complete rim of this crater with different illumination angles. The
mosaic of Shackleton crater was extended in a global map of the south
pole region. Eventually, the method used will be applied to mapping all
areas of interest where AMIE has provided high resolution observations.
The AMIE maps of the north and south pole of the Moon are presented.
@--------------------------------------------------------------------
Title: Photometric anomalies of the lunar surface studied
with SMART-1 AMIE data
Authors: Kaydash, V.; Kreslavsky, M.; Shkuratov, Yu.;
Gerasimenko, S.; Pinet, P.; Josset, J.-L.;
Beauvivre, S.; Foing, B.; AMIE SMART-1 Team
Bibliographic Code: 2009Icar..202..393K
Abstract
We present new results from the mapping of lunar photometric function
parameters using images acquired by the spacecraft SMART-1 (European
Space Agency). The source data for selected lunar areas imaged by the
AMIE camera of SMART-1 and the data processing are described. We
interpret the behavior of photometric function in terms of lunar
regolith properties. Our study reveals photometric anomalies on both
small (sub-kilometer) and large (tens of kilometers) scales. We found
the regolith mesoscale roughness of lunar swirls to be similar in Mare
Marginis, Mare Ingenii, and the surrounding terrains. Unique photometric
properties related to peculiarities of the millimeter-scale regolith
structure for the Reiner Gamma swirl are confirmed. We identified
several impact craters of subkilometer sizes as the source of
photometric anomalies created by an increase in mesoscale roughness
within the proximal crater ejecta zones. The extended ray systems reveal
differences in the photometric properties between proximal and distant
ejecta blankets. Basaltic lava flows within Mare Imbrium and Oceanus
Procellarum indicate higher regolith porosity for the redder soils due
to differences in the chemical composition of lavas.
@--------------------------------------------------------------------
Title: Special issue with papers from the ESLAB 2008
Symposium on `Cosmic Cataclysms and Life'
Authors: André, N.; Foing, B. H.; Cockell, C. S.
Bibliographic Code: 2009IJAsB...8..145A
Abstract
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Title: X-ray fluorescence observations of the moon by
SMART-1/D-CIXS and the first detection of Ti Kalpha from
the lunar surface
Authors: The SMART-1 Team; Swinyard, B. M.; Joy, K. H.;
Kellett, B. J.; Crawford, I. A.; Grande, M.;
Howe, C. J.; Fernandes, V. A.; Gasnault, O.;
Lawrence, D. J.; Russell, S. S.; Wieczorek, M. A.;
Foing, B. H.; The SMART-1 team
Bibliographic Code: 2009P&SS...57..744T
Abstract
The demonstration of a compact imaging X-ray spectrometer (D-CIXS),
which flew on ESA's SMART-1 mission to the Moon (Racca et al., 2001;
Foing et al., 2006), was designed to test innovative new technologies
for orbital X-ray fluorescence spectroscopy. D-CIXS conducted
observations of the lunar surface from January 2005 until SMART-1
impacted the Moon in September 2006. Here, we present scientific
observations made during two solar flare events and show the first
detection of Titanium Kalpha from the lunar surface. We discuss the
geological implications of these results. We also discuss how experience
from D-CIXS has aided the design of a similar instrument (Chandrayaan-1
X-ray Spectrometer (C1XS)) that was launched on the 22nd October 2008 on
India's Chandrayaan-1 mission to the Moon.
@--------------------------------------------------------------------
Title: The C1XS X-ray Spectrometer on Chandrayaan-1
Authors: Grande, M.; Maddison, B. J.; Howe, C. J.;
Kellett, B. J.; Sreekumar, P.; Huovelin, J.;
Crawford, I. A.; Duston, C. L.; Smith, D.; Anand, M.;
Bhandari, N.; Cook, A.; Fernandes, V.; Foing, B.;
Gasnaut, O.; Goswami, J. N.; Holland, A.; Joy, K. H.;
Kochney, D.; Lawrence, D.; Maurice, S.; Okada, T.;
Narendranath, S.; Pieters, C.; Rothery, D.;
Russell, S. S.; Shrivastava, A.; Swinyard, B.;
Wilding, M.; Wieczorek, M.
Bibliographic Code: 2009P&SS...57..717G
Abstract
The Chandrayaan-1 X-ray Spectrometer (C1XS) is a compact X-ray
spectrometer for the Indian Space Research Organisation (ISRO)
Chandrayaan-1 lunar mission. It exploits heritage from the D-CIXS
instrument on ESA's SMART-1 mission. As a result of detailed
developments to all aspects of the design, its performance as measured
in the laboratory greatly surpasses that of D-CIXS. In comparison with
SMART-1, Chandrayaan-1 is a science-oriented rather than a technology
mission, leading to far more favourable conditions for science
measurements. C1XS is designed to measure absolute and relative
abundances of major rock-forming elements (principally Mg, Al, Si, Ca
and Fe) in the lunar crust with spatial resolution <=25 FWHM km, and
to achieve relative elemental abundances of better than 10%.
@--------------------------------------------------------------------
Title: SMART-1 Results and Targets for LRO
Authors: Foing, B. H.; Koschny, D.; Grieger, B.;
Josset, J.-L.; Beauvivre, S.; Grande, M.;
Huovelin, J.; Keller, H. U.; Mall, U.; Nathues, A.;
Malkki, A.; Noci, G.; Sodnik, Z.; Kellett, B.;
Pinet, P.; Chevrel, S.; Cerroni, P.;
de Sanctis, M. C.; Barucci, M. A.; Erard, S.;
Despan, D.; Muinonen, K.; Shevchenko, V.;
Shkuratov, Y.; Ellouzi, M.; Peters, S.; Borst, A.;
Baxkens, F.; Boche-Sauvan, L.; Mahapatra, P.;
Almeida, M.; Frew, D.; Volp, J.; Heather, D.;
McMannamon, P.; Camino, O.; Racca, G.
Bibliographic Code: 2009LPICo1483...39F
Abstract
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Title: Search for organics and life on Mars
Authors: Ehrenfreund, P.; Foing, B. H.
Bibliographic Code: 2009GeCAS..73Q.320E
Abstract
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Title: UV And Space Exposure Of Aromatic Compounds On The
EXPOSE-R Facility Onboard ISS
Authors: Bryson, Kathryn; Salama, F.; Enhrenfreund, P.;
Ricco, A. J.; Peeters, Z.; Foing, B. H.;
Monaghan, E.; Wills, D.; Breitfellner, M.;
Jessberger, E.; Robert, F.; Mumma, M.
Bibliographic Code: 2009AAS...21440210B
Abstract
PAHs and fullerenes are thought to be among the carriers for numerous
astronomical absorption and emission features and have been identified
in meteorites. In addition, aromatic networks are likely the most
abundant organic material in space. Thin films of selected PAHs and
fullerenes will be subjected to the low Earth orbit environment as part
of the Organics experiment on the multi-user facility EXPOSE-R onboard
the International Space Station. EXPOSE-R will be mounted on the
International Space Station ISS in spring 2009. The Organics experiment
on EXPOSE-R will monitor the chemical evolution, survival, destruction
and chemical modification of polycyclic aromatic hydrocarbons (PAHs) and
fullerenes in space environment. The radiation dose that is collected by
the samples during flight exceeds the limits of simulations in the
laboratory and will greatly enhance our knowledge on the evolution of
large molecules in space environments. Dark samples will be shielded
from the UV photons and will enable us to differentiate between the
effects of exposure to photons and cosmic rays. In addition, the
experiment hosts pressurized and vented sample cells. All the samples
will be monitored before and after exposure to space environment. We
present spectra measured in the UV-Vis-NIR range of the flight samples
prior to space exposure.
@--------------------------------------------------------------------
Title: PCR-based Analysis of Microbial Communities in
Extreme Environment: Results from EuroGeoMars MDRS
campaign
Authors: Thiel, C.; Wills, D.; Foing, B.; Wadham, J.;
Cullen, D.; van Sluis, C.
Bibliographic Code: 2009EGUGA..1113414T
Abstract
Deoxyribonucleic acid (DNA) is found in almost all living organisms. The
main function of DNA molecules is the long-term storage of genetic
information.They are passed on from generation to generation as the
hereditary material. This molecular structure is often compared to a
genetic blueprint, a fingerprint, which is unique for each organism and
can therefore be used as a mean of identification. In 1984 a
revolutionary technique called polymerase chain reaction (PCR) was
established, able to amplify a single or few copies of DNA molecules
across several orders of magnitude, generating millions of copies of the
original DNA fragment. PCR is nowadays a common technique used in
medical and biological research laboratories for a large variety of
applications like functional analysis of genes, DNA-based phylogeny,
diagnosis of hereditary diseases, detection and diagnosis of infectious
diseases, and identification of genetic fingerprints. This powerful tool
gives us the opportunity to investigate, if there is or was life on Mars
since DNA fragments are highly stable what allows not only amplification
from living organisms but also from samples with an age of several
thousand years. If we assume that micro-organisms were exchanged between
Mars and Earth via meteorites, it is imaginable that Martian life might
also be based on DNA as carrier of genetic information. Therefore our
goal is to establish a routine for detection of DNA from micro-organisms
based on the effective but also robust and simple PCR technique,
demonstrated during the EuroGeoMars simulation campaign at Mars Desert
Research Station (MDRS). We have already analysed some MDRS soil samples
at ESTEC ExoGeoLab facility. During the MDRS simulation we will show
that it is possible to establish a minimal molecular biology lab in the
habitat for an immediate on site analysis by PCR after sample
collection. Samples will be taken from different locations and soil
depths. The sample analysis will start immediately after returning to
the habitat and will be finished during the following days. DNA will be
isolated from micro-organisms by Powersoil DNA isolation kit and serves
as template for PCR using oligonucleotides specific for ribosomal DNA to
identify representatives of the different groups of micro-organisms:
archaea, bacteria and eukaryotes. PCR products will be analysed by
agarose gel electrophoresis and documented via UV-trans-illuminator and
digital camera.
@--------------------------------------------------------------------
Title: EuroGeoMars mission and techniques: First results
for geology and geochemistry
Authors: Peters, S. T. M.; Borst, A.; Wendt, L.; Gross, C.;
Stoker, C.; Zhavaleta, J.; Sarrazin, P.; Slob, E.;
Pletser, V.; Foing, B.
Bibliographic Code: 2009EGUGA..1113353P
Abstract
The EuroGeoMars expedition forms part of the European Space Agency's
ExoGeoLab research project and is a test campaign at the MDRS (Mars
Desert Research Station), which is operated by the Mars Society, in the
Utah desert, US. MDRS has yet been used by research groups of various
interest as an analogue site to the Martian environment. The goal of
this expedition is to simulate the employment of various instruments and
sample return under Martian conditions, while carrying out several
geological and biological investigations. In this paper we present our
methods and first results for the geological and geochemistry
investigations. Two main geological investigations have been carried
out, of which one includes mapping of the sequence stratigraphy and
internal structure of Quaternary alluvial fan deposits, 5 km South-West
of the MDRS. Alluvial fans are formed when a stream gradient decreases
over a relatively small area and therefore coarse-grained sediments are
being deposited. Alluvial fans on Mars are of particular interest
because they may have formed, as they do on Earth, a niche for life at
deposition time. If any was present, the sediments may contain detritus
that was transported by the river from the hinterland. Furthermore, the
internal structure and lithology represent the depositional environment,
water activity, and climatological perturbations. These three factors
provide main implications for the conditions and possibilities of
maintaining life. Mineralogical variations represent changes in the
source area of the sediments and hence possible tectonic activity. The
fan that we investigated measures 1.5 x 1.5 km and is made up of several
stratigraphic sequences that we defined by classic geological methods.
We followed the sedimentary sequences laterally using a Ground
Penetrating Radar system (GPR) and taking samples for ground truth by
drilling. All samples were analyzed on mineral content using Raman
spectroscopy and XRF (X-Ray Fluorescence) for mineralogical and
elemental analysis respectively. We created lacquer peels from several
sequences in order to sample and study sedimentary structures. The
procedure to make lacquer peels is to poor lacquer over an outcrop and
sticking the unconsolidated sediments to a piece of cloth, which is
subsequently pasted upon a hardboard plank. Another investigation that
was carried out focuses on the possibilities and restrictions to the
geologist for future fieldwork on Mars. Hence the investigators did
similar type of experiments as for the alluvial fan, wearing spacesuits
and spending restricted time outside as they would on a Martian base.
The EuroGeoMars expedition is the first in a series of manned planetary
mission simulations.
@--------------------------------------------------------------------
Title: Human Aspects and Habitat Studies from EuroGeoMars
Campaign
Authors: Boche-Sauvan, L.; Pletser, V.; Foing, B. H.;
Eurogeomars Team
Bibliographic Code: 2009EGUGA..1113323B
Abstract
Introduction: In a human space mission, the human factor is one of the
dominant aspects, which may strongly influence work results and
efficiency. To quantify such a difficult and uncontrollable aspect of
space missions, it is necessary to reproduce as exactly as possible the
environmental and technical conditions in which astronauts may be
confronted: limited re-sources, social interactions in an isolated and
cramped area... We will take the benefit of the EuroGeoMars campaign
in the Mars Desert Research Station (MDRS, Mars Society) in Utah to
observe and measure these characteristics. EuroGeoMars campaign: The
EuroGeoMars team aims at assessing the development of scientific
protocols and techniques in geology and biology research in planetary
conditions. In this framework, MRDS simulation constitutes its main
achievement. The scientific investigations conducted in MRDS are
expected to provide valuable results, beyond the simple reflection on
how managing planetary specific conditions. Nevertheless, the different
scientific protocols, even tailored for extreme environmental
conditions, require an exhaustive analysis to evaluate how the results
and their timing may possibly be affected. MDRS: The MDRS habitat will
demand the crew members to work in a cramped environment, surrounded by
dust and very limited manpower. Moreover, energy power and communication
bandwidth will be limited to the crew members. Human aspects and
habitat studies: The crewmember will work in an uncomfortable
environment in the habitat: dust, cramping and crowd. Moreover, the
sustainibility of the mission will relie on an optimal energy and
ressources sharing. This will impose a planification of the different
investigating activities. The study of the human aspects and habitat
will be performed in terms of impact on scientific and technical tasks
rather than in terms of crew's comfort. As any astronaut will previously
be aware of the daily condition, we want to improve the working
conditions in the aim of optimizing the obtaining of scientific results.
A mission off the land will be worth only with a real scientific gain.
Moreover, as the schedule is focused on the work time, better working
conditions will provide better general living resentment. Following
this approach, observations and interviews of the crewmembers in the
simulation will be done. That will cover several sides: layout,
equipment, area, and mostly man-machine interface. This last side will
be the most studied in different situation: during daily life, in the
laboratory, in the workshop and during the EVA. Indeed, the
specifications for such an interface will be different according to the
use: easy use in EVA, but with a good layout in the habitat.
Acknowledgements: We thank the EuroGeo-Mars teams for their support in
this study, and Mars Society for the opportunity of such a campaign.
@--------------------------------------------------------------------
Title: SMART-1 Results and Lessons for Future Exploration
Authors: Foing, B. H.
Bibliographic Code: 2009EGUGA..1113267F
Abstract
We summarise SMART-1 lunar highlights relevant for future lunar
exploration. SMART-1 has been useful in the preparation of Selene
Kaguya, the Indian lunar mission Chandrayaan-1, Chinese Chang'E 1 , the
US Lunar Reconnaissance Orbiter, LCROSS, and subsequent lunar landers
(Google Lunar X-prize, International Lunar Network, Moon-NEXT, cargo and
manned landers). SMART-1 is contributing to prepare the next steps for
exploration: survey of resources, search for ice, monitoring polar
illumination, and mapping of sites for potential landings, international
robotic villages and for future human activities and lunar bases.
Overview of SMART-1 mission and payload: SMART-1 is the first in the
programme of ESA's Small Missions for Advanced Research and Technology
[1,2,3]. Its first objective has been achieved to demonstrate Solar
Electric Primary Propulsion (SEP) for future Cornerstones (such as
Bepi-Colombo) and to test new technologies for spacecraft and
instruments. The SMART-1 spacecraft has been launched on 27 Sept. 2003,
as an Ariane-5 auxiliary passenger and injected in GTO Geostationary
Transfer Orbit. The SMART-1 spacecraft reached on 15 March 2005 a lunar
orbit 400-3000 km for a nominal science period of six months, with 1
year extension until impact on 3 September 2006. SMART-1 science
payload, with a total mass of some 19 kg, featured many innovative
instruments and advanced technologies [1], with a miniaturised
high-resolution camera (AMIE) for lunar surface imaging, a near-infrared
point-spectrometer (SIR) for lunar mineralogy investigation, and a very
compact X-ray spectrometer (D-CIXS) [4-6] for fluorescence spectroscopy
and imagery of the Moon's sur-face elemental composition. The payload
also included two plasma experiments: SPEDE (Spacecraft Potential,
Electron and Dust Experiment) and EPDP (Electric propulsion diagnostic
Package), an experiment (KaTE) that demonstrated deep-space telemetry
and telecommand communications in the X and Ka-bands, a radio-science
experiment (RSIS), a deep space optical link (Laser-Link Experiment),
using the ESA Optical Ground station in Tenerife, and the validation of
a system of autonomous navigation (OBAN) based on image processing.
SMART-1 lunar science and exploration results: A package of three
multiband mapping instruments has performed science and exploration at
the Moon. AMIE (Advanced-Moon micro-Imager Experiment). AMIE is a
miniature high resolution (35 m pixel at 350 km perilune height) camera,
equipped with a fixed panchromatic and 3-colour filter, for Moon
topography and imaging support to other experiments [7,10,11]. The micro
camera AMIE has provided high-resolution CCD images of selected lunar
areas. It included filters deposited on the CCD in white light + three
filters for colour analyses, with bands at 750 nm, 900 nm and 950 nm
(measuring the absorption of pyroxene and olivine). Lunar North polar
maps and South pole repeated high resolution images have been obtained,
giving a monitoring of illumination to map potential sites relevant for
future exploration. AMIE images provided a geological context for
SIR and D-CIXS data, and colour or multi-phase angle complement. AMIE
has been used to map sites of interest in the South Pole -Aitken basin
relevant to the study of cataclysm bombardment, and to preview future
sites for sampling return. SMART-1 studied also volcanic processes, and
the coupling between impacts and volcanism. D-CIXS (Demonstration of a
Compact Imaging X-ray Spectrometer). DCIXS is based on novel detector
and filter/collimator technologies, and has performing the first lunar
X-ray fluorescence global mapping in the 0.5-10 keV range [4,5,9], in
order to map the lunar elemental composition. It was supported in its
operation by XSM (X-ray Solar Monitor) which also moni-tored coronal
X-ray emission and solar flares [6]. For instance, D-CIXS measurements
of Si, Mg, Al, Si, Ca & Fe lines at 1.25, 1.49, 1.74, 3.7 & 6.4
keV, were made over North of Mare Crisium during the 15 Jan 2005 solar
flare, permitting the first detection of Calcium from lunar orbit [9].
Bulk crustal composition has bearing on theories of origin and evolution
of the Moon. D-CIXS produced the first global measurements of the lunar
surface in X-ray fluorescence (XRF), elemental abundances of Mg, Al and
Si (and Fe when solar activity permitted) across the whole Moon. The
South Pole-Aitken Basin (SPA) and large lunar impact basins have been
also measured with D-CIXS. D-CIXS has been improved for the C1XS
instrument adapted to ISRO Chandrayaan-1. SIR (Smart-1 Infra-Red
Spectrometer). SIR has been operating in the 0.9-2.6 mum wavelength
range and carrying out mineralogical survey of the lunar crust. SIR had
high enough spectral resolution to separate the pyroxene and olivine
signatures in lunar soils. SIR data with spatial resolution as good as
400 m permitted to distinguish units on central peaks, walls, rims and
ejecta blankets of large impact craters, allowing for stratigraphic
studies of the lunar crust. SIR has been improved for the Chandrayaan-1
SIR2 instrument. SMART-1 overall planetary science: SMART-1 science
investigations included studies of the chemical composition of the Moon,
of geophysical processes (volcanism, tectonics, cratering, erosion,
deposition of ices and volatiles) for comparative planetology, and high
resolution studies in preparation for future steps of lunar exploration.
The mission addressed several topics such as the accretional processes
that led to the formation of rocky planets, and the origin and evolution
of the Earth-Moon system [8]. SMART-1 operations and coordination: The
Experiments have been run according to illumination and altitude
conditions during the nominal science phase of 6-months and 1 yr
extension, in elliptical Moon orbit. The planning and co-ordination of
the Technology and science experiments operations was carried out at
ESA/ESTEC (SMART-1 STOC). The data archiving is based on the PDS
(Planetary Data System) Standard. The SMART-1 observations have been
coordinated with follow-up missions. References: [1] Foing, B. et al
(2001) Earth Moon Planets, 85, 523 . [2] Racca, G.D. et al. (2002) Earth
Moon Planets, 85, 379. [3] Racca, G.D. et al. (2002) P&SS, 50, 1323.
[4] Grande, M. et al. (2003) P&SS, 51, 427. [5] Dunkin, S. et al.
(2003) P&SS, 51, 435. [6] Huovelin, J. et al. (2002) P&SS, 50,
1345. [7] Shkuratov, Y. et al (2003) JGRE 108, E4, 1. [8] Foing, B.H. et
al (2003) Adv. Space Res., 31, 2323. [9] Grande, M. et al (2007)
P&SS 55, 494. [10] Pinet, P. et al (2005) P&SS, 53, 1309. [11]
Josset J.L. et al (2006) Adv Space Res, 37, 14. [12] Foing B.H. et al
(2006) Adv Space Res, 37, 6. Links: http://sci.esa.int/smart-1/,
http://sci.esa.int/ilewg/
@--------------------------------------------------------------------
Title: Design and Demonstration of Minimal Lunar Base
Authors: Boche-Sauvan, L.; Foing, B. H.; Exohab Team
Bibliographic Code: 2009EGUGA..1113254B
Abstract
Introduction: We propose a conceptual analysis of a first minimal lunar
base, in focussing on the system aspects and coordinating every
different part as part an evolving architecture [1-3]. We justify the
case for a scientific outpost allowing experiments, sample analysis in
laboratory (relevant to the origin and evolution of the Earth,
geophysical and geochemical studies of the Moon, life sciences,
observation from the Moon). Research: Research activities will be
conducted with this first settlement in: - science (of, from and on the
Moon) - exploration (robotic mobility, rover, drilling), - technology
(communication, command, organisation, automatism). Life sciences. The
life sciences aspects are considered through a life support for a crew
of 4 (habitat) and a laboratory activity with biological experiments
performed on Earth or LEO, but then without any magnetosphere protection
and therefore with direct cosmic rays and solar particle effects.
Moreover, the ability of studying the lunar environment in the field
will be a big asset before settling a permanent base [3-5]. Lunar
environment. The lunar environment adds constraints to instruments
specifications (vacuum, extreme temperature, regolith, seism,
micrometeorites). SMART-1 and other missions data will bring
geometrical, chemical and physical details about the environment (soil
material characteristics, on surface conditions...). Test bench. To
assess planetary technologies and operations preparing for Mars human
exploration. Lunar outpost predesign modular concept: To allow a human
presence on the moon and to carry out these experiments, we will give a
pre-design of a human minimal lunar base. Through a modular concept,
this base will be possibly evolved into a long duration or permanent
base. We will analyse the possibilities of settling such a minimal base
by means of the current and near term propulsion technology, as a full
Ariane 5 ME carrying 1.7 T of gross payload to the surface of the Moon
(Integrated Exploration Study, ESA ESTEC [1,2]). We will focus on the
easiest and the soonest way in settling a minimal base immediately
operational in scientific experimentation, but not immediately
autonomous. It will prepare the next permanent lunar base by assessing
its technologies, and give scientific results about the environment. The
autonomy will be gained in the evolution of the base, and added
equipment. A lunar outpost in a polar region would allow missions longer
than 14 days, and a frequent addition of equipments. Moreover, a polar
outpost will get both advantages of far-side for simulating direct or
indirect communications to Earth and dark-side for observations. The low
solar rays incidence may permit having ice in deep craters, which will
be beneficial for the evolution of the outpost into a autonomous base.
The South Pole, by its position on the edge of the South Pole Aitken
(SPA) Basin, will allow different fast new data in analysis mantle
samples, easily reachable due to the crater morphology. These samples
will constrain the putative Late Heavy Bombarment (LHB). After a robotic
sample return mission, a human presence will allow deeper research
through well chosen geological samples [6]. In this modular concept, we
consider various infrastructure elements: core habitat, EVA, crew
mobility, energy supply, recycling module, communication, green house
and food production, operations. Many of these elements have already
been studied in space agencies' architecture proposals, with the
tech-nological possibilities of industrial partners (lunar landers,
lunar orbiter, rovers...). A deeper reflection will be therefore
done about the core habitat and the laboratory equipment, proposing
scientific priority experiments. Each element will be added in a range
considering their priority to life support in duration [7]. Considering
surface operations, protocols will be specified in the use of certain
elements. After a reflexion on the different dependancies and priorities
between these modules, a demonstration can assess the reliability of the
concept and develop the evolution according to the practical needs. We
shall also discuss experience form the ExoHab project and EuroGeoMars
cmapign at Mars Desert Research station. References: [1] "Exploration
Architecture Trade Report", ESA, 2008, [2] "Integrated Exploration
Architecture", ESA, 2008, [3] 9th ILEWG International Conference on
Exploration and Utilization of the moon, 2007, Foing et al Eds.,
(http://sci.esa.int/ilewg) [4] "The Moon: Resources, Future Development
and Colonization", David Schrunk, Burton Sharpe, Bonnie Cooper and Madhu
Thangavelu, 1999. [5] "The Moon as a Platform for Astronomy and Space
Science", B.H. Foing, ASR 14 (6), 1994. [6] "The Moon after Apollo, 40
Years Later: Why and what Samples to Return?", Johannes Geiss, Alpbach
summer school 2008. [7] "Advanced Life Support, Baseline Values and
Assumptions Document", Anthony J. Hanford, 2004
@--------------------------------------------------------------------
Title: Basic Mars Navigation System For Local Areas
Authors: Petitfils, E.-A.; Boche-Sauvan, L.; Foing, B. H.;
Monaghan, E.; Crews, Eurogeomars
Bibliographic Code: 2009EGUGA..1113242P
Abstract
Introduction: This project has been first set up as a basic solution in
navigation during EVA (extra-vehicular activities) in the Mars Society
Desert Research Station in the desert of Utah. The main idea is to keep
the system as simple as possible so that it can be easily adaptable and
portable. The purpose of such a device is to tell the astronauts in EVA
where they roughly are and then letting them reaching different points
in avoiding any risky way. Thus the precision needed has not to be
really high: even if it is about 50m, every astronaut can then look on a
map and be able to design a way to another point. This navigation system
will improve the safety of the EVA as it is an added reliable
orientating tool. Concept: To look at a simple way to localize oneself,
one should have a look at what has been done by mankind on Earth. Today,
everyone can think of the GPS because it's simple and very reliable.
However the infrastructure for such a system is huge and will not be for
sure available during the first missions. We can think of course of a
basic GPS using the satellites being in orbit but this approach is not
yet as simple as we would like. If we want to keep the sky in sight, we
can use the stars and the moons of Mars. Yet this would be a good
solution and we can even have a star tracker that would give a good
position according to the time of the picture. This solution has to be
kept in mind but a star tracker is quite big for an astronaut without
any rover nearby and using the sky may not be as precise as one should
expect. Another useful tool is the compass. It has been used for
centuries by sailors but on Mars, without a good magnetic field for this
purpose. But sailors also use lighthouses and some placemarks on the
land to localize themselves. This is done with a compass, measuring the
angle between a placemark and the magnetic North. With two angles, we
can then have the position of the boat. The idea here is the same:
measuring the angles between different placemarks so that we can compute
the position. But which placemarks? We have to think about something
that can be installed on Mars and is light enough to be brought there.
Balloons are really light, and in order to place them, we need a gas as
helium (or hydrogen) and also some rope. Hydrogen is likely to be
produced in situ and rope will be useful for astronauts. So we started
on a concept with some balloons around the base, with different colors
or patterns. The crew in EVA can thus know where the base is every time
they are in sight of a balloon and with at least three balloons; they
can compute their position according to the base. Procedure of the
test: During EVA, the astronauts will measure the angle between the
different balloons. The balloons are high in the sky so they can be seen
far from their location. This is particularly important on Mars where
the horizon is nearer than on Earth. The balloons have different colors
so they can be identified and we can even think of adding an autonomous
colored light under so they can be observed during the night. With good
quality balloons, we can keep them in the sky for a few days without
maintenance. Angle measurement is done thanks to a camera. A numeric
camera can have a precision of less than 0.01°/pixel, which is
enough for our application. The distance between the different balloons
can easily be seen in a free picture management software and a Matlab
tool is under development for this. An algorithm is then run and it
gives the positions that fit with the observations on a map. Simulation
gave areas 20m width, which is enough for the astronaut who has a map.
The exact precision will be investigated in situ, at the MDRS. For this
first test bench, computations will be manually done on a computer in
order to validate the concept without huge development. Afterwards, one
can imagine an implementation on a PDA brought by the astronauts. This
PDA would have its own camera so the process can be fully automatic.
Such a system can also implement other navigation system as a Martian
GPS or a radio localization system like a VOR in order to enhance the
reliability of the system and use all the advantages of each method.
Acknowledgements: We thank the ExoGeoLab, EuroGeoMars teams for support
during tests, operations and data analysis. References: [1]
"ExoGeoLab Lander/Rover instruments and EuroGeoMars MDRS campaign", B.H.
Foing, LPSC abstract 2009
@--------------------------------------------------------------------
Title: Report from ILEWG and Cape Canaveral Lunar
Declaration 2008
Authors: Foing, B. H.
Bibliographic Code: 2009EGUGA..1113223F
Abstract
We shall report on the ILEWG charter, goals and activities, on ICEUM
"lunar declarations" and follow-up activities, with focus on societal
questions, and the Cape Canaveral Lunar Declaration 2008. ILEWG
charter: ILEWG, the International Lunar Exploration Working Group is a
public forum created in 1994, sponsored by the world's space agencies to
support "international cooperation towards a world strategy for the
exploration and utilization of the Moon - our natural satellite". The
charter of ILEWG is: - To develop an international strategy for the
exploration of the Moon - To establish a forum and mechanisms for the
communication and coordination of activities - To implement
international coordination and cooperation - In order to facilitate
communication among all interested parties ILEWG agrees to establish an
electronic communication network for exchange of science, technology and
programmatic information related to lunar activities ILEWG meets
regularly, at least, once a year, and leads the organization of an
International Conference in order to discuss the state of lunar
exploration. Formal reports are given at COSPAR meetings and to space
agencies. ILEWG is sponsored by the world's space agencies and is
intended to serve three relevant groups: - actual members of the ILEWG,
ie delegates and repre-sentatives of the participating Space Agencies
and organizations - allowing them to discuss and possibly harmonize
their draft concepts and plans - team members of the relevant space
projects - allowing them to coordinate their internal work according to
the guidelines provided by the Charter of the ILEWG - members of the
general public and of the Lunar Explorer's Society who are interested
and wish to be informed on the progress of the Moon projects and
possibly contribute their own ideas ILEWG activities and working
groups: ILEWG task groups include science, technology, human aspects,
socio-economics, young explorers and outreach, programmatics, roadmaps
and synergies with Mars exploration. Users can obtain information on how
to participate, as well as details on the latest news and events
regarding lunar exploration, forthcoming meetings, relevant reports and
documents of importance for the work of the ILEWG, summary descriptions
of current lunar exploration projects (such as SMART-1, Chang'E1,
Selene, Chandrayaan-1, LRO, LCROSS) funded by various space agencies,
and basic data on the Moon itself. Activities of the related space
agencies and organizations can also be found. ILEWG has been organising
International Conferences on Exploration and Utilisation of the Moon
(ICEUM) since 1994, whose proceedings are published. It has also
sponsored a number of activities, workshops, tasks groups and
publications in collabora-tions with other organisations: COSPAR, space
agencies, IAA, IAF, EGU (see references below). In accor-dance with its
charter, ILEWG reports to COSPAR, and a summary was given at Montreal
COSPAR2008 on ILEWG activities conducted since the previous COSPAR2006
assembly in Beijing. The recent ILEWG International Conference on
Exploration and Utilisation of the Moon, were held respectively in
Udaipur, India (ICEUM6, 2004), in Toronto, Canada (ICEUM7, 2005), in
Beijing (ICEUM8, 2006), Sorrento (ICEUM9, 2007) and Port Canaveral
(ICEUM10/LEAG/SRR, 2008 in conjunction with the NASA Lunar Exploration
Analysis Groups and Space Resources Roundtable annual meetings). We'll
report on the Cape Canaveral Lunar Declaration and on follow-up
activities, in particular in coordination with space agencies, COSPAR
and IAF. References: [1] 1st International Lunar Workshop, Balsiger H.
et al., Editors, European Space Agency, 1994. ESA-SP-1170. [2] 2nd
International Lunar Workshop, Kyoto, H. Mizutani, editor, Japan Space
Forum Publisher, 1997. [3] 3rd International Lunar Workshop, Moscow
1998, E. Galimov, editor. [4] ICEUM4, ESTEC, 2000, ESA SP-462, B.H.
Foing & M. Perry, editors. [5] ICEUM5, Hawaii Nov 2003, Durst S.M.
et al, Editors, Vol 108, 1-576 pp, Science and Technology Series,
American Astronautical Society, 2004. [6] ICEUM6, Udaipur 2004, Bhandari
N., Editor, Journal Earth System Science, India, 114, No6, Dec 2005, pp.
573-841. [7] ICEUM7, Toronto Sept 2005, sci.esa.int/ilewg. [8] ICEUM8,
Beijing July 2006, Journal of Chinese Society of Astronautics, Vol. 28
Sup., 2007, Ji W., Editor. [9] ICEUM9, Sorrento, Italy, Foing B.,
Espinasse S., Kosters G., Editors. http://sci.esa.int/iceum9, Dec.
2007), [11] Ehrenfreund, P., Foing, B.H., Cellino, A. Editors, The Moon
and Near Earth Objects, ASR Vol 37, 1, 2006. [12] Foing, B.H. et al
editors, 'Astronomy and Space Science from the Moon', ASR 14, 6, 1994.
[13] Foing, B.H. et al, editor, Lunar Exploration, Planetary and Space
Science, Vol 50, 14-15, 2002. [14] Foing, B.H., Heather, D. editors,
'Lunar Exploration 2000', ASR Vol 30, Nr 8, 2002. [15] Hunt-ress, W. et
al 'The next steps in exploring deep space - A cosmic study by the IAA',
Acta Astronautica, Vol 58, Issues 6-7, 2006, p302-377. [16] Ip W.-H.,
Foing, B.H., Masson Ph.L., editors, The Moon and Mars, ASR Vol 23, 11,
1999.
@--------------------------------------------------------------------
Title: EuroGeoMars campaign at Mars Desert Research
Station: Preparing for Future Mars Landers and
Sample
Authors: Foing, B. H.; Pletser, V.; Stoker, C.;
Boche-Sauvan, L.
Bibliographic Code: 2009EGUGA..1113180F
Abstract
Background: Surface science is one of the prime objectives of current
and future Mars, Moon, or planetary missions and encompasses a wide
range of activities from global mapping via specific studies of
localised regions until microscopic scales. The studies of rocks and
soil in situ, or with sample return missions, require the development of
systematic multi-instruments protocols, characterisation diagnostics,
and merging of data from various techniques. Both photogeology and
mineralogical wide scale mapping have been performed to some extent
previously so significant new surface science results may only come from
co-ordinated multi-instrument operations operating from the surface.
EuroGeoMars MDRS campaign: The goal of the mission (from 24 January to 1
March 2009) is to demonstrate and validate a procedure for Martian
surface in-situ and return science. This chain begins with
characterisation of the local surface and close sub-surface environment,
before moving on to sample extraction and analysis. The characterisation
stage involves a survey of a sample area in the vicinity of the MDRS
site by our geologists and other team members. This utilises satellite
and aerial photography to inform the overallmorphology and geological
unit distribution, with the specific geological and geochemical context
being provided through the use of imagers and spectrometers. Further
reconnaissance is used to plan sample-extraction EVAs at sites of
geochemical and astrobiological significance. Characterisation of
larger-scale features is conducted in-situ (for example using ground
penetrating radar to investigate the close sub-surface). Results from
these sorties inform the choice and planning of sites for surface and
sub-surface sampling. The sample extraction step - the nature of which
is dependent on the identified areas of interest - involves standard
geological tools such as rock drills and scoops etc, as well as more
specific techniques such as lacquer peels. These samples are returned to
the MDRS for analysis using microscopes and other analysis techniques.
These documented samples are afterward taken to ESTEC and collaborators
institutes for analysis by various techniques.
@--------------------------------------------------------------------
Title: A Small Lunar Rover for Reconnaissance in the
Framework of ExoGeoLab Project, System Level Design
Authors: Noroozi, A.; Ha, L.; van Dalen, P.; Maas, A.;
de Raedt, S.; Poulakis, P.; Foing, B. H.
Bibliographic Code: 2009EGUGA..1113167N
Abstract
Scientific research is based on accurate measurement and so depends on
the possibilities of accurate instruments. In planetary science and
exploration it is often difficult or even impossible in some cases to
gather accurate and direct information from a specified target. It is
important to gather as much information as possible to be able to
analyze and extract scientific data from them. One possibility to do so
is to send equipments to the target and perform the measurements
locally. The measurement data is then sent to base station for further
analysis. To send measurement instruments to measurement point it is
important to have a good estimation of the environmental situation
there. This information can be collected by sending a pilot rover to the
area of interest to collect visual information. The aim of this work is
to develop a tele-operated small rover, Google Lunar X-Prize (GLXP)
class, which is capable of surviving in the Moon environment and perform
reconnaissance to provide visual information to base station of
ExoGeoLab project of ESA/ESTEC. Using the state of the art developments
in electronics, software and communication technologies allows us to
achieve increase in accuracy while reducing size and power consumption.
Target mass of the rover is lees than 5 kg and its target dimension is
300 x 60 x 80 mm3. The small size of the rover gives the possibility of
accessing places which are normally out of reach. The required power for
operation and the cost of launch is considerably reduced compared to
large rovers which makes the mission more cost effective. The mission
of the rover is to capture high resolution images and transmit them to
base station. Data link between lover and base station is wireless and
rover should supply its own energy. The base station can be either a
habitat or a relay station. The navigation of the rover is controlled by
an operator in a habitat who has a view from the stereo camera on the
rover. This stereo camera gives image information to the base and gives
the possibility for future autonomous navigation by using
three-dimensional image recognition software. As the navigation view
should have minimum delay, the resolution of stereo camera is not very
high. The rover design is divided into four work packages. These work
packages are remote imaging, remote manual navigation, locomotion and
structure, and power system. Remote imaging work package is responsible
for capturing high resolution images, transmitting image data to base
station via wireless link and store the data for further processing.
Remote manual navigation is handling the tele-operation. It collects
stereo images and navigation sensor readouts, transmits stereo images
and navigation data to base station via wireless link, displays the
image and sensor status in a real-time fashion on operator's monitor,
receives command from operator's joystick, transfers navigation commands
to rover via wireless link, and operates the actuators accordingly.
Locomotion and structure takes care of designing the body structure and
locomotion system based on the Moon environment specifications. The
target specifications of rover locomotion system are maximum speed of
200 m/h, maximum acceleration of 0.554 m/s2, and maximum slope angle of
20Ëš . The power system for the rover includes the solar
panel, batteries and power electronics mounted on the rover. The energy
storage in the rover should be able to survive for minimum 500 m
movement on the moon. Subsequently, it should provide energy for other
sub-systems to communicate, navigate and transmit the data. Considering
the harsh environmental issues on the Moon such as dust, temperature
range and radiation, it is vital for the mission that these issues are
considered in the design to correctly dimension reliability and if
necessary redundancy. Corrosion resistive material should be used to
ensure the survival of mechanical structure, moving parts and other
sensitive parts such as electronics. High temperature variation should
be considered in the design of structure and electronics and finally
electronics should be radiation protected.
@--------------------------------------------------------------------
Title: ExoGeoLab Test Bench for Landers, Rovers and
Instruments
Authors: Foing, B. H.
Bibliographic Code: 2009EGUGA..1113122F
Abstract
In the frame of ESTEC technology and research pilot project, we have
started a small pilot facility with a ExoGeoLab and a mini-Habitat,
supported by two design and control offices in the European Space
Incubator (ESI), as well as infrastructure support and manpower. We have
in addition to contribution on external instruments and manpower from
partner institutes. From this test bench and kit of ExoGeoLab
instruments, we plan to operate comprehensive instruments packages that
could help in the technical research and science preparation of
lander/rover missions studied in the frame of Cosmic Vision or the
Exploration programme. The ExoGeoLab research incubator project includes
a sequence of activities: - Data analysis and interpretation of remote
sensing data (MEX, SMART-1, VEX, Cassini-Huygens) and in-situ (Huygens,
MER) , and merging of multi-scale data sets - Procurement and
integration of geophysical, geochemical and astrobiological breadboard
instruments in an surface station and rover (ExoGeoLab) - Research
operations and exploitation of ExoGeoLab test bench for various
conceptual configurations (Moon, Mars, NEO, Titan) - Contribution to the
exploitation of surface lander results (MER, Phenix, MSL, preparation
Exomars) - Scientific simulation of planetary surfaces using laboratory
and modelling tools - Support research for definition and design of
science surface packages on the Moon, Mars, NEO, Titan - Research
support to community preparation of payload for surface lander
opportunities Specific goals and methods of ESTEC ExoGeoLab: we have
started to integrate instruments in an ExoGeoLab crossing various
techniques. The methodic steps for this hands-on research are: 1) We
have procured and adapted instruments to equip a mid-size ExoGeoRover
(made available in collaboration with ESTEC robotics section), and a
small surface station. 2) This terrestrial payload (instruments,
sensors, data handling) will be deployed, operated and used as
collaborative research pilot facility (ExoGeoLab), first tested and
operated at ESTEC, and later transportable 3) We shall perform
functional tests of these instruments, and operate them in terrestrial
conditions to correlate measurements using various techniques. 4) We
shall implement progressively the possibility of remote control of
instruments from an adjacent habitat (ExoHab 6-crew caravan recently
acquired as part of ESTEC skunks pilot project), and a remote science
desk. 5) The suite of measurements includes a comprehensive set with
telescopic imaging reconnaissance and monitoring, geophysical studies,
general geology and morphology context, geochemistry (minerals,
volatiles, organics), subsurface probe, sample extraction and retrieval,
sample analysis. 6) We shall reproduce some simulation of diverse soil
and rocks conditions (mixture of minerals, organics, ice, penetrations
of water, oxydant, organics) and diagnostics 7) We shall use these
instrument packages to characterise geological context, soil and rock
properties, 8) Science investigations will include geology,
geochemistry, measurements relevant to penetration/survival of water,
oxydant, organics, mineral and volatiles diagnostics. 9) After first
validations we shall exploit the facility for collaboration with
partners that will provide some additional guest instruments, and
perform specific investigations, 10) We shall organise field campaigns
in specific locations of scientific and exploration interest, making use
of the ExoHab habitat for logistics support and local operations
@--------------------------------------------------------------------
Title: Geological and geochemical analysis of stratigraphic
units in the South Pole - Aitken Basin
Authors: Borst, A.; Bexkens, F.; Foing, B.; Koschny, D.;
Davies, G.; van Westrenen, W.
Bibliographic Code: 2009EGUGA..1112255B
Abstract
The South Pole-Aitken (SPA) Basin, located on the Lunar far side, is one
of the oldest and largest recognized impact structure in the solar
system. This PreNectarian basin (>3.9 Ga) measures 2500 km in
diameter with depths up to 13 km. A large mafic province was formed by
the impact that effectively removed the upper crust [1]. Hence,
deep-seated lower crustal and possibly even mantle materials are exposed
in the severely modified Basin interior, providing the unique
opportunity to probe and study the composition and structure of the
Lunar interior. Consequently, the SPA Basin is a frequently proposed
site for future sample return missions and detailed multispectral
studies will required to aid landing site selection [2]. Previous
studies on the multispectral dataset of Clementine (1994) by Pieters and
Tompkins [1,3] revealed fresh mafic compositions of both low-Ca pyroxene
or high-Ca pyroxene dominated rocks, referred to as norites and gabbros
respectively. Some regions contained spectral features of olivine
(troctolite), such as in Olivine Hill, which could suggest the presence
of mantle derived deposits tapped during SPA impact. Using an
algorithm developed by Pieters et al. [1] we have produced images for
three subregions, covering the central and northern part of the SPA
Basin. The algorithm is based on three diagnostic features in the UV/VIS
spectrum of Clementine's 11 band multispectral dataset. The parameters
are assigned to an RGB composite and allow distinction between mature
soils, anorthosite (blue), norite (pink) and gabbro/troctolite
compositions (green). Furthermore, we have used Clementine's Near
Infrared database to produce a NIR band ratio image (2000 nm/1250 nm),
as a parameter to distinguish between olivine and pyroxene-rich
materials where we aim to detect traces of excavated mantle material
(modified from LeMoeulic et al. [4]). Regretfully, we found that the
NIR ratio method does not confirm olivine-rich material exposed in
Olivine Hill as it shows no significant bright colors compared to the
surroundings. This means that we have no firm evidence of mantle
material being excavated during SPA impact. Instead, we have identified
an overall noritic composition as the deepest stratigraphic unit exposed
on the basin floor. Norite is found in nearly all central peaks of both
small and large size and in large topographical structures that have
punched through the upper, often gabbroic layer, such as in the Leibnitz
and Apollo basins. This thin layer of gabbroic composition is
distributed over large parts of the basin floor and presumably overlays
the noritic basement of apparent lower-crustal origin. The origin of
these high-Ca pyroxene dominated rocks emplaced on the basin floor could
be attributed to several processes and possibly represent remnants of
the SPA impact melt sheet; some form of cryptomare or cooled and exposed
mafic plutons formed during crustal differentiation. We have combined
the multispectral results with topographical Clementine LIDAR data and
SMART-1 AMIE images containing additional morphological information, in
order to produce geochemical-geomorphological maps which provide a clear
geological overview of the rock types within the SPA Basin. [1]
Pieters, C.M., et al. (2001) JGR, 106, 28,001- 8,022 [2] Duke, M.B.
(2003) Adv. Space. Res., 31, 2347-2352 [3] Tompkins, S., Pieters, C.M.
(1999). Meteor. Planet. Sci., 34(1), 25-41 [4] LeMouelic, S., et al.
(2001) Planet. and Space Sci., 49, 65-70
@--------------------------------------------------------------------
Title: Characterisation of sites of astrobiology interest
for Mars landers and sample return missions
Authors: Wills, D. E. S.; Monaghan, E. P.; Foing, B. H.
Bibliographic Code: 2009EGUGA..1111568W
Abstract
Introduction: The aim of this work is to nominate and assess candidate
landing sites for missions of astrobiological interest to Mars. We
report in particular on science and technical criteria and our data
analysis for sites suitable for an ExoMars-class mission. This includes
information from previous missions (such as Mars Express, MGS, Odyssey,
MRO and MER rovers) on mineralogical composition, geomorphology,
evidence from past water history from imaging and spectroscopic data,
and existence of in-situ prior information from landers and rovers
(concerning evidences for volatiles, organics and habitability
conditions). Science Goals and Objectives: Firstly, we look for
morphological evidence of hydrological activity, including sedimentary
deposits (deltas, valley networks), areas of ancient hydrothermal
activity (spring deposits). Secondly, we look for mineralogical evidence
of hydrological activity, such as phyllosilicates (formed by alteration
due to water, indicate prolonged exposure to standing water), hydrated
sulphates (formed by alteration due to water, not necessarily standing
water), other water-containing minerals. Thirdly, we prioritise Noachian
terrain (during this epoch, ~3.5 billion years ago, the Martian climate
may have been warmer, and liquid water may have been stable on the
surface). Finally, we look for sites where the potential for
preservation of biosignatures is high (exposed bedrock, subsurface
regions, spring sinters). Engineering Constraints: We consider the
engineering constraints placed on the ExoMars misson. These include
latitude (sufficient insolation for power), landing altitude (sufficient
atmosphere for EDL), horizontal winds, shear, and wind turbulence
(airbag free fall), radar altimeter reflectivity (for descent and
landing control), obstacles and rock distribution (airbag landing),
slopes (airbag landing), rover egress, and rover locomotion. The
Priority Sites: Out of a short-list of ten proposed locations, we select
two top priority sites and a safe-haven. The sites chosen are Mawrth
Vallis (21.6°N, 344.0°E) and Vernal Crater (5.9°N,
355.3°E), and a safe-haven in Eastern Meridiani (0° N,
3.7°E). The entire length of Mawrth Vallis is of interest, not least
because the source is unknown. It doesn't begin in chaotic terrain like
the majority of outflow channels. Weathered phyllosilicates are
prevalent and their variety, concentration and surface area are
currently unmatched compared to anywhere on Mars. They exist in layered
outcrops. Structures in Vernal Crater are strongly suggestive of spring
deposits, which would have a high potential for preservation of
biosignatures. Other key features of interest at this site include
probable lake-shore and regional fluvial deposits, lacustrine layers and
evidence of methane activity. Eastern Meridiani has been nominated as a
potential safe-haven. The science interest of this site includes many
diverse layers, evidence of phyllosilicates, and excavation of
underlying material by cratering. General references: G. Neukum, R.
Jaumann et al., HRSC: The High Resolution Stereo Camera of Mars Express,
in Mars Express: The scientific payload, edited by A. Wilson, pp. 17-35,
ESA, Noordwijk, The Netherlands, 2004; R. Jaumann, G. Neukum, T. Behnke,
T.C. Duxburry, K. Eichentopf, S. van Gasselt, B. Giese, K. Gwinner, E.
Hauber, H. Hoffmann, A. Hoffmeister, U. Köhler, K.D; Matz, T.B.
McCord, V. Mertens, J. Oberst, R. Pischel, D. Reiß, E. Ress, T.
Roatsch, P. Saiger, F. Scholten, G. Schwarz, K. Stephan, M.
Wählisch, and the HRSC; Co-Investigator Team: The High Resolution
Stereo Camera (HRSC) Experiment on Mars Express: Instrument Aspects and
Experiment Conduct from Interplanetary; Cruise through Nominal Mission,
Planetary and Space Science, 55, 928-952, 2007.
@--------------------------------------------------------------------
Title: Flexure and isostasy of lunar mascons
Authors: Peters, S. T. M.; Foing, B. H.
Bibliographic Code: 2009EGUGA..1111546P
Abstract
A mascon is a region of a planet's or moon's crust that contains an
excess positive gravity anomaly, indicating the presence of additional
mass in this area. Mascons on the Moon coincide with the locations of
circular basins and hence a related origin for both is likely. The
formation of a circular basin includes the excavation of the upper parts
of the crust and subsequent upwelling of the lower parts as a result of
isostatic compensation [1]. Afterwards, filling of the basins by mare
basalts leads to concentrations of dense rocks and is hence suggested as
the origin of the mascon. The present day presence of mascons indicates
that there was no subsequent isostasy leading to downward migration of
the moho and that they are hence supported by an elastic layer on the
surface of the Moon. The interaction between mascons and this elastic
shell is the main topic of our modeling. Since they were discovered by
Muller and Sjogren (1968), the origin of mascons and their interaction
with the crust became clearer. As we point out below, several questions
have however remained unsolved. Our contribution includes the usage of
recent gravity and topography models that have not been applied in
mascon studies yet. Mascons act like a dense load on the lunar
lithosphere and hence flexure it. Flexure profiles of circular basins
have been made by previous authors [2], however, only a single-layered
crust was considered until now. Our modeling includes the two-layered
crustal model preferred by Wieczorek and Phillips (1997) which explains
the gravity to topography ratios of the lunar highlands. On the hand of
previously existing data it has been suggested that rings of negative
gravity anomalies surround the mascons [3]. Whereas this observation was
first questionable, prereleases of the high-resolution KAGUYA gravity
measurements recently clearly confirmed the presence of these features.
Part of our modeling focuses on the location and extent of the negative
anomalies in respect to the flexural depression. Furthermore we model
the locations of failure that result from flexural stresses and compare
these with the observed faults on the lunar surface, using
high-resolution AMIE-images from ESA's SMART-1 mission. We produced
flexure profiles for circular basins Humorum, Imbrium, Serenitates and
Orientale, that all coincide with mascon locations. We use a modified
version of COBRA[4] for PC. The program input and output is managed by
macros included in a Microsoft Excel file. Because the mascons have
rather an axially symmetric than elongated shape, we calculate the
flexure to point loads. The gravity and topography data that we use is
provided on the web by Wieczorek (2006)
(http://www.ipgp.jussieu.fr/~wieczor). By combining the most recent
topography model [GLTM2C by Smith et al. (1997)], with the most recent
gravity model [LP150Q by Konopliv et al. (2001)], he calculated crustal
thicknesses for three model types. The first model examines the crust as
a single layer in which gravity is assumed to result from Moho relief
and Mare basalt fill. The second model has the only difference that
Bouguer correction was set to zero before inverting for the relief along
the crust-mantle interface. The third model examines a dual-layered
crust. Since crustal thickness equals Moho depth on the Moon, we can use
these different models as input for our software. We define the
characteristics of the initial situation, i.e. height, depth and density
contrast of the load before flexure. We vary elastic parameters like
elastic thickness and yield strength, and use a Poisson's ration of 0.25
and an average Young's Modulus of 1.1x1011 N/m2. Shearforce and bending
moment are assumed to be zero. The coming together of negative gravity
anomalies related to distinct mascons (e.g. Mare Imbrium and Mare
Serenitatis) suggests interaction of flexure. We aim to use 3D finite
element models to visualize this interaction. Furthermore we aim to
include the effects of viscous deformation of the lunar interior as a
result of mascon loading in our models. References: [1] Neumann et
al., (1996), JGR, 101, 16841-16864 [2] Arkani-Hamed, (1998), 103,
3709-3739 [3] Sjogren et al., (1972), Science, 175, 165-168 [5] program
originally based on Bodine (1982), modifications by Zoetemeijer (2001)
@--------------------------------------------------------------------
Title: Lunar single-scattering, porosity, and
surface-roughness properties with SMART-1/AMIE
Authors: Parviainen, H.; Muinonen, K.; Näränen, J.;
Josset, J.-L.; Beauvivre, S.; Pinet, P.; Chevrel, S.;
Koschny, D.; Grieger, B.; Foing, B.
Bibliographic Code: 2009EGUGA..11.7966P
Abstract
We analyze the single-scattering albedo and phase function, local
surface roughness and regolith porosity, and the coherent
backscattering, single scattering, and shadowing contributions to the
opposition effect for specific lunar mare regions imaged by the
SMART-1/AMIE camera. We account for shadowing due to surface roughness
and mutual shadowing among the regolith particles with ray-tracing
computations for densely-packed particulate media with a
fractional-Brownian-motion interface with free space. The shadowing
modeling allows us to derive the hundred-micron-scale volume-element
scattering phase function for the lunar mare regolith. We explain the
volume-element phase function by a coherent-backscattering model, where
the single scatterers are the submicron-to-micron-scale particle
inhomogeneities and/or the smallest particles on the lunar surface. We
express the single-scatterer phase function as a sum of three
Henyey-Greenstein terms, accounting for increased backward scattering in
both narrow and wide angular ranges. The Moon exhibits an opposition
effect, that is, a nonlinear increase of disk-integrated brightness with
decreasing solar phase angle, the angle between the Sun and the observer
as seen from the object. Recently, the coherent-backscattering mechanism
(CBM) has been introduced to explain the opposition effect. CBM is a
multiple-scattering interference mechanism, where reciprocal waves
propagating through the same scatterers in opposite directions always
interfere constructively in the backward-scattering direction but with
varying interference characteristics in other directions. In addition
to CBM, mutual shadowing among regolith particles (SMp) and
rough-surface shadowing (SMr) have their effect on the behavior of the
observed lunar surface brightness. In order to accrue knowledge on the
volume-element and, ultimately, single-scattering properties of the
lunar regolith, both SMp and SMr need to be accurately accounted for. We
included four different lunar mare regions in our study. Each of these
regions covers several hundreds of square kilometers of lunar surface.
When selecting the regions, we have required that they have been imaged
by AMIE across a wide range of phase angles, including the opposition
geometry. The phase-angle range covered is 0-109 °, with incidence
and emergence angles (ι and ε) ranging within
7-87 ° and 0-53 °, respectively. The pixel scale varies from
288m down to 29m. Biases and dark currents were subtracted from the
images in the usual way, followed by a flat-field correction. New
dark-current reduction procedures have recently been derived from
in-flight measurements to replace the ground-calibration images. The
clear filter was chosen for the present study as it provides the largest
field of view and is currently the best-calibrated channel.
Off-nadir-pointing observations allowed for the extensive phase-angle
coverage. In total, 220 images are used for the present study. The
photometric data points were extracted as follows. First, on average, 50
sample areas of 10 Ã- 10 pixels were chosen by hand from each
image. Second, the surface normal, ι, ε, °,
and alpha were computed for each pixel in each sample area using the
NASA/NAIF SPICE software toolkit with the latest and corrected
SMART-1/AMIE SPICE kernels. Finally, the illumination angles and the
observed intensity were averaged over each sample area. In total, the
images used in the study resulted in approximately 11000 photometric
sample points for the four mare regions. We make use of
fractional-Brownian-motion surfaces in modeling the interface between
free space and regolith and a size distribution of spherical particles
in modeling the particulate medium. We extract the effects of the
stochastic geometry from the lunar photometry and, simultaneously,
obtain the volume-element scattering phase function of the lunar
regolith locations studied. The volume-element phase function allows us
to constrain the physical properties of the regolith particles. Based
on the present theoretical modeling of the lunar photometry from
SMART-1/AMIE, we conclude that most of the lunar mare opposition effect
is caused by coherent backscattering and single scattering within volume
elements comparable to lunar particle sizes, with only a small
contribution from shadowing effects. We thus suggest that the lunar
single scatterers exhibit intensity enhancement towards the backward
scattering direction in resemblance to the scattering characteristics
experimentally measured and theoretically computed for realistic small
particles. Further interpretations of the lunar volume-element phase
function will be the subject of future research.
@--------------------------------------------------------------------
Title: ExoGeoLab Lander/Rover Instruments and EuroGeoMars
MDRS Campaign
Authors: Foing, B. H.; Batenburg, P.; Drijkoningen, G.;
Slob, E.; Poulakis, P.; Visentin, G.; Page, J.;
Noroozi, A.; Gill, E.; Guglielmi, M.; Freire, M.;
Walker, R.; Sabbatini, M.; Pletser, V.; Monaghan, E.;
Boche-Sauvan, L.; Ernst, R.; Oosthoek, J.;
Peters, S.; Borst, A.; Mahapatra, P.; Wills, D.;
Thiel, C.; Wendt, L.; Gross, C.; Petrova, D.;
Lebreton, J. P.; Zegers, T.; Stoker, C.;
Zhavaleta, J.; Sarrazin, P.; Blake, C.; McKay, C.;
Ehrenfreund, P.; Chicarro, A.; Koschny, D.; Vago, J.;
Svedhem, H.; Davies, G.; Exogeolab Team;
Eurogeomars Team
Bibliographic Code: 2009LPI....40.2567F
Abstract
We describe ExoGeoLab a planetary surface instruments research
incubator, and the EuroGeoMars campaign at the Mars Desert Research
station aimed at validating a procedure for martian surface in-situ and
return science.
@--------------------------------------------------------------------
Title: Reflection Seismology Systems for Planetary Geology:
First Tests at ESTEC ExoGeoLab and MDRS, Utah
Authors: Batenburg, P. A. W.; Foing, B. H.;
Drijkonigen, G. G.; Gill, E. K. A.; Poulakis, P.;
Visentin, G.; Page, J.; Pletser, V.; Peters, S.;
Borst, A.; Mahapatra, P.; Exogeolab Team;
Eurogeomars Team
Bibliographic Code: 2009LPI....40.2536B
Abstract
The authors investigated the use of reflective seismology for Planetary
geology within ESA's ExoGeoLab pilot project. During the
EuroGeoMars expedition tests were performed to test the influence of
surface coupling and composition on data quality.
@--------------------------------------------------------------------
Title: SMART-1: Review of Lunar Highlights
Authors: Foing, B. H.; Koschny, D.; Grieger, B.;
Lossett, J.-L.; Beauvivre, S.; Grande, M.;
Huovelin, J.; Keller, H. U.; Mall, U.; Nathues, A.;
Malkki, A.; Noci, G.; Sodnik, Z.; Kellett, B.;
Pinet, P.; Chevrel, S.; Cerroni, P.;
de Sanctis, M. C.; Barucci, M. A.; Erard, S.;
Despan, D.; Muinonen, K.; Shevchenko, V.;
Shkuratov, Y.; Ellouzi, M.; Peters, S.; Borst, A.;
Bexkens, F.; Almeida, M.; Frew, D.; Volp, J.;
Heather, D.; McMannamon, P.; Camino, O.; Racca, G.;
Peters, S.
Bibliographic Code: 2009LPI....40.2298F
Abstract
The SMART-1 spacecraft operated from 400-3000 km for 1.5 year until
impact. We shall report at LPSC2009 on SMART-1 lunar highlights relevant
for science and exploration, in relation with subsequent missions
Kaguya, Chang'E1 and Chandrayaan-1.
@--------------------------------------------------------------------
Title: CoRot observations of active giants: preliminary
results
Authors: Gondoin, P.; Fridlund, M.; Goupil, M. J.; Baudin, F.;
Samadi, R.; Barban, C.; Belkacem, K.; Corbard, T.;
Dupret, M. A.; Foing, B.; den Hartog, R.;
Lebreton, Y.; Lochard, J.; Mathias, P.; Michel, E.;
Morel, P.; Moya, A.; Palacios, A.; Zahn, J. P.
Bibliographic Code: 2009AIPC.1094..864G
Abstract
We have analysed rotation modulated light-curves of active giants
observed with CoRot using spots model. Preliminary results suggest an
increase of the surface spot coverage with decreasing rotation period. A
maximum of the surface spot coverage seems to occur on giants with
effective temperature around 5100 K. Confirmation and interpretation of
these preliminary results require groundbased follow-up observations to
measure activity indicators, to identify binary systems, and to
determine the stellar parameters and evolutionary status of the sample
giants.
@--------------------------------------------------------------------
Title: Doppler maps and surface differential rotation of EI
Eri from the MUSICOS 1998 observations
Authors: Kovári, Zs.; Washuettl, A.; Foing, B. H.; Vida, K.;
Bartus, J.; Oláh, K.; MUSICOS 98 Team
Bibliographic Code: 2009AIPC.1094..676K
Abstract
We present time-series Doppler images of the rapidly-rotating active
binary star EI Eri from spectroscopic observations collected during the
MUSICOS multi-site campaign in 1998, since the critical rotation period
of 1.947 days makes it impossible to obtain time-resolved images from a
single site. From the surface reconstructions a weak solar-type
differential rotation, as well as a tiny poleward meridional flow are
measured.
@--------------------------------------------------------------------
Title: Magnetic activity in the photosphere of
CoRoT-Exo-2a. Active longitudes and short-term spot
cycle in a young Sun-like star
Authors: Lanza, A. F.; Pagano, I.; Leto, G.; Messina, S.;
Aigrain, S.; Alonso, R.; Auvergne, M.; Baglin, A.;
Barge, P.; Bonomo, A. S.; Boumier, P.;
Collier Cameron, A.; Comparato, M.; Cutispoto, G.;
de Medeiros, J. R.; Foing, B.; Kaiser, A.;
Moutou, C.; Parihar, P. S.; Silva-Valio, A.;
Weiss, W. W.
Bibliographic Code: 2009A&A...493..193L
Abstract
Context: The space experiment CoRoT has recently detected transits by a
hot Jupiter across the disc of an active G7V star (CoRoT-Exo-2a) that
can be considered as a good proxy for the Sun at an age of approximately
0.5 Gyr.
Aims: We present a spot modelling of the optical
variability of the star during 142 days of uninterrupted observations
performed by CoRoT with unprecedented photometric precision.
Methods: We apply spot modelling approaches previously tested in the
case of the Sun by modelling total solar irradiance variations, a good
proxy for the optical flux variations of the Sun as a star. The best
results in terms of mapping of the surface brightness inhomogeneities
are obtained by means of maximum entropy regularized models. To model
the light curve of CoRoT-Exo-2a, we take into account the photometric
effects of both cool spots and solar-like faculae, adopting solar
analogy.
Results: Two active longitudes initially on opposite
hemispheres are found on the photosphere of CoRoT-Exo-2a with a rotation
period of 4.522 ± 0.024 days. Their separation changes by
≈80° during the time span of the observations. From this
variation, a relative amplitude of the surface differential rotation
lower than ~1 percent is estimated. Individual spots form within the
active longitudes and show an angular velocity ~1 percent lower than
that of the longitude pattern. The total spotted area shows a cyclic
oscillation with a period of 28.9 ± 4.3 days, which is close to
10 times the synodic period of the planet as seen by the rotating active
longitudes. We discuss the effects of solar-like faculae on our models,
finding indications of a facular contribution to the optical flux
variations of CoRoT-Exo-2a being significantly smaller than in the
present Sun.
Conclusions: The implications of such results for
the internal rotation of CoRoT-Exo-2a are discussed, based on solar
analogy. A possible magnetic star-planet interaction is suggested by the
cyclic variation of the spotted area. Alternatively, the 28.9-d cycle
may be related to Rossby-type waves propagating in the subphotospheric
layers of the star.
Based on observations obtained with CoRoT, a space project operated by
the French Space Agency, CNES, with partecipation of the Science
Programme of ESA, ESTEC/RSSD, Austria, Belgium, Brazil, Germany, and
Spain.
@--------------------------------------------------------------------
Title: Astrobiology and Exposure Experiments from the Lunar
Surface
Authors: Wills, D. E.; Foing, B.; Wills, H. H.
Bibliographic Code: 2008LPICo1446..140W
Abstract
@--------------------------------------------------------------------
Title: ESA's Lunar Robotics Challenge
Authors: Visentin, G.; Foing, B.; Walker, R.; Galvez, A.
Bibliographic Code: 2008LPICo1446..134V
Abstract
@--------------------------------------------------------------------
Title: Future Robotic Study of Lunar Basins: Goals for
Geochemistry and Geophysics
Authors: Peters, S. T. M.; Monaghan, M. P.; Foing, B. H.
Bibliographic Code: 2008LPICo1446..103P
Abstract
@--------------------------------------------------------------------
Title: Addressing International Lunar Surface Operations
Authors: Lupisella, M.; Eppler, D.; Arnold, L.; Landis, R.;
Gates, M.; Hovland, S.; Foing, B.; Olds, J.;
Depasquale, D.; Lewis, R.; Hyatt, M.; Conley, C.;
Mandl, D.; Talabac, S.; McNamara, K.; Perino, M. A.;
Alkalai, L.; Morrow, C.; Burke, J.
Bibliographic Code: 2008LPICo1446...84L
Abstract
@--------------------------------------------------------------------
Title: Astronomy from the Moon: Possible Science
Investigations and Precursors
Authors: Kissi-Ameyaw, J.; Monaghan, E. P.; Foing, B. H.
Bibliographic Code: 2008LPICo1446...73K
Abstract
@--------------------------------------------------------------------
Title: SMART-1 Results and Lessons Learned for Preparing
Future Exploration
Authors: Foing, B. H.; Koschny, D.; Grieger, B.;
Josset, J.-L.; Beauvivre, S.; Grande, M.;
Crawford, I.; Swinyard, B.; Huovelin, J.; Alha, L.;
Keller, H. U.; Mall, U.; Nathues, A.; Malkki, A.;
Noci, G.; Sodnik, Z.; Kellett, B.; Pinet, P.;
Chevrel, S.; Cerroni, P.; de Sanctis, M. C.;
Barucci, M. A.; Erard, S.; Despan, D.; Muinonen, K.;
Naranen, J.; Shevchenko, V.; Shkuratov, Y.;
Ellouzi, M.; Peters, S.; Bexkens, F.; Borst, A.;
Odum, C.; Boche-Sauvan, L.; Monaghan, E.; Wills, D.;
Almeida, M.; Frew, D.; Volp, J.; Heather, D.;
McMannamon, P.; Camino, O.; Racca, G.
Bibliographic Code: 2008LPICo1446...55F
Abstract
@--------------------------------------------------------------------
Title: Report from ILEWG on Science and Exploration
Questions
Authors: Foing, B. H.;
International Lunar Exploration Working Group
Bibliographic Code: 2008LPICo1446...54F
Abstract
@--------------------------------------------------------------------
Title: What Astrobiology Investigations are Needed and
Possible on the Moon?
Authors: Ehrenfreund, P.; Foing, B. H.
Bibliographic Code: 2008LPICo1446...51E
Abstract
@--------------------------------------------------------------------
Title: High Resolution Maps of the Moon Surface with
AMIE/SMART-1
Authors: Despan, D.; Erard, S.; Barucci, A.; Josset, J.-L.;
Beauvivre, S.; Chevrel, S.; Pinet, P.; Koschny, D.;
Almeida, M.; Grieger, B.; Foing, B. H.; Amie Team
Bibliographic Code: 2008LPICo1446...48D
Abstract
@--------------------------------------------------------------------
Title: Geological and Geochemical Study of South
Pole-Aitken Basin and Future Sample Return Missions
Authors: Borst, A. M.; Bexkens, F.; Foing, B. H.
Bibliographic Code: 2008LPICo1446...26B
Abstract
@--------------------------------------------------------------------
Title: Constraints on the Pre-Design of a Minimal Human
Lunar Outpost
Authors: Boche-Sauvan, L.; Foing, B. H.
Bibliographic Code: 2008LPICo1446...24B
Abstract
@--------------------------------------------------------------------
Title: Selecting a landing site of astrobiological interest
for Mars landers and sample return missions
Authors: Wills, D.; Monaghan, E.; Foing, B. H.
Bibliographic Code: 2008epsc.conf..855W
Abstract
Abstract The landscape of Mars, despite its apparent hostility to life,
is riddled with geological and mineralogical signs of past or present
hydrological activity. As such, it is a key target for astrobiological
exploration. There are, however, many factors that will need to be
considered when planning in-situ and sample return missions, if these
missions are indeed to adequately exploit the science potential of this
intriguing world. These will not only take into account the environment
of the landing site in terms of topography and ambient atmosphere etc.,
but also the geochemical make up of the surface regolith, evidence of
hydrological processes and various other considerations. The knowledge
base in all aspects of Martian science is being added to on an almost
daily basis, and the aim of this work is to combine data and studies to
nominate top priority landing locations for the search for evidence of
life on Mars. We report in particular on science and technical criteria
and our data analysis for sites of astrobiological interest. This
includes information from previous missions (such as Mars Express, MGS,
Odyssey, MRO and MER rovers) on mineralogical composition,
geomorphology, evidence from past water history from imaging and
spectroscopic data, and existence of in-situ prior information from
landers and rovers (concerning evidences for volatiles, organics and
habitability conditions). We discuss key mission objectives, and assess
what sort of sites should be targeted in the light of these. We consider
the accessibility of chosen locations, taking into account difficulties
presented in accessing the polar regions and other regions of high
altitude. We describe what additional measurements are needed, and
outline the technical and scientific operations requirements of such
in-situ landers and sample return missions. Approach In the first step
of this study we focus on the science objectives of in-situ and sample
return missions to Mars. We investigate the evidence for extinct or
extant life, propose a criteria for astrobiological interest, and
characterise landing sites in the light of this criteria. This first
step thus focuses on the question of where such missions should land,
and why. In the second step, we extend this analysis into utilising real
data to design mission scenarios for each of the proposed sites. This
further step takes into account the safety, instruments and payloads, as
well as the technological and engineering constraints of such missions.
In this way, the second step addresses the question of what could be
done, and how, once the landing sites have been chosen. In the final
step we conduct a comparative study of in-situ and sample return
missions with reference to the candidate sites.
@--------------------------------------------------------------------
Title: Isostasy in lunar mascon areas: comparison between
far side and near side
Authors: Peters, S. T. M.; Foing, B. H.
Bibliographic Code: 2008epsc.conf..133P
Abstract
We have studied the isostatic response on mascon loading for impact
basins on the far side and near side to determine geophysical properties
and geodynamic processes on the Moon. We modeled the isostatic rebound
for Maria Orientale, Moscoviense and the South Pole Aitken Basin (far
side); Maria Humorum, Imbrium and Serenitates (near side). High positive
gravity anomalies on the Moon coincide with the low topography of impact
basins. It is currently accepted that this results from disruption of
the lithosphere by basin forming impacts that triggered superisostatic
uplift of the mantle. It has been observed that gravity anomalies are
lower in ancient basins as a function of time (Neumann et al., 1998),
which suggests that they are closer to isostatic equilibrium than
younger ones. Our numerical modeling includes basins of varying ages and
considers lateral variations of lithospheric properties such as
thickness and density. We used gravity data from the Clementine mission
and sample analyses from e.g. Apollo17 to determine input values for our
models. Clementine and SMART-1 images were studied for comparison
between structures on the lunar surface and those predicted by models of
mascon loading.
@--------------------------------------------------------------------
Title: The global geological context and impact signatures
in the SPA basin
Authors: Bexkens, F. S.; Borst, A. M.; Foing, B. H.;
Koschny, D.; Peters, S. T. M.
Bibliographic Code: 2008epsc.conf..130B
Abstract
Abstract The giant South Pole – Aitken basin (SPA) is the largest
recognised impact structure in the solar system. The basin is located on
the far side of the moon and measures 3500 km in diameter, including the
outermost ringstructure [2]. It is believed to be one of the oldest
lunar structures, > 4 billion years [1]. Due to its old age and
maturity the SPA structure has been severely reworked, and primary
ejecta have been redistributed by later impacts. The smoothing effect of
later smaller impacts on original basin structure and topography
complicates studies of the primary impact signature of the basin
structure. Here, we combine Clementine and SMART-1 data to provide
additional constraints on the large-scale structure of the SPA impact
basin. The impact’s outer ring is best developed on the
north-eastern side of the basin. Two possible explanations for this
observation have been brought forward: (1) The ring structure is simply
best preserved in this area because by chance it has not been reworked
by later impacts as extensively as the rest of the outer ring. (2) The
SPA was formed by an oblique impact of a low density body [2]. Such an
impact could also explain the extremely low depth-diameter ratio of the
basin [2]. Clementine LIDAR gravity and topography data are used to
address the large-scale structure of the South Pole – Aitken Basin.
Using the IDL and ENVI software gravity and topography profiles across
the SPA with different orientations have been produced and compared. The
results are also used to quantify the mass distribution as a result of
the basin forming impact and later impacts, to try and assess how mass
was distributed during and after the impact. The Clementine data are
augmented with mosaics of highresolution SMART-1 AMIE images to improve
on a detailed description of the geological context of the SPA. One
northsouth profile through the SPA will be compared with the topography
and gravity profiles. In a companion study (A.M. Borst et al., this
conference) Clementine UV/VIS and NIR images are employed to constrain
the geochemical signatures of exposed rock types within the SPA Basin. A
synthesis of our studies enables a comparison between structure and
mineralogical compositions / soil maturity, and may lead to the
identification of possible landing sites for future sample return
missions. References [1] Duke, M.B., 2003. Sample return from the lunar
south pole-aitken basin. Adv. Space. Res. Vol. 31, No. 11, pp.
2347-2352. [2] Shevchenko, V.V., Chikmachev, V.I., Pugacheva, S.G.,
2007. Structure of the South Pole-Aitkan lunar basin. Solar system
research, Vol. 41, No 6, pp. 447-462.
@--------------------------------------------------------------------
Title: Geochemical analysis of units within the South Pole
- Aitken Basin
Authors: Borst, A. M.; Bexkens, F.; Foing, B. H.; Koschny, D.;
Peters, S. T. M.
Bibliographic Code: 2008epsc.conf..129B
Abstract
The South Pole - Aitken (SPA) Basin, situated on the southern farside of
the Moon, is of critical importance to unravelling the composition and
evolution of the Moon. This PreNectarian basin ( >3.9 Ga), measuring
2500 km in diameter with a depth of up to 12 km, is commonly alleged to
have excavated deep into the lunar crust (Fig. 1). Therefore the SPA
Basin floor may provide a unique opportunity to study deep seated lunar
materials. However, rocks initially exposed by the impact event have
been heavily altered or hidden from view, due to subsequent weathering
and impact processes. Consequently the identification of pristine SPA
Basin floor material, which would provide a new window into the lunar
interior, has become severely complicated [1]. Previous research using
multispectral and gamma-ray data obtained by the Clementine and Lunar
Prospector missions revealed the localised presence of noritic and
gabbroic/troctolitic rocks, exposed underneath the mixing regolith layer
[2, 4]. Approach In this study we combine structural and geochemical
analyses of the SPA Basin. The research presented here aims at improving
mineralogical descriptions of mafic rock types within the South Pole -
Aitken Basin using a similar approach as described by Tompkins and
Pieters [2, 3]. Multispectral data from Clementine ultraviolet/visible
and near-infrared cameras are used and processed in ENVI. The method
relies on diagnostic shapes of band absorptions for key mafic minerals
olivine and high Ca-pyroxene, in order to discriminate between geologic
units of noritic, gabbroic and troctolitic compositions. We synthesise
our results with a companion complementary study of the global
geological structure of the SPA Basin using Clementine altimetry and
gravity data obtained by LIDAR instruments (F. Bexkens et al., this
conference). Based on both mineralogical and structural analysis local
mosaics of SMART-1 high resolution AMIE images will be produced to
provide improved geological context for areas exposing deep crustal
materials. In particular we will discuss the Bhabha- Bose region located
in central SPA Basin, which has been previously proposed as a possible
sample return landing site [4, 5]. Ultimately this study aims to
contribute to identifying target areas of future sample return missions
to ensure optimal scientific gain. References [1] Jolliff, B.L., et al.
(2002), LPSXXXIII, 1156 [2] Pieters, C.M., et al. (1997) Geophysical
Research Letters, 24, 1903-1906 [3] Tompkins, S., and Pieters, C.M.
(1999). Meteor. Planet. Sci., 34(1), 25-41 [4] Pieters, C.M., et al.
(2001) JGR, 106, 28,001- 28,022. [5] Duke, M.B. (2003) Adv. Space. Res.,
31, 2347- 2352. EPSC Abstracts, Vol. 3, EPSC2008-A-00129, 2008 European
Planetary Science Congress, Author(s) 2008
@--------------------------------------------------------------------
Title: Selecting A Landing Site Of Astrobiological Interest
For Mars Landers And Sample Return Missions
Authors: Wills, Danielle; Monaghan, E.; Foing, B.
Bibliographic Code: 2008DPS....40.1507W
Abstract
The landscape of Mars, despite its apparent hostility to life, is
riddled with geological and mineralogical signs of past or present
hydrological activity. As such, it is a key target for astrobiological
exploration. The aim of this work is to combine data and studies to
select top priority landing locations for in-situ landers and sample
return missions to Mars. We report in particular on science and
technical criteria and our data analysis for sites of astrobiological
interest. This includes information from previous missions (such as Mars
Express, MGS, Odyssey, MRO and MER rovers) on mineralogical composition,
geomorphology, evidence from past water history from imaging and
spectroscopic data, and existence of in-situ prior information from
landers and rovers (concerning evidence for volatiles, organics and
habitability conditions). We discuss key mission objectives, and
consider the accessibility of chosen locations. We describe what
additional measurements are needed, and outline the technical and
scientific operations requirements of in-situ landers and sample return
missions to Mars.
@--------------------------------------------------------------------
Title: High Resolution Maps of the Moon Surface with
AMIE/SMART-1
Authors: Despan, Daniela; Erard, S.; Barucci, A.;
Josset, J. L.; Beauvivre, S.; Chevrel, S.; Pinet, P.;
Koschny, D.; Almeida, M.; Grieger, B.; Foing, B.;
AMIE Team
Bibliographic Code: 2008DPS....40.1301D
Abstract
The Advanced Moon micro-Imager Experiment (AMIE) on board the ESA lunar
mission Smart-1 has performed colour imaging of the lunar surface using
various filters in the visible and NIR range. This micro-camera provided
high resolution images of selected parts of the lunar surface, including
the North and South pole areas. Being give that the SMART-1 mission was
in a 300km x 300km orbit with perilune over the South pole, the coverage
between the North and the South regions is different.
The AMIE images were obtained using a tele-objective with 5.3° x
5.3° field of view and a sensor of 1024 x 1024 pixels. The output
images have resolution 45m/pixel at 500km, and are encoded with 10
bits/pixel. The data for the North pole were obtained at a much higher
altitude than the South pole data. From the 300 Km pericenter altitude,
the same field of view corresponds to a spatial resolution about 27
m/pixel. The high resolution imaging of the Moon surface makes possible
detailed analysis of the morphological features and physical
characteristics of the lunar surface. In order to construct AMIE data
maps, systematic analysis and processing is being carried on using the
whole data set. Geometrical analysis of AMIE images relies on the SPICE
system: image coordinates are computed to get precise projection at the
surface, and illumination angles are computed to analyze the photometric
sequences. Using this method, high resolution mosaics were constructed
then compared to lower resolution Clementine UV-Vis and NIR images. Maps
of both North and South pole were obtained as well as other regions of
interest. Eventually, this method will be applied in all areas where
AMIE has provided high resolution observations of the surface, typically
a factor of 3 higher than the Clementine UV-Vis camera. New results will
be presented at the conference.
@--------------------------------------------------------------------
Title: SMART-1 highlights and relevant studies on early
bombardment and geological processes on rocky
planets
Authors: Foing, B. H.; Racca, G. D.; Josset, J. L.;
Koschny, D.; Frew, D.; Almeida, M.; Zender, J.;
Heather, D.; Peters, S.; Marini, A.; Stagnaro, L.;
Beauvivre, S.; Grande, M.; Kellett, B.; Huovelin, J.;
Nathues, A.; Mall, U.; Ehrenfreund, P.; McCannon, P.
Bibliographic Code: 2008PhST..130a4026F
Abstract
We present results from SMART-1 science and technology payload, in the
context of the Nobel symposium on 'Physics of Planetary Systems'.
SMART-1 is Europe' first lunar mission (Foing et al 2000 LPSC XXXI
Abstract \#1677 (CDROM); Foing et al 2001 Earth, Moon Planets 85 86 523
31 Marini et al 2002 Adv. Space Res. 30 1895 900 Racca et al 2001 Earth
Moon Planets 85 86 379 95, Racca et al 2002 Planet Space Sci. 50 1323
37) demonstrating technologies for future science and exploration
missions, and providing advances in our understanding of lunar origin
and evolution, and general planetary questions. The mission also
contributes a step in developing an international program of lunar
exploration. The spacecraft, launched on 27 September 2003 as an Ariane
5 Auxiliary passenger to geostationary transfer orbit (GTO), performed a
14-month long cruise using a tiny thrust of electric propulsion alone,
reached lunar capture in November 2004, and lunar science orbit in March
2005. SMART-1 carried 7 hardware experiments (Foing et al 2003 Adv.
Space Res. 31 2323, Foing et al 2005 LPI/LPSC XXXVI 2404 (CDROM))
performing 10 investigations, including 3 remote-sensing instruments,
used during the cruise, the mission' nominal six-months and one-year
extension in lunar science orbit. Three remote sensing instruments,
D-CIXS, SIR and AMIE, have returned data that are relevant to a broad
range of lunar studies. The mission provided regional and global x-ray
measurements of the Moon, global high-spectral resolution NIR
spectrometry, high spatial resolution colour imaging of selected
regions. The South Pole-Aitken Basin (SPA) and other impact basins have
been prime targets for studies using the SMART-1 suite of instruments.
Combined, these should aid a large number of science studies, from bulk
crustal composition and theories of lunar origin/evolution, the global
and local crustal composition, to the search for cold traps at the lunar
poles and the mapping of potential lunar resources. We present here
SMART-1 results relevant to the study of the early bombardment and
geological processes on rocky planets. Further information and updates
on the SMART-1 mission can be found on the ESA Science and Technology
web pages, at: http://sci.esa.int/smart-1/.
@--------------------------------------------------------------------
Title: Large-scale spring deposits on Mars?
Authors: Rossi, Angelo Pio; Neukum, Gerhard;
Pondrelli, Monica; van Gasselt, Stephan;
Zegers, Tanja; Hauber, Ernst; Chicarro, Agustin;
Foing, Bernard
Bibliographic Code: 2008JGRE..11308016R
Abstract
We present a large-scale spring hypothesis for the formation of various
enigmatic light-toned deposits (LTDs) on Mars. Layered to massive LTDs
occur extensively in Valles Marineris, chaotic terrains, and several
large craters, in particular, those located in Arabia Terra. Most of
these deposits are not easily explained with either a single process or
multiple ones, either in combination or occurring sequentially. Spring
deposits can have a very wide range of internal facies and exhibit
complex architectural variations. We propose the concept of large-scale
spring deposits for explaining LTDs on Mars. Stable volcano-tectonic
settings, such as the ones typical on Mars, are compatible with a
large-scale, long-term, multistage formation of spring deposits. The
large-scale spring deposit model can explain the formation of LTDs with
a common process, although active in different times and locations,
compatible with coeval local or regional processes and deposits, such as
volcaniclastic ones. LTDs, if formed as spring deposits derived from
subsurface fluids, could potentially offer favorable conditions both to
life and to the fossilization of past life forms.
@--------------------------------------------------------------------
Title: Astrobiology, Habitability and the Moon
Authors: Ehrenfreund, P.; Foing, B. H.
Bibliographic Code: 2008LPICo1415.2133E
Abstract
Lunar exploration provides a high potential to foster the objectives of
astrobiology. We review how to acquire knowledge to make the Moon
habitable (using advanced and sustained technological support), and
expand life beyond Earth planet of origin.
@--------------------------------------------------------------------
Title: SMART-1/Clementine Study of Humorum, Procellarum and
South-Pole Aitken Basins: Coupling Between Impacts,
Volcanism and Tectonics
Authors: Peters, S. T.; Foing, B. H.; Borst, A.; Bexkens, F.;
Koschny, D.; Rossi, A.; Josset, J. L.; Beauvivre, S.;
SMART-1 Amie Team
Bibliographic Code: 2008LPICo1415.2115P
Abstract
We have combined SMART-1 AMIE camera images with Clementine UV/VIS data
for three lunar basins (Mare Humorum, Oceanus Procellarum and South
Pole-Aitken Basin), to determine the coupling between basin origin,
tectonics and volcanism.
@--------------------------------------------------------------------
Title: ICEUM8 Highlights and Beijing Lunar Declaration 2006
Authors: Foing, B. H.; Iceum8 Participants
Bibliographic Code: 2008LPICo1415.2106F
Abstract
We report the highlights from ICEUM8, the 8th ILEWG International
Conference on the Exploration and Utilization of the Moon (ICEUM8,
Beijing 23-27 July 2006) and present the "Beijing Lunar Declaration"
endorsed unanimously by the participants.
@--------------------------------------------------------------------
Title: ICEUM9 Highlights and Sorrento Lunar Declaration
2007
Authors: Foing, B. H.; Iceum9 Participants
Bibliographic Code: 2008LPICo1415.2099F
Abstract
We report the highlights from ICEUM9, 9th ILEWG International Conference
on the Exploration and Utilization of the Moon (Sorrento, Italy, 23-27
July 2006) and present the "Sorrento Lunar Declaration" endorsed
unanimously by the participants (http://sci.esa.int/iceum9).
@--------------------------------------------------------------------
Title: Report from ILEWG to the Lunar Science Workshop 2008
Authors: Foing, B. H.;
International Lunar Exploration Working Group
Bibliographic Code: 2008LPICo1415.2090F
Abstract
We report on activities from ILEWG, the International Lunar Exploration
Working Group, created in 1994, by the world's space agencies to support
"international cooperation towards a world strategy for the exploration
and utilization of the Moon".
@--------------------------------------------------------------------
Title: SMART-1 Lunar Highlights: Impact Craters, Basins,
Tectonics and Volcanism
Authors: Foing, B. H.; Grieger, B.; Josset, J.-L.;
Beauvivre, S.; Grande, M.; Huovelin, J.;
Keller, H. U.; Mall, U.; Nathues, A.; Malkki, A.;
Noci, G.; Sodnik, Z.; Kellett, B.; Pinet, P.;
Chevrel, S.; Cerroni, P.; de Sanctis, M. C.;
Barucci, M. A.; Erard, S.; Despan, D.; Muinonen, K.;
Shevchenko, V.; Shkuratov, Y.; Ellouzi, M.;
Peters, S.; Bexkens, F.; Borst, A.; Odum, C.;
Boche-Sauvan, L.; Almeida, M.; Frew, D.; Volp, J.;
Heather, D.; McMannamon, P.; Camino, O.; Racca, G.
Bibliographic Code: 2008LPICo1415.2079F
Abstract
We shall report at the Lunar Science Workshop 2008 on SMART-1 lunar
highlights relevant for science and exploration, with emphasis on impact
craters, basins, tectonics and volcanism.
@--------------------------------------------------------------------
Title: Lunar international science coordination/calibration
targets (L-ISCT)
Authors: Pieters, Carle M.; Head, James W.; Isaacson, Peter;
Petro, Noah; Runyon, Cassandra; Ohtake, M.;
Föing, B.; Grande, M.
Bibliographic Code: 2008AdSpR..42..248P
Abstract
Eight lunar areas, each ˜200 km in diameter, are identified as
targets for coordinated science and instrument calibration for the
orbital missions soon to be flown. Instrument teams from SELENE,
Chang'E, Chandrayaan-1, and LRO are encouraged to participate in a
coordinated activity of early-release data that will improve calibration
and validation of data across independent and diverse instruments. The
targets are representative of important lunar terrains and geologic
processes and thus will also provide a broad introduction to lunar
science for new investigators. We briefly identify additional
cross-calibration issues for instruments that produce time series data
rather than maps.
@--------------------------------------------------------------------
Title: Sorrento Lunar Declaration 2007
Authors: Foing, B. H.; Espinasse, S.; Wargo, M.; di Pippo, S.;
ICEUM9 participants
Bibliographic Code: 2008AdSpR..42..246F
Abstract
We report to COSPAR the ``Sorrento Lunar Declaration'' from
the participants to the Ninth ILEWG International Conference on the
Exploration and Utilisation of the Moon (ICEUM9, Sorrento, Italy, 23 27
July 2006). Further information, abstracts and presentations can be
found on ILEWG website http://sci.esa.int/ilewg and the conference
website http://sci.esa.int/iceum9 [Foing, B., Kosters, G., Espinasse,
S., Del Vecchio Blanco, C., Sangiovanni, G., Salatti, M. (Eds.),
Programme and Abstracts, Ninth ILEWG International Conference on
Exploration and Utilisation of the Moon, 22 26 October 2007, Sorrento,
Italy, 2007; Foing, B., Espinasse, S., Kosters, G. (Eds.), Proceedings
of the Ninth ILEWG International Conference on Exploration and
Utilisation of the Moon. Available online:
, ESA/ASI/ILEWG December, 2007].
@--------------------------------------------------------------------
Title: Beijing Lunar Declaration 2006
Authors: Foing, B. H.; Wu, J.; ICEUM8 participants
Bibliographic Code: 2008AdSpR..42..244F
Abstract
We report to COSPAR the ``Lunar Beijing Declaration'' from the
participants to The Eighth ILEWG International Conference on the
Exploration and Utilization of the Moon (ICEUM8, 23 27 July 2006).
Further information can be found on ILEWG website
http://sci.esa.int/ilewg and selected 38 proceedings papers have been
published in Journal of Astronautics of Chinese Society of Astronautics,
vol. 28, Suppl., 2007.
@--------------------------------------------------------------------
Title: Toronto Lunar Declaration 2005
Authors: Foing, B. H.; Richards, R.; Sallaberger, C.;
ICEUM7 participants
Bibliographic Code: 2008AdSpR..42..242F
Abstract
We report to COSPAR the ``Toronto Declaration'' from the
participants to Seventh ILEWG International Conference on the
Exploration and Utilization of the Moon (ICEUM7, 18 23 September 2005).
Further information can be found on the ILEWG website
http://sci.esa.int/ilewg.
@--------------------------------------------------------------------
Title: Udaipur Lunar Declaration 2004
Authors: Foing, B. H.; Bhandari, N.; Goswami, J. N.;
ICEUM6 participants
Bibliographic Code: 2008AdSpR..42..240F
Abstract
We report to COSPAR the ``Udaipur Declaration'' from the
participants of Sixth ILEWG International Conference on the Exploration
and Utilization of the Moon (ICEUM6, 22 26 November 2004). Further
information can be found on the ILEWG website http://sci.esa.int/ilewg
and publications in the Journal of Earth System Science [Bhandari, N.
(Ed.), Proceedings of the International Conference on Exploration and
Utilization of the Moon 22 26 November 2004, Udaipur, Rajasthan, India.
J. Earth Syst. Sci. 114(6), 573 841, 2005].
@--------------------------------------------------------------------
Title: Reports to COSPAR from the International Lunar
Exploration Working Group (ILEWG)
Authors: Foing, Bernard H.
Bibliographic Code: 2008AdSpR..42..238F
Abstract
In accordance with its charter, the International Lunar Exploration
Working Group (ILEWG) reports to COSPAR, and a summary was given at the
Beijing COSPAR 2006 Assembly on ILEWG activities conducted since the
previous COSPAR 2004 assembly held in Paris. This included reports from
the 6th and 7th ILEWG International Conference on Exploration and
Utilization of the Moon, held respectively in Udaipur, India on 22 26
November 2004 (ICEUM6) and in Toronto, Canada on 18 23 September 2005
(ICEUM7). We give in this issue of Advances in Space Research the
``lunar declarations'' from these ICEUM conferences, as well
as for the ICEUM8 conference held in Beijing immediately after the 2006
COSPAR Assembly. One year after the COSPAR Beijing assembly, the 9th
ILEWG International Conference on Exploration and Utilization of the
Moon (ICEUM9), was held in Sorrento, Italy on 18 23 September 2007. We
report also in this issue the ``Sorrento Lunar Declaration''
in advance of the ILEWG formal report to be given at the COSPAR Assembly
to be held in Montreal, Canada in July 2008.
@--------------------------------------------------------------------
Title: Journey to the Moon: Recent results, science, future
robotic and human exploration
Authors: Foing, Bernard H.; Ehrenfreund, Pascale
Bibliographic Code: 2008AdSpR..42..235F
Abstract
The upcoming fleet of lunar missions, and the announcement of new lunar
exploration initiatives, show an exciting ``Journey to the
Moon'', covering recent results, science, future robotic and human
exploration. We review some of the questions, findings and perspectives
given in the papers included in this issue of Advances in Space
Research.
@--------------------------------------------------------------------
Title: A Cryogenic Liquid-Mirror Telescope on the Moon to
Study the Early Universe
Authors: Angel, Roger; Worden, Simon P.; Borra, Ermanno F.;
Eisenstein, Daniel J.; Foing, Bernard; Hickson, Paul;
Josset, Jean-Luc; Ma, Ki Bui; Seddiki, Omar;
Sivanandam, Suresh; Thibault, Simon;
van Susante, Paul
Bibliographic Code: 2008ApJ...680.1582A, eprint = 0806.2241
Abstract
We have studied the feasibility and scientific potential of zenith
observing liquid-mirror telescopes having 20-100 m diameters located on
the Moon. They would carry out deep infrared surveys to study the
distant universe and follow up discoveries made with the 6 m James Webb
Space Telescope (JWST), with more detailed images and spectroscopic
studies. They could detect objects 100 times fainter than JWST,
observing the first high-redshift stars in the early universe and their
assembly into galaxies. We explored the scientific opportunities, key
technologies, and optimum location of such telescopes. We have
demonstrated critical technologies. For example, the primary mirror
would necessitate a high-reflectivity liquid that does not evaporate in
the lunar vacuum and remains liquid at less than 100 K. We have made a
crucial demonstration by successfully coating an ionic liquid that has
negligible vapor pressure. We also successfully experimented with a
liquid mirror spinning on a superconducting bearing, as will be needed
for the cryogenic, vacuum environment of the telescope. We have
investigated issues related to lunar locations, concluding that
locations within a few kilometers of a pole are ideal for deep sky cover
and long integration times. We have located ridges and crater rims
within 0.5° of the north pole that are illuminated for at least some
sun angles during lunar winter, providing power and temperature control.
We also have identified potential problems, like lunar dust. Issues
raised by our preliminary study demand additional in-depth analyses.
These issues must be fully examined as part of a scientific debate that
we hope to start with the present article.
@--------------------------------------------------------------------
Title: Lunar landers and sample return: science and
technologies
Authors: Foing, Bernard H.
Bibliographic Code: 2008SPIE.6960E...7F
Abstract
We review in the context of latest lunar results the case for future
lunar landers and sample returns, as discussed by various ILEWG science
and technology task groups, addressing: - ESA Lunar Polar Lander Study
(LES3) - A generic lander platform that can be adapted to sample return
or to a lunar lander /rover fetcher. - New Science opportunities from
lunar landers - Clues on mantle/lower crust (South Pole Aitken Basin),
polar ice, cometary/meteoritic record - Technology demonstration
preparation for Mars sample return - Technology demonstrator for lunar
ascent vehicle, Earth reentry, and human return vehicle Technologies
that can be developed for lunar sample return missions: entry airless
bodies, Descent and landing, robotics, Instruments, Sample acquisition,
Return and Earth reentry.
@--------------------------------------------------------------------
Title: ILEWG technology roadmap for Moon exploration
Authors: Foing, Bernard H.
Bibliographic Code: 2008SPIE.6960E...6F
Abstract
We discuss the charter and activities of the International Lunar
Exploration Working Group (ILEWG), and give an update from the related
ILEWG task groups. We discuss the different rationale and technology
roadmap for Moon exploration, as debated in previous ILEWG conferences.
The Technology rationale includes: 1) The advancement of
instrumentation: 2) Technologies in robotic and human exploration 3)
Moon-Mars Exploration can inspire solutions to global Earth sustained
development. We finally discuss a possible roadmap for development of
technologies necessary for Moon and Mars exploration.
@--------------------------------------------------------------------
Title: SMART-1 results and future lunar exploration
Authors: Foing, Bernard H.
Bibliographic Code: 2008SPIE.6960E...5F
Abstract
We present some highlights from SMART-1's science and technology
payload, and the relevance of SMART-1 results and lessons for future
lunar exploration. SMART-1 is the first ESA mission that reached the
Moon. It is the first of Small Missions for Advanced Research and
Technology. It has fulfilled its technology objectives to demonstrate
Solar Electric Primary Propulsion (SEP) and to test new technologies for
spacecraft and instruments. After a 15-month cruise with primary SEP and
successful technology demonstration, the SMART-1 science and exploration
phase, provided first lunar orbit results. The mission has been extended
one year and ended with an impact on 3 September 2006.
@--------------------------------------------------------------------
Title: SMART-1/Clementine Study of Humorum and Procellarum
Basins: Coupling Between Impacts, Volcanism and
Tectonics
Authors: Peters, S. Tm.; Foing, B. H.; Koschmy, D.;
Rossi, A. P.; Josset, J. L.; Beauvivre, S.;
SMART-1 Amie Team
Bibliographic Code: 2008LPI....39.2548P
Abstract
We combined SMART-1 AMIE and Clementine UV/VIS data for two end-member
lunar basins to determine the coupling between basin and tectonics. For
Humorum but not Procellarum, tectonic-induced features agree well with
an idealized tectonic model.
@--------------------------------------------------------------------
Title: SMART-1 Lunar Science Planning
Authors: Koschny, D.; Foing, B. H.; Frew, D.; Grieger, B.;
Almeida, M.; Sarkarati, M.; Volp, J.; Josset, J.-L.;
Beauvivre, S.; Grande, M.; Huovelin, J.; Nathues, A.;
Malkki, A.; Noci, G.; Kellett, B.; Heather, D. J.;
Zender, J.; McMannamon, P.; Schwehm, G.; Camino
Bibliographic Code: 2008LPI....39.2282K
Abstract
The SMART-1 spacecraft reached on 15 March 2005 a lunar orbit 400-3000
km for a nominal science period of six months, with a one year science
extension until impact on 3 September 2006. We report on the SMART-1
science planning methods, tools, and lessons learned.
@--------------------------------------------------------------------
Title: Coverage and Pointing Accuracy of SMART-1/AMIE
Images
Authors: Grieger, B.; Foing, B. H.; Koschny, D.;
Josset, J. L.; Beauvivre, S.; Frew, D.; Almeida, M.;
Sarkarati, M.; Volp, J.; Pinet, P.; Chevrel, S.;
Cerroni, P.; de Sanctis, M. C.; Barucci, M. A.;
Erard, S.; Despan, D.; Muinonen, K.; Shevchenko, V.;
Shkuratov, Y.
Bibliographic Code: 2008LPI....39.2221G
Abstract
During 18 months of science operations from 400-3000 km lunar orbit, the
AMIE camera onboard the SMART-1 spacecraft acquired about 32,000 images.
We report on the coverage at various resolutions (until 50 m/pixel) and
the pointing accuracy.
@--------------------------------------------------------------------
Title: SMART-1 Lunar Highlights
Authors: Foing, B. H.; Koschny, D.; Grieger, B.;
Josset, J.-L.; Beauvivre, S.; Grande, M.;
Huovelin, J.; Keller, H. U.; Mall, U.; Nathues, A.;
Malkki, A.; Noci, G.; Sodnik, Z.; Kellett, B.;
Pinet, P.; Chevrel, S.; Cerroni, P.;
de Sanctis, M. C.; Barucci, M. A.; Er
Bibliographic Code: 2008LPI....39.1987F
Abstract
We report on SMART-1 lunar highlights results relevant for science and
exploration. We address impact and volcanic processes. We analyse images
of lunar north and south poles, for the characterisation of sites for
future landers, rovers, and human bases.
@--------------------------------------------------------------------
Title: The Opposition Effect of the Moon from SMART-1 AMIE
Data
Authors: Kaydash, V.; Kreslavsky, M. A.; Shkuratov, Yu.;
Gerasimenko, S.; Pinet, P.; Chevrel, S.;
Josset, J.-L.; Beauvivre, S.; Foing, B. H.;
Amie SMART-1 Team
Bibliographic Code: 2008LPI....39.1195K
Abstract
Images obtained by the AMIE camera onboard SMART-1 spacecraft allow
access to low-phase-angle data. We use AMIE data to study the opposition
spike for lunar sites and estimate the steepness of phase function in
the phase angle range 0°-2.5°.
@--------------------------------------------------------------------
Title: Microbial community induces a plant defense system
under growing on the lunar regolith analogue
Authors: Zaetz, Irina; Mytrokhyn, Olexander; Lukashov, Dmitry;
Mashkovska, Svitlana; Kozyrovska, Natalia;
Foing, Bernard H.
Bibliographic Code: 2008cosp...37.3584Z
Abstract
The lunar rock considered as a potential source of chemical elements
essential for plant nutrition, however, this substrate is of a low
bioavailability. The use of microorganisms for decomposition of silicate
rocks and stimulation of plant growth is a key idea in precursory
scenario of growing pioneer plants for a lunar base (Kozyrovska et al.,
2004; 2006; Zaetz et al., 2006). In model experiments a consortium of
well-defined plant-associated bacteria were used for growing of French
marigold (Tagetes patula L.) in anorthosite, analogous to a lunar rock.
Inoculated plants appeared better seed germination, more fast
development and also increased accumulation of K, Mg, Mn, Co, Cu and
lowered level of the toxic Zn, Ni, Cr, comparing to control tagetes'.
Bacteria regulate metal homeostasis in plants by changing their
bioavailability and by stimulating of plant defense mechanisms.
Inoculated plants were being accommodated to growth under stress
conditions on anorthosite used as a substrate. In contrast, control
plants manifested a heavy metal-induced oxidative stress, as quantified
by protein carbonyl accumulation. Depending on the plant organ sampled
and developmental stage there were increases or loses in the antioxidant
enzyme activities (guaiacol peroxidase and glutathione-S-transferase).
These changes were most evident in inoculated plants. Production of
phenolic compounds, known as antioxidants and heavy metal chelators, is
rised in variants of inoculated marigolds. Guaiacol peroxidase plays the
main role, finally, in a reducing toxicity of heavy metals in plant
leaves, while glutathione-S-transferase and phenolics overcome stress in
roots.
@--------------------------------------------------------------------
Title: Photometric study of the Moon with SMART-1/AMIE
Authors: Naranen, Jyri; Parviainen, Hannu; Muinonen, Karri;
Josset, Jean-Luc; Beauvivre, Stephane;
Koschny, Detlef; Foing, Bernard H.; Krieger, Bjoern;
Amie Team
Bibliographic Code: 2008cosp...37.2178N
Abstract
The Advanced Moon micro-Imager Experiment (AMIE) onboard the ESA SMART-1
lunar mission performed imaging of the Moon between November 2004 and
September 2006, when the mission was ended by crashing the spacecraft
into the lunar surface. AMIE was a 1024X1024 pixel miniaturized CCD
camera with three colour filters and a panchromatic channel (clear
filter). The images are of medium-to-high resolution, e.g. at 300 km
pericenter altitude the resolution was 27 m/pix. We selected four
different regions on the lunar surface imaged by AMIE for the
photometric investigation reported here. These regions were selected so
that as large phase angle coverage as possible was available, including
the opposition geometry. Each of the regions cover a few hundred square
kilometers of the lunar surface and were imaged by AMIE several tens of
times. The regions examined include, e.g., Reiner gamma and Oceanus
Procellarum near the crater Mairan. We utilized the latest in-flight
calibration data available and we also georetrified the images to
account for the aspect distortions. For the study reported here, the
panchromatic filter was chosen since it is the best calibrated channel
at the moment. The data was analyzed by implementing a numerical light
scattering model with which we have inverted the regolith porosity and
macroscopic surface roughness properties for the target areas. The model
computes the bidirectional reflectance function using the
geometric-optics approximation from a particulate medium constrained by
a self-affine fractal random fields mimicking the regolith-covered lunar
surface. Fractal description of the surface roughness is used, since it
gives a more realistic way to model the true macroscopic surface
roughness than the often used Gaussian correlation-model. Unlike in the
previous studies, the azimuthal shadowing effects are taken into
account, allowing for a more reliable inversion of surface statistics
from images with large phase angles. In addition, we have fitted an
empirical photometric function to the data which can be used to perform
photometric correction to the images in, e.g., image mosaicking. A
comparison with the results from the relevant previous photometric
studies of the Moon is given. We end by presenting plans for future
studies, especially the possible multi-colour photometry.
@--------------------------------------------------------------------
Title: Lunar landers and sample return: science and
exploration
Authors: Foing, Bernard H.
Bibliographic Code: 2008cosp...37..908F
Abstract
We present the results of a study for a lunar polar lander conducted at
ESA CDF Concurrent Design Facility and follow up activities. The goal is
to demonstrate lunar landing, survival and exploration technologies for
the future, geochemical studies of the piles, and search for ice in
permanent shadows. We describe the top objectives, mission analysis,
design and associated lander and rover. We also describe the possible
payload complement in discussion with the community. We also describe
the rationale for Lunar Sample Return missions, and give some concept
studies. Finally, we discuss the required advances in planetary
robotics, required for both the polar lunar lander and for the sample
return missions.
@--------------------------------------------------------------------
Title: Synthesis of SMART-1 lunar results: Science and
Exploration
Authors: Foing, Bernard H.
Bibliographic Code: 2008cosp...37..907F
Abstract
We shall give a synthesis on SMART-1 lunar highlights relevant for
science and exploration. The SMART-1 spacecraft reached on 15 March 2005
a lunar orbit 400-3000 km for a nominal science period of six months,
with 1 year extension until impact on 3 September 2006. SMART-1 lunar
science investigations include studies of the chemical composition of
the Moon, of geophysical processes (volcanism, tectonics, cratering,
erosion, deposition of ices and volatiles) for comparative planetology,
and high resolution studies in preparation for future steps of lunar
exploration. The mission addresses several topics such as the
accretional processes that led to the formation of rocky planets, and
the origin and evolution of the Earth-Moon system. SMART-1 AMIE camera
has been used to map sites of interest that are relevant to the study of
cataclysm bombardment, and to preview future sites for sampling return.
Lunar North polar maps and South pole repeated high resolution images
have been obtained, giving a monitoring of illumination to map potential
sites relevant for future exploration. The SMART-1 observations have
been coordinated with upcoming missions. SMART-1 has been useful in the
preparation of Selene Kaguya, the Indian lunar mission Chandrayaan-1,
Chinese Chang'E 1 , the US Lunar Reconnaissance Orbiter, LCROSS, and
subsequent lunar landers. SMART-1 is contributing to prepare the next
steps for exploration: survey of resources, search for ice, monitoring
polar illumination, and mapping of sites for potential landings,
international robotic villages and for future human activities and lunar
bases.
@--------------------------------------------------------------------
Title: ILEWG roadmap Robotic and Human Lunar Exploration
Authors: Foing, Bernard H.
Bibliographic Code: 2008cosp...37..906F
Abstract
We shall discuss the rationale and roadmap of ongoing Moon missions, and
how they can prepare for future human exploration. Various fundamental
scientific investigations can be performed with robots and humans: clues
on the formation and evolution of rocky planets, accretion and
bombardment in the inner solar system, comparative planetology processes
(tectonic, volcanic, impact cratering, volatile delivery), records
astrobiology, survival of organics; past, present and future life. The
roadmap includes also enabling technologies that prepare for the best
syenrgies between robots and humans: Remote sensing miniaturised
instruments; Surface geophysical and geochemistry package;Instrument
deployment and robotic arm, nano-rover, sampling, drilling; Sample
finder and collector, Support equipment for astronaut sorties; life
science precursors for life support systems. We shall adddress
requirements for robotic precursor programmes, global robotic village,
technology development, resource utilisation, human aspects, science and
exploration from lunar sorties, transition towards permanent settlements
and lunar bases.
@--------------------------------------------------------------------
Title: SMART-1 Moon impact on 3 Sept 2006: results from
observation campaign
Authors: Foing, Bernard H.
Bibliographic Code: 2008cosp...37..905F
Abstract
SMART-1 was launched in 2003 and orbited the Moon on a 5 hours period
until impact on 3 sept 2006. A controlled impact took place in grazing
incidence with mass of 285 kg at a velocity of 2 km/s in the Lake of
Excellence. We called the community to make predictions of impact
magnitude, cloud ejecta dynamics, exospheric effects. We also called the
ground based observers to perform coordinated measurements of the
impact. We shall discuss results from the coordinated multi-site
campaign, in particular observations from CFHT of the flash impact and
debris clouds. We shall draw lessons for future lunar impacts including
LCROSS.
@--------------------------------------------------------------------
Title: Diffuse Interstellar Bands and Complex Organics
Authors: Foing, Bernard H.; Ehrenfreund, Pascale; Cox, Nick
Bibliographic Code: 2008cosp...37..904F
Abstract
The origin of Diffuse Interstellar Bands (Herbig 1995), more than 300 in
recent surveys (O' Tuairisg et al 2000) is still a mystery. However the
measurements of sub-structures rotational contours in DIBs (Ehrenfreund
Foing 1996) indicate large molecules such as chains (12-18C), rings, 50
C PAHs or fullerenes. The distribution of DIB widths permit to estimate
a distribution of size of molecular carriers. The environment properties
of DIB carriers also indicate ionisation potentials similar to those of
cations of large carbonaceous molecules, such as large PAHs or
fullerenes (Sonnentrucker et al 1997). The correlation studies of DIBS
also indicate different carriers for the strong DIBs observed in the
visible (Cami et al 1997). Polarisation studies could also give
constraints on the carriers (Cox et al 2007). DIBS are weakened in the
low-metallicity Magellanic clouds (Ehrenfreund et al 2002, Cox et al
2006, 2007). The detection of near IR bands at 9577 and 9632 A
coinciding with laboratory transitions of C60+ (Foing, Ehrenfreund 1994,
1997) suggest that significant interstellar carbon could reside in
complex fullerene type compounds or PAHs. We report on new CFHT Espadons
observations of the C60+ and other diffuse bands.
@--------------------------------------------------------------------
Title: Search for Mars climatic signal in Pavonis Mons Fan
& other periglacial deposits
Authors: Foing, Bernard H.; Forget, Francois;
Pio Rossi, Angelo; Head, James; Neukum, Gerhard
Bibliographic Code: 2008cosp...37..903F
Abstract
Mars has experienced large variations in its orbital parameters
through-out its history. They are calculable for the last 10 million
years, with periodicity of 120 000 years for its obliquity, 95 to
100,000 years for its excentricity, and 51,000 years for its precession,
however they become undetermined beyond 20 Myr. Laskar et al determined
a standard model of Mars' insolation parameters over 4 Gyr with the most
probable values 0.068 for the eccentricity and 41.80 degrees for the
obliquity. At high obliquity, signicant amount of ice can be deposited
as ice at low latitudes. This can be relevant for understanding features
from the modern Polar Layered Deposits, the Elysium frozen sea (Murray
et al 2005),or Ellas hourglass (Head et al 2005). General circulation
models predict an annual net accumulation rate of ice on the west of
Tharsis volcanoes. We analysed Mars Express images obtained over orbit
946, of the west fan deposit at Pavonis Mons. The analysis of the HRSC
images shows around 15 ridges, with interval 0.5 -4.5 km. The
interaction with the under-lying surface can be seen, indicating the
overlap of different episodes. The ridges are interpreted as drop debris
on the front edge of a cold glaciar during its slow retreat. On the
other hand isotropic knobbies, circular sub-kmscale hills are
interpreted as results of fast glaciar sublimation. By texture analysis
we could distinguish ridges, knobbies from various episodes and relate
them with geological studies. For this basic study, we choose the
simplest model of glacier profile. The bed is believed to be horizontal,
and does not interfere with the glacier. If the ridges are due to
obliquity oscillation, the rate of snow fall and sublimation depend
strongly on obliquity. Indeed, with the balance of accumulation rates
and ablation rates, we can predict oscillations of the glacier extent.
We discuss how this can be used to serach for Martian climatic signal.
@--------------------------------------------------------------------
Title: High Resolution North and South Polar Maps of the
Moon with AMIE/SMART-1
Authors: Despan, Daniela; Erard, Stephane;
Beauvivre, Stephane; Chevrel, Serge; Pinet, Patrick;
Almeida, Miguel; Grieger, Bjoern; Cerroni, Priscilla;
Barucci, M. A.; Josset, Jean-Luc; Koschny, Detlef;
Foing, Bernard H.
Bibliographic Code: 2008cosp...37..703D
Abstract
The northern and southern polar areas maps of the Moon are obtained by
processing and mosaiking of the AMIE, SMART-1 images. The Advanced Moon
micro-Imager Experiment (AMIE) on board the ESA lunar mission Smart-1
has performed colour imaging of the lunar surface using various filters
in the visible and NIR. The low pericenter, polar orbit, allowed to
obtain high resolution images in various locations at the surface. From
the 300 km pericenter altitude, the field of view (5,3° x5,3° )
corresponds to a spatial resolution about 30 m. The 1024x1024 images are
shared by the various filters, allowing to derive mosaics of the surface
in up to 3 colors depending on pointing mode. Spot-pointing observations
and multiple observations from different orbits have provided
photometric sequences that allow to study the surface properties in
restricted areas. Geometrical analysis of the AMIE images relies on the
SPICE system: image coordinates are computed to get precise projection
at the surface, and illumination angles are computed to analyze the
photometric sequences. Images from various orbits are first identified
for each selected region of interest. These images are then selected
according to signal to noise ratio, spatial coverage, and spatial
resolution. The best images obtained with the neutral filter are
calibrated, and mosaicked using the coordinates of the image frames
corners. In the polar areas, images are selected so as to provide the
best possible viewing of surface topography, depending on solar
illumination angle, while preserving images continuity in shadowed
areas. The maps of other regions of interest are yielded: Marius Hills,
the Gruitheisen Domes, Rumker Hills, Aristarchus Plateau. Eventually,
this method will be applied in all regions where AMIE has provided high
resolution observations of the surface, typically a factor of 3 higher
than the Clementine UV-vis camera. These regions are essentially located
at latitude ranging from 80 to 40° S, specially in the eastern
hemisphere.
@--------------------------------------------------------------------
Title: SMART-1/CLEMENTINE Study of Humorum and Procellarum
Basins
Authors: Carey, William; Foing, Bernard H.; Koschny, Detlef;
Pio Rossi, Angelo; Josset, Jean-Luc
Bibliographic Code: 2008cosp...37..457C
Abstract
A study undertaken by ESA to define a European Reference Architecture
for Space Exploration is due to be completed in September 2008. The
development of this architecture over the past twelve months has
identified a number of key capabilities, among them a lunar lander
system, which could form the basis for Europe's contribution to the
future exploration of space in collaboration with International
Partners. The focus of this paper will be on the lunar lander system,
and will present the results of an analysis of possible payloads that
could be accommodated by the lander. As the industrial study is at the
Phase 0 or Pre-Phase A level, the design of such a lander system is at a
very early stage in its development, but an estimation of the payload
capacity allows a general assessment of the types of possible payloads
that could be carried, currently this capacity is estimated at 1.1
tonnes of gross payload mass to the lunar surface (assuming an Ariane 5
ECA launch). An important characteristic of the lunar lander is that it
provides a versatile and flexible system for utilisation in a broad
range of lunar missions which include: - Independent lunar exploration
missions for science, technology demonstration and research. - Delivery
of logistics and cargo to support human surface sortie missions. -
Delivery of logistics to a lunar base/outpost. - Deployment of
individual infrastructure elements in support of a lunar base/outpost.
Based on the above different types of missions, a number of
configurations of "reference payload" sets are in the process of being
defined that cover specific exploration objectives related primarily to
capability demonstration, exploration enabling research and enabled
science. Aspects covered include: ISRU, robotics, mobility, human
preparation, life science and geology. This paper will present the
current status of definition of the Reference Payload sets.
@--------------------------------------------------------------------
Title: Coverage, resolution, and calibration of
SMART-1/AMIE images
Authors: Bjoern, Grieger; Foing, Bernard H.; Almeida, Miguel;
Beauvivre, Stephane; Josset, Jean-Luc;
Koschny, Detlef; Dougnac, Virgile; Martinez, Santa
Bibliographic Code: 2008cosp...37..310B
Abstract
The SMART-1 spacecraft was launched on 27 September 2003 end reached its
lunar baseline science orbit on 13 March 2005 for a nominal science
period of six months and one year extension. During these 18 months, the
AMIE camera aboard the spacecraft acquired about 32 000 images. SMART-1
operated in an eccentric polar orbit with the perilune close to the
South pole at a minimum distance of 400 km and an apolune distance of
about 6400 km. The small but scientifically quite interesting area south
off 87° S and various spots in the southern hemisphere are covered
by the AMIE camera with a resolution better than 50 meters per pixel.
The complete Southern hemisphere is covered with a resolution better
than 100 meters per pixel. Finally, global coverage is achieved with a
resolution better than 250 meters per pixel. Each AMIE image frame of
1024 × 1024 pixels is divided into areas covered by four different
filters and one area of 512 × 512 pixels which is uncovered. First
inspections of the images had revealed that the dark current of the CCD
increased significantly during the cruise phase when the space craft
crossed the radiation belt several times. Therefore, the dark frames
acquired in the laboratory prior to the mission are not adequate to
perform the dark correction. From the analysis of dark sky images taken
during the lunar phase of the mission, new master dark frames were
estimated which have been used to calibrate the images. We discuss the
calibration of AMIE images and present examples from different regions
of the lunar surface.
@--------------------------------------------------------------------
Title: Surface roughness and geological mapping at
subhectometer scale from the High Resolution Stereo
Camera onboard Mars Express
Authors: Cord, Aurélien; Baratoux, David; Mangold, Nicolas;
Martin, Patrick; Pinet, Patrick; Greeley, Ronald;
Costard, Francois; Masson, Philippe; Foing, Bernard;
Neukum, Gerhard
Bibliographic Code: 2007Icar..191...38C
Abstract
The quantitative measurement of surface roughness of planetary surfaces
at all scales provides insights into geological processes. A
characterization of roughness variations at the scale of a few tens of
meters is proposed that complements the analysis of local topographic
data of the martian surface at kilometer scale, as achieved from the
Mars Orbiter Laser Altimeter (MOLA) data, and at the subcentimeter scale
using photometric properties derived from multi-angular observations.
Relying on a Gabor filtering process, an algorithm developed in the
context of image classification for the purpose of texture analysis has
been adapted to handle data from the High Resolution Stereo Camera
(HRSC). The derivation of roughness within a wavelength range of tens of
meters, combined with analyses at even longer wavelengths, gives an
original view of the martian surface. The potential of this approach is
evaluated for different examples for which the geological processes are
identified and the geological units are mapped and characterized in
terms of roughness.
@--------------------------------------------------------------------
Title: Site Selection and Lunar Outpost: SMART-1 Results
and ESA Studies
Authors: Foing, B.
Bibliographic Code: 2007LPICo1371.3062F
Abstract
@--------------------------------------------------------------------
Title: Geometrical Analysis of AMIE/Smart-1 Images and
Applications to Photometric Studies of the Lunar
Surface
Authors: Despan, Daniela; Erard, S.; Barucci, M. A.;
Josset, J. L.; Beauvivre, S.; Chevrel, S.; Pinet, P.;
Koschny, D.; Almeida, M.; Foing, B. H.; AMIE Team
Bibliographic Code: 2007DPS....39.2508D
Abstract
AMIE, the Advanced Moon micro-Imager Experiment on board the ESA lunar
mission SMART-1, is an imaging system to survey the terrain in visible
and near-infrared light. AMIE provides high resolution images obtained
using a tele-objective with 5.3° x 5.3° field of view and a
sensor of 1024 x 1024 pixels. The output images have resolution
45m/pixel at 500km, and are encoded with 10 bits/pixel. From the 300 Km
pericenter altitude, the same field of view corresponds to a spatial
resolution about 30 m/pixel. The FOV is shared by various filters,
allowing to reconstruct mosaics of the surface in 3 colors, depending on
pointing mode. Spot-pointing observations provide photometric sequences
that allow to study the surface properties in restricted areas. One of
the scientific objectives of the mission is to get high resolution
imaging of the Moon surface, e.g. high latitude regions in the southern
hemisphere.
In order to map the lunar surface with AMIE, systematic analysis and
processing is being carried on using the whole data set. Geometrical
analysis of AMIE images relies on the SPICE system: image coordinates
are computed to get precise projection at the surface, and illumination
angles are computed to analyze the photometric sequences. High
resolution mosaics were constructed then compared to lower resolution
Clementine UV-Vis and NIR images. Spot-pointing sequences are used to
constrain the photometric and physical properties of surface materials
in areas of interest, based on Hapke's modeling.
Optical alignment parameters in the Spice kernels have been refined and
provide absolute coordinates in the IAU lunar frame (ULCN). They provide
discrepancies with the Clementine basemap, ranging up to some 0.1°
in the equatorial regions, as expected (e.g., Cook et al DPS 2002;
Arcinal et al. EPSC 2006). A progress report will be presented at the
conference.
@--------------------------------------------------------------------
Title: Results from the SMART-1 lunar mission
Authors: Foing, Bernhard H.
Bibliographic Code: 2007HiA....14..329F
Abstract
Results of the SMART-1 mission to Earth's Moon are summarized.
@--------------------------------------------------------------------
Title: Search for Climatic Signal in Pavonis Mons Fan
Deposits, Mars
Authors: Foing, B. H.; Orsi, A.; Cord, A.; Rossi, A.
Bibliographic Code: 2007epsc.conf..601F
Abstract
Introduction: Mars has experienced large variations in its orbital
parameters throughout its history. They are calculable for the last 10
million years, with periodicity of 120 000 years for its obliquity, 95
to 100 000 years for its excentricity, and 51 000 years for its
precession, however they become undetermined beyond 20 Myr [1]. Laskar
et al [2] define a standard model of Mars' insolation parameters over 4
Gyr with the most probable values 0.068 for the eccentricity and 41.80
degree for the obliquity. Climatic consequences: At high obliquity,
significant amount of ice can be deposited as ice at low latitudes.
General circulation models predict an annual net accumulation rate of
ice on the west of Tharsis volcanoes. Pavonis fan shaped deposits: We
analysed Mars Express images obtained over orbit 946, of the west fan
deposit at Pavonis Mons. The analysis of the HRSC images shows around 15
ridges, with interval 0.5 - 4.5 km. The interaction with the underlying
surface can be seen, indicating the overlap of different episodes. The
ridges are interpreted as drop debris on the front edge of a cold
glaciar during its slow retreat. On the other hand isotropic knobbies,
circular sub-km-scale hills are interpreted as results of fast glaciar
sublimation. By texture analysis we could distinguish ridges, knobbies
from various episodes and relate them with geological studies [3].
Glaciar model: For this basic study, we choose the simplest model of
glacier. The bed is believed to be horizontal, and does not interfere
with the glacier. If the ridges are due to obliquity oscillation, the
rate of snow fall and sublimation must depend slightly on obliquity.
Indeed, with accumulation rates and ablation rates at the same order, we
are able to find oscillation of the glacier extent. We can see
oscillations of the glacier extent from the beginning. It is interesting
to notice that this shape is consistent with the observation of older
outer sets of ridges, and young inner ones. The maximum extents, which
we intent to link to the position of the ridges are organized by groups
of 4 or 5. The outer ridges we see on Pavonis Mons date back to 10-200
million years ago. We know that the obliquity raised 5 million years
ago. The recent lowering of the obliquity could have triggered inner
ridges too, but the outer ones we see look older. To account for their
formation, we have to find an area of great variation in obliquity,
allowing the glacier to form and retreat, before 10 millions years ago.
A threshold obliquity angle above 35 deg for effective ice deposition is
needed to account for a glacier older than 10 million years. Conclusions
and Perspectives: Ridges in Pavonis Mons Fan deposits could be
interpreted as cold glaciar debris tracing climate changes. Texture
analysis to distinguish units and episodes from different obliquity and
climate variations. We developed a simple qualitative glaciar
progression/recession model. One needs to better quantify ice
deposition/ablation net rates vs obliquity. We find that a 45 deg
obliquity deposition threshold could better describe the Pavonis Mons
Fan deposits data. Next steps in modeling should include the effect of
topography, slopes, orientation. The geologic stratigraphy can constrain
the evolution of fan deposits [3], in conjunction with crater counts
dating and chronology. The climatic signal imprinted as ridges could be
determined over the period of large extend of glaciar, and could permit
to constrain the undetermined obliquity variations beyond 15 Myr [2].
References: [1] Laskar et al 2002 Nature 419, 375, [2] Laskar et al
(2004, Icarus, Volume 170, Issue 2, p. 343-364. [3] Shean, D.E., Head,
J.W., Marchant, D.R. 2005, JGR, 110, E5
@--------------------------------------------------------------------
Title: SMART-1 Collaborations with Upcoming Lunar Missions
Authors: Foing, B. H.
Bibliographic Code: 2007epsc.conf..444F
Abstract
We discuss ongoing collaborations between SMART-1 and upcoming Lunar
missions (Chang'e1, Selene, Chandrayaan-1, LRO, LCROSS, future Lunar
Landers and Rovers) . This includes: - Data analysis and PSA archiving;
- Merging data between different missions; - Coordinate systems and
reference grid; - Scientific interpretation; - Survey of possible
landing sites; - Lessons from SMART-1 Impact experiment - Survey of
illumination and resources for future exploration - New miniaturised
instruments development; - Lessons from SMART-1 development; - SMART-1
science planning tool; - Public outreach and education.
@--------------------------------------------------------------------
Title: SMART-1 Moon impact on 3 Sept 2006: results from
observation campaign
Authors: Ehrenfreund, P.; Foing, B. H.; Veillet, C.
Bibliographic Code: 2007epsc.conf..425E
Abstract
SMART-1 operations ended with an impact on the lunar near-side on 3 sept
2006, adjusted in time to allow ground-based observations. The impact
took place in grazing incidence with mass of 285 kg at a velocity of 2
km/s in the Lake of Excellence. We called the community to make
predictions of impact magnitude, cloud ejecta dynamics, exospheric
effects. We also called the ground based observers to perform
coordinated measurements of the impact. Results from the SMART-1 impact
campaign will be discussed.
@--------------------------------------------------------------------
Title: Highlights of SMART-1 Lunar Science results
Authors: Foing, B. H.
Bibliographic Code: 2007epsc.conf..424F
Abstract
We shall present the highlights of lunar science results from SMART-1
payload, featuring many innovative instruments and advanced
technologies. SMART-1 lunar science investigations include studies of
the chemical composition of the Moon, of geophysical processes
(volcanism, tectonics, cratering, erosion, deposition of ices and
volatiles) for comparative planetology, and high resolution studies in
preparation for future steps of lunar exploration. The mission science
addresses several topics such as the accretional processes that led to
the formation of rocky planets, and the origin and evolution of the
Earth-Moon system.
@--------------------------------------------------------------------
Title: Science rationale and payload for lunar landers and
sample return missions
Authors: Foing, B. H.
Bibliographic Code: 2007epsc.conf..423F
Abstract
We present the results of a study for a lunar polar lander conducted at
ESA CDF Concurrent Design Facility and follow up activities. The goal is
to demonstrate lunar precise landing, survival and exploration
technologies for the future, geochemical studies of the poles, and
search for ice in permanent shadows. We describe the top science
objectives, the associated lander and rover, and the possible payload
complement now in discussion with the community. We also describe the
science rationale for Lunar Sample Return missions, and give update on
some ongoing concept studies performed at ESA.
@--------------------------------------------------------------------
Title: Concept studies for lunar landers and sample return
missions: challenges for robotics
Authors: Foing, B. H.
Bibliographic Code: 2007epsc.conf..422F
Abstract
We present the results of a study for a lunar polar lander conducted at
ESA CDF Concurrent Design Facility and follow up activities. The goal is
to demonstrate lunar landing, survival and exploration technologies for
the future, geochemical studies of the piles, and search for ice in
permanent shadows. We describe the top objectives, mission analysis,
design and associated lander and rover. We also describe the rationale
for Lunar Sample Return missions, and give some ongoing concept studies
performed at ESA. Finally, we discuss the required advances in planetary
robotics, required for the polar lunar lander and for the sample return
missions.
@--------------------------------------------------------------------
Title: Coupling between impacts and lunar volcanism for
Humorum and Procellarum basins
Authors: Peters, S. T. M.; Koschny, D.; Foing, B. H.
Bibliographic Code: 2007epsc.conf..355P
Abstract
A lot of knowledge has been obtained by ground-based observations and
previous space missions on Mare Humorum and Oceanus Procellarum, which
are a circular and irregular basin, respectively. Correlating tectonic
signatures and volcanic outflows within this area gives information on
the development of both basins; and thus on their origin of impact. By
marking different fracture patterns, paleo-stress fields occurring in
the area of both maria become visible. These stresses are believed to be
caused by the contrast in density of the solidified lava and the
anorthosite crust and therefore to be post-volcanic. The presence of
underlying topography and structures of fault systems influence the
formation of new zones of weakness within the basins. Therefore they
induce faults which do not properly reflect the stress field under which
they are formed. To exclude this distortion, only the most inner parts
of the basins are measured. Images from the AMIE-camera on SMART-1 Moon
mission were annotated for tectonic interpretation using ARC-GIS. A
volcanic outflow analysis is made using Clementine UVVIS-data: Lava
outflows from different origin were distinguished on base of their FeO
and TiO2 contents. Ages of the units were determined by cratercounting
methods from other authors. The eruptional and structural analyses
provide a model for the stratigraphic development and spatial occurrence
of the volcanic processes that flooded the maria. This model is compared
with both irregular and circular impact basins for different shape, age
and geographical positions. The results show how these impact-related
parameters influence volcanic mare evolution. With the geographical
position, also the depth and thickness of the KREEP-layer has been taken
in account.
@--------------------------------------------------------------------
Title: Potential rovers and payload for a future polar
lunar lander
Authors: Ellouzi, M.; Foing, B.; Hovland, S.
Bibliographic Code: 2007epsc.conf..238E
Abstract
Lunar poles are thought of being of high interest to land on, because
they have not been explored so far, they are near regions of
quasi-eternal light, or permanent shadow for potential ices and
volatiles, they are thermally benign and are promising sites for future
human outposts and permanent bases. In order to explore the Poles, a
future landing mission would need the help of one or more rovers, of
different sizes, allowing different levels of mobility around the
landing module. They would carry on experiments, which results could
improve our knowledge of the polar areas. Therefore, we describe here
possible rovers and payload capable of meeting both technological and
scientific requirements for Moon missions to the Poles.
@--------------------------------------------------------------------
Title: Interstellar gas, dust and diffuse bands in the SMC
Authors: Cox, N. L. J.; Cordiner, M. A.; Ehrenfreund, P.;
Kaper, L.; Sarre, P. J.; Foing, B. H.; Spaans, M.;
Cami, J.; Sofia, U. J.; Clayton, G. C.;
Gordon, K. D.; Salama, F.
Bibliographic Code: 2007A&A...470..941C
Abstract
Aims:In order to gain new insight into the unidentified identity of the
diffuse interstellar band (DIB) carriers, this paper describes research
into possible links between the shape of the interstellar extinction
curve (including the 2175 Å bump and far-UV rise), the presence or
absence of DIBs, and physical and chemical conditions of the diffuse
interstellar medium (gas and dust) in the Small Magellanic Cloud (SMC).
Methods: We searched for DIB absorption features in VLT/UVES
spectra of early-type stars in the SMC whose reddened lines-of-sight
probe the diffuse interstellar medium of the SMC. Apparent column
density profiles of interstellar atomic species (Na i, K i, Ca ii and Ti
ii) are constructed to provide information on the distribution and
conditions of the interstellar gas.
Results: The characteristics
of eight DIBs detected toward the SMC wing target AzV
456 are studied and upper limits are derived for the DIB
equivalent widths toward the SMC stars AzV 398,
AzV 214, AzV 18, AzV
65 and Sk 191. The amount of reddening is
derived for these SMC sightlines, and, using RV and the H i
column density, converted into a gas-to-dust ratio. From the atomic
column density ratios we infer an indication of the strength of the
interstellar radiation field, the titanium depletion level and a
relative measure of turbulence/quiescence. The presence or absence of
DIBs appears to be related to the shape of the extinction curve, in
particular with respect to the presence or absence of the 2175 Å
feature. Our measurements indicate that the DIB characteristics depend
on the local physical conditions and chemical composition of the
interstellar medium of the SMC, which apparently determine the rate of
formation (and/or) destruction of the DIB carriers. The UV radiation
field (via photoionisation and photo-destruction) and the metallicity
(i.e. carbon abundance) are important factors in determining diffuse
band strengths which can differ greatly both between and within
galaxies.
Based on observations collected with VLT/UVES at the European Southern
Observatory, Paranal, Chile (ESO programs 67.C-0281 and 71.C-0679).
Tables [see full text]-[see full text] and Fig. [see full text] are only
available in electronic form at http://www.aanda.org
@--------------------------------------------------------------------
Title: Search for Climatic Signal in Pavonis Mons Fan
Deposits
Authors: Foing, B. H.; Orsi, A.; Cord, A.; Zegers, T.;
Rossi, A.; HRSC Co-I Team
Bibliographic Code: 2007LPICo1353.3273F
Abstract
We analysed Mars Express HRSC images of the west fan deposits at Pavonis
Mons. We use the deposit ridges, interpreted as drop debris from cold
glaciar slow retreat, to search for climatic signal induced by the
variations of obliquity beyond 15 Myr ago.
@--------------------------------------------------------------------
Title: Linear and circular polarisation of diffuse
interstellar bands
Authors: Cox, N. L. J.; Boudin, N.; Foing, B. H.;
Schnerr, R. S.; Kaper, L.; Neiner, C.; Henrichs, H.;
Donati, J.-F.; Ehrenfreund, P.
Bibliographic Code: 2007A&A...465..899C
Abstract
Context: The detection or absence of a polarisation signal in the
diffuse interstellar band (DIB) profile can possibly give important
clues on the identity of its carrier. For molecular gas-phase carriers
the effect of polarisation on its electronic transitions depends,
although uncertain how exactly, on its physical properties (e.g.
molecular structure). On the other hand, if the carriers are grains,
impurities or defects in grain mantles are also expected to show up in
the polarisation of DIBs.
Aims: Our aim is to detect a
polarisation signal in a DIB profile or to derive stricter upper limits
on the polarisation efficiency of DIB carriers.
Methods: In
order to detect and measure the linear and circular polarisation of the
DIBs we observe reddened lines of sight showing continuum polarisation;
for this study we select the stars HD 21219,
HD 198478, HD 197770, HD
183143 and HD 163472. We use
spectropolarimetry in the wavelength range 4480 to 6620 Å with the
MuSiCoS échelle spectrograph mounted at the Télescope
Bernard Lyot.
Results: Linear polarisation spectra are
constructed in order to search for a polarisation signal in the DIB
profiles. No significant change in the linear polarisation degree is
found. We obtain a 2sigma polarisation detection limit (per DIB FWHM)
of 0.01-0.04% for HD 21219, 0.04-0.14% for
HD 197770, 0.01-0.14% for HD
183143 and 0.01-0.14% for HD 198478, for
the six investigated DIBs. We derive upper limits for the polarisation
efficiency factor f for six strong narrow DIBs; f_max of 0.31, 0.44,
0.45, 0.18, 0.47 and 0.68 for the lambdalambda 5780, 5797, 6196,
6284, 6379 and 6613 DIBs, respectively. The derived detection limits are
similar to those derived by Adamson & Whittet (1995), although for
more lines of sight and more DIBs. Circular polarisation (Stokes V)
spectra of high signal-to-noise have been obtained for the first time
for the 5780, 5797, 6196, 6203, 6284, 6376, 6379 and 6613 Å DIB
profiles. No circular polarisation signal is detected. The
2sigmaV (per 0.1 Å) noise level limits are 1.0-2.5%
for the DIBs in the line of sight towards HD 197770
and 0.06-0.10% for the DIBs towards HD 163472.
Conclusions: . The lack of polarisation of the DIB profiles is
consistent with DIB carriers that are not directly related to solid
features, like impurities in grain mantles. However, large
(carbonaceous) gas phase molecules remain viable DIB carrier candidates.
Based on observation
at the Observatoir du Pic du Midi, France with the MuSiCoS
spectropolarimeter.
@--------------------------------------------------------------------
Title: The D-CIXS X-ray spectrometer on the SMART-1 mission
to the Moon---First results
Authors: Grande, M.; Kellett, B. J.; Howe, C.; Perry, C. H.;
Swinyard, B.; Dunkin, S.; Huovelin, J.; Alha, L.;
D'Uston, L. C.; Maurice, S.; Gasnault, O.;
Couturier-Doux, S.; Barabash, S.; Joy, K. H.;
Crawford, I. A.; Lawrence, D.; Fernandes, V.;
Casanova, I.; Wieczorek, M.; Thomas, N.; Mall, U.;
Foing, B.; Hughes, D.; Alleyne, H.; Russell, S.;
Grady, M.; Lundin, R.; Baker, D.; Murray, C. D.;
Guest, J.; Christou, A.
Bibliographic Code: 2007P&SS...55..494G
Abstract
The SMART-1 mission has recently arrived at the Moon. Its payload
includes D-CIXS, a compact X-ray spectrometer. SMART-1 is a technology
evaluation mission, and D-CIXS is the first of a new generation of
planetary X-ray spectrometers. Novel technologies enable new
capabilities for measuring the fluorescent yield of a planetary surface
or atmosphere which is illuminated by solar X-rays. During the extended
SMART-1 cruise phase, observations of the Earth showed strong argon
emission, providing a good source for calibration and demonstrating the
potential of the technique. At the Moon, our initial observations over
Mare Crisium show a first unambiguous remote sensing of calcium in the
lunar regolith. Data obtained are broadly consistent with current
understanding of mare and highland composition. Ground truth is provided
by the returned Luna 20 and 24 sample sets.
@--------------------------------------------------------------------
Title: The ORGANICS experiment on BIOPAN V: UV and space
exposure of aromatic compounds
Authors: Ehrenfreund, Pascale; Ruiterkamp, Richard;
Peeters, Zan; Foing, Bernard; Salama, Farid;
Martins, Zita
Bibliographic Code: 2007P&SS...55..383E
Abstract
We studied the stability of aromatic compounds in low Earth orbit
environment and describe the scientific results and successful flight of
the ORGANICS experiment on-board the BIOPAN V space exposure facility.
This experiment investigated the photo stability of large organic
molecules in low Earth orbit. Thin films of selected organic molecules,
such as polycyclic aromatic hydrocarbons (PAHs) and the fullerene
C60 were subjected to the low Earth orbit environment and the
samples were monitored before and after flight. PAHs and fullerenes have
been proposed as carriers for a number of astronomical absorption and
emission features and are also identified in meteorites. Our experiment
on BIOPAN V was exposed to a total fluence of 602.45 kJ
m-2 for photons in the range 170 280 nm. The experiment
was also intended as a hardware test-flight for a long-term exposure
experiment (Survival of organics in space) on the EXPOSE facility on the
International Space Station (ISS). For the small fluence that was
collected during the BIOPAN V experiment we found little evidence of
photo-destruction. The results confirm that PAH molecules are very
stable compounds in space. The small differences in destruction rates
that are expected to arise among the PAH samples as a function of
molecular size and structure will only show after the longer irradiation
fluences that are expected in the exposure experiment on the ISS.
@--------------------------------------------------------------------
Title: SMART-1 Impact Ground-based Campaign
Authors: Ehrenfreund, P.; Foing, B. H.; Veillet, C.;
Wooden, D.; Gurvits, L.; Cook, A. C.; Koschny, D.;
Biver, N.; Buckley, D.; Ortiz, J. L.; di Martino, M.;
Dantowitz, R.; Cooke, B.; Reddy, V.; Wood, M.;
Vennes, S.; Albert, L.; Sugita, S.; Kasuga, T.;
Meech, K.
Bibliographic Code: 2007LPI....38.2446E
Abstract
Based on predictions of impact magnitude and cloud ejecta dynamics, we
organized a SMART-1 ground-based observation campaign to perform
coordinated measurements of the impact. Results from the coordinated
multi-site campaign will be discussed.
@--------------------------------------------------------------------
Title: SMART-1 Lunar Science Planning
Authors: Koschny, D.; Foing, B. H.; Frew, D.; Almeida, M.;
Sarkarati, M.; Volp, J.; Grande, M.; Huovelin, J.;
Josset, J.-L.; Nathues, A.; Malkki, A.; Noci, G.;
Kellett, B.; Beauvivre, S.; Heather, D.; Zender, J.;
McMannamon, P.; Schwehm, G.; Camino, O.; Blake, R.
Bibliographic Code: 2007LPI....38.1996K
Abstract
The SMART-1 spacecraft reached lunar capture on 17 November 2004, and on
15 March 2005 a lunar orbit 400-3000 km for a nominal science period of
six months, with 1 year science extension. We report on the SMART-1
science planning methods, tools and lesson
@--------------------------------------------------------------------
Title: SMART-1 Mission: Highlights of Lunar Results
Authors: Foing, B. H.; Grande, M.; Huovelin, J.;
Josset, J.-L.; Keller, H. U.; Nathues, A.;
Malkki, A.; Noci, G.; Kellett, B.; Beauvivre, S.;
Cerroni, P.; Pinet, P.; Makkinen, H.; Mall, U.;
Almeida, M.; Frew, D.; Volp, J.; Sarkarati, M.;
Heather, D.; Koschny, D.
Bibliographic Code: 2007LPI....38.1953F
Abstract
The SMART-1 spacecraft reached on 15 March 2005 a lunar orbit 400-3000
km for a nominal science period of six months, with 1 year science
extension until September 2006. We shall report on highlights of lunar
science and exploration results.
@--------------------------------------------------------------------
Title: SMART-1 Mission Overview from Launch, Lunar Orbit to
Impact
Authors: Foing, B. H.; Camino, O.; Schoenmakers, J.;
de Bruin, J.; Gestal, D.; Alonso, M.; Blake, R.;
Ricken, S.; Pardo, P.; Koschny, D.; Frew, D.;
Almeida, M.; Sarkarati, M.; Volp, J.; Schwehm, G.;
Josset, J. L.; Beauvivre, S.; Sodnik, Z.; Grande, M.;
Keller, U.
Bibliographic Code: 2007LPI....38.1915F
Abstract
We shall give an overview of the SMART-1 mission, travel and operations
from launch, lunar capture, lunar science orbit to impact.
@--------------------------------------------------------------------
Title: 3D Mapping of Aram Chaos: S Record of Fracturing and
Fluid Activity
Authors: Oosthoek, J. H. P.; Zegers, T. E.; Rossi, A.;
Foing, B.; Neukum, G.; HRSC Co-Investigation Team
Bibliographic Code: 2007LPI....38.1577O
Abstract
Mapping of structures and stratigraphic units of Aram Chaos was
performed with HRSC data, using in particular the stereo (3D)
capabilities of HRSC. In combination with published spectral information
from TES, THEMIS and OMEGA, 3D mapping was used to deriv
@--------------------------------------------------------------------
Title: HRSC-based Mapping and Internal Architecture of Gale
Crater (Mars)
Authors: Rossi, A. P.; Zegers, T.; Pondrelli, M.; Gwinner, K.;
Hauber, E.; Neukum, G.; Velasco, E.; Stesky, R.;
Fueten, F.; Chicarro, A.; Foing, B.
Bibliographic Code: 2007LPI....38.1553R
Abstract
New observations on the geomorphology and internal geometry of Gale
crater central bulge are presented. We used a new HRSC stereo-derived
DTM in order to better define morphology and layering attitude within
bulge deposits.
@--------------------------------------------------------------------
Title: The Case for Large-Scale Spring Deposits on Mars:
Light-toned Deposits in Crater Bulges, Valles
Marineris and Chaos
Authors: Rossi, A. P.; Neukum, G.; Pondrelli, M.; Zegers, T.;
Mason, P.; Hauber, E.; Ori, G. G.; Fueten, F.;
Oosthoek, J.; Chicarro, A.; Foing, B.
Bibliographic Code: 2007LPI....38.1549R
Abstract
We investigate and propose the possibility of a common origin as spring
deposits for various materials on Mars: light-toned deposits in Valles
Marineris, crater bulges and chaotic terrains.
@--------------------------------------------------------------------
Title: Photometric Characterization of Selected Lunar Sites
by SMART-1 AMIE Data
Authors: Kaydash, V.; Kreslavsky, M.; Shkuratov, Yu.;
Gerasimenko, S.; Pinet, P.; Chevrel, S.;
Josset, J.-L.; Beauvivre, S.; Almeida, M.; Foing, B.
Bibliographic Code: 2007LPI....38.1535K
Abstract
We use images obtained in 2006 by Advanced Moon Micro-Imager Experiment
(AMIE) camera onboard SMART-1 spacecraft to access photometric
properties of selected lunar areas in the context of geological and
structural properties of the regolith.
@--------------------------------------------------------------------
Title: SMART-1 Impact Observation at the
Canada-France-Hawaii Telescope
Authors: Veillet, C.; Foing, B.
Bibliographic Code: 2007LPI....38.1520V
Abstract
This talk will present the current status of the processing of the
sequence of impact images obtained at CFHT, from the analysis of the
impact flash to the geometry of the plume seen spreading over the 90
seconds following the impact.
@--------------------------------------------------------------------
Title: Radio Observations of the Moon at 3.6 cm Before and
After SMART-1 Impact
Authors: Volvach, A. E.; Berezhnoy, A. A.; Foing, B.;
Ehrenfreund, P.; Khavroshkin, O. B.; Volvach, L. N.
Bibliographic Code: 2007LPI....38.1015V
Abstract
Influence of SMART-1 impact on lunar radio flux at 3.6 cm was not
detected. Parameters of SMART-1 impact radio flash are estimated. Upper
limit of the intensity of radio flashes caused by meteoroid impacts is
estimated.
@--------------------------------------------------------------------
Title: The SMART 1 Impact Event: From the Laboratory to the
Moon
Authors: Burchell, M. J.; Robin-Williams, R.; Foing, B. H.
Bibliographic Code: 2007bget.conf...25B
Abstract
@--------------------------------------------------------------------
Title: CFHT Observation of SMART-1 Impact
Authors: Veillet, Christian; Albert, L.; Foing, B.;
Ehrenfreund, P.
Bibliographic Code: 2006DPS....38.5717V
Abstract
Through the use of Director's Discretionary Time on the
Canada-France-Hawaii Telescope on top of Mauna Kea, Hawaii, an attempt
was made at observing the planned impact of the SMART-1 spacecraft. Even
though the instrumentation available on the telescope the evening of the
impact was not the best suited to the observation of such a fugitive
event, a reconnaissance at the impact site the prior evening to tune to
the observing strategy and some luck with weather and timing at impact
time allowed us to obtain a good temporal series (10-s exposure time
images every 15 seconds) of the crash area covering 17mn before the
crash and a full hour after. Observations were made with the wide-field
infrared camera WIRCam through a molecular H2 narrow-band filter. The
flash of the impact itself was captured, allowing us to independently
locate the point of impact with respect to the lunar features seen on
the Earthshine lit lunar landscape. The images taken over the minutes
following the impact provided the first ever observations of an ejecta
cloud in expansion from an impact on the Moon. The last results from the
analysis of the images of the impact itself and the subsequent dust
cloud will be presented at the time of the meeting.
@--------------------------------------------------------------------
Title: The Research and Scientific Support Department of
ESA and CoRoT
Authors: Fridlund, M.; Beaufort, T.; Favata, F.; Foing, B.;
Gimenéz, A.; Gondoin, P.; Johlander, B.; Smit, H.;
Sunter, W.; Appourchaux, T.
Bibliographic Code: 2006ESASP1306..133F
Abstract
@--------------------------------------------------------------------
Title: SMART-1 Impact Campaign: Predictions, Observations,
LCROSS Implications
Authors: Foing, B. H.; Frew, D.; Almeida, A.; Sarkarati, M.;
Volp, J.; Racca, G.; Camino, O.; Schoenmaker, J.;
Schwehm, G.; Josset, J. L.; Beauvivre, S.;
Sodnik, Z.; Cerroni, P.; Barucci, A.; Grande, M.;
Keller, U.; Nathues, A.; Muinonen, K.;
Ehrenfreund, P.; Wood, M.; Vennes, S.; Meech, K.;
Taylor, C.; Hanslmeyer, A.; Vaubaillon, J.;
Khodachenko, M.; Rucker, H.; Leibundgut, B.;
Hainaut, O.; Gondoin, P.; Ortiz, J. L.; Schultz, R.;
Erd, C.; SMART-1 Coordinated Observations Group;
SMART-1 Impact Prediction Group; Smart-1 Outreach;
Amateur Astronomer Coordination
Bibliographic Code: 2006LPICo1327....9F
Abstract
@--------------------------------------------------------------------
Title: SMART-1 Implications for LCROSS: Operations and
Lunar Science Results
Authors: Foing, B. H.; Frew, D.; Almeida, M.; Koschny, D.;
Volp, J.; Josset, J.-L.; Grande, M.; Houvelin, J.;
Keller, H. U.; Nathues, A.; Malkki, A.; Noci, G.;
Kellett, B.; Beauvivre, S.; Heather, D.; Zender, J.;
McMannamon, P.; Camino, O.; Colaprete, T.;
Wooden, D.; Lcross Team
Bibliographic Code: 2006LPICo1327....7F
Abstract
@--------------------------------------------------------------------
Title: Colour Images Of The Moon From Amie On Smart-1: A
Preliminary Analysys Of The Region Of Oppenheimer.
Authors: Cerroni, Priscilla; Besse, S.; De Sanctis, M. C.;
Josset, J.; Beauvivre, S.; Pinet, P.; Chevrel, S.;
Barucci, M. A.; Langevin, Y.; Koshny, D.;
Almeida, M.; Foing, B.; the AMIE Team
Bibliographic Code: 2006DPS....38.5711C
Abstract
The Advanced Moon micro-Imager Experiment (AMIE) is the imaging system
on board the ESA mission to the Moon SMART-1 which is closing towards
its end on September 3rd, 2006. During the time spent in
lunar orbit the AMIE camera provided high resolution CCD images of
selected lunar areas where it performed colour imaging through three
filters at 750, 915 and 960 nm with a maximum resolution of 27 m /pixel
at the perilune of 300 km.
The spectral bands have been selected in order to allow discrimination
between mafic minerals which dominate the mare (revealed by the Fe2+
absorption feature at 950 nm) and the anorthosite rich highland
materials.
Data acquired by AMIE in push-broom modality on November 25th, 2005 for
the lunar region of Oppenheimer centered at 36 S, 194 E have been
preliminarily analysed. The ground resolution for these observations is
of 73 m/px. A new calibration has been applied to the images based on
flat-fielding from in-flight data; for the region considered three
filters images have been co-registered, colour images and band-ratio
images have been produced.
An assessment of the results and a comparison with Clementine data from
the same region is presented. Spectra have been extracted from a region
in the floor of Oppenheimer and on the rim of a crater: a comparison
with spectra from Clementine yields consistent results.
Acknowledgements: P. Cerroni and M.C. De Sanctis acknowledge the support
of ASI grant I/030/05
@--------------------------------------------------------------------
Title: Results from SMART-1 Lunar Mission
Authors: Foing, B. H.
Bibliographic Code: 2006IAUJD..10E...7F
Abstract
SMART-1 is the first ESA mission that reached the Moon. It demonstrated
Solar Electric Primary Propulsion (SEP) and tested new technologies for
spacecraft and instruments. Launched on 27 Sept. 2003, as Ariane-5
auxiliary passenger, SMART-1 has spiralled out towards lunar capture on
15 November 2004, and then towards lunar science orbit reached on 1
March 2005. The mission has been extended and is due to end with an
impact on 2-3 September 2006. This is permitting science but also to
prepare future international lunar exploration, in collaboration with
upcoming missions. We shall present the first year lunar results from
SMART-1's science and technology payload. The 19 kg payload includes a
miniaturized high-resolution camera (AMIE), a near-infrared
point-spectrometer (SIR) for mineralogy investigation, and a very
compact X-ray spectrometer (D-CIXS) for surface elemental composition.
There is also an experiment (KaTE) aimed at demonstrating deep-space
telemetry and telecommand communications in the X and Ka-bands, a
radio-science experiment (RSIS), a deep space optical link (Laser-Link
Experiment), using the ESA Optical Ground station in Tenerife, and the
validation of a system of autonomous navigation (OBAN) based on image
processing. SMART-1 lunar science investigations include studies of the
chemical composition of the Moon, of geophysical processes (volcanism,
tectonics, cratering, erosion, deposition of ices and volatiles) for
comparative planetology, and high resolution studies in preparation for
future steps of lunar exploration. The mission addresses several topics
such as the accretional processes that led to the formation of rocky
planets, and the origin and evolution of the Earth-Moon system.
@--------------------------------------------------------------------
Title: A lunar liquid mirror telescope (LLMT) for
deep-field infrared observations near the lunar pole
Authors: Angel, Roger; Eisenstein, Dan; Sivanandam, Suresh;
Worden, Simon P.; Burge, Jim; Borra, Ermanno;
Gosselin, Clément; Seddiki, Omar; Hickson, Paul;
Ma, Ki Bui; Foing, Bernard; Josset, Jean-Luc;
Thibault, Simon; Van Susante, Paul
Bibliographic Code: 2006SPIE.6265E..54A
Abstract
We have studied the feasibility and scientific potential of a 20 - 100 m
aperture astronomical telescope at the lunar pole, with its primary
mirror made of spinning liquid at less than 100K. Such a telescope,
equipped with imaging and multiplexed spectroscopic instruments for a
deep infrared survey, would be revolutionary in its power to study the
distant universe, including the formation of the first stars and their
assembly into galaxies. The LLMT could be used to follow up discoveries
made with the 6 m James Webb Space Telescope, with more detailed images
and spectroscopic studies, as well as to detect objects 100 times
fainter, such as the first, high-red shift stars in the early universe.
Our preliminary analysis based on SMART-1 AMIE images shows ridges and
crater rims within 0.5° of the North Pole are illuminated for at
least some sun angles during lunar winter. Locations near these points
may prove to be ideal for the LLMT. Lunar dust deposited on the optics
or in a thin atmosphere could be problematic. An in-situ site survey
appears necessary to resolve the dust questions.
@--------------------------------------------------------------------
Title: Analysis and modeling of high temporal resolution
spectroscopic observations of flares on AD Leonis
Authors: Crespo-Chacón, I.; Montes, D.; García-Alvarez, D.;
Fernández-Figueroa, M. J.; López-Santiago, J.;
Foing, B. H.
Bibliographic Code: 2006A&A...452..987C, eprint = astro-ph/0602123
Abstract
We report the results of a high temporal resolution spectroscopic
monitoring of the flare star AD Leo. During 4 nights,
more than 600 spectra were taken in the optical range using the Isaac
Newton Telescope (INT) and the Intermediate Dispersion Spectrograph
(IDS). We observed a large number of short and weak flares occurring
very frequently (flare activity > 0.71 h-1). This is
consistent with the very important role that flares can play in stellar
coronal heating. The detected flares are non white-light flares and,
although most solar flares are of this kind, very few such events have
been observed previously in stars. The behaviour of different
chromospheric lines (Balmer series from Halpha to H{11}, Ca II H &
K, Na I D1 and D2, He I 4026 Å and He I D3) was studied in detail
for a total of 14 flares. We estimated the physical parameters of the
flaring plasma by using a procedure that assumes a simplified slab model
of flares. All the obtained physical parameters are consistent with
previously derived values for stellar flares, and the areas - less than
2.3% of the stellar surface - are comparable with the size inferred for
other solar and stellar flares. We studied the relationships between the
physical parameters and the area, duration, maximum flux and energy
released during the detected flares.
@--------------------------------------------------------------------
Title: The effects of Martian near surface conditions on
the photochemistry of amino acids
Authors: ten Kate, Inge Loes; Garry, James R. C.;
Peeters, Zan; Foing, Bernard; Ehrenfreund, Pascale
Bibliographic Code: 2006P&SS...54..296T
Abstract
In order to understand the complex multi-parameter system of destruction
of organic material on the surface of Mars, step-by-step laboratory
simulations of processes occurring on the surface of Mars are necessary.
This paper describes the measured effects of two parameters, a
CO2 atmosphere and low temperature, on the destruction rate
of amino acids when irradiated with Mars-like ultraviolet light (UV).
The results show that the presence of a 7 mbar CO2 atmosphere
does not affect the destruction rate of glycine, and that cooling the
sample to 210 K (average Mars temperature) lowers the destruction rate
by a factor of 7. The decrease in the destruction rate of glycine by
cooling the sample is thought to be predominantly caused by the slower
reaction kinetics. When these results are scaled to Martian lighting
conditions, cold thin films of glycine are assumed to have half-lives of
250 h under noontime peak illumination. It has been hypothesised that
the absence of detectable native organic material in the Martian
regolith points to the presence of oxidising agents. Some of these
agents might form via the interaction of UV with compounds in the
atmosphere. Water, although a trace component of Mars' atmosphere,
is suggested to be a significant source of oxidising species. However,
gaseous CO2 or adsorbed H2O layers do not
influence the photodestruction of amino acids significantly in the
absence of reactive soil. Other mechanisms such as chemical processes in
the Martian regolith need to be effective for rapid organic destruction.
@--------------------------------------------------------------------
Title: Amino Acid Destruction in the Martian Surface
Environment
Authors: ten Kate, I. L.; Garry, J. R. C.; Peeters, Z.;
Foing, B. H.; Ehrenfreund, P.
Bibliographic Code: 2006LPI....37.2397T
Abstract
In this paper we present the results of experiments, in which thin films
of glycine have been irradiated with UV in a CO2 atmosphere, and cooled
to an average martian surface temperature of 210 K.
@--------------------------------------------------------------------
Title: Mapping of Photometric Anomaly of Martian Surface
with HRSC Data
Authors: Kreslavsky, M. A.; Bondarenko, N. V.; Pinet, P. C.;
Raitala, J.; Foing, B. H.; Neukum, G.;
Mars Express HRSC Co-Investigator Team
Bibliographic Code: 2006LPI....37.2211K
Abstract
We propose a practical method for mapping photometric anomaly of Mars
surface from five panchromatic HRSC channels. The method tolerates
atmospheric effect and calibration errors. We show examples of
interpretation in terms of the surface structure.
@--------------------------------------------------------------------
Title: ESA's SMART-1 Mission: Lunar Science Results After
One Year
Authors: Foing, B. H.; Grande, M.; Huovelin, J.;
Josset, J. L.; Keller, H. U.; Nathues, A.;
Malkki, A.; Noci, G.; Kellett, B.; Beauvivre, S.;
Almeida, M.; Frew, D.; Volp, J.; Heather, D.;
Schwehm, G.; Koschny, D.; Zender, J.; McMannamon, P.;
Camino, O.; Racca, G. D.
Bibliographic Code: 2006LPI....37.1920F
Abstract
We summarise one year of SMART-1 lunar science results with the optical
camera (polar and colour high res imaging), infrared spectrometer
(mineralogy), and X-ray spectrometer (elemental composition). We
describe the plan for operations until end of mission impact in August
2006.
@--------------------------------------------------------------------
Title: SMART-1/AMIE Camera System
Authors: Josset, J.-L.; Beauvivre, S.; Cerroni, P.;
de Sanctis, M. C.; Pinet, P.; Chevrel, S.;
Langevin, Y.; Barucci, M. A.; Plancke, P.;
Koschny, D.; Almeida, M.; Sodnik, Z.; Mancuso, S.;
Hofmann, B. A.; Muinonen, K.; Shevchenko, V.;
Shkuratov, Y.; Ehrenfreund, P.; Foing, B. H.
Bibliographic Code: 2006LPI....37.1847J
Abstract
The Advanced Moon micro-Imager Experiment (AMIE), on board ESA SMART-1,
the first European mission to the Moon (launched on 27th September
2003), is a camera system with scientific, technical and public outreach
oriented objectives.
@--------------------------------------------------------------------
Title: Preliminary Analysis of Colour Information from AMIE
on Smart-1
Authors: Cerroni, P.; de Sanctis, M. C.; Josset, J.-L.;
Beauvivre, S.; Koschny, D.; Pinet, P.; Chevrel, S.;
Langevin, Y.; Barucci, M. A.; Plancke, P.;
Almeida, M.; Hofmann, B. A.; Muinonen, K.;
Shevchenko, V.; Shkuratov, Yu.; Ehrenfreund, P.;
Foing, B. H.
Bibliographic Code: 2006LPI....37.1831C
Abstract
The Advanced Moon micro-Imager Experiment (AMIE) is the imaging system
on board the ESA mission to the Moon SMART-1. We present a preliminary
assessment of push-broom data acquired during the first push-broom
orbital phase of Smart-1 mission.
@--------------------------------------------------------------------
Title: Widespread Periglacial Landforms in Thaumasia
Highland, Mars
Authors: Rossi, A. P.; Chicarro, A. F.; Pacifici, A.;
Pondrelli, M.; Helbert, J.; Benkhoff, J.; Zegers, T.;
Foing, B.; Neukum, G.
Bibliographic Code: 2006LPI....37.1568R
Abstract
Recent glacial and periglacial landforms appear widespread in Thaumasia
Highland. We are mapping them using HRSC data and, locally, MOC NA and
Themis VIS. We started ice stability modeling for these landforms.
@--------------------------------------------------------------------
Title: The next steps in exploring deep space---A cosmic
study by the IAA
Authors: Huntress, W.; Stetson, D.; Farquhar, R.;
Zimmerman, J.; Clark, B.; O'Neil, W.; Bourke, R.;
Foing, B.
Bibliographic Code: 2006AcAau..58..304H
Abstract
This paper presents the results of an IAA cosmic study on the Next Steps
in Exploring Deep Space, the goal of which is to provide a vision for
the scientific exploration of space by humans in the first half of the
21st Century. The study provides a roadmap for a systematic, logical,
and science-driven plan for exploration of the Solar System and
unlocking the mysteries of the Universe---a program that builds
gradually and systematically to establish a permanent presence at each
outpost along the way, and that builds the communications,
transportation and other logistical infrastructure as it proceeds. The
study suggests a set of long-term scientific goals for space exploration
that provide the context for carrying out scientific investigations at
specific destinations in space. An architecture is derived for the space
flight infrastructure required to pursue these science goals at the
specified destinations, including examination of the relevant policy and
public engagement in this enterprise.
@--------------------------------------------------------------------
Title: The Large Magellanic Cloud: diffuse interstellar
bands, atomic lines and the local environmental
conditions
Authors: Cox, N. L. J.; Cordiner, M. A.; Cami, J.;
Foing, B. H.; Sarre, P. J.; Kaper, L.;
Ehrenfreund, P.
Bibliographic Code: 2006A&A...447..991C
Abstract
The Large Magellanic Cloud (LMC) offers a unique laboratory to study the
diffuse interstellar bands (DIBs) under conditions that are profoundly
different from those in the Galaxy. DIB carrier abundances depend on
several environmental factors, in particular the local UV radiation
field. In this paper we present measurements of twelve DIBs in five
lines of sight to early-type stars in the LMC, including the 30
Doradus region. From the high resolution spectra obtained with
VLT/UVES we also derive environmental parameters that characterise the
local interstellar medium (ISM) in the probed LMC clouds. These include
the column density components (including total column density) for the
atomic resonance lines of Na I, Ca II, Ti II, K I. In addition, we
derive the H I column density from 21 cm line profiles, the
total-to-selective visual extinction RV and the gas-to-dust
ratio N(H I)/A_V. Furthermore, from atomic line ratios we derive the
ionisation balance and relative UV field strength in these environments.
We discuss the properties of the LMC ISM in the context of DIB carrier
formation. The behaviour of DIBs in the LMC is compared to that of DIBs
in different local environmental conditions in the Milky Way. A key
result is that in most cases the diffuse band strengths are weak (up to
factor 5) with respect to Galactic lines of sight of comparable
reddening, EB-V. In the line of sight towards Sk -69
223 the 5780 and 5797 Å DIBs are very similar in
strength and profile to those observed towards HD
144217, which is typical of an environment exposed to a strong
UV field. From the velocity analysis we find that DIB carriers (towards
Sk -69 243) are better correlated with the ionised
species like Ca II than with neutrals (like Na I and CO). The most
significant parameter that governs the behaviour of the DIB carrier is
the strength of the UV field.
@--------------------------------------------------------------------
Title: Fullerenes and Related Carbon Compounds in
Interstellar Environments
Authors: Ehrenfreund, P.; Cox, N.; Foing, B.
Bibliographic Code: 2006nfrs.book...53E
Abstract
@--------------------------------------------------------------------
Title: Optimization of plant mineral nutrition under
growth-limiting conditions in a lunar greenhouse
Authors: Zaets, I.; Voznyuk, T.; Kovalchuk, M.; Rogutskyy, I.;
Lukashov, D.; Mytrokhyn, O.; Mashkovska, S.;
Foing, B.; Kozyrovska, N.
Bibliographic Code: 2006KosNT..12f..36Z
Abstract
It may be assumed that the first plants in a lunar base will play a main
role in forming a protosoil of acceptable fertility needed for
purposively growing second generation plants like wheat, rice, tulips,
etc. The residues of the first-generation plants could be composted and
transformed by microorganisms into a soil-like substrate within a loop
of regenerative life support system. The lunar regolith may be used as a
substrate for plant growth at the very beginning of a mission to reduce
its cost. The use of microbial communities for priming plants will allow
one to facilitate adaption to stressful conditions and to support the
plant development under growth limiting conditions. Well-defined
plant-associated bacteria were used for growing three cultivars to
colonize French marigold (Tagetes patula L.) in anorthosite, a substrate
of low bioavailability, analogous to a lunar rock. The consortium was
composed of plant growth promoting rhizobacteria and the bacterium
Paenibacillus sp. IMBG156 which stimulated seed germination, better
plant development, and finally, the flowering of inoculated tagetes. In
contrast, control plants grew poorly in the anorthosite and practically
did not survive until flowering. Analysis of bacterial community
composition showed that all species colonized plant roots, however, the
rate of colonization depended on the allelopatic characteristics of
marigold varieties. Bacteria of consortium were able to liberate some
elements (Ca, Fe, Mn, Si, Ni, Cu, Zn) from substrate anorthosite. Plant
colonization by mixed culture of bacterial strains resulted in the
increase of accumulation of K, Mg, Mn by the plant and in the lowering
of the level of toxic metal accumulation. It was assumed that a
rationally assembled consortium of bacterial strains promoted
germination of marygold seeds and supported the plant development under
growth limiting conditions by means of bioleaching plant essential
nutritional elements and by protecting the plant against
hyperaccumulation of some toxic metals.
@--------------------------------------------------------------------
Title: Other campaign contributions TBD
Authors: Foing, B.
Bibliographic Code: 2006epsc.conf..724F
Abstract
@--------------------------------------------------------------------
Title: Other STWT contributions TBD
Authors: Foing, B.
Bibliographic Code: 2006epsc.conf..721F
Abstract
@--------------------------------------------------------------------
Title: SMART-1 Moon impact on 3 Sept 2006: predictions and
observation campaign
Authors: Foing, B. H.; Ehrenfreund, P.; Koschny, D.; Frew, D.;
SMART-1 Impact Campaign Team
Bibliographic Code: 2006epsc.conf..655F
Abstract
SMART-1 was launched in 2003 and is currently orbiting the Moon on a 5
hours period until impact around 31 August 2006. The impact will take
place in grazing incidence with mass of 285 kg at a velocity of 2 km/s
in a latitude around 37 degree south. A slight thrusting will be
operated in June to fine tune the exact time of contact. At present
possible arrival time scenarios are around 3 Sept 2006, to permit
nearside impact and adequate illumination conditions. We'll describe the
operations until impact. We called the community to make predictions of
impact magnitude, cloud ejecta dynamics, exospheric effects. We also
called the ground based observers to perform coordinated measurements of
the impact. Results from the coordinated multisite campaign will be
discussed.
@--------------------------------------------------------------------
Title: International lunar missions: results and
implications for astrobiologyInternational lunar
missions: results and implications for astrobiology
Authors: Foing, B. H.; Ilewg
Bibliographic Code: 2006epsc.conf..654F
Abstract
Results from recent lunar missions have changed our view of the Moon.
ESA SMART1 was launched in 2003 and is currently orbiting the Moon until
impact in August 2006. Lunar orbiters are readying for launch in 2007
(Japanese SELENE, Indian Chandrayaan-1 orbiter and the Chinese
Chang'E1), as well as US Lunar Reconnaissance Orbiter in 2008. From 2010
a series of soft lander missions to the Moon could emplace a global
robotic presence with precursor life science experiments. The results of
these missions will continue to answer open questions about the origin
of the Earth-Moon system, the early evolution of life, the planetary
environment and habitability. Lunar geoscience studies help to
understand the origin and evolution of our unique Earth-Moon system and
other rocky planets. Lunar or cislunar telescopes on the Moon can detect
and characterize if life exists elsewhere in the universe. We can search
for samples of the early Earth on the Moon. We can use in-situ resources
necessary to support future life and human presence (e.g. water,
oxygen). The Moon will be used for life sciences, astrobiology
laboratories, human bases and biospheres that will play a key role in
the future of life beyond Earth.
@--------------------------------------------------------------------
Title: Highlights of SMART-1 Lunar Science results
Authors: Foing, B. H.; Smart-1 Science;
Technology Working Team
Bibliographic Code: 2006epsc.conf..653F
Abstract
We shall present the highlights of lunar science results from SMART-1
payload, featuring many innovative instruments and advanced technologies
with a total mass of some 19 kg. SMART-1 lunar science investigations
include studies of the chemical composition of the Moon, of geophysical
processes (volcanism, tectonics, cratering, erosion, deposition of ices
and volatiles) for comparative planetology, and high resolution studies
in preparation for future steps of lunar exploration. The mission
addresses several topics such as the accretional processes that led to
the formation of rocky planets, and the origin and evolution of the
Earth-Moon system.
@--------------------------------------------------------------------
Title: Rationale and robotics payload for a lunar polar
lander
Authors: Foing, B.; Hovland, S.; Les3 Lander Study Team
Bibliographic Code: 2006epsc.conf..652F
Abstract
We present the results of a study for a lunar polar lander conducted at
ESA CDF Concurrent Design Facility until December 2005. The goal is to
demonstrate lunar landing, survival and exploration technologies for the
future, geochemical studies of the piles, and search for ice in
permanent shadows. We describe the top objectives, mission analysis,
design and associated lander and rover. We also describe the possible
payload complement in discussion with the community. The robotic payload
includes a nanorover, a regional rover with robotic arm and drilling
capability. The sensors include cameras, spectrometers and analysis
facilities.
@--------------------------------------------------------------------
Title: Rationale and Roadmap for Moon Exploration
Authors: Foing, B. H.; ILEWG Team
Bibliographic Code: 2006epsc.conf..651F
Abstract
We discuss the different rationale for Moon exploration. This starts
with areas of scientific investigations: clues on the formation and
evolution of rocky planets, accretion and bombardment in the inner solar
system, comparative planetology processes (tectonic, volcanic, impact
cratering, volatile delivery), records astrobiology, survival of
organics; past, present and future life. The rationale includes also the
advancement of instrumentation: Remote sensing miniaturised instruments;
Surface geophysical and geochemistry package; Instrument deployment and
robotic arm, nano-rover, sampling, drilling; Sample finder and
collector. There are technologies in robotic and human exploration that
are a drive for the creativity and economical competitivity of our
industries: Mecha-electronics-sensors; Tele control, telepresence,
virtual reality; Regional mobility rover; Autonomy and Navigation;
Artificially intelligent robots, Complex systems, Man-Machine interface
and performances. Moon-Mars Exploration can inspire solutions to global
Earth sustained development: In-Situ Utilisation of resources;
Establishment of permanent robotic infrastructures, Environmental
protection aspects; Life sciences laboratories; Support to human
exploration. We also report on the IAA Cosmic Study on Next Steps In
Exploring Deep Space, and ongoing IAA Cosmic Studies, ILEWG/IMEWG
ongoing activities, and we finally discuss possible roadmaps for robotic
and human exploration, starting with the Moon-Mars missions for the
coming decade, and building effectively on joint technology
developments.
@--------------------------------------------------------------------
Title: Regional mapping and structural analysis of Aram
Chaos area
Authors: Oosthoek, J. H. P.; Zegers, T. E.; Rossi, A. P.;
Martin, P.; Foing, B.; Neukum, G.
Bibliographic Code: 2006epsc.conf..560O
Abstract
Aram Chaos is a typical chaotic terrain within a ˜280 km crater
located 2.5o N and 338.5o E, in the Xanthe and Margaritifer Terrae (XMT)
region. Most large craters in the XMT region, such as the Aram Chaos
crater, formed in the Noachian Period. In the subsequent Hesperian
Period and into the Amazonian Period the XMT region has been dissected
by five of the circum-Chryse outflow channels: Shalbatana, Simud, Tiu,
Ares and Mawrth Valles. We are mapping and analysing the geology of Aram
Chaos using (1) HRSC image data from the ESA Mars Express orbiter, (2)
THEMIS and MOC image data and MOLA elevation data.. The data was
processed and map projected and incorporated in ESRI ArcGIS. HRSC data
is particularly important in this mapping study. The large swath width,
the high resolution, and the sharpness of the images combine both
context and detail in one image. In addition, HRSC anaglyphs were
incorporated in the GIS database. Using red/blue glasses, these provide
direct detailed elevation information, essential to geometry based
geological mapping. Apart from the general mapping the focus of this
study is on (1) investigating the structural and geometric relations of
the chaotic terrain and the surrounding Noachian cratered terrain, and
(2) investigating the light toned deposits in the chaotic terrain and
their relation to the chaotic terrain and outflow channels. 5 major
units were distinguished: Highland terrain, Fractured highland terrain,
Intermediate chaotic terrain, Chaos floor terrain and Light toned
deposits. Inside Aram Chaos a morphologically distinct chaotic terrain
unit was mapped which also shows a distinct fault pattern. The outflow
channels were considered geomorphological units and the channel flow
boundaries and directions are shown as lines in the map. Faults and
fault blocks were mapped. On the Aram Chaos end of the channel
connecting Ares Vallis and Aram Chaos a delta-like feature is located.
@--------------------------------------------------------------------
Title: Analysis of the SMART-1 impact flash as seen from
several observatories in Spain
Authors: Ortiz, J. L.; Llorca, J.; Foing, B. H.; Koschny, D.;
Trigo-Rodriguez, J. M.; Lopez-Moreno, J. J.;
Aceituno, F. J.; Santos-Sanz, P.; Morales, N.;
Moreno, F.
Bibliographic Code: 2006epsc.conf..347O
Abstract
The first results of our scheduled SMART-1 impact observations from
Calar Alto, Sierra Nevada and other observatories in Spain are
presented. The emphasis is made on the determination of the luminous
efficiency of the impact at different wavelength ranges from the optical
to the near infrared.
@--------------------------------------------------------------------
Title: Recent ice-related landforms at high altitude on
Mars (Thaumasia Highland)
Authors: Rossi, A. P.; Helbert, J.; Pacifici, A.;
Pondrelli, M.; Benkhoff, J.; Zegers, T.;
Chicarro, A.; Foing, B.
Bibliographic Code: 2006epsc.conf..212R
Abstract
Pristine and deflated periglacial-like landforms are visible on HRSC
data over Thaumasia Highland, Mars. They include lineated crater/valley
fills, protalus lobes and protalus ramparts. Lineated crater/valley fill
appear to be larger in size and slightly older than protalus lobe-like
landforms in the area, suggesting a decrease in ice-related landform
development with time. The estimated age of the youngest periglacial
landforms is less than a few tens of million years, consistent with what
has been calculated for glacial/periglacial deposits in various other
regions on Mars. In order to assess the likelihood of finding ice rich
deposits within the mapped features we are using the Berlin Mars near
Surface Thermal Model (BMST). Our modeling results are consistent with
the presence of ground ice in some of the areas where we found
periglacial landforms. The most pristine looking rock glaciers mainly
occur on south facing slopes. This is consistent with modeling results
and inferred flow directions.
@--------------------------------------------------------------------
Title: NASA Lunar Exploration Programme
Authors: Foing, B. H.; Ilewg
Bibliographic Code: 2006cosp...36.3727F
Abstract
@--------------------------------------------------------------------
Title: SMART-1 Moon impact around 2-3 Sept 2006:
predictions and observation campaign
Authors: Foing, B. H.; SMART-1 Impact Campaign Team
Bibliographic Code: 2006cosp...36.3723F
Abstract
@--------------------------------------------------------------------
Title: Astrobiology on the Moon
Authors: Foing, B. H.
Bibliographic Code: 2006cosp...36.3722F
Abstract
@--------------------------------------------------------------------
Title: Highlights of SMART-1 Lunar Science results
Authors: Foing, B. H.; SMART-1 Team
Bibliographic Code: 2006cosp...36.3721F
Abstract
@--------------------------------------------------------------------
Title: Highlights of SMART-1 Lunar Mission
Authors: Foing, B. H.; SMART-1 Team
Bibliographic Code: 2006cosp...36.3720F
Abstract
@--------------------------------------------------------------------
Title: ESA Lunar Polar Lander Study
Authors: Foing, B. H.; Hovland, S.;
Lunar Polar Lander Study Team
Bibliographic Code: 2006cosp...36.3719F
Abstract
@--------------------------------------------------------------------
Title: The ORGANICS experiments on BIOPAN V: UV and space
exposure of aromatic compounds
Authors: Ehrenfreund, P.; Ruiterkamp, R.; Peeters, Z.;
Foing, B.; Salama, F.; Martins, Z.
Bibliographic Code: 2006cosp...36.3635E
Abstract
We studied the stability of aromatic compounds in low Earth orbit
environment and describe the scientific results and successful flight of
the ORGANICS experiment on-board the BIOPAN V space exposure facility
This experiment investigated the photo stability of large organic
molecules in near Earth orbit Thin films of selected organic molecules
such as polycyclic aromatic hydrocarbons PAHs and the fullerene C 60
were subjected to the near Earth orbit environment and the samples were
monitored before and after flight PAHs and fullerenes have been proposed
as carriers for a number of astronomical absorption and emission
features and are also identified in meteorites Our experiment on BIOPAN
V was exposed to a total fluence of 602 45 kJ m -2 for photons between
170 and 280 nm The experiment was also intended as a hardware
test-flight for a long-term exposure experiment on the EXPOSE facility
on the International Space Station ISS For the small fluence that was
collected during the BIOPAN V experiment we found little evidence of
photo-destruction The results confirm that PAH molecules are very stable
compounds in space
@--------------------------------------------------------------------
Title: Growing pioneer plants for a lunar base
Authors: Kozyrovska, N. O.; Lutvynenko, T. L.;
Korniichuk, O. S.; Kovalchuk, M. V.; Voznyuk, T. M.;
Kononuchenko, O.; Zaetz, I.; Rogutskyy, I. S.;
Mytrokhyn, O. V.; Mashkovska, S. P.; Foing, B. H.;
Kordyum, V. A.
Bibliographic Code: 2006AdSpR..37...93K
Abstract
A precursory scenario of cultivating the first plants in a lunar
greenhouse was elaborated in frames of a conceptual study to grow plants
for a permanently manned lunar base. A prototype plant growth system
represents an ornamental plant Tagetes patula L. for growing in a lunar
rock anorthosite as a substrate. Microbial community anticipated to be
in use to support a growth and development of the plant in a substrate
of low bioavailability and provide an acceptable growth and blossoming
of T. patula under growth limiting conditions.
@--------------------------------------------------------------------
Title: Science objectives and first results from the
SMART-1/AMIE multicolour micro-camera
Authors: Josset, J.-L.; Beauvivre, S.; Cerroni, P.;
de Sanctis, M. C.; Pinet, P.; Chevrel, S.;
Langevin, Y.; Barucci, M. A.; Plancke, P.;
Koschny, D.; Almeida, M.; Sodnik, Z.; Mancuso, S.;
Hofmann, B. A.; Muinonen, K.; Shevchenko, V.;
Shkuratov, Yu.; Ehrenfreund, P.; Foing, B. H.
Bibliographic Code: 2006AdSpR..37...14J
Abstract
The Advanced Moon micro-Imager Experiment (AMIE), on-board SMART-1, the
first European mission to the Moon, is an imaging system with
scientific, technical and public outreach objectives. The science
objectives are to image the lunar South Pole, permanent shadow areas
(ice deposit), eternal light (crater rims), ancient lunar non-mare
volcanism, local spectrophotometry and physical state of the lunar
surface, and to map high latitudes regions (south) mainly at far side
(South Pole Aitken basin). The technical objectives are to perform a
Laserlink experiment (detection of laser beam emitted by ESA/Tenerife
ground station), flight demonstration of new technologies and on-board
autonomy navigation. The public outreach and educational objectives are
to promote planetary exploration and space. We present here the first
results obtained during the cruise phase.
@--------------------------------------------------------------------
Title: SMART-1 mission to the Moon: Status, first results
and goals
Authors: Foing, B. H.; Racca, G. D.; Marini, A.; Evrard, E.;
Stagnaro, L.; Almeida, M.; Koschny, D.; Frew, D.;
Zender, J.; Heather, J.; Grande, M.; Huovelin, J.;
Keller, H. U.; Nathues, A.; Josset, J. L.;
Malkki, A.; Schmidt, W.; Noci, G.; Birkl, R.;
Iess, L.; Sodnik, Z.; McManamon, P.
Bibliographic Code: 2006AdSpR..37....6F
Abstract
We present the first results from SMART-1's science and technology
payload. SMART-1 is Europe's first lunar mission and will provide
some significant advances to many issues currently active in lunar
science, such as our understanding of lunar origin and evolution. The
mission also contributes a step in developing an international program
of lunar exploration. The spacecraft was launched on 27 September 2003
on an Ariane 5, as an auxiliary passenger to Geostationary Transfer
Orbit (GTO), performed a 14-month long cruise using the tiny thrust of
electric propulsion alone, reached lunar capture in November 2004, and
lunar science orbit in March 2005. SMART-1 carries seven hardware
experiments (performing 10 investigations, including three remote
sensing instruments, used during the cruise, the mission's nominal
six months and one year extension in lunar science orbit). The remote
sensing instruments will contribute to key planetary scientific
questions related to theories of lunar origin and evolution, the global
and local crustal composition, the search for cold traps at the lunar
poles and the mapping of potential lunar resources. Display Omitted
@--------------------------------------------------------------------
Title: Prelude to The Moon: Science, Technology,
Utilization and Human Exploration
Authors: Ehrenfreund, P.; Foing, B. H.
Bibliographic Code: 2006AdSpR..37....5E
Abstract
@--------------------------------------------------------------------
Title: Planetary science: Are there active glaciers on
Mars? (Reply)
Authors: Head, J. W.; Neukum, G.; Jaumann, R.; Hiesinger, H.;
Hauber, E.; Carr, M.; Masson, P.; Foing, B.;
Hoffmann, H.; Kreslavsky, M.; Werner, S.;
Milkovich, S.; van Gasselt, S.;
The HRSC Co-Investigator Team,
Bibliographic Code: 2005Natur.438E..10H
Abstract
Gillespie et al. concur with our interpretation that certain lobate
equatorial and mid-latitude features on Mars are due to debris-covered
glaciers formed largely during past periods of increased spin-axis
obliquity, when climate regimes favoured snow and ice accumulation and
glacial flow. They suggest that the `hourglass' deposit, dated at more
than 40 Myr old, could be active today owing to an additional mechanism
that supports ``local augmentation of accumulation from snowfall''
without climate change on Mars. This mechanism requires the present, or
very recent, release of groundwater to the surface to form aufeis
(groundwater-fed `glaciers') where the groundwater is generated by
dewatering of hydrous compounds or melting by magmatic or
impact-generated heat. We assess whether this suggestion applies to the
deposits in question - it was previously proposed for much older
deposits in other areas of Mars. We make particular reference to the key
relationships in the accumulation zones.
@--------------------------------------------------------------------
Title: SMART-1 after lunar capture: First results and
perspectives
Authors: Foing, B. H.; Racca, G. D.; Marini, A.; Evrard, E.;
Stagnaro, L.; Almeida, M.; Koschny, D.; Frew, D.;
Zender, J.; Heather, D.; Grande, M.; Huovelin, J.;
Keller, H. U.; Nathues, A.; Josset, J. L.;
Malkki, A.; Schmidt, W.; Noci, G.; Birkl, R.;
Iess, L.; Sodnik, Z.; McManamon, P.
Bibliographic Code: 2005JESS..114..689F
Abstract
@--------------------------------------------------------------------
Title: The life of stars and their planets
Authors: Catala, C.; Aerts, C.; Aigrain, S.; Antonello, E.;
Appourchaux, T.; Auvergne, M.; Baglin, A.; Barge, P.;
Barstow, M. A.; Baudin, F.; Boumier, P.;
Collier Cameron, A.; Christensen-Dalsgaard, J.;
Cutispoto, G.; Deeg, H.; Deleuil, M.; Desidera, S.;
Donati, J.-F.; Favata, F.; Foing, B. H.;
Gameiro, J. F.; Garcia, R.; Garrido, F.; Horne, K.;
Lanza, A. F.; Lanzafame, A. C.;
Lecavelier Des Etangs, A.; Léger, A.; Mas-Hesse, M.;
Messina, S.; Micela, G.; Michel, E.;
Monteiro, M. J. P. F. G.; Mosser, B.; Noels, A.;
Pagano, I.; Piotto, G.; Poretti, E.; Rauer, H.;
Roca-Cortes, T.; Rodono, M.; Rouan, D.; Roxburgh, I.;
Schneider, J.; Strassmeier, K.; Turck-Chièze, S.;
Vauclair, S.; Vidal-Madjar, A.; Weiss, W. W.;
Wheatley, P.
Bibliographic Code: 2005ESASP.588...99C
Abstract
We lack a reliable scenario for the formation and evolution of stars and
their
planetary systems, involving key factors such as magnetic fields and
turbulence. We present the case for a mission concept that will clarify
these
problems and give us a global view of the evolution of combined star and
planetary systems. This will be achieved by simultaneously addressing
the
search for planetary transits in front of a large number of stars,
including
many nearby stars, the study of their internal structure and evolution
via
asteroseismology, and that of their magnetic activity, via UV
monitoring.
@--------------------------------------------------------------------
Title: SMART-1 Mission: First Lunar Results
Authors: Foing, B. H.
Bibliographic Code: 2005AGUFM.P51A0892F
Abstract
The SMART-1 mission arrived in lunar science orbit in March 2005. We'll
present results obtained during the nominal science phase of the
mission, using the AMIE camera for geology context, SIR infrared
spectrometer for mineralogy distrbution and the D-CIXs X-ray
spectrometer for elemental mapping. SMART-1 contributes to the themes of
geophysics(volcanism, cratering, tectonics) and geochemistry constraints
on Moon formation and evolution. It is also used for monitoring
illumination, mapping resources, and preparation of future international
lunar missions. We'll describe also the planning for the mission
extension from October 2005 to August 2006, and the involvement of the
science community.
@--------------------------------------------------------------------
Title: From Crater to Graph: Manual and Automated Crater
Counting Techniques
Authors: Plesko, C. S.; Werner, S. C.; Brumby, S. P.;
Foing, B. H.; Asphaug, E.; Neukum, G.; Team, H.;
Team, I.
Bibliographic Code: 2005AGUFM.P23A0185P
Abstract
Impact craters are some of the most abundant, and most interesting
features on Mars. They hold a wealth of information about Martian
geology, providing clues to the relative age, local composition and
erosional history of the surface. A great deal of effort has been
expended to count and understand the nature of planetary crater
populations (Hartman and Neukum, 2001). Highly trained experts have
developed personal methods for conducting manual crater surveys. In
addition, several efforts are underway to automate this process in
order to keep up with the rapid increase in planetary surface image
data. These efforts make use of a variety of methods, including the
direct application of traditional image processing algorithms such as
the Hough transform, and recent developments in genetic programming, an
artificial intelligence-based technique, in which manual crater surveys
are used as examples to `grow' or `evolve' crater counting algorithms.
(Plesko, C. S. et al., LPSC 2005, Kim, J. R. et al., LPSC 2001,
Michael, G. G. P&SS 2003, Earl, J. et al, LPSC 2005) In this study
we examine automated crater counting techniques, and compare them with
traditional manual techniques on MOC imagery, and demonstrate
capabilities for the analysis of multi-spectral and HRSC Digital Terrain
Model data as well. Techniques are compared and discussed to define and
develop a robust automated crater detection strategy.
@--------------------------------------------------------------------
Title: The advanced Moon micro-imager experiment (AMIE) on
SMART-1: Scientific goals and expected results
Authors: Pinet, P.; Cerroni, P.; Josset, J.-L.; Beauvivre, S.;
Chevrel, S.; Muinonen, K.; Langevin, Y.;
Barucci, M. A.; de Sanctis, M. C.; Shkuratov, Yu.;
Shevchenko, V.; Plancke, P.; Hofmann, B. A.;
Josset, M.; Ehrenfreund, P.; Sodnik, Z.; Koschny, D.;
Almeida, M.; Foing, B.
Bibliographic Code: 2005P&SS...53.1309P
Abstract
The advanced Moon micro-imager experiment (AMIE) is the imaging system
on board ESA mission to the Moon SMART-1; it makes use of a miniaturised
detector and micro-processor electronics developed by SPACE X in the
frame of the ESA technical programme. The AMIE micro-imager will provide
high resolution CCD images of selected lunar areas and it will perform
colour imaging through three filters at 750, 915 and 960 nm with a
maximum resolution of 46 m/pixel at the perilune of 500 km. Specific
scientific objectives will include (1) imaging of high latitude regions
in the southern hemisphere, in particular the South Pole Aitken basin
(SPA) and the permanently shadowed regions close to the South Pole, (2)
determination of the photometric properties of the lunar surface from
observations at different phase angles (physical properties of the
regolith), (3) multi-band imaging for constraining the chemical and
mineral composition of the surface, (4) detection and characterisation
of lunar non-mare volcanic units, (5) study of lithological variations
from impact craters and implications for crustal heterogeneity. The AMIE
micro-imager will also support a Laser-link experiment to Earth, an On
Board Autonomous Navigation investigation and a Lunar libration
experiment coordinated with radio science measurements.
@--------------------------------------------------------------------
Title: Amino acid photostability on the Martian surface
Authors: ten Kate, I. L.; Garry, J. R. C.; Peeters, Z.;
Quinn, R.; Foing, B.; Ehrenfreund, P.
Bibliographic Code: 2005M&PS...40.1185T
Abstract
@--------------------------------------------------------------------
Title: SMART-1 Mission Overview: Lunar Results and
Perspectives
Authors: Foing, B. H.; SMART-1 Team
Bibliographic Code: 2005DPS....37.4802F
Abstract
SMART-1 is the first ESA mission that reached the Moon. It is the first
of Small Missions for Advanced Research and Technology as part of ESA
science programme Cosmic Vision. Its objective is to demonstrate Solar
Electric Primary Propulsion (SEP) for future Cornerstones (such as
Bepi-Colombo) and to test new technologies for spacecraft and
instruments. The spacecraft was launched on 27 Sept. 2003, as Ariane-5
auxiliary passenger, left the inner radiation belt, and spiralled out
towards lunar capture on 15 November 2004, and then towards lunar
science orbit reached on 1 March 2005. The mission has been extended
until August 2006. This will permit science but also to prepare future
international lunar exploration. We shall present an overiew of the
mission, and of the first lunar results from SMART-1's science and
technology payload, featuring many innovative instruments and advanced
technologies with a total mass of some 19 kg. Besides navigation to the
Moon, the technology demonstration included an experiment (KaTE) for
deep-space communications in the X and Ka-bands, a radio-science
experiment (RSIS), a deep space optical link (Laser-Link Experiment),
using the ESA Optical Ground station in Tenerife, and the validation of
a system of autonomous navigation (OBAN). The payload includes a
miniaturized high-resolution camera (AMIE) for lunar surface imaging, a
near-infrared point-spectrometer (SIR) for lunar mineralogy
investigation, and a very compact X-ray spectrometer (D-CIXS) measuring
fluorescence spectroscopy and imagery of the Moon's surface elemental
composition. SMART-1 lunar science investigations include studies of the
chemical composition of the Moon, of geophysical processes (volcanism,
tectonics, cratering, erosion, deposition of ices and volatiles) for
comparative planetology, and high resolution studies in preparation for
future steps of lunar exploration. The mission could address several
topics such as the accretional processes that led to the formation of
rocky planets, and the origin and evolution of the Earth-Moon system.
@--------------------------------------------------------------------
Title: SMART-1: Development and lessons learnt
Authors: Rathsman, Peter; Kugelberg, Joakim; Bodin, Per;
Racca, Giuseppe D.; Foing, Bernard; Stagnaro, Luca
Bibliographic Code: 2005AcAau..57..455R
Abstract
SMART-1 is the first of the small missions for advanced research and
technology as part of ESA's science programme ``Cosmic
vision''. It was successfully launched on September 27, 2003 and is
presently traveling towards its destination, the Moon. The main
objective of the mission, to demonstrate solar electric primary
propulsion for future Cornerstones (such as Bepi-Colombo), has already
been achieved. At the time of writing the electric propulsion system has
been working already for more than 3400 h and has provided a Delta-V to
the spacecraft of more than 2500 m/s. The other technology objectives
are also being fulfilled by the verification of the proper functioning
of such on-board experiments like the X-Ka band transponder, the X-ray
spectrometer, the near IR spectrometer, the laser link, etc. The
scientific objectives are related to lunar science and will be fulfilled
once the spacecraft enters its operational lunar orbit, currently
expected for January 2005. SMART-1 lunar science investigations will
include studies of the chemical composition of the Moon, of geophysical
processes, environment and high-resolution studies in preparation for
future steps of lunar exploration. SMART-1 has been an innovative
mission in many aspects and we are now drawing some preliminary
conclusions about the lessons to be learnt. The paper describes the
spacecraft and the technology elements with particular emphasis to the
technology nature of the mission. The on-board avionics employs many
novel designs for spacecraft, including a serial CAN bus for data
communication, autonomous star trackers and extensive use of auto-code
generation for implementing the attitude control system and the failure,
detection, isolation and recovery (FDIR). Finally, the orbital operation
phase currently ongoing, including the routine electric propulsion
operations and the instrument commissioning, is providing a wealth of
data and lesson-learnt useful for future autonomous planetary missions.
@--------------------------------------------------------------------
Title: Diffuse interstellar bands of unprecedented strength
in the line of sight towards high-mass X-ray binary
4U 1907+09
Authors: Cox, N. L. J.; Kaper, L.; Foing, B. H.;
Ehrenfreund, P.
Bibliographic Code: 2005A&A...438..187C
Abstract
High-resolution VLT/UVES spectra of the strongly reddened O supergiant
companion to the X-ray pulsar 4U 1907+09 provide a
unique opportunity to study the nature of the diffuse interstellar bands
(DIBs) at unprecedented strength. We detect about 180 known DIBs, of
which about 25 were listed as tentative and are now confirmed. A dozen
new DIB candidates longwards of 6900 Å are identified. We show
that the observed 5797 Å DIB strength is in line with the Galactic
correlation with reddening, whereas the 5780 Å DIB strength is
relatively weak. This indicates the contribution of denser regions,
where the UV penetration is reduced. The presence of dense cloud cores
is supported by the detection of C2 rotational transitions. Members of
one DIB family (5797, 6379 Å and 6196, 6613 Å) behave
coherently, although one can make a distinction between the two
correlated pairs. The broadened profiles of narrow DIBs are shown to be
consistent with the premise that each of the main clouds in the line of
sight discerned in the interstellar K I profile is contributing
proportionally to the DIB profile. We complement and extend the relation
of DIB strength with reddening {E}(B-V), as well as with
neutral hydrogen column density N(H I), respectively, using strongly
reddened sightlines towards another four distant HMXBs. The 5780 Å
DIB, and tentatively also the 5797 and 6613 Å DIBs, are better
correlated to the gas tracer H I than to the dust tracer
{E}(B-V). The resulting relationship can be applied to any
line of sight to obtain an estimate of the H I column density. In the
search for the nature of the DIB carrier, this strongly reddened line of
sight is a complementary addition to single cloud line of sight studies.
@--------------------------------------------------------------------
Title: Fluid lava flows in Gusev crater, Mars
Authors: Greeley, Ronald; Foing, Bernard H.;
McSween, Harry Y.; Neukum, Gerhard; Pinet, Patrick;
van Kan, Mirjam; Werner, Stephanie C.;
Williams, David A.; Zegers, Tanja E.
Bibliographic Code: 2005JGRE..11005008G
Abstract
Rocks on the floor of Gusev crater are basaltic in composition, as
determined from measurements by the Mars Exploration Rover, Spirit. On
the basis of compositional data, models of the basaltic lavas at the
time of their emplacement suggest viscosities of 2.3 to 50 Pa. s
(dependent on the number of phenocrysts and vesicles that were present),
which would be more fluid than terrestrial tholeiitic lavas and
comparable to mare lavas on the Moon or Archean high-Mg basalts on
Earth. Morphological data and crater counts derived from the High
Resolution Stereo Camera on Mars Express and other orbiters suggest that
the lavas flooded Gusev crater at about 3.65 b.y. and postdate older
floor materials, such as putative sediments emplaced by Ma'adim Vallis.
@--------------------------------------------------------------------
Title: Evidence from the Mars Express High Resolution
Stereo Camera for a frozen sea close to Mars'
equator
Authors: Murray, John B.; Muller, Jan-Peter; Neukum, Gerhard;
Werner, Stephanie C.; van Gasselt, Stephan;
Hauber, Ernst; Markiewicz, Wojciech J.;
Head, James W.; Foing, Bernard H.; Page, David;
Mitchell, Karl L.; Portyankina, Ganna;
The HRSC Co-Investigator Team
Bibliographic Code: 2005Natur.434..352M
Abstract
It is thought that the Cerberus Fossae fissures on Mars were the source
of both lava and water floods two to ten million years ago. Evidence for
the resulting lava plains has been identified in eastern Elysium, but
seas and lakes from these fissures and previous water flooding events
were presumed to have evaporated and sublimed away. Here we present High
Resolution Stereo Camera images from the European Space Agency Mars
Express spacecraft that indicate that such lakes may still exist. We
infer that the evidence is consistent with a frozen body of water, with
surface pack-ice, around 5° north latitude and 150° east
longitude in southern Elysium. The frozen lake measures about 800
× 900km in lateral extent and may be up to 45metres deep-similar
in size and depth to the North Sea. From crater counts, we determined
its age to be 5 +/- 2 million years old. If our interpretation is
confirmed, this is a place that might preserve evidence of primitive
life, if it has ever developed on Mars.
@--------------------------------------------------------------------
Title: Tropical to mid-latitude snow and ice accumulation,
flow and glaciation on Mars
Authors: Head, J. W.; Neukum, G.; Jaumann, R.; Hiesinger, H.;
Hauber, E.; Carr, M.; Masson, P.; Foing, B.;
Hoffmann, H.; Kreslavsky, M.; Werner, S.;
Milkovich, S.; van Gasselt, S.;
HRSC Co-Investigator Team
Bibliographic Code: 2005Natur.434..346H
Abstract
Images from the Mars Express HRSC (High-Resolution Stereo Camera) of
debris aprons at the base of massifs in eastern Hellas reveal numerous
concentrically ridged lobate and pitted features and related evidence of
extremely ice-rich glacier-like viscous flow and sublimation. Together
with new evidence for recent ice-rich rock glaciers at the base of the
Olympus Mons scarp superposed on larger Late Amazonian debris-covered
piedmont glaciers, we interpret these deposits as evidence for
geologically recent and recurring glacial activity in tropical and
mid-latitude regions of Mars during periods of increased spin-axis
obliquity when polar ice was mobilized and redeposited in
microenvironments at lower latitudes. The data indicate that abundant
residual ice probably remains in these deposits and that these records
of geologically recent climate changes are accessible to future
automated and human surface exploration.
@--------------------------------------------------------------------
Title: ESA's SMART-1 Mission at the Moon: First Results,
Status and Next Steps
Authors: Foing, B. H.; Racca, G. D.; Grande, M.; Huovelin, J.;
Josset, J. L.; Keller, H. U.; Nathues, A.;
Malkki, A.; Heather, D.; Koschny, D.; Almeida, M.;
Frew, D.; Lumb, R.; Volp, J.; Zender, J.
Bibliographic Code: 2005LPI....36.2404F
Abstract
ESA's SMART-1 is at the Moon! Launched by Ariane-5 in Sept. 2003, it
used primary solar electric propulsion to reach lunar capture on 17
November 2004, and to spiral down to lunar science orbit. First data and
results from the cruise approach and lunar commissioning will be
presented.
@--------------------------------------------------------------------
Title: Fluid Lava Flows in Gusev Crater, Mars
Authors: Greeley, R.; Williams, D. A.; Neukum, G.;
Werner, S. C.; Zegers, T. E.; Foing, B. H.;
van Kan, M.; Lanagan, P. D.; Pinet, P. C.;
The Mars Express HRSC Team
Bibliographic Code: 2005LPI....36.2094G
Abstract
Basaltic rocks in Gusev are modeled to have viscosities of 2.3 to 50
Pa•s at the time of eruption and thus were emplaced as very fluid
flood lavas, consistent with the morphologies seen in orbiter data, at
3.65 by based on crater counts.
@--------------------------------------------------------------------
Title: Evidence for Snow and Ice Accumulation Aiding Debris
Flow and Glacial Flow at Mid- to Low-Latitudes on
Mars
Authors: Hiesinger, H.; Head, J. W., III; Neukum, G.;
Jaumann, R.; Hauber, E.; Carr, M. H.; Masson, Ph.;
Foing, B. H.
Bibliographic Code: 2005LPI....36.1988H
Abstract
HRSC image data show debris aprons suggesting extremely ice-rich
glacier-like viscous flow and sublimation, and ice-rich debris-covered
glaciers suggesting geologically recurring glacial activity in low- and
mid-latitude regions.
@--------------------------------------------------------------------
Title: Evolutionary History of Gusev -- The MER Landing
Site -- Seen by MEX-HRSC
Authors: Werner, S. C.; Ivanov, B. A.; Neukum, G.;
van Kan, M.; Zegers, T. E.; Foing, B. H.;
Greeley, R.; Williams, D. A.;
The HRSC Co-Investigator Team
Bibliographic Code: 2005LPI....36.1777W
Abstract
The evolutionary history of Gusev and its vicinity is discussed.
Comparing Gusev--sized impact craters the level of infill of Gusev is
about 1 -- 1.5 km more than for others, possibly due to the contribution
of fluvial activity of Ma'adim Vallis.
@--------------------------------------------------------------------
Title: Evidence from HRSC Mars Express for a Frozen Sea
Close to Mars' Equator
Authors: Murray, J. B.; Muller, J.-P.; Neukum, G.;
Werner, S. C.; Hauber, E.; Markiewicz, W. J.;
Head, J. W., III; Foing, B. H.; Page, D.;
Mitchell, K. L.; Portyankina, G.;
The HRSC Investigator Team
Bibliographic Code: 2005LPI....36.1741M
Abstract
We present evidence for a presently-existing frozen sea, with surface
pack-ice, at 5° N, 150° E, age c. 5 million years. It measures
c. 800 x 900 km and averages c. 45 m deep. It has probably been
protected from complete sublimation by ash and a sublimation lag of
exposed sediment.
@--------------------------------------------------------------------
Title: Photometric and Compositional Surface Properties of
the Gusev Crater Region, Mars, as Derived from
Multi-Angle, Multi-Spectral Investigation of Mars
Express HRSC Data
Authors: Martin, P. D.; Cord, A.; Foing, B. H.; Zegers, T. E.;
van Kan, M.; Pinet, P. C.; Daydou, Y.; Hoffmann, H.;
Hauber, E.; Jaumann, R.; Neukum, G.;
The HRSC Co-Investigator Team
Bibliographic Code: 2005LPI....36.1687M
Abstract
The focus of this investigation is to use the potential of the HRSC
multi-angular and multi-spectral data sets for identifying photometric,
color and compositional units and their heterogeneity.
@--------------------------------------------------------------------
Title: Mountainous Units in the Martian Gusev Highland
Region: Volcanic, Tectonic, or Impact Related?
Authors: Zegers, T. E.; van Kan, M.; Foing, B. H.;
Pischel, R.; Gwinner, K.; Scholten, F.;
Werner, S. C.; Neukum, G.;
The HRSC Co-Investigator Team
Bibliographic Code: 2005LPI....36.1651Z
Abstract
Geological mapping and structural analysis of the highland region of
Gusev crater was carried out, combining THEMIS and HRSC image data and
HRSC digital terrain models (DTM), based on HRSC stereo capabilities.
@--------------------------------------------------------------------
Title: Diurnal Variability in Martian Atmospheric Water
Vapour: Near Surface Ice Out of Equilibrium as a
Source
Authors: Boettger, H. M.; Foing, B. H.; Read, P. L.;
Lewis, S. R.
Bibliographic Code: 2005LPI....36.1647B
Abstract
We attempt to reconcile model and observationsal data from GRS and
atmospheric probes, in reference to the diurnal behaviour of atmospheric
water vapour.
@--------------------------------------------------------------------
Title: Macroscopic Texture of the Martian Surface:
Application of a Filtering Method Using Mars Express
HRSC Data
Authors: Cord, A.; Martin, P.; Foing, B. H.; Jaumann, R.;
Hauber, E.; Hoffman, H.; Neukum, G.;
The HRSC Co-Investigator Team
Bibliographic Code: 2005LPI....36.1615C
Abstract
We quantify the texture of Martian surface at the scale of a few pixels
using images from HRSC (Mars Express). This can be linked with the
relative thickness of dust deposit and then with some geological and
geomorphological properties of the surface.
@--------------------------------------------------------------------
Title: Attitude Determination of Geological Layers Using
HRSC Data and Orion Software
Authors: Fueten, F.; Stesky, R.; MacKinnon, P.; Zegers, T. E.;
Hauber, E.; Foing, B. H.; Pischel, R.; Gwinner, K.;
Scholten, F.; Neukem, G.;
The HRSC Co-Investigator Team
Bibliographic Code: 2005LPI....36.1498F
Abstract
Attitude of ILD layering in Valles Marineris, Mars, is measured using
HRSC data and Orion software.
@--------------------------------------------------------------------
Title: PAH charge state distribution and DIB carriers:
Implications from the line of sight toward HD 147889
Authors: Ruiterkamp, R.; Cox, N. L. J.; Spaans, M.; Kaper, L.;
Foing, B. H.; Salama, F.; Ehrenfreund, P.
Bibliographic Code: 2005A&A...432..515R
Abstract
We have computed physical parameters such as density, degree of
ionization and temperature, constrained by a large observational data
set on atomic and molecular species, for the line of sight toward the
single cloud HD 147889. Diffuse interstellar bands
(DIBs) produced along this line of sight are well documented and can be
used to test the PAH hypothesis. To this effect, the charge state
fractions of different polycyclic aromatic hydrocarbons (PAHs) are
calculated in HD 147889 as a function of depth for
the derived density, electron abundance and temperature profile. As
input for the construction of these charge state distributions, the
microscopic properties of the PAHs, e.g., ionization potential and
electron affinity, are determined for a series of symmetry groups. The
combination of a physical model for the chemical and thermal balance of
the gas toward HD 147889 with a detailed treatment of
the PAH charge state distribution, and laboratory and theoretical data
on specific PAHs, allow us to compute electronic spectra of gas phase
PAH molecules and to draw conclusions about the required properties of
PAHs as DIB carriers. We find the following. 1) The variation of the
total charge state distribution of each specific class (series) of PAH
in the translucent cloud toward HD 147889 (and also
of course for any other diffuse/translucent cloud) depends strongly on
the molecular symmetry and size (number of pi electrons). This is due
to the strong effects of these parameters on the ionization potential of
a PAH. 2) Different wavelength regions in the DIB spectrum are populated
preferentially by different PAH charge states depending on the
underlying PAH size distribution. 3) The PAH size distribution for
HD 147889 is constrained by the observed DIB spectrum
to be Gaussian with a mean of 50 carbon atoms. 4) For the given PAH size
distribution it is possible to constrain the total small catacondensed
PAH column density along the line of sight to HD
147889 to 2.4×1014 cm-2 by
comparing the total observed UV extinction to the strong UV absorptions
of neutral PAHs in the 2000-3000 Å region. 5) Catacondensed PAHs
with sizes above some 40 C-atoms are expected to show strong DIBS
longward of 10 000 Å. Large condensed PAHs in the series, pyrene,
coronene, ovalene, .... , on the other hand, mainly absorb between 4000
and 10 000 Å but extrapolation to even larger pericondensed PAHs
in this series also shows strong absorptions longward of 10 000 Å.
6) Only the weak DIBs in HD 147889 could be
reproduced by a mix of small catacondensed PAHs (<50 C atoms) while
for large pericondensed PAHs (50 < C atoms < 100) the intermediate
DIBs are well reproduced. Small catacondensed PAHs cannot contribute
more than 50% of the total observed equivalent width toward HD
147889. Strong DIBs can only be reproduced by addition of very
specific PAH molecules or homologue series to the sample set (i.e., a
small number of PAHs with high oscillator strength or a large number of
PAHs with a low oscillator strength). An outline is provided for a more
general application of this method to other lines of sight, which can be
used as a pipeline to compute the spectroscopic response of a PAH or
group of PAHs in a physical environment constrained by independent
(non-DIB) observations.
Based on observations made at the European Southern Observatory,
Paranal, Chile (ESO programs 67.C-0281 and 64.H-0224). Appendices A-C
are only available in electronic form at http://www.edpsciences.org
@--------------------------------------------------------------------
Title: Magellanic Diffuse Interstellar Bands and Carbon
Chemistry
Authors: Ehrenfreund, P.; Cox, N.; Cami, J.; Foing, B. H.;
Kaper, L.; D'Hendecourt, L.; Maier, J. P.;
Salama, F.; Sarre, P.; Snow, T.; Sonnentrucker, P.
Bibliographic Code: 2005HiA....13..864E
Abstract
With the Ultraviolet Visual Echelle Spectrograph mounted at the Very
Large Telescope we have observed at unprecedented spectral resolution
the absorption spectrum toward reddened stars in the Magellanic Clouds
over the wavelength range of 3500-10500 Å. This range covers the
strong transitions associated with neutral and charged large carbon
molecules of varying sizes and structures. We report the first detection
of diffuse interstellar bands (DIBs) at 5780 and 5797 Å in the
Small Magellanic Cloud and the variation of the 6284 Å DIB toward
several targets in the Large Magellanic Cloud. The variation of DIBs in
the Magellanic Clouds compared with Galactic targets may be governed by
a combination of the different chemical processes prevailing in
low-metallicity regions and the local environmental conditions. The
analysis of high-resolution absorption spectra allows us to reveal the
global effects in the chemistry and recycling of cosmic dust in the
Magellanic clouds which are relevant for the chemical pathways forming
large organic molecules in external galaxies.
@--------------------------------------------------------------------
Title: Extra-Galactic Diffuse Interstellar Bands
Authors: Cox, N.; Ehrenfreund, Pascale; Kaper, Lex;
Spaans, Marco; Foing, Bernard
Bibliographic Code: 2005IAUS..235P.267C
Abstract
Diffuse Interstellar Bands (DIBs) have been observed ubiquitously along
many sight-lines probing the interstellar medium of the Milky Way.
Despite extensive efforts, their carrier(s) have not yet been
identified, although they are very likely of a carbonaceous nature and
reside in the gas phase. Possible candidates include, but are not
limited to, polycyclic aromatic hydro- carbons (PAHs), fullerenes and
carbon chains. To advance our understanding of DIB behaviour and thus
DIB carrier properties we need to study environments inherently
different from those observed in the Milky Way. Only recent advances in
instrumentation and telescope capabilities are providing us with new
exciting possibilities for extra-galactic DIB research. We present here
a selection of our recent observational results for (extra)-galactic
DIBs in the Local Group and beyond. In particular, DIBs in the
Magellanic Clouds and in the spiral galaxy NGC1448. These first results
show surprising similarities between certain DIB profiles as well as
differences in DIB behaviour. Understanding diffuse cloud chemistry, in
particular with respect to complex (carbonaceous) molecules, is crucial
to any DIB carrier identification. In this respect, external galaxies
offer a unique window as they exhibit local interstellar conditions
(such as metallicity, UV-field and gas-to-dust ratio) very different
from those observed in the Milky Way. We discuss briefly the effect of
metallicity and the gas-to-dust ratio on the physi-chemical properties
of diffuse clouds and the subsequent effects on the PAH charge state
distribution and the DIB carriers.
@--------------------------------------------------------------------
Title: Wind Patterns at the Mars Exploration Rover (MER)
Sites Inferred from Mars Express HRSC and MER Images
Authors: Greeley, R.; Thompson, S.; Whelley, P.; Neukum, G.;
Squyres, S.; Sullivan, R. J.; Rafkin, S. C.;
Michaels, T.; Golombek, M. P.; Arvidson, R.;
Foing, B. H.; Richter, L.; Rongxing, L.; Pinet, P.;
HRSC Science Team,.; Athena Science Team,.
Bibliographic Code: 2004AGUFM.P21B..05G
Abstract
Various wind-related features exist at the Spirit (Gusev) and
Opportunity (Sinus Meridiani) sites, including those seen from the
surface (e.g., ripples, "wind tails" associated with rocks, and
ventifacts), and from orbit (e.g., linear low-albedo patterns, some of
which change with time). The orientations of these features suggest that
formative winds at the Spirit site are from the northwest, consistent
with predictions of prevailing winds from the Mars Regional Atmospheric
Modeling System (MRAMS). Most of the aeolian features seen from orbit at
the Spirit site are dark tracks thought to represent the passage of dust
devils. HRSC images show that many tracks formed recently, including the
one on which Spirit landed; MER Microscopic Imager data show that sands
within the track zone are moderately dust free, while sands outside the
track are dusty. Thus, dark dust devil tracks here and perhaps elsewhere
on Mars are confirmed to represent the removal of bright dust to expose
a darker substrate, which, at the Spirit site, consists of
coarser-grained sands and granules in the bedforms and silt- to
fine-sand in the soils. MRAMS suggests that strong winds occur in the
afternoon in Gusev crater, a time consistent with dust-devil formation
on both Earth and Mars. At the Meridiani site, prevailing wind-related
features seen from orbit are bright wind streaks associated with
craters, the orientations of which suggest formative winds from the
northwest. Detailed mapping of aeolian features using MER data shows
that local topography (such as craters and other depressions) at both
rover sites can have a strong influence on the inferred wind patterns.
Thus, data from both orbit and the surface are required to determine the
general wind regime.
@--------------------------------------------------------------------
Title: Gusev Crater and Early Martian History: Clues from
Mars-Express & MGS Study
Authors: Foing, B. H.; Zegers, T. E.; van Kan, M.;
Pischel, R.; Martin, P.; Jaumann, R.; Hauber, E.;
Greeley, R.; Hoffmann, H.; Neukum, G.;
The HRSC Co-Investigator Team
Bibliographic Code: 2004emge.conf.8070F
Abstract
@--------------------------------------------------------------------
Title: High Temporal Resolution Spectroscopic Observations
of the Flare Star V1054 Oph
Authors: Crespo-Chacón, Inés; Montes, David;
Fernández-Figueroa, María José
López-Santiago, Javier; García-Alvarez, David;
Foing, Bernard H.
Bibliographic Code: 2004Ap&SS.292..697C
Abstract
We present the results of a high temporal resolution spectroscopic
monitoring of the flare (UV Cet type) star V1054 Oph (Wolf 630AB),
classified as a dM3.5e visual binary system. Intermediate resolution
spectra have been taken during four nights (2 5 April 2001) using the
IDS spectrograph of the 2.5 m Isaac Newton Telescope (INT) (La Palma,
Canary Islands, Spain). The V1054 Oph spectra show very strong emission
lines even in its quiescent state. The analysis of the temporal
evolution of the observed emission lines (from Hbeta to
H11 and the Ca II H and K lines) reveals four strong flares
and several weak flares. We have studied in detail the behaviour of the
chromospheric lines during the different phases (pre-flare, impulsive
and gradual decay) of these flares. The observed flares last from
˜25 to 95 min. The equivalent width of the Hbeta line
changes by a factor up to ˜2.3. Broad wings and asymmetric
(red-shifted) lines are observed as well.
@--------------------------------------------------------------------
Title: Photospheric and stellar wind variability in ε Ori
(B0 Ia)
Authors: Prinja, R. K.; Rivinius, Th.; Stahl, O.; Kaufer, A.;
Foing, B. H.; Cami, J.; Orlando, S.
Bibliographic Code: 2004A&A...418..727P
Abstract
We provide direct observational evidence for a link between photospheric
activity and perturbations in the dense inner-most stellar wind regions
of the B supergiant star ε Ori. The results, which are relevant
to our understanding of the origin of wind structure, are based on a
multi-spectral line analysis of optical time-series data secured in 1998
using the HEROS spectrograph on the ESO Dutch 0.9-m telescope in La
Silla. A period of ˜1.9 days is consistently identified in Balmer,
He I absorption, and weak metal lines such as Si III and C II. The
primary characteristic is a large-amplitude swaying of the central
absorption trough of the line, with differential velocities in lines
formed at varying depths in the atmosphere. The variance resulting from
the ``S-wave'' velocity behaviour of the lines is constrained within
± the projected rotation velocity (˜80 km s-1)
in the weakest absorption lines, but extends blue-ward to over -200 km
s-1 in Halpha. A second (superimposed) 1.9 day signal is
present at more extended blue-ward velocities (to ˜-300 km
s-1) in lines containing stronger circumstellar components.
Inspection of archival optical data from 1996 provides evidence that
this modulation signal has persisted for at least 2.5 years. Non-radial
pulsational modelling is carried out in an attempt to reproduce the key
observational characteristics of the line profile variability. Only
limited success is obtained with prograde (m=-1) modes. The principal
S-wave pattern cannot be matched by these models and remains enigmatic.
Based on observations obtained as part of the MUSICOS 98 campaign from
ESO La Silla, Chile.
@--------------------------------------------------------------------
Title: Multisite observations of SU Aurigae
Authors: Unruh, Y. C.; Donati, J.-F.; Oliveira, J. M.;
Collier Cameron, A.; Catala, C.; Henrichs, H. F.;
Johns-Krull, C. M.; Foing, B.; Hao, J.; Cao, H.;
Landstreet, J. D.; Stempels, H. C.; de Jong, J. A.;
Telting, J.; Walton, N.; Ehrenfreund, P.;
Hatzes, A. P.; Neff, J. E.; Böhm, T.; Simon, T.;
Kaper, L.; Strassmeier, K. G.; Granzer, Th.
Bibliographic Code: 2004MNRAS.348.1301U
Abstract
We present results from the 1996 Multi-Site Continuous Spectroscopy
(MUSICOS) campaign on the T Tauri star SU Aurigae. We find a 2.7-d
periodicity in the HeI (587.6 nm) line, and somewhat longer, less
well-pronounced periodicities in the Balmer lines and in Na D. Our
observations support the suggestion that the wind and infall signatures
are out of phase on SU Aur. We present Doppler images of SU Aur that
have been obtained from least-squares deconvolved profiles. Images taken
about one rotation apart show only limited overlap, in particular at low
latitudes. This is due in part to limitations in signal-to-noise ratio,
and in part to line-profile deformations that arise from short-lived
and/or non-surface features. The agreement at high latitudes is better
and suggests that at least some longer-lived features are present. The
analysis of Stokes V profiles yields a marginal magnetic field detection
during one of the phases.
@--------------------------------------------------------------------
Title: Geology of Noachian Martian Highlands Surrounding
the Gusev Crater
Authors: Zegers, T. E.; Conan, Y. G.; Foing, B.
Bibliographic Code: 2004LPI....35.1767Z
Abstract
To characterize the highland areas neighboring the Spirit landing site
we study the available visual and IR image data (THEMIS, MOC), MOLA
altimetry data and possibly new HRSC data from Mars Express.
@--------------------------------------------------------------------
Title: Amino Acid Survival Under Ambient Martian Surface UV
Lighting
Authors: Garry, J. R. C.; ten Kate, I. L.; Ruiterkamp, R.;
Peeters, Z.; Lehmann, B.; Foing, B. H.;
Ehrenfreund, P.
Bibliographic Code: 2004LPI....35.1686G
Abstract
Thin layers of glycine have been exposed to low ambient pressures and
ultra-violet lighting conditions similar to those on Mars. Scaling times
for sample alteration will be shown for these Mars-like conditions.
@--------------------------------------------------------------------
Title: Lunar Elemental Composition and Ivestigations with
D-CIXS X-Ray Mapping Spectrometer on SMART-1
Authors: Grande, M.; Dunkin, S.; Howe, C.; Browning, R.;
Kellett, B.; Perry, C. H.; Swinyard, B.; Waltham, N.;
Kent, B.; Huovenin, J.; Thomas, N.; Mal, U.;
Hughes, D.; Alleyne, H.; Russell, S.; Grady, M.;
Lundin, R.; Barabash, S.; Baker, D.; Murray, C. D.;
Guest, J.; Casanova, I.; Maurice, S.; Foing, B.
Bibliographic Code: 2004LPI....35.1519G
Abstract
The D-CIXS Compact X-ray Spectrometer on ESA SMART-1 successfully
launched in Sept 2003 can derive 45 km resolution images of the Moon
with a spectral resolution of 185 eV, providing the first
high-resolution global map of rock forming element abundances.
@--------------------------------------------------------------------
Title: ESA's SMART-1 Mission to the Moon: Goals, Status and
First Results
Authors: Foing, B. H.; Racca, G. D.; Marini, A.; Grande, M.;
Huovelin, J.; Josset, J. L.; Keller, H. U.;
Nathues, A.; Heather, D.; Koschny, D.; Malkki, A.
Bibliographic Code: 2004LPI....35.1413F
Abstract
SMART-1 has been launched on 27 Sept. 2003. We shall report at LPSC2004
on the commissioning and first results from the spacecraft and the
instruments.
@--------------------------------------------------------------------
Title: Noachian Martian highlands; the habitat of ancient
life?
Authors: Zegers, T. E.; Conan, Y. G.; Foing, B. H.
Bibliographic Code: 2004ESASP.545..313Z
Abstract
@--------------------------------------------------------------------
Title: High Temporal Resolution Spectra of Flare Stars
Authors: Montes, D.; Crespo-Chacón, I.;
Fernández-Figueroa, M. J.; López-Santiago, J.;
García-Alvarez, D.; Foing, B. H.
Bibliographic Code: 2004IAUS..219..910M
Abstract
The results of a high temporal resolution spectroscopic monitoring of
the
UV Cet type fare stars AD Leo and V1054 Oph are reported. Intermediate
resolution optical spectra of these stars were taken using the IDS
spectrograph of the 2.5 m Isaac Newton Telescope (INT) of El Roque de
los
Muchachos Observatory (Spain) during 4 nights (2-5 April 2001). We have
obtained high temporal resolution by taking series of spectra with short
exposure times (15-300 sec) separated only by the CCD readout time (~60
sec).
The great number of spectra observed each night has allowed us to
analyse the
temporal evolution of the emission lines and to identify several fares
of
different intensity and duration.
@--------------------------------------------------------------------
Title: Microbial community in a precursory scenario of
growing Tagetes patula in a lunar greenhouse
Authors: Kozyrovska, N. O.; Korniichuk, O. S.; Voznyuk, T. M.;
Kovalchuk, M. V.; Lytvynenko, T. L.;
Rogutskyy, I. S.; Mytrokhyn, O. V.;
Estrella-Liopis, V. R.; Borodinova, T. I.;
Mashkovska, S. P.; Foing, B. H.; Kordyum, V. A.
Bibliographic Code: 2004KosNT..10e.221K
Abstract
A confined prototype plant-microbial system is elaborated for
demonstration of growing pioneer plants in a lunar greenhouse. A
precursory scenario of growing Tagetes patula L. in a substrate
anorthosite which is similar mineralogically and chemically to lunar
silicate rocks includes the use of a microbial community. Microorganisms
served for preventive substrate colonization to avoid infection by
deleterious microorganisms as well as for bioleaching and delivering of
nutritional elements from anorthosite to plants. A model consortium of a
siliceous bacterium, biocontrol agents, and arbuscular mycorrhizal fungi
provided an acceptable growth and blossoming of Tagetes patula L. under
growth limiting factors in terrestrial conditions.
@--------------------------------------------------------------------
Title: Preface To The Proceedings Of Hawaii International
Lunar Exploration Conference 2003
Authors: Foing, Bernard H.
Bibliographic Code: 2004ilc..conf..531F
Abstract
@--------------------------------------------------------------------
Title: Europe En Route To The Moon: SMART-1 Final
Preparation, Launch And Early Flight (AAS 03-727)
Authors: Racca, G. D.; Foing, B. H.; Brinkmann, J.;
de Bijl, J.; di Napoli, L.; Estublier, D.;
Evrard, E.; Grünagel, R.; Lumb, R.; Marini, A.;
Rumler, P.; Stagnaro, L.; van Dooren, J.
Bibliographic Code: 2004ilc..conf..213R
Abstract
@--------------------------------------------------------------------
Title: ESA's SMART-1 Mission Launched To The Moon:
Technology And Science Goals (AAS 03-700)
Authors: Foing, B. H.; Racca, G. D.; Marini, A.; Evrard, E.;
Stagnaro, L.; Almeida, M.; Koschny, D.; Frew, D.;
Zender, J.; Heather, J.; Grande, M.; Huovelin, J.;
Keller, H. U.; Nathues, A.; Josset, J. L.;
Malkki, A.; Schmidt, W.; Noci, G.; Birkl, R.;
Iess, L.; Sodnik, Z.; McManamon, P.
Bibliographic Code: 2004ilc..conf....3F
Abstract
@--------------------------------------------------------------------
Title: The response of two amino acids to a subset of Mars'
surface conditions
Authors: Garry, J.; ten Kate, I.; Ruiterkamp, R.; Peeters, Z.;
Foing, B.; Ehrenfreund, P.
Bibliographic Code: 2004cosp...35.4171G
Abstract
A multi-year project is underway to characterize and understand the
behaviour of organic molecules to the nominal average near-surface
environment of Mars. Such materials are expected to have been delivered
by meteoritic infall and studies of the longevity of organic matter
under present and past martian conditions may provide useful data to
test exobiological concepts. The use of this system as a payload test
chamber is also being pursued as an active side-issue. The project
centres around a simulation system that can accommodate objects up to
0.2m3 in volume, and which can recreate the thermal and UV
conditions experienced by a range of martian locales. An auxiliary
chamber has been built to produce samples with a high degree of
repeatability and control. These samples have consisted of sub-micron
layers of solid glycine and beta-alanine vacuum deposited onto silicon
discs. Changes in the material content of each sample are measured with
the use of an IR transmission spectrometer with a spectral resolution of
4cm-1, and 'forward contamination' of these samples is
lessened through the use of vacuum-tight transfer vessels and sterile
handling techniques.
@--------------------------------------------------------------------
Title: Space Science and Interdisciplinary Education
Authors: Foing, B. H.
Bibliographic Code: 2004cosp...35.4078F
Abstract
The contribution of space science to an education cursus can be
conceived as a series of educational modules (each including text books
for teacher and pupil, exercises, CD-roms, observations or study
projects, kits for hands-on projects, and Internet products from space
agencies) covering different age groups (elementary 7-10, middle 10-14,
high school 15-17). These modules should not be limited to the science
teacher area, but must pervade in all topics of education the same way
as space is part of everyday life. Space agencies can contribute to this
by supporting a pilot group of teachers on sabbatical residence to
develop these modules. These teachers should cover different European
languages (e.g. English, French, German, other languages), different
educational systems experience, and different backgrounds
(Language/arts, science, history, technology). These modules could be
developed in one year, in partnership with education ministers,
publishers, for validation and production. They should be distributed
and inserted in curricula via education authorities and networks of
teachers. We list some examples of space (science) modules to be
developed, in different teachers courses for a total of about 20 hours
courses/yr, with basic modules for age group (7-10 yr) and Advanced
Modules for (10-15 yr).
@--------------------------------------------------------------------
Title: Bringing the Moon and Space to the Public
Authors: Foing, B. H.;
International Lunar Exploration Working Group
Bibliographic Code: 2004cosp...35.4076F
Abstract
We give some examples of public outreach activities using the Moon to
engage the public in space exploration. We describe the public relations
and science communication campaign organized by ESA and partners during
the preparation of the SMART-1, and surrounding the launch and
commissioning. We also describe some P.R. activities developed by the
International Lunar Exploration Working Group (ILEWG) and the Lunar
Explorers Society (LUNEX), founded by the participants of the 4th
International Conference on the Exploration and Utilisation of the Moon
(ICEUM-4) in July 2000. We illustrate how people from diverse
backgrounds with a common interest in the exploration of the Moon and
beyond, are promoting research, exploration and outreach programmes, by
educating the public using web-based information and organising
activities or events. This provides a global structure of partnerships
that can be used to raise the awareness of the general public on lunar,
planetary and space related issues, and be used for future actions.
ILEWG: http://sci.esa.int/ilewg/ LUNEX: www.lunarexplorer.org SMART-1:
http://sci.esa.int/smart-1/
@--------------------------------------------------------------------
Title: Roadmap for Future Lunar Exploration
Authors: Foing, B. H.;
International Lunar Exploration Working Group
Bibliographic Code: 2004cosp...35.4061F
Abstract
We discuss strategies for future lunar exploration. This includes open
science questions about comparative planetology, the origin of the Earth
--Moon system, the early evolution of life, the planetary environment
and the existence of in-situ resources necessary to support human
presence. We discuss areas of instrumentation: Remote sensing
miniaturised instruments; Surface geophysical and geochemistry package;
Instrument deployment and robotic arm, nano-rover, sampling, drilling;
Sample finder and collector. We discuss technologies in robotic
exploration: Mecha-electronics-sensors; Tele control, telepresence,
virtual reality; Regional mobility rover; Autonomy and Navigation;
Artificially intelligent robots. We compare Moon-Mars system aspects
related to In-Situ Utilisation of resources; Establishment of permanent
robotic infrastructure, Environmental protection aspects; Life sciences
laboratories; Support to human exploration. Finally, we discuss possible
roadmaps and synergies for Moon-Mars exploration, starting with the
missions for the coming decade, and building effectively on joint
technology developments.
@--------------------------------------------------------------------
Title: SMART-1 Payload First Results
Authors: Foing, B. H.;
SMART-1 Science Technology Working Team
Bibliographic Code: 2004cosp...35.4059F
Abstract
We present first results from SMART-1's science and technology payload,
with a total mass of some 19 kg, featuring many innovative instruments
and advanced technologies. A miniaturised high-resolution camera (AMIE)
for lunar surface imaging, a near-infrared point-spectrometer (SIR) for
lunar mineralogy investigation, and a very compact X-ray spectrometer
(D-CIXS) with a new type of detector and micro-collimator which will
provide fluorescence spectroscopy and imagery of the Moon's surface
elemental composition. The payload also includes an experiment (KaTE)
aimed at demonstrating deep-space telemetry and telecommand
communications in the X and Ka-bands, a radio-science experiment (RSIS),
a deep space optical link (Laser-Link Experiment), using the ESA Optical
Ground station in Tenerife, and the validation of a system of autonomous
navigation (OBAN) based on image processing. SMART-1 lunar science
investigations include studies of the chemical composition of the Moon,
of geophysical processes (volcanism, tectonics, cratering, erosion,
deposition of ices and volatiles) for comparative planetology, and high
resolution studies in preparation for future steps of lunar exploration.
The mission could address several topics such as the accretional
processes that led to the formation of rocky planets, and the origin and
evolution of the Earth-Moon system. The SMART-1 observations will be
coordinated with Japanese missions Lunar-A and SELENE, to answer open
questions about comparative planetology, the origin of the Earth --Moon
system, the early evolution of life, the planetary environment and the
existence of in-situ resources necessary to support human presence (e.g.
water, oxygen). With their science and technology results, these
missions can be considered as preparatory missions for future robotic
and human exploration of the solar system.
@--------------------------------------------------------------------
Title: ESA's SMART-1 Mission: Status
Authors: Racca, G.; Foing, B. H.; SMART-1 Project Team
Bibliographic Code: 2004cosp...35.4057R
Abstract
SMART-1 is the first of Small Missions for Advanced Research and
Technology as part of ESA science programme ``Cosmic Vision''. Its
objective is to demonstrate Solar Electric Primary Propulsion (SEP) for
future Cornerstones (such as Bepi-Colombo) and to test new technologies
for spacecraft and instruments. The spacecraft has been launched on 27
sept. 2003, as an Ariane-5 auxiliary passenger. SMART-1 orbit pericenter
is now outside the inner radiation belt. The current status of SMART-1
will be given at the symposium. After a 15 month cruise with primary
SEP, the SMART-1 mission is to orbit the Moon for a nominal period of
six months, with possible extension. The spacecraft will carry out a
complete programme of scientific observations during the cruise and in
lunar orbit.
@--------------------------------------------------------------------
Title: Complex Organics in Interstellar Space
Authors: Foing, B.; Ehrenfreund, P.; Ruiterkamp, R.; Cox, N.
Bibliographic Code: 2004cosp...35.4056F
Abstract
There are signatures of large organic molecules in the interstellar
medium, from the ultraviolet to the infrared. Some infrared emission
bands, which have been ascribed to families of large aromatic compounds
are not specific for individual identification (and for discriminating
free floating PAH molecules from loosely bound aromatics in amorphous
carbon compounds). Red fluorescence and FUV absorption have also been
ascribed to these aromatic compounds. Electronic transitions in the
visible are a key to identify free gas phase molecules. The origin of
Diffuse Interstellar Bands (Herbig 1995), more than 300 in recent
surveys (O' Tuairisg et al 2000) is still a mystery. However the
measurements of sub-structures rotational contours in DIBs (Ehrenfreund
Foing 1996) indicate large molecules such as chains (12-18C), rings, 50
C PAHs or fullerenes. The distribution of DIB widths permit to estimate
a distribution of size of molecular carriers. The environment properties
of DIB carriers also indicate ionisation potentials similar to those of
cations of large carbonaceous molecules, such as large PAHs or
fullerenes (Sonnentrucker et al 1997). The correlation studies of DIBS
also indicate different carriers for the strong DIBs observed in the
visible (Cami et al 1997). DIBS are weakened in the in the
low-metallicity Magellanic clouds (Ehrenfreund et al 2002, Cox et al
2004). The detection of near IR bands at 9577 and 9632 A coinciding with
laboratory transitions of C60+ (Foing, Ehrenfreund 1994, 1997,
Galatzudinov et al 2000 ) suggest that significant interstellar carbon
could reside in complex fullerene type compounds. These results indicate
that many different large and complex organic molecules can form and
survive in the very harsh interstellar environments. A follow up
interdisciplinary work is required between astronomical observations,
laboratory matrix and gas phase spectroscopy, theoretical work and
modelling, and active experiments in space to study the formation,
evolution, survival and transport of these complex organics.
@--------------------------------------------------------------------
Title: Synergies and roadmap for Moon-Mars Exploration
Authors: Foing, B. H.; Pieters, C.; Ilewg
Bibliographic Code: 2004cosp...35.3357F
Abstract
There are large synergies between Moon and Mars exploration. This
includes joint areas of instrumentation: Remote sensing miniaturised
instruments; Surface geophysical and geochemistry package; Instrument
deployment and robotic arm, nano-rover, sampling, drilling; Sample
finder and collector. There are also common technologies in robotic
exploration: Mecha-electronics-sensors; Tele control, telepresence,
virtual reality; Regional mobility rover; Autonomy and Navigation;
Artificially intelligent robots. We compare Moon-Mars system aspects
related to In-Situ Utilisation of resources; Establishment of permanent
robotic infrastructure, Environmental protection aspects; Life sciences
laboratories; Support to human exploration. Finally, we discuss possible
roadmaps for exploration, starting with the Moon-Mars missions for the
coming decade, and building effectively on joint technology
developments.
@--------------------------------------------------------------------
Title: Gusev Crater and surrounding Highlands: preliminary
HRSC results
Authors: Foing, B. H.; Zegers, T.; Pischel, R.; Greeley, R.;
Jaumann, R.; Hoffmann, H.; Neukum, G.;
HRSC Co-Investigators Team, &
Bibliographic Code: 2004cosp...35.3345F
Abstract
We report on the preliminary analysis of data on Gusev crater and
surroundings, obtained with the Mars Express HRSC camera. The Gusev
crater lies in the northern part of the highlands that contain the
remanent magnetization.The highlands around Gusev crater are
characterized by a plateau of most likely basalt. The most conspicuous
features in the highland plateau are impact craters. Towards the
northwest of Gusev crater the plateau is transformed into a chaotic
terrain, with lower altitude. The basalt plateau rises about 2000 m
above the crater basin. It was suggested that Gusev impact depression
might have been filled with water, if available then. The brecciation of
target rocks could have resulted in a porous host rock with a large
subsurface water-rock interface that can provide sheltered conditions
for early life. To characterize the highland and the crater floor areas,
we study the new HRSC data obtained in January 2004 and compare them to
available visual and IR image data (THEMIS, MOC), TES spectroscopy data
and MOLA altimetry data. These data are also used to provide geological
context for the MER Lander Spirit that landed in the crater.
@--------------------------------------------------------------------
Title: Scenario of Growing Crops on Silicates in Lunar
Gargens
Authors: Kozyrovska, N.; Kovalchuk, M.; Negutska, V.; Lar, O.;
Korniichuk, O.; Alpatov, A.; Rogutskiy, I.;
Kordyum, V.; Foing, B.
Bibliographic Code: 2004cosp...35..745K
Abstract
Self-perpetuating gardens will be a practical necessity for humans,
living in permanently manned lunar bases. A lunar garden has to
supplement less appetizing packaged food brought from the Earth, and the
ornamental plants have to serve as valuable means for emotional
relaxation of crews in a hostile lunar environment. The plants are less
prone to the inevitable pests and diseases when they are in optimum
condition, however, in lunar greenhouses there is a threat for plants to
be hosts for pests and predators. Although the lunar rocks are
microorganism free, there will be a problem with the acquired infection
(pathogens brought from the Earth) in the substrate used for the plant
growing. On the Moon pests can be removed by total fumigation, including
seed fumigation. However, such a treatment is not required when
probiotics (biocontrol bacteria) for seed inoculation are used. A
consortium of bacteria, controlling plant diseases, provides the
production of an acceptable harvest under growth limiting factors and a
threatening infection. To model lunar conditions we have used
terrestrial alumino-silicate mineral anorthosite (Malyn, Ukraine) which
served us as a lunar mineral analog for a substrate composition. With
the idea to provide a plant with some essential growth elements
siliceous bacterium Paenibacillus sp. has been isolated from
alumino-silicate mineral, and a mineral leaching has been simulated in
laboratory condition. The combination of mineral anorthosite and
siliceous bacteria, on one hand, and a consortium of beneficial bacteria
for biocontrol of plant diseases, on the other hand, are currently used
in model experiments to examine the wheat and potato growth and
production in cultivating chambers under controlled conditions.
@--------------------------------------------------------------------
Title: MUSICOS Observations of the Chromospherically Active
Binary Star EI Eridani
Authors: Washuettl, A.; Strassmeier, K. G.; Foing, B.;
MUSICOS98 Team
Bibliographic Code: 2003csss...12.1008W
Abstract
We present first results on spectroscopic observations of the
rapidly-rotating active binary star EI Eridani obtained during the
MUSICOS multi-site campaign in 1998. Eight sites around the globe were
involved in order to achieve surface images within a few rotations as EI
Eridani's critical rotation period of 1.945 days makes it impossible to
obtain time-resolved images from a single site. The data were split into
groups in order to obtain consecutive, independent Doppler images. The
preliminary results confirm the existence of a stable polar spot that
changes in size and shape while low-latitute spots are found to be short
lived. For the first time, it is possible to achieve consecutive,
time-resolved Doppler images for EI Eridani. A preliminary investigation
of differential rotation contradicts the results from Hatzes & Vogt
(1992).
@--------------------------------------------------------------------
Title: MUSICOS 1998: Observations of Rotational Modulation
and Flares on the RS CVn Binary HR1099
Authors: García-Alvarez, D.; Foing, B. H.; Montes, D.;
Oliveira, J.; Doyle, J. G.; MUSICOS 98 Collaboration
Bibliographic Code: 2003csss...12..958G
Abstract
We present simultaneous and continuous observations of Halpha,
Hbeta, ion{Na}{1} D1, D2, ion{He}{1}
D3 and ion{Ca}{2} H & K lines of the chromospherically
active binary HR 1099. We have observed HR 1099 for more than 3 weeks
almost continuously and monitored two flares. An increase in Halpha
and ion{Ca}{2} H & K, Hbeta and ion{He}{1} D3 and a
strong filling-in of the ion{Na}{1} D1, D2 during
the flares are observed. We have found that the flares took place at the
same phase (0.85) of the binary orbit, and both of them seems to occur
near the limb.
@--------------------------------------------------------------------
Title: The SMART-1 Mission: Photometric Studies of the Moon
with the AMIE Camera
Authors: Shkuratov, Yu. G.; Kreslavsky, M. A.;
Stankevich, D. G.; Kaydash, V. G.; Pinet, P.;
Shevchenko, V. V.; Foing, B. H.; Josset, J.-L.
Bibliographic Code: 2003SoSyR..37..251S
Abstract
We describe the future SMART-1 European Space Mission whose objective is
to study the lunar surface from a polar lunar orbit. In particular, it
is anticipated that selected regions of the Moon will be photographed
using the AMIE camera with a mean spatial resolution of about 100 m in
three spectral channels (0.75, 0.92, and 0.96 mum) over a wide range
of phase angles. Since these spectral channels and the AMIE resolution
are close to those of the UVVIS camera onboard the Clementine
spacecraft, the simultaneous processing of SMART-1 and Clementine data
can be planned, for example, to obtain phase-ratio images. These images
carry information on the structural features of the lunar surface. In
particular, UVVIS/Clementine data revealed a photometric anomaly at the
Apollo-15 landing site associated with the blowing of the lunar regolith
by the lander engine. Anomalies were found in the ejection zones of
several fresh craters.
@--------------------------------------------------------------------
Title: www.lunarexplorer.org: Educating the general public
Authors: Volp, J.; Foing, B.
Bibliographic Code: 2003AdSpR..31.2455V
Abstract
The Lunar Explorers Society (LUNEX) was founded by the participants of
the 4th International Conference on the Exploration and Utilisation of
the Moon (ICUEM4), which was organised under the auspices of the
International Lunar Exploration Working Group (ILEWG), and aimed to draw
together people from diverse backgrounds with a common interest in the
exploration of the Moon. At the end of the conference, a formal ICEUM4
Declaration was drawn up detailing the recommendations of the
participants for the future of lunar exploration. LUNEX is a society
open to all Lunar Explorers and will aim to promote research,
exploration and outreach programmes that work towards the realisation of
the goals outlined in the ICEUM4 Declaration by educating the public
using web-based information and activities. LUNEX provides a global
structure that can be used to raise the awareness of the general public
on lunar related issues. We are looking for partnerships with other Moon
Societies to join efforts. For more information on the Lunar Explorers
Society, its activities, how to become an active member, or how your
organisation can work together with LUNEX, please visit our website on
www.lunarexplorer.org.
@--------------------------------------------------------------------
Title: SMART-1 mission to the moon: Technology and science
goals
Authors: Foing, B. H.; Racca, G. D.; Marini, A.;
Heather, D. J.; Koschny, D.; Grande, M.;
Huovelin, J.; Keller, H. U.; Nathues, A.;
Josset, J. L.; Malkki, A.; Schmidt, W.; Noci, G.;
Birkl, R.; Iess, L.; Sodnik, Z.; McManamon, P.
Bibliographic Code: 2003AdSpR..31.2323F
Abstract
SMART-1 is a technology demonstration mission for deep space solar
electrical propulsion and Technologies for the Future. SMART-1 will be
Europe's first lunar mission and will contribute to developing an
international program of lunar exploration. The spacecraft has been
readied in April 2003 for a launch in summer 2003, as an auxiliary
passenger to GTO on Ariane 5, to reach the Moon after 15 month's cruise.
SMART-1 will carry six experiments, including three remote sensing
instruments that will be used during the mission's nominal six months in
lunar orbit. These instruments will contribute to key planetary
scientific questions, related to theories of lunar origin and evolution,
the global and local crustal composition, the search for cold traps at
the lunar poles and the mapping of potential lunar resources.
@--------------------------------------------------------------------
Title: Preface
Authors: Duke, Michael B.; Foing, Bernard H.
Bibliographic Code: 2003AdSpR..31.2291D
Abstract
@--------------------------------------------------------------------
Title: Scientific rationale for the D-CIXS X-ray
spectrometer on board ESA's SMART-1 mission to the
Moon
Authors: Dunkin, S. K.; Grande, M.; Casanova, I.;
Fernandes, V.; Heather, D. J.; Kellett, B.;
Muinonen, K.; Russell, S. S.; Browning, R.;
Waltham, N.; Parker, D.; Kent, B.; Perry, C. H.;
Swinyard, B.; Perry, A.; Feraday, J.; Howe, C.;
Phillips, K.; McBride, G.; Huovelin, J.; Muhli, P.;
Hakala, P. J.; Vilhu, O.; Thomas, N.; Hughes, D.;
Alleyne, H.; Grady, M.; Lundin, R.; Barabash, S.;
Baker, D.; Clark, P. E.; Murray, C. D.; Guest, J.;
D'Uston, L. C.; Maurice, S.; Foing, B.; Christou, A.;
Owen, C.; Charles, P.; Laukkanen, J.; Koskinen, H.;
Kato, M.; Sipila, K.; Nenonen, S.; Holmstrom, M.;
Bhandari, N.; Elphic, R.; Lawrence, D.
Bibliographic Code: 2003P&SS...51..435D
Abstract
The D-CIXS X-ray spectrometer on ESA's SMART-1 mission will provide the
first global coverage of the lunar surface in X-rays, providing absolute
measurements of elemental abundances. The instrument will be able to
detect elemental Fe, Mg, Al and Si under normal solar conditions and
several other elements during solar flare events. These data will allow
for advances in several areas of lunar science, including an improved
estimate of the bulk composition of the Moon, detailed observations of
the lateral and vertical nature of the crust, chemical observations of
the maria, investigations into the lunar regolith, and mapping of
potential lunar resources. In combination with information to be
obtained by the other instruments on SMART-1 and the data already
provided by the Clementine and Lunar Prospector missions, this
information will allow for a more detailed look at some of the
fundamental questions that remain regarding the origin and evolution of
the Moon.
@--------------------------------------------------------------------
Title: The D-CIXS X-ray mapping spectrometer on SMART-1
Authors: Grande, M.; Browning, R.; Waltham, N.; Parker, D.;
Dunkin, S. K.; Kent, B.; Kellett, B.; Perry, C. H.;
Swinyard, B.; Perry, A.; Feraday, J.; Howe, C.;
McBride, G.; Phillips, K.; Huovelin, J.; Muhli, P.;
Hakala, P. J.; Vilhu, O.; Laukkanen, J.; Thomas, N.;
Hughes, D.; Alleyne, H.; Grady, M.; Lundin, R.;
Barabash, S.; Baker, D.; Clark, P. E.; Murray, C. D.;
Guest, J.; Casanova, I.; D'Uston, L. C.; Maurice, S.;
Foing, B.; Heather, D. J.; Fernandes, V.;
Muinonen, K.; Russell, S. S.; Christou, A.; Owen, C.;
Charles, P.; Koskinen, H.; Kato, M.; Sipila, K.;
Nenonen, S.; Holmstrom, M.; Bhandari, N.; Elphic, R.;
Lawrence, D.
Bibliographic Code: 2003P&SS...51..427G
Abstract
The D-CIXS Compact X-ray Spectrometer will provide high quality
spectroscopic mapping of the Moon, the primary science target of the ESA
SMART-1 mission. D-CIXS consists of a high throughput spectrometer,
which will perform spatially localised X-ray fluorescence spectroscopy.
It will also carry a solar monitor, to provide the direct calibration
needed to produce a global map of absolute lunar elemental abundances,
the first time this has been done. Thus it will achieve ground breaking
science within a resource envelope far smaller than previously thought
possible for this type of instrument, by exploiting two new
technologies, swept charge devices and micro-structure collimators. The
new technology does not require cold running, with its associated
overheads to the spacecraft. At the same time it will demonstrate a
radically novel approach to building a type of instrument essential for
the BepiColombo mission and potential future planetary science targets.
@--------------------------------------------------------------------
Title: Composition of the lunar surface as will be seen
from SMART-1: A simulation using Clementine data
Authors: Shkuratov, Yuriy G.; Stankevich, Dmitriy G.;
Kaydash, Vadim G.; Omelchenko, Vitaliy V.;
Pieters, Carle M.; Pinet, Patrick C.;
Chevrel, Serge D.; Daydou, Yves H.;
Foing, Bernard H.; Sodnik, Zoran; Josset, Jean-Luc;
Taylor, Lawrence A.; Shevchenko, Vladislav V.
Bibliographic Code: 2003JGRE..108.5020S
Abstract
We present a new technique for remote sensing determination of lunar
surface composition in the context of the SMART-1 mission. The technique
is based on spectral and composition data obtained by Lunar Soil
Characterization Consortium for a few particle-size separates of lunar
soils. We map the abundance of TiO2 and FeO, pyroxene
content, maturity degree (Is/FeO), and a characteristic size
of particles. Comparison of the TiO2 and FeO abundance maps
with proper distributions obtained by Lucey et al. [2000a] shows high
correlation. We found also an inverse correlation between the
Is/FeO distribution and Lucey et al.'s [2000b] parameter OM.
Application of this approach shows that fresh mare crater regolith is
characterized with a higher abundance of pyroxenes, coarse particles,
and low maturity degree. The pyroxene abundance map can be used to
identify pyroclastic regions. An excess of small particles is predicted
for highland areas. We note appreciable variations of the characteristic
size of particles in mare regions. Our preliminary results for the
Reiner-gamma formation show that there is no composition anomaly for
the TiO2 and FeO abundance, in agreement with previous
analyses. Our maps also indicate that the formation contains a surface
material characterized with low maturity and high degree of
crystallinity, consistent with the occurrence of immature regolith
possibly contaminated with dust.
@--------------------------------------------------------------------
Title: bringing the moon to people: lunar explorers society
Authors: Foing, B. H.; Volp, J.; Almeida, M.; Heather, D.;
van Susante, P.; The Lunar Explorers Society
Bibliographic Code: 2003EAEJA....14858F
Abstract
The Lunar Explorers Society (LUNEX) was founded by the participants of
the 4th International Conference on the Exploration and
Utilisation of the Moon (ICEUM4), held in July 2000 at the European
Space Research and Technology Centre (ESTEC) in The Netherlands. ICEUM4
was organised under the auspices of the International Lunar Exploration
Working Group (ILEWG), and aimed to draw together people from diverse
backgrounds with a common interest in the exploration of the Moon. At
the end of the conference, a formal ICEUM4 Declaration was drawn up
detailing the recommendations of the participants for the future of
lunar exploration. LUNEX will be a society open to all Lunar Explorers
and will aim to promote research, exploration and outreach programmes
that will work towards the realisation of the goals outlined in the
ICEUM4 Declaration. Following ICEUM4, a core group of active LUNEX
members was identified to begin to shape the new-born society with
guidance from ILEWG. A series of task groups have been installed to
address the key LUNEX issues, with strong participation of young lunar
explorers, and work is progressing towards the first LUNEX activities,
both at the level of the task groups and to form national chapters. The
first LUNEX convention was held in Paris in March 2001. Further
information about the Lunar Explorers Society can be found on our
Website: http://www.lunarexplorer.org.
@--------------------------------------------------------------------
Title: Status of esa smart-1 mission to the moon
Authors: Foing, B. H.; Racca, G. R.; Marini, A.; Smart-1;
Technology Working Team,
Bibliographic Code: 2003EAEJA....14857F
Abstract
SMART-1 is the first in the programme of ESA's Small Missions for
Advanced Research and Technology. Its objective is to demonstrate Solar
Electric Primary Propulsion (SEP) for future Cornerstones (such as
Bepi-Colombo) and to test new technologies for spacecraft and
instruments. The spacecraft has been readied for launch in spring 2003
as an Ariane-5 auxiliary passenger. After a cruise with primary SEP, the
SMART-1 mission is to orbit the Moon for a nominal period of six months,
with possible extension. The spacecraft will carry out a complete
programme of scientific observations during the cruise and in lunar
orbit. SMART-1's science payload, with a total mass of some 19 kg,
features many innovative instruments and advanced technologies. A
miniaturised high-resolution camera (AMIE) for lunar surface imaging, a
near-infrared point-spectrometer (SIR) for lunar mineralogy
investigation, and a very compact X-ray spectrometer (D-CIXS) with a new
type of detector and micro-collimator which will provide fluorescence
spectroscopy and imagery of the Moon's surface elemental composition.
The payload also includes an experiment (KaTE) aimed at demonstrating
deep-space telemetry and telecommand communications in the X and
Ka-bands, a radio-science experiment (RSIS), a deep space optical link
(Laser-Link Experiment), using the ESA Optical Ground station in
Tenerife, and the validation of a system of autonomous navigation
SMART-1 lunar science investigations include studies of the chemical
(OBAN) based on image processing. SMART-1 lunar science investigations
include studies of the chemical composition and evolution of the Moon,
of geophysical processes (volcanism, tectonics, cratering, erosion,
deposition of ices and volatiles) for comparative planetology, and high
resolution studies in preparation for future steps of lunar exploration.
The mission could address several topics such as the accretional
processes that led to the formation of planets, and the origin of the
Earth-Moon system.
@--------------------------------------------------------------------
Title: Organics in space: spectroscopic characterizations
Authors: Boudin, N.; Ruiterkamp, R.; Foing, B.
Bibliographic Code: 2003EAEJA.....6771B
Abstract
There are signatures of large organic molecules in the interstellar
medium, from the ultraviolet to the infrared. Some infrared emission
bands, which have been ascribed to families of large aromatic compounds
are not specific for individual identification (and for discriminating
free floating PAH molecules from loosely bound aromatics in amorphous
carbon compounds). Red fluorescence and FUV absorption have also been
ascribed to these aromatic compounds. Electronic transitions in the
visible are a key to identify free gas phase molecules. The origin of
Diffuse Interstellar Bands (Herbig 1995), more than 300 in recent
surveys (O' Tuairisg et al 2000) is still a mystery. However the
measurements of sub-structures rotational contours in DIBs (Ehrenfreund
Foing 1996) indicate large molecules such as chains (12-18C), rings, 50
C PAHs or fullerenes. The distribution of DIB widths permit to estimate
a distribution of size of molecular carriers. The correlation studies of
DIBS also indicate different carriers for the strong DIBs observed in
the visible (Cami et al 1997). Finally the detection of NIR bands at
9577 and 9632 A coinciding with laboratory transitions of C60+ (Foing,
Ehrenfreund 1994, 1997, Galatzudinov et al 2000) suggest that
significant interstellar carbon could reside in complex fullerene type
compounds. These results indicate that many different large and
complex organic molecules can form and survive in the very harsh
interstellar environments. Several spectroscopic studies of these
aromatics molecules are reported and their advantages and drawbacks
discussed. A follow up interdisciplinary work is required between
astronomical observations, laboratory matrix and gas phase spectroscopy,
theoretical work and modelling, and active experiments in space to study
the formation, evolution, survival and transport of these complex
organics.
@--------------------------------------------------------------------
Title: Mars Simulation Chamber 2 - goals, instrumentation
and methods
Authors: Ehrenfreund, P.; ten Kate, I. L.; Ruiterkamp, R.;
Botta, O.; Lehmann, B.; Boudin, N.; Foing, B. H.
Bibliographic Code: 2003EAEJA.....4298E
Abstract
We have installed at ESTEC and instrumented a Mars Simulation Chamber
(MSC), in order to answer a range of questions on the subject of the
apparent absence of organic compounds on Mars. We shall investigate: A.
The effects of the changes of the Martian atmosphere over the history of
Mars. B. The effect of UV irradiation on organic molecules embedded in
the soil. C. The effect of oxidation on organic molecules embedded in
the soil. D. The effect of thermal cycling on the surface. E. A
combination of the above mentioned parameters. Techniques to be used
include gas analysis, environmental sensors, HPLC, spectroscopy and
other analytical techniques. We shall also assess the sensitivity of
instruments for the detection of minerals and organic compounds of
exobiological relevance in Martian analogue soils (mixed under
controlled conditions with traces of these organics). The results
concerning the simulation of complex organics on Mars, as well as lander
instrument chamber simulations will be included in a database to serve
for the interpretation of Beagle 2 data and other future Mars missions.
The results of the experiments can also provide constraints for the
observations from orbit, such as spectroscopy of minerals, measurements
of the water cycle, frost and subsurface water, the CO2 cycle, and the
landing site selection. In summary, the experiments have as a main goal
to simulate various processes on organics, such as the effects of UV
radiation, diffusion, and temperature, as a function of their depth in
the soil. The specific organics will be embedded in either porous or
compact Martian soil analogues or quartz beads. In this presentation
we will concentrate on the goals, the instrumentation and the methods,
used to operate the chamber.
@--------------------------------------------------------------------
Title: Mars Simulation Chamber 1 - preparation for Mars
Express and future Mars missions
Authors: Ehrenfreund, P.; ten Kate, I. L.; Ruiterkamp, R.;
Botta, O.; Lehmann, B.; Boudin, N.; Foing, B. H.
Bibliographic Code: 2003EAEJA.....4277E
Abstract
We have installed at ESTEC and instrumented a Mars Simulation Chamber
(MSC), in order to answer a range of questions on the subject of the
apparent absence of organic compounds on Mars. We shall investigate: A.
The effects of the changes of the Martian atmosphere over the history of
Mars. B. The effect of UV irradiation on organic molecules embedded in
the soil. C. The effect of oxidation on organic molecules embedded in
the soil. D. The effect of thermal cycling on the surface. E. A
combination of the above mentioned parameters. Techniques to be used
include gas analysis, environmental sensors, HPLC, spectroscopy and
other analytical techniques. We shall also assess the sensitivity of
instruments for the detection of minerals and organic compounds of
exobiological relevance in Martian analogue soils (mixed under
controlled conditions with traces of these organics). The results
concerning the simulation of complex organics on Mars, as well as lander
instrument chamber simulations will be included in a database to serve
for the interpretation of Beagle 2 data and other future Mars missions.
The results of the experiments can also provide constraints for the
observations from orbit, such as spectroscopy of minerals, measurements
of the water cycle, frost and subsurface water, the CO2 cycle, and the
landing site selection. In summary, the experiments have as a main goal
to simulate various processes on organics, such as the effects of UV
radiation, diffusion, and temperature, as a function of their depth in
the soil. The specific organics will be embedded in either porous or
compact Martian soil analogues or quartz beads. In this presentation
we will concentrate on the preparation for Mars Express.
@--------------------------------------------------------------------
Title: Simulations of Martian Surface and Subsurface
Processes
Authors: ten Kate, I. L.; Ruiterkamp, R.; Botta, O.;
Lehmann, B.; Gomez Hernandez, C.; Boudin, N.;
Foing, B. H.; Ehrenfreund, P.
Bibliographic Code: 2003LPI....34.1313T
Abstract
Laboratory investigations on organic chemical processes occurring in the
martian surface and subsurface using a Mars Simulation Chamber.
@--------------------------------------------------------------------
Title: A solar-powered visit to the Moon. The SMART-1
misson
Authors: Racca, Giuseppe; Foing, Bernard
Bibliographic Code: 2003ESABu.113...14R
Abstract
SMART stands for Small Missions for Advanced Research in Technology.
Europe's space scientists have fitted SMART-1 with very modern and
compact sensors to map lunar minerals in greater detail than ever
before, using infrared rays. With X-rays too, it will make the first
comprehensive inventory of key chemical elements in the lunar surface.
@--------------------------------------------------------------------
Title: Simultaneous optical and X-ray observations of
flares and rotational modulation on the RS CVn
binary HR 1099 (V711 Tau) from the MUSICOS 1998
campaign
Authors: García-Alvarez, D.; Foing, B. H.; Montes, D.;
Oliveira, J.; Doyle, J. G.; Messina, S.;
Lanza, A. F.; Rodonò, M.; Abbott, J.; Ash, T. D. C.;
Baldry, I. K.; Bedding, T. R.; Buckley, D. A. H.;
Cami, J.; Cao, H.; Catala, C.; Cheng, K. P.;
Domiciano de Souza, A., Jr.; Donati, J.-F.;
Hubert, A.-M.; Janot-Pacheco, E.; Hao, J. X.;
Kaper, L.; Kaufer, A.; Leister, N. V.; Neff, J. E.;
Neiner, C.; Orlando, S.; O'Toole, S. J.; Schäfer, D.;
Smartt, S. J.; Stahl, O.; Telting, J.; Tubbesing, S.
Bibliographic Code: 2003A&A...397..285G
Abstract
We present simultaneous and continuous observations of the Halpha,
Hbeta, He I D3, Na I D1, D2 doublet
and the Ca II H & K lines for the RS CVn system HR 1099. The
spectroscopic observations were obtained during the MUSICOS 1998
campaign involving several observatories and instruments, both echelle
and long-slit spectrographs. During this campaign, HR 1099 was observed
almost continuously for more than 8 orbits of 2.8 deg. Two large optical
flares were observed, both showing an increase in the emission of
Halpha, Ca II H & K, Hbeta and He I D3 and a strong
filling-in of the Na I D1, D2 doublet.
Contemporary photometric observations were carried out with the robotic
telescopes APT-80 of Catania and Phoenix-25 of Fairborn Observatories.
Maps of the distribution of the spotted regions on the photosphere of
the binary components were derived using the Maximum Entropy and
Tikhonov photometric regularization criteria. Rotational modulation was
observed in Halpha and He I D3 in anti-correlation with the
photometric light curves. Both flares occurred at the same binary phase
(0.85), suggesting that these events took place in the same active
region. Simultaneous X-ray observations, performed by ASM on board RXTE,
show several flare-like events, some of which correlate well with the
observed optical flares. Rotational modulation in the X-ray light curve
has been detected with minimum flux when the less active G5 V star was
in front. A possible periodicity in the X-ray flare-like events was also
found.
Based on observations obtained during the MUSICOS 98 MUlti-SIte
COntinuous Spectroscopic campaign from Observatoire de Haute-Provence,
France, Kitt Peak National Observatory, USA, ESO La Silla, Chile, Mt.
Stromlo Observatory, Australia, Xinglong National Observatory, China,
Isaac Newton Telescope, Spain, Laboratório Nacional de
Astrofísica, Brazil, and South African Astronomical Observatory,
South Africa. Contemporaneous observations from Catania, Italy and
Fairborn Observatories, USA, and on data obtained with the Rossi X-ray
Timing Explorer.
@--------------------------------------------------------------------
Title: ESA SMART-1 Mission to the Moon
Authors: Foing, Bernard H.; Racca, Giuseppe D.;
Marini, Andrea; Grande, Manuel; Huovelin, Juhani;
Josset, Jean-Luc; Keller, Horst Uwe;
Nathues, Andreas; Koschny, Detlef; Malkki, Ansi
Bibliographic Code: 2003IAUSS...1E..35F
Abstract
SMART-1 is the first of ESA's Small Missions for Advanced Research
and Technology. Its objective is to demonstrate Primary Solar Electric
Propulsion for future Cornerstones (such as Bepi-Colombo) and to test
new technologies for spacecraft and instruments. The 370 kg spacecraft
is to be launched in summer 2003 as Ariane-5 auxiliary passenger and
after a 15 month cruise is to orbit the Moon for 6 months with possible
extension. SMART-1 will carry out observations during the cruise and in
lunar orbit with a science and technology payload (19 kg total mass): a
miniaturised high-resolution camera (AMIE) a near-infrared
point-spectrometer (SIR) for lunar mineralogy a very compact X-ray
spectrometer (D-CIXS) mapping surface elemental composition a Deep Space
Communication experiment (KaTE) a radio-science investigations (RSIS) a
Laser-Link Experiment an On Board Autonomous Navigation experiment
(OBAN) and plasma sensors (SPEDE). SMART-1 will study accretional and
bombardment processes that led to the formation of rocky planets and the
origin and evolution of the Earth-Moon system. Its science
investigations include studies of the chemical composition of the Moon
of geophysical processes (volcanism tectonics cratering erosion
deposition of ices and volatiles) for comparative planetology and the
preparation for future lunar and planetary exploration.
@--------------------------------------------------------------------
Title: Magellanic Diffuse Interstellar Bands and Carbon
Chemistry
Authors: Ehrenfreund, Pascale; Cami, Jan; Foing, Bernard H.;
Kaper, Lex; Cox, Nick; Jimenez-Vicente, Jorge;
Salama, Farid; Sarre, Peter; Snow, Ted;
Maier, John Paul
Bibliographic Code: 2003IAUJD..21E...2E
Abstract
With the Ultraviolet Visual Echelle Spectrograph mounted at the Very
Large Telescope we have observed at unprecedented spectral resolution
the absorption spectrum toward reddened stars in the Magellanic Clouds
over the wavelength range of 3500-10500 Å. This range covers the
strong transitions associated with neutral and charged large carbon
molecules of varying sizes and structures. We report the first detection
of diffuse interstellar bands (DIBs) at 5780 and 5797 Å in the
Small Magellanic Cloud and the variation of the 6284 Å DIB toward
several targets in the Large Magellanic Cloud. The variation of DIBs in
the Magellanic Clouds compared with Galactic targets may be governed by
a combination of the different chemical processes prevailing in
low-metallicity regions and the local environmental conditions. The
analysis of high-resolution absorption spectra allows us to reveal the
global effects in the chemistry and recycling of cosmic dust in the
Magellanic clouds which are relevant for the chemical pathways forming
large organic molecules in external galaxies
@--------------------------------------------------------------------
Title: Observing stellar activity from space
Authors: Foing, B. H.; Neiner, C.
Bibliographic Code: 2003EAS.....9..147F
Abstract
In this paper we present a review of the past, current and future space
missions relevant for observing stellar activity from space. In the
past, missions were focused on UV and X-ray fluxes, variability and
spectroscopy. Currently coronal spectroscopy diagnostics are developed.
HST high resolution imaging in the visible and near IR give access to
circumstellar disks and outflows. The future space missions will
concentrate on space photometry (for asteroseismology, exoplanets search
and microvariability due to activity) and interferometry (for measuring
stellar sizes and environments).
@--------------------------------------------------------------------
Title: A survey of the PAH electronic spectra and their
search in the Interstellar Medium
Authors: Boudin, N.; Ruiterkamp, R.; Foing, B. H.
Bibliographic Code: 2003asdu.confE.162B
Abstract
The understanding of physical and chemical processes in the interstellar
medium is currently an important challenge for our Universe knowledge
since these processes are involved in the control of stars and planets
formation. Polycyclic Aromatic Hydrocarbons (PAHs) are now recognized as
an important constituent of the interstellar medium gaseous phase,
mainly through observations of their IR emission bands. This family of
molecules and in particular their ionic and radical derivatives seems to
be one of the most promising candidates for the identification of the
Diffuse Interstellar Bands (DIBs). These absorption bands, observed -
throughout the visible and near infrared spectral range - over spectra
of stars masked by gas cloud, were first discovered in 1922. Their
spectral properties indicate that DIBs could originate from gaseous
phase carbonaceous molecules. The identification of PAHs as molecules
responsible for these bands must be done through direct comparison with
PAHs spectra recorded in conditions as close as possible to those of the
interstellar medium.
An exhaustive survey of all the literature spectra of the PAHs in the
neutral or ionic (cation and anion) forms was achieved and will be
reported here, allowing us to find some trends among the PAH spectra:
for instance, concerning the band shift due to the interaction with the
matrix; concerning the distribution of transitions of a large amount of
PAH cations, through their PhotoElectron Spectra (N. Boudin, R.
Ruiterkamp and B. H. Foing, A&A, 2003). The advantages and drawbacks
of all the experimental techniques (PhotoElectron Spectroscopy, Matrix
Isolation Spectroscopy, gas phase techniques) will be discussed.
Concurrently, this large database allow us to search these laboratory
transitions in the astronomical spectra already published.
A follow up interdisciplinary work is required between astronomical
observations, laboratory matrix and gas phase spectroscopy, theoretical
work and modelling, and active experiments in space to study the
formation, evolution, survival and transport of these complex organics.
@--------------------------------------------------------------------
Title: Carbon chemistry and diffuse interstellar bands in
the Magellanic Clouds
Authors: Cox, Nick; Ehrenfreund, Pascale; Cami, Jan;
Kaper, Lex; Foing, Bernard; Cordiner, Martin;
Sarre, Peter; Snow, Ted; Salama, Farid
Bibliographic Code: 2003asdu.confE..43C
Abstract
To unravel the carbon chemistry prevailing in (diffuse) interstellar
clouds we seek to disentangle the different environmental effects that
influence the existence and strength of the diffuse interstellar bands
(DIBs). DIBs are weak unidentified interstellar absorption bands
observed towards reddened stars. Their carriers are presently believed
to be large carbonaceous molecules (e.g PAHs). The Large and Small
Magellanic Cloud (LMC and SMC) offer a unique opportunity to link DIB
behaviour to widely varying environmental conditions (e.g. metallicity,
UV radiation field and star formation activity). This in turn imposes
useful constraints on the nature of the DIB carrier, which hopefully
leads to its much desired identification.
To this aim we have observed the absorption spectra of reddened OB stars
in the Magellanic Clouds at unprecedented high resolution (R
≅100.000) and high S/N (>˜100) with the Ultraviolet Visual
Echelle Spectrograph (UVES) mounted at the Very Large Telescope (VLT).
These spectra provide the first observational evidence for the presence
of DIBs in the SMC (Ehrenfreund et al. 2002, ApJ, 576, L117). Analysis
of the spectra of the LMC and SMC targets indicates that a delicate
balance must exist for DIBs to be present. Noteworthy in this respect is
the 30 Doradus region in the LMC in which these special conditions seem
to prevail. Of all LMC stars observed, only the two situated in the 30
Dor region have detectable DIBs. This balance appears to be strongly
dependent on the UV radiation field, which is represented by the shape
of the extinction curve (i.e. the presence of the 2200Å bump and
the steepness of the far-UV rise).
@--------------------------------------------------------------------
Title: The SMART-1 X-ray solar monitor (XSM): calibrations
for D-CIXS and independent coronal science
Authors: Huovelin, J.; Alha, L.; Andersson, H.; Andersson, T.;
Browning, R.; Drummond, D.; Foing, B.; Grande, M.;
Hämäläinen, K.; Laukkanen, J.; Lämsä, V.;
Muinonen, K.; Murray, M.; Nenonen, S.; Salminen, A.;
Sipilä, H.; Taylor, I.; Vilhu, O.; Waltham, N.;
Lopez-Jorkama, M.
Bibliographic Code: 2002P&SS...50.1345H
Abstract
The X-ray solar monitor (XSM) is a calibration instrument of the
demonstration of compact imaging X-ray spectrometer (D-CIXS) experiment,
with a separate Silicon detector unit on the SMART-1 spacecraft. The
non-imaging HPSi PIN sensor has a wide field-of-view (FOV) to enable Sun
visibility during a significant fraction of the mission lifetime, which
is essential for obtaining calibration spectra for the X-ray
fluorescence measurements by the imaging D-CIXS spectrometer. The energy
range (1-20keV), spectral resolution (about 250eV at 6keV), and
sensitivity (about 7000cps at flux level of
10-4Wm-2 in the range 1-8Å) are tuned to
provide optimal knowledge about the Solar X-ray flux on the Lunar
surface, matching well with the activating energy range for the
fluorescence measured by D-CIXS. The independent science of the XSM will
also be valuable, since the XSM energy range is very sensitive to solar
flares. The countrate during the top of an X1 flare will be about 35
times higher than the average quiescent countrate at solar maximum. The
relative increase will be the same for an M1 flare during the SMART-1
mission, which will be closer to the next solar minimum. Since the XSM
will observe the Sun as a star, and the energy range and spectral
resolution are close to those of present astronomical X-ray satellites
(e.g., XMM-Newton, ASCA, Chandra), we will obtain an X-ray database of
the Sun which can be related with the stellar X-ray observations more
easily than the data from present solar X-ray instruments. In this
publication we give a detailed description of the design, performance,
and tasks of the XSM instrument, and view the science perspectives.
@--------------------------------------------------------------------
Title: SMART-1 mission description and development status
Authors: Racca, G. D.; Marini, A.; Stagnaro, L.;
van Dooren, J.; di Napoli, L.; Foing, B. H.;
Lumb, R.; Volp, J.; Brinkmann, J.; Grünagel, R.;
Estublier, D.; Tremolizzo, E.; McKay, M.; Camino, O.;
Schoemaekers, J.; Hechler, M.; Khan, M.;
Rathsman, P.; Andersson, G.; Anflo, K.; Berge, S.;
Bodin, P.; Edfors, A.; Hussain, A.; Kugelberg, J.;
Larsson, N.; Ljung, B.; Meijer, L.; Mörtsell, A.;
Nordebäck, T.; Persson, S.; Sjöberg, F.
Bibliographic Code: 2002P&SS...50.1323R
Abstract
SMART-1 is the first of the Small Missions for Advanced Research in
Technology of the ESA Horizons 2000 scientific programme. The SMART-1
mission is dedicated to testing of new technologies for future
cornerstone missions, using Solar-Electric Primary Propulsion (SEPP) in
Deep Space. The chosen mission planetary target is the Moon. The target
orbit will be polar with the pericentre close to the South-Pole. The
pericentre altitude lies between 300 and 2000km, while the apocentre
will extend to about 10,000km. During the cruise phase, before reaching
the Moon, the spacecraft thrusting profile allows extended periods for
cruise science. The SMART-1 spacecraft will be launched in the spring of
2003 as an auxiliary passenger on an Ariane 5 and placed into a
Geostationary Transfer Orbit (GTO). The expected launch mass is about
370kg, including 19kg of payload. The selected type of SEPP is a
Hall-effect thruster called PPS-1350. The thruster is used to spiral out
of the GTO and for all orbit maneuvers including lunar capture and
descent. The trajectory has been optimised by inserting coast arcs and
the presence of the Moon's gravitational field is exploited in multiple
weak gravity assists. The Development Phase started in October 1999 and
is expected to be concluded by a Flight Acceptance Review in January
2003. The short development time for this high technology spacecraft
requires a concerted effort by industry, science institutes and ESA
centres. This paper describes the mission and the project development
status both from a technical and programmatic standpoint.
@--------------------------------------------------------------------
Title: Lunar exploration
Authors: Foing, Bernard H.
Bibliographic Code: 2002P&SS...50.....F
Abstract
@--------------------------------------------------------------------
Title: MUSICOS 1998: Optical and X-rays Observations of
Flares on the RS CVn Binary HR 1099
Authors: García-Alvarez, D.; Doyle, J. G.; Foing, B. H.;
Oliveira, J. M.; Montes, D.
Bibliographic Code: 2002ASPC..277..479G, eprint = astro-ph/0110305
Abstract
We present simultaneous and continuous observations of H_alpha, H_beta,
NaI D_1, D_2 and HeI D_3 lines of the chromospherically active binary HR
1099. We have observed HR 1099 for more than 3 weeks almost continuously
and monitored two flares. An increase in H_alpha, CaII H & K,
H_beta, HeI D_3 and HeI lambda6678 and a strong filling-in of the NaI
D_1, D_2 and MgI b triplet during one of the flares are observed. We
have found that the flares took place at the same phase (0.85) of the
binary orbit, and both of them seems to occur near the limb. Several
X-rays flares were also detected by ASM on board RXTE. Rotational
modulation in the X-rays light curve has been detected with maximum flux
when the active K1IV star is in front.
@--------------------------------------------------------------------
Title: Laboratory Calibration Studies in Support of
ORGANICS on the International Space Station:
Evolution of Organic Matter in Space
Authors: Ruiterkamp, R.; Ehrenfreund, P.; Halasinski, T.;
Salama, F.; Foing, B.; Schmidt, W.
Bibliographic Code: 2002nla..work..149R
Abstract
This paper describes the scientific overview and current status of
ORGANICS an exposure experiment per- formed on the International Space
Station (ISS) to study the evolution of organic matter in space (P1: P.
Ehrenfreund), with supporting laboratory experiments performed at NASA
Ames. ORGANICS investigates the chemical evolution of samples submitted
to long-duration exposure to space environment in near-Earth orbit. This
experiment will provide information on the nature, evolution, and
survival of carbon species in the interstellar medium (ISM) and in solar
system targets.
@--------------------------------------------------------------------
Title: Complex carbon chemistry and the diffuse
interstellar bands in the Magellanic Clouds
Authors: Cox, N.; Ehrenfreund, P.; Cami, J.;
Jimenez-Vicente, J.; Foing, B. H.; Kaper, L.;
van der Meer, A.; D'Hendecourt, L.; Maier, J.;
Salama, F.; Sarre, P.; Snow, T.; Sonnetrucker, P.
Bibliographic Code: 2002ESASP.518..447C
Abstract
@--------------------------------------------------------------------
Title: Laboratory studies on complex organic molecules on
Mars. Part 2 - experimental set-up and related work
Authors: ten Kate, I. L.; Ruiterkamp, R.; Botta, O.;
Lehmann, B.; Gomez Hernandez, C.; Boudin, N.;
Foing, B. H.; Ehrenfreund, P.
Bibliographic Code: 2002ESASP.518...81T
Abstract
In 1976 the Viking missions arrived at Mars to search for traces of
extinct and extant life. Although this mission brought a range of
sophisticated instruments it neiter detected any traces of life, nor any
organic compounds in the Martian soil. Since it is still unclear why the
Viking landers did not detect any organic molecules, laboratory
experiments under simulated Martian conditions are crucial in support of
future life-seeking Mars missions. This paper describes ongoing
experiments investigating the stability of organic molecules in the
Martian soil. We present a short rationale, the experimental set-up and
approach and a description of the organic compounds that will be used
during the experiments. The research programme described in this article
is developed at the European Space Research and Technology Centre of
ESA, ESTEC and at Leiden University, in the frame of a Mars Express
Recognised Cooperating Laboratory RCL.
@--------------------------------------------------------------------
Title: Investigating complex organic compounds in a
simulated Mars environment
Authors: ten Kate, I. L.; Ruiterkamp, R.; Botta, O.;
Lehmann, B.; Gomez Hernandez, C.; Boudin, N.;
Foing, B. H.; Ehrenfreund, P.
Bibliographic Code: 2002IJAsB...1..387T
Abstract
Available from http://dx.doi.org/10.1017/S1473550403001277
@--------------------------------------------------------------------
Title: Preface (Earth-like planets and moons)
Authors: Foing, Bernard H.
Bibliographic Code: 2002ESASP.514D...7F
Abstract
These proceedings contain a selection of papers from 20 invited review
talks and 30 contributed oral or poster presentations given at the
ESLAB36 symposium on "Earth-like planets and moons", at ESTEC Noordwijk
on 3-8 June 2002. This covers bodies such as Earth, Mercury, Venus,
Mars, Moon, Vesta, Io, Europa, Ganymede, Callisto, Titan, Triton,
Pluto/Charon and terrestrial exoplanets. The goal is to understand their
observed similarities and differences, and give both an Earth-oriented
and a cosmic perspective. We reviewed the contribution of recent and
upcoming space missions to these studies. The programme was based on
comprehensive invited reviews, supported with interdisciplinary
contributed papers, and a large body of posters on specific results,
methods or planetary objects.
@--------------------------------------------------------------------
Title: Closing remarks on ESLAB36 symposium on "Earth-like
planets and moons"
Authors: Foing, Bernard H.; The Organisers Of Eslab36
Bibliographic Code: 2002ESASP.514..345F
Abstract
We give a summary of ESLAB36 symposium on "Earth-like planets and moons"
that took place at ESTEC, Noordwijk on 3-7 June 2002. The different
sessions included: - A family portrait of Earth-like planets and moons -
The contribution of space missions for understanding Earth-like planets
and moons - Earth as a planet - Methods for comparative planetology -
Interiors, surfaces, exospheres and impact processes - Comparing
atmospheres and fluids - Earth-like planets and moons in the galaxy -
Habitable Earth-like planets and moons - ESLAB Symposium summary and
roundtable discussion - Robotic and Human exploration - Young Planetary
Explorers (YPE) special session.
@--------------------------------------------------------------------
Title: Laboratory studies on complex organic molecules on
Mars. Part 1 - rationale
Authors: ten Kate, I. L.; Ruiterkamp, R.; Botta, O.;
Lehmann, B.; Gomez Hernandez, C.; Boudin, N.;
Foing, B. H.; Ehrenfreund, P.
Bibliographic Code: 2002ESASP.514..293T
Abstract
The search for organic molecules and traces of life is the future
perspective of several missions to Mars. In order to know what those
mission should be looking for, laboratory experiments under simulated
Mars conditions are necessary. Especially since the Viking mission did
not find any traces of organic compounds in the Martian soil. In this
paper the history of the search for life on Mars and the context of our
laboratory studies, are described. Furthermore it gives a short
description of the experiments. This paper is the first part of a series
of three papers. The second paper will describe the experiments and
methods, the third paper will be a status report. Both the second and
the third paper can be found in the proceedings of the Second European
Workshop on Exo/Astrobiology, ESA Special Publication SP-518.
@--------------------------------------------------------------------
Title: Lunar data simulations for SMART-1
Authors: Vilar, Eduard; Almeida, Miguel; Koschny, Detlef;
Foing, Bernhard H.
Bibliographic Code: 2002ESASP.514..101V
Abstract
The value of the data collected on a planetary mission does not depend
only on the data by itself or its amount, but also on its joint
analysis, comparison and integration with previous and/or expected data.
The SMART-1 mission has also been prepared to get an opportunity for new
science. We have done a search on the past missions that studied our
satellite, the Moon. Therefore, previous lunar missions like Luna,
Apollo, Hiten, Clementine or Lunar Prospector offer the possibility of
comparing the existing lunar databases. This also helps in selecting for
SMART-1 a wide range of luanr targets between the hundreds of Mares,
Sinus, Catenas and Craters. On the other hand, simulation is necessary
in order to reach this aim, and a simulation program has been developed
to plan the SMART-1 payload operations and to pre-evaluate SMART-1
representative data and science return. Finally, we discuss perspectives
how to enhance SMART-1 return in order to get the best results building
on the knowledge of the Past with the present ESA technology.
@--------------------------------------------------------------------
Title: Technology and science from Earth to Moon: SMART-1
experiments and their operations
Authors: Marini, A. E.; Lumb, R.; Racca, G. D.; Foing, B. H.;
Dias-Almeida, M.
Bibliographic Code: 2002ESASP.514...95M
Abstract
SMART-1, the first European mission to the Moon aimed at demonstrating
the Solar Electric propulsion hosts 10 Technology and Science
experiments. The monitoring of the spacecraft plasma environment and the
thruster contamination produced by thruster is carried out by SPEDE
(Spacecraft Potential, Electron and Dust Experiment) and EPDP (Electric
Propulsion Diagnostic Package). The miniaturised remote sensing
instruments on-board SMART-1 are: AMIE (Advanced Moon micro-Imager
Experiment), D-CIXS (Demonstration of a Compact Imaging X-ray
Spectrometer), supported in its operation by XSM (X-ray Solar Monitor),
and SIR (SMART-1 Infrared Spectrometer). Technology experiments for
deep-space communications and navigation are: KATE (Ka-Band TT&C
Experiment), based on X/Kaband transponder which also supports RSIS
(Radio-Science Investigations for SMART-1), Laser-link, demonstrating a
deep-space laser communication link and OBAN (On-Board Autonomous
Navigation experiment). The Experiments will be performed during two
distinct phases of the SMART-1 mission, including 17-month Earth escape
phase and a nominal 6-month operational phase in elliptical Moon orbit.
The SMART-1 STOC (Science and Technology Operations Co-ordination)
carries out the planning and co-ordination of the Technology and science
experiments.
@--------------------------------------------------------------------
Title: SMART-1 science experiments co-ordination
Authors: Almeida, M.; Foing, B.; Vilar, E.; Heather, D.;
Koschny, D.; Marini, A.
Bibliographic Code: 2002ESASP.514...55A
Abstract
SMART-1 is the first European Space Agency mission to the Moon, due for
launch in the first months of 2003. Its primary goal is to test new
technologies for space navigation and science. In its science
experiments, SMART-1 will include new, very compact experiments. This
paper aims to demonstrate some of the science experiment operations
foreseen for the mission. We describe the SMART-1 mission, its orbit and
example scenarios for imaging specific targets (such as Tycho and
Copernicus craters).
@--------------------------------------------------------------------
Title: Lunar missions: science and exploration
Authors: Foing, Bernard H.;
International Lunar Exploration Working Group
Bibliographic Code: 2002ESASP.514....3F
Abstract
Results from the recent US missions "Clementine" and Lunar Prospector,
will, in the near future, be used to prepare the ESA SMART-1 and
Japanese Lunar-A and SELENE missions to the Moon. The scientific results
of these missions will continue to answer open questions about the
origin of the Earth-Moon system, the early evolution of life, the
planetary environment and the existence of in-situ resources necessary
to support human presence (e.g. water, oxygen). These science and
technology missions can be considered as precursor missions for future
human exploration of the solar system.
@--------------------------------------------------------------------
Title: Earth-like Planets and Moons
Authors: Foing, Bernard H.; Battrick, Bruce
Bibliographic Code: 2002ESASP.514.....F
Abstract
Contents: The contribution of space missions for understanding
earth-like planets and moons. Earth as a planet & space experiments.
Methods for comparative planetology. Interiors, surfaces, exospheres and
impact processes. Impact interactions with planets and moons. Comparing
atmospheres and fluids (with emphasis on Earth, Mars, Venus, Titan,
Europa). Earth-like planets and moons in the Galaxy. Young planetary
explorers (YPE).
@--------------------------------------------------------------------
Title: Detection of Diffuse Interstellar Bands in the
Magellanic Clouds
Authors: Ehrenfreund, P.; Cami, J.; Jiménez-Vicente, J.;
Foing, B. H.; Kaper, L.; van der Meer, A.; Cox, N.;
D'Hendecourt, L.; Maier, J. P.; Salama, F.;
Sarre, P. J.; Snow, T. P.; Sonnentrucker, P.
Bibliographic Code: 2002ApJ...576L.117E
Abstract
With the Ultraviolet Visual Echelle Spectrograph mounted at the Very
Large Telescope, we have observed at unprecedented spectral resolution
the absorption spectrum toward reddened stars in the Magellanic Clouds
over the wavelength range of 3500-10500 Å. This range covers the
strong transitions associated with neutral and charged large carbon
molecules of varying sizes and structures. We report the first detection
of diffuse interstellar bands (DIBs) at 5780 and 5797 Å in the
Small Magellanic Cloud and the variation of the 6284 Å DIB toward
several targets in the Large Magellanic Cloud. The variation of DIBs in
the Magellanic Clouds compared with Galactic targets may be governed by
a combination of the different chemical processes prevailing in
low-metallicity regions and the local environmental conditions. Based on
observations made at the European Southern Observatory, Paranal, Chile
(ESO program 67.C-0281).
@--------------------------------------------------------------------
Title: Spectroscopy of large PAHs. Laboratory studies and
comparison to the Diffuse Interstellar Bands
Authors: Ruiterkamp, R.; Halasinski, T.; Salama, F.;
Foing, B. H.; Allamandola, L. J.; Schmidt, W.;
Ehrenfreund, P.
Bibliographic Code: 2002A&A...390.1153R
Abstract
Polycyclic Aromatic Hydrocarbons (PAHs) are thought to be the carriers
of the ubiquitous infrared emission bands (UIBs). Data from the Infrared
Space Observatory (ISO) have provided new insights into the size
distribution and the structure of interstellar PAH molecules pointing to
a trend towards larger-size PAHs. The mid-infrared spectra of galactic
and extragalactic sources have also indicated the presence of 5-ring
structures and PAH structures with attached side groups. This paper
reports for the first time the laboratory measurement of the UV-Vis-NIR
absorption spectra of a representative set of large PAHs that have also
been selected for a long duration exposure experiment on the
International Space Station ISS. PAHs with sizes up to 600 amu,
including 5-ring species and PAHs containing heteroatoms, have been
synthesized and their spectra measured using matrix isolation
spectroscopy. The spectra of the neutral species and the associated
cations and anions measured in this work are also compared to
astronomical spectra of Diffuse Interstellar Bands (DIBs).
@--------------------------------------------------------------------
Title: Automated detection of CMEs in LASCO data
Authors: Berghmans, D.; Foing, B. H.; Fleck, B.
Bibliographic Code: 2002ESASP.508..437B
Abstract
We have developed software that autonomously detects CMEs in image
sequences from LASCO. the crux of the software is the detection of CMEs
as bright ridges in (height, time) maps using the Hough transform. The
output is a list of events, similar to the classic catalogs, with
principle angle, angular width and velocity estimation for each CME. In
contrast to catalogs assembled by human operators, these CME detections
by software can be faster, which is especially important in the context
of space weather, and possibly also more objective, as the detection
criterion is written explicitly in a program. In this paper we describe
the software and validate its performance by comparing its output with
the visually assembled CME catalogs. We discuss its present success rate
(about 75%) and prospects for improvement. Finally, we show that the
software can also reveal CMEs that have not been listed in the catalogs.
Such unreported cases might be of influence on CME statistics and prove
that also the present catalogs do not have a 100% success rate.
@--------------------------------------------------------------------
Title: Non-radial pulsation, rotation and outburst in the
Be star omega Orionis from the MuSiCoS 1998 campaign
Authors: Neiner, C.; Hubert, A.-M.; Floquet, M.; Jankov, S.;
Henrichs, H. F.; Foing, B.; Oliveira, J.;
Orlando, S.; Abbott, J.; Baldry, I. K.;
Bedding, T. R.; Cami, J.; Cao, H.; Catala, C.;
Cheng, K. P.; Domiciano de Souza, A., Jr.;
Janot-Pacheco, E.; Hao, J. X.; Kaper, L.; Kaufer, A.;
Leister, N. V.; Neff, J. E.; O'Toole, S. J.;
Schäfer, D.; Smartt, S. J.; Stahl, O.; Telting, J.;
Tubbesing, S.; Zorec, J.
Bibliographic Code: 2002A&A...388..899N
Abstract
omega Ori (HD 37490, HR
1934) is a Be star known to have presented variations. In
order to investigate the nature and origin of its short-term and
mid-term variability, a study is performed of several spectral lines
(Halpha, Hdelta, ion {He}i 4471, 4713, 4921, 5876, 6678, ion {C}{ii}
4267, 6578, 6583, ion {Mg}{ii} 4481, ion {Si}{iii} 4553 and ion {Si}{ii}
6347), based on 249 high signal-to-noise high-resolution spectra taken
with 8 telescopes over 22 consecutive nights during the MuSiCoS (Multi
SIte COntinuous Spectroscopy) campaign in November-December 1998. The
stellar parameters are revisited and the projected rotational velocity
(vsin i = 179 km s-1) is redetermined using several methods.
With the MuSiCoS 98 dataset, a time series analysis of line-profile
variations (LPVs) is performed using the Restricted Local Cleanest (RLC)
algorithm and a least squares method. The behaviour of the velocity of
the centroid of the lines, the equivalent widths and the apparent vsini
for several lines, as well as Violet and Red components of photospheric
lines affected by emission (red ion {He}i lines, ion {Si}{ii} 6347, ion
{C}{ii} 6578, 6583) are analyzed. The non-radial pulsation (NRP) model
is examined using phase diagrams and the Fourier-Doppler Imaging (FDI)
method. The LPVs are consistent with a NRP mode with l = 2 or 3, |m| = 2
with frequency 1.03 c d-1. It is shown that an emission line
outburst occurred in the middle of the campaign. Two scenarios are
proposed to explain the behaviour of a dense cloud, temporarily orbiting
around the star with a frequency 0.46 c d-1, in relation to
the outburst. Based on observations taken during the MuSiCoS 98 campaign
at OHP (France), La Silla (ESO, Chile, ID 62.H-0270), Mount Stromlo
(Australia), Xinglong Station (China), Kitt Peak (USA), MCT/LNA (Brazil)
and INT (Isaac Newton Group, La Palma Island).
@--------------------------------------------------------------------
Title: SMART-1 Technology and Science Experiments and their
Operations
Authors: Marini, A.; Lumb, R.; Dias-Almeida, M.; Foing, B. H.
Bibliographic Code: 2002iaf..confE.713M
Abstract
SMART-1, the first European mission to the Moon, hosts 10 Technology and
science experiments run by 7 on-board instruments. The primary objective
of the mission is the demonstration of the solar electric propulsion.
Therefore the monitoring of the spacecraft plasma environment and the
contamination produced by the Stationary Plasma thruster is a key-task,
which will be carried out by two experiments (SPEDE - Spacecraft
Potential, Electron and Dust Experiment - and EPDP - Electric propulsion
diagnostic Package). SPEDE and EPDP will contribute also to the
characterisation of the near-Earth and interplanetary plasma environment
and to study the solar wind. A package of three spectroscopy and imaging
instruments has been selected to run technology demonstration of
miniaturised compact instrument for planetary remote sensing and for
carrying out valuable science at the Moon. AMIE (Asteroid-Moon
micro-Imager Experiment) is a miniature medium-resolution (30 m at 300
km height) camera, equipped with a fixed panchromatic and 3-colour
filter, for Moon topography and imaging support to other experiments.
D-CIXS (Demonstration of a Compact Imaging X-ray Spectrometer) is based
on novel detector and filter/collimator technologies, and will perform
the first global mapping of the lunar elemental composition, by looking
at X-ray fluorescence in the 0.5-10 keV range. It is supported in its
operation by XSM (X-ray Solar Monitor) that also monitors long-term
coronal X-ray emission and solar flares. SIR is a miniature
near-infrared spectrometer operating in the 0.9-2.6 mum wavelength
range and will carry out mineralogical survey of the lunar crust in a
previously uncovered bandwidth. Technology experiments for deep space
communications are: The SMART-1 Instruments have been integrated in the
Spacecraft in the current year and have undergone functional
verification following environmental tests. The Experiments will be
performed during two distinct phases of the SMART-1 mission, including:
- the 17-month Earth escape phase when the spacecraft will spiral out
our planet to perform a weak - a nominal 6-month operational phase in
elliptical Moon orbit with peri-centre around the south The planning and
co-ordination of the Technology and science experiments operations is
carried out at ESA/ESTEC, where an agile service has been set up to
connect and co-ordinate remotely the technology and science
experimenters and to provide the experiment master plan to the Mission
Operations Centre located at ESOC. The SMART-1 STOC (Science and
Technology Operations Co- ordination) facility works in close synergy
with the science operations teams of other ESA Planetary missions
(Rosetta, Mars Express and Bepi-Colombo), making use of Internet
communication and flexible scheduling and simulations tools. The SMART-1
STOC supports also the mission data archiving and is designed to provide
the engineering and scientist communities with mission data access based
on the PDS (Planetary Data System) Standard.
@--------------------------------------------------------------------
Title: Lunar Explorers Society: International Outreach
Programme
Authors: Volp, J.; Foing, B.; ten Kate, I.; Rombaut, H.;
Koppeschaar, C.; van Susante, P.; Pachera, S.;
Groemer, G.; Sanctuary, H.; Marshall, W.
Bibliographic Code: 2002EGSGA..27.6860V
Abstract
"Aiming for the permanent presence of humanity on the Moon."
The Lunar Explorers Society was founded in 2000 by the attendees of the
International Conference on Exploration and Utilisation of the Moon
(ICEUM-4) held at ESTEC, Noordwijk the Netherlands. LUNEX is a society
open to all lunar explorers. Interested individuals or organisations are
invited to become members or sponsors.
The main objectives of LUNEX are: - to promote the exploration of the
Moon for the benefit of humanity. - to raise awareness of what could be
achieved by returning to the Moon - to promote international cooperation
between scientists working on Lunar missions by providing a neutral
platform for their discussions
We want to reach as many people as possible, world-wide, with our
educational and outreach activities to explain our cause and its
benefits to humanity.
We will give an overview of LUNEX and the education and outreach
activities under- taken and planned by it's National Chapters.
http://www.lunarexplorers.org
@--------------------------------------------------------------------
Title: Science Operations For Esa's Smart-1 Mission To The
Moon
Authors: Almeida, M.; Foing, B.; Heather, D.; Marini, A.;
Lumb, R.; Racca, G.
Bibliographic Code: 2002EGSGA..27.5134A
Abstract
The primary objective of the European Space Agency's SMART-1 mission to
the Moon is to test and validate a new electric propulsion engine for
potential use on other larger ESA Cornerstone missions. However, the
SMART-1 spacecraft will also carry a number of scientific instruments
and experiments for use en-route to and in orbit about the Moon.
SMART-1's major operational constraint is that it will be only contacted
twice per week. As a result, there will be a stronger emphasis on
mid-term planning, and the spacecraft will be operated using a large
list of telecommands sent during the communication windows. This
approach leads to a higher probability of there being resource and/or
instruments conflicts. To eliminate these, two software tools were
developed: the Experiment Planning System (EPS), and the Project Test
Bed (PTB). These tools will also allow us to predict the lunar coverage
of the scien- tific instruments, and to simulate target selections.
@--------------------------------------------------------------------
Title: Public Outreach With Smart-1
Authors: Almeida, M.; Foing, B.; Heather, D.; Marini, A.;
Lumb, R.; Racca, G.
Bibliographic Code: 2002EGSGA..27.5132A
Abstract
SMART-1 will be the first European Space Agency mission to the Moon.
Therefore it is possible to foresee that any public outreach activity
related to the mission can have a big impact in the media and public in
general. This expectation for a large audience carries with it the large
responsibility to create a program where is maximized the quality, both
didactic and ludic, of the public outreach products, in order to keep
the interest in the mission for a longer period. In order to assure the
good quality of these products it is important that even when planning
the mission some of the targets are selected for its rich outreach
content. This presentation will focus on some of the public outreach
activities envisaged for SMART-1 as well as the selection of the most
suitable targets for that end.
@--------------------------------------------------------------------
Title: Smart-1 Science Experiments Co-ordination and
Expected Outputs
Authors: Almeida, M.; Foing, B.; Heather, D.; Marini, A.;
Lumb, R.; Racca, G.
Bibliographic Code: 2002EGSGA..27.5101A
Abstract
SMART-1 is the first European Space Agency mission to the Moon. The
primary ob- jective of the mission is to test and validate a new
electric propulsion engine for poten- tial use on other larger ESA
cornerstone missions. However the SMART-1 spacecraft will also carry a
number of scientific instruments and experiments for use en-route to and
in Orbit about the Moon. The payload comprises several instruments and
ex- periments: the Asteroid Moon Micro Imager Experiment (AMIE), the
Demonstration Compact Imaging X-ray Spectrometer (D-CIXS), the X-ray
Solar Monitor (XSM), the SMART-1 Near-Infrared Spectrometer (SIR), the
Electric Propulsion Diagnostic Package (EPDP), the Deep Space X/Ka Band
TTC Experiment (KaTE), the Radio Science Investigation for SMART-1
(RSIS), and the Spacecraft Potential, Electron and Dust Experiment
(SPEDE). During Lunar Orbit, the great majority of scientific activ-
ities will be carried out. The AMIE multispectral high resolution camera
will mainly aim to image the lunar South Pole and map the southern
regions of the Moon. D-CIXS will look for the spatial distribution of
major lunar rock types and the X-ray emission from impact of solar wind
electrons on the night-side Moon. SIR will gather data to study the
mineralogy of the lunar surface. During this phase the RSIS experiment
will also take place, using AMIE images and the high accuracy tracking
provided by KaTE to measure the lunar libration. Also in the frame of
the mission a co-ordinated utilization of the experiments is envisaged.
The Science and Technology Operations Co-Ordination (STOC) will be in
charge of this task. The STOC will, in face of the capabilities of the
experiments, advise experiments teams, to study specific features of the
Moon at the same time. The data acquired this way, when cross-checked,
will be able to produce higher value results. The STOC will also study
SMART-1 data in comparison with former Moon data. Examples of these
activities and what enhanced science results can be obtained will be
presented.
@--------------------------------------------------------------------
Title: Exoplanets and Formation of Planetary Systems:
Studies With Esa Science Missions
Authors: Foing, B. H.
Bibliographic Code: 2002EGSGA..27.5074F
Abstract
Several space missions from the ESA Science Horizons 2000 Programme
address key questions on the formation/evolution of planetary systems
and on the study of ex- oplanets: - How do solar systems form? (with
HST, ISO, NGST, FIRST/Herschel, Rosetta, Gaia) - Geological evolution of
terrestrial planets (with Living planet, Mars- express, SMART-1,
Venus-express, Bepi-Colombo) - History and Role of impacts (with
SMART-1, Bepi-Colombo, outer planets missions) - How to detect other
solar systems and habitable zones (with space photometry, COROT,
Eddington, Gaia, Dar- win) - Water and ices on other planets and comets
(with instruments on Mars Express, Rosetta and other planetary missions)
- Signature of biosphere and photosynthesis evolution (living Planet
missions, Darwin)
We shall review how the results from these ESA missions (and other
relevant missions from other agencies) can be exploited in synergy to
advance our knowledge on the formation of solar systems and on
exoplanets.
@--------------------------------------------------------------------
Title: Introduction To Ere5 Special Session "challenges And
Outreach In Geophysics For Young Geoscientists"
Authors: Foing, B. H.
Bibliographic Code: 2002EGSGA..27.4932F
Abstract
The ERE5 special session "Challenges and Outreach in Geophysics" will
start with re- view lectures, complemented by short poster
presentations, on the different topics: 0- Introduction on "Challenges
and Outreach in Geophysics" 1- Challenges in Prospec- tion of subsurface
Mineral and Energy resources 2- Challenges in Hydrology studies and
water management 3- Challenges in Climate studies and Global change 4-
Chal- lenges in prediction of and prevention from geophysical hazards 5-
Challenges in Geo- physical technologies and instrumentation 6-
Challenges in Solar system exploration It will continue with an open
discussion forum including: 7- a brainstorming session led by young
participants on these topical challenges, with special emphasis on "So-
cial benefits, Outreach and Education in Geophysics" 8- the formulation
of a series of recommendations by young geo scientists (YGS) 9-
presentation and selection by session participants of the
recommendations to be carried to other EGS sessions 10- the discussion
and preparation of an EGS2002 Young Geo-Scientists declaration
@--------------------------------------------------------------------
Title: Introduction To Ere4/ps Session On "risk Assesment
And Implications Of Near Earth Object Impacts"
Authors: Foing, B. H.
Bibliographic Code: 2002EGSGA..27.4926F
Abstract
The ERE4/PS session "Risk assessment and Implications of Near Earth
Object Im- pacts" will cover in particular the following topics:
Origin of Near Earh Objects, orbital dynamics, and collision
probabilities Proper- ties of Near Earth Objects In situ space
investigations of Near Earth Objects Studies of impact craters and
Historical events Simulations of Impact effects on at- mosphere,
biosphere and humans International Programmes for ground and space-
based detection Risk assessment and strategies for prevention and
mitigation
The session will include invited papers, as well as contributed oral,
and poster presen- tations.
@--------------------------------------------------------------------
Title: Ground Support Programme For Future Mars Missions
Authors: ten Kate, I. L.; Ruiterkamp, R.; Lehmann, B.;
Gomez Hernandez, C.; Foing, B. H.; Becker, L.;
Berstein, M.; Jessberger, E.; Ehrenfreund, P.
Bibliographic Code: 2002EGSGA..27.4768T
Abstract
The search for organic molecules and tracers of life on Mars is the
future perspective of several Mars missions. The experimental research
programme described here in- vestigates the most abundant organic
molecules identified in solar system bodies and beyond, which may have
been exogeneously delivered to the Martian surface.
A vacuum chamber, located at ESTEC, NL, equipped with a solar simulator
will be used to collect data on the combined effects of UV
photoprocessing, atmospheric con- ditions and the presence/absence of
oxidzing agents on organic molecules. The cham- ber has a possibility of
thermal and pressure control. A window allows the attachment of UV lamps
and filters. Samples will be introduced into the chamber on a specially
designed tray. Sample trays will be filled with organic molecules
embedded in soil analogues, either porous or compact. During the
simulation in situ measurements are taken in the chamber, using a GCMS.
Samples will be retrieved with various deriva- tization techniques.
Thereafter the probes are subjected to various analyses, such as HPLC,
spectroscopy, GC, LDMS and TOF-SIMS.
The results of those simulations are part of a ground support experiment
programme for future Mars missions.
@--------------------------------------------------------------------
Title: Complex Organics On Mars
Authors: ten Kate, I. L.; Ruiterkamp, R.; Lehmann, B.;
Gomez Hernandez, C.; Foing, B. H.; Ehrenfreund, P.
Bibliographic Code: 2002EGSGA..27.4134T
Abstract
One of the key questions in Astrobiology is to search for organic
molecules and to characterise their survival in Martian rocks and in the
Martian subsurface. The most relevant molecules in this context, which
can be studied in the laboratory are organic compounds identified in
meteorites. Among those are aliphatic and aromatic hydrocar- bons, amino
acids, polycyclic aromatic hydrocarbons (PAHs), fullerens and kerogens.
Using a Mars simulation chamber, we will study those prebiotic and large
stable car- bon compounds embedded in Martian soil analogues. To perform
the above described tasks the chamber will be equipped with a sample
tray, a solar simulator and will be able to serve as a glovebox. The
chamber will be used to validate some measurements to be made by Beagle
2 with representative or complementary ground instruments. The results
of the simulation studies will be compiled in a database to serve the
inter- pretation of future Mars missions.
@--------------------------------------------------------------------
Title: Smart-1 Project Development Status
Authors: Racca, G. D.; Foing, B. H.; The SMART-1 Project Team
Bibliographic Code: 2002EGSGA..27.1152R
Abstract
SMART-1 is the first of the Small Missions for Advanced Research in
Technology of the ESA Horizons 2000 Science Plan. The main mission
objective of SMART-1 is to demonstrate key technologies for Bepi-Colombo
and other scientific deep-space missions. One of the key technologies is
the solar electric propulsion used as primary propulsion. The electric
propulsion will be using 1400W to transfer the 350 kg space- craft from
an Ariane-5 standard GTO to an elliptic Moon polar orbit, 10000x300 km.
The total mission time is 24 months including a maximum of 18 months
transfer time. The spacecraft development entered the detailed design
and implementation phase in October 1999, under the responsibility of
the Swedish Space Corporation as prime contractor, and the flight
acceptance is targeted for the end of 2002. Apart from the in-orbit
demonstration of electric propulsion as primary propulsion, SMART-1 is
im- plementing many other enabling technologies for deep-space missions.
In addition, the spacecraft avionics design is tailored to the low cost
philosophy by enabling flexi- ble integration of Commercial Off The
Shelf (COTS) equipment. The scientific instru- ments support the
characterisation of the electric propulsion thrust environment during
the long transfer phase and detailed imaging and spectroscopy of the
lunar surface in visible, infrared and X-ray during the Moon orbiting
phase. The paper summarises the baseline mission and spacecraft design.
The main part of the paper highlights the spacecraft design status and
the assembly, integration and verification activities.
@--------------------------------------------------------------------
Title: Photometric studies of the Moon with AMIE/Smart-1
Authors: Shkuratov, Y.; Kreslavsky, M.; Foing, B.
Bibliographic Code: 2002cosp...34E1510S
Abstract
Three different directions of photometric studies with AMIE camera of
Smart-1 mission might be possible: (1) mapping slope of phase function
to search for photometric anomalies; (2) studying the opposition spike;
and (3) detailed study of photometric function in tracking mode of
Smart-1. The first direction allows studies of photometric anomalies
related with fresh impact craters with implications for estimates of the
regolith gardening rate and projectile flux in recent epoch;
investigations of regolith structure anomalies associated with swirls;
searching for traces of geologically recent seismic events. The second
direction makes it possible to study regional variations of the
characteristic soil particle size and particle aggregate structure. The
third one (tracking mode) allows us to study subtle characteristics of
photometric function that gives information about meso-scale structure
of the lunar surface. Specific demands for the photometric studies are
the following. At least 2 i ages of the same scene are needed to provide
the firstm direction. The best choice of the phase angles: 10-20°
for one of images and 30-50° for the other one. The phase angle
difference should be >15° but < 30° One of the images can
be taken from the Clementine data set, though pairs of AMIE images are
preferable. Only Clementine images without compression losses can be
used for this. Two images of the same scene are needed to study the
opposition spike. One of them should contain the zero phase angle point.
The other should be taken at a phase angle 10 - 40° One of the
images can be taken from the Clementine data set. The tracking mode
assumes taking a set of AMIE images for the same scene while the
spacecraft is moving along its orbits. Including the zero phase angle
point into the imaging sequence would increase the scientific output of
the tracking mode series of images. Flat surface is necessary for
photometric mapping with AMIE. Regions for mapping with the highest
priority are the Apollo-11, -12, -14, and -16 landing sites; the
tracking mode is desirable in these cases. The prospective regions are
also: Surveyor and Luna landing sites, swirls, selected typical mare
areas, and sites that have been imaged with Clementine in the
opposition.
@--------------------------------------------------------------------
Title: Astrobiology with ESA Science Missions
Authors: Foing, B. H.
Bibliographic Code: 2002ASPC..269..361F
Abstract
@--------------------------------------------------------------------
Title: The D-CIXS X-ray spectrometer, and its capabilities
for lunar science
Authors: Grande, M.; Dunkin, S.; Heather, D.; Kellett, B.;
Perry, C. H.; Browning, R.; Waltham, N.; Parker, D.;
Kent, B.; Swinyard, B.; Fereday, J.; Howe, C.;
Huovelin, J.; Muhli, P.; Hakala, P. J.; Vilhu, O.;
Thomas, N.; Hughes, D.; Alleyne, H.; Grady, M.;
Russell, S.; Lundin, R.; Barabash, S.; Baker, D.;
Clark, P. E.; Murray, C. D.; Christou, A.; Guest, J.;
Casanova, I.; D'Uston, L. C.; Maurice, S.; Foing, B.;
Kato, M.
Bibliographic Code: 2002AdSpR..30.1901G
Abstract
@--------------------------------------------------------------------
Title: SMART-1 technology preparation for future planetary
missions
Authors: Marini, A. E.; Racca, G. D.; Foing, B. H.
Bibliographic Code: 2002AdSpR..30.1895M
Abstract
SMART-1 is the first ESA Small Mission for Advanced Research in
Technology, with the prime objective of demonstrating the use of Solar
Electric Primary Propulsion in a planetary mission. Further to this,
SMART-1 will test novel spacecraft technologies and will host six
instruments carrying out nine technology and science experiments, all
aimed at preparing future ESA Cornerstones, including the ESA Mercury
Cornerstone (now named BepiColombo) and other future planetary missions
under study, as well as solar and fundamental physics missions.
@--------------------------------------------------------------------
Title: Preface
Authors: Foing, Bernard H.; Heather, David
Bibliographic Code: 2002AdSpR..30.1867F
Abstract
@--------------------------------------------------------------------
Title: Space activities in exo-astrobiology
Authors: Foing, Bernard H.
Bibliographic Code: 2002abqc.book..389F
Abstract
A brief overview is given about astronomical (NGST, GAIA, COROT,
EDDINGTON, KEPLER and DARWIN) and planetary (CASSINI-HUYGENS, STARDUST,
ROSETTA, MARS-EXPRESS and future Mars missions, Europa missions, Moon,
Mercury missions) space missions, which will investigate astrobiological
aspects during their operation phase.
@--------------------------------------------------------------------
Title: An elemental abundance analysis of the mercury
manganese star HD 29647
Authors: Adelman, S. J.; Snow, T. P.; Wood, E. L.;
Ivans, I. I.; Sneden, C.; Ehrenfreund, P.;
Foing, B. H.
Bibliographic Code: 2001MNRAS.328.1144A
Abstract
The sharp-lined mercury manganese (HgMn) star HD 29647, which is located
behind the outer envelope of the Taurus Molecular Cloud 1, is of
interest for both its stellar properties and its utility as a probe of
interstellar gas and dust along its line of sight. In this paper we
review the properties of the star, summarize its line identifications
and present an abundance analysis based on spectrograms obtained at the
McDonald Observatory and the Observatoire de Haute-Provence. This star
has elemental abundances similar to those of other HgMn stars except
that its He/H ratio is closer to solar, possibly indicating a young age,
and that it, like HR 7775, is overabundant in selected elements
including the rare earths. The stellar radial velocity, unfortunately,
closely matches that of the foreground cloud.
@--------------------------------------------------------------------
Title: Characteristics of the Plasma Environment for the
SMART-1 Mission
Authors: Laakso, H.; Foing, B.
Bibliographic Code: 2001ESASP.476..601L
Abstract
@--------------------------------------------------------------------
Title: Modelling of the Electric Propulsion Induced Plasma
Environment on SMART-1
Authors: Tajmar, M.; Gonzalez, J.; Foing, B.; Marini, A.;
Noci, G.; Laakso, H.
Bibliographic Code: 2001ESASP.476..575T
Abstract
@--------------------------------------------------------------------
Title: The Diffuse Interstellar Bands and Organic Molecules
in Space
Authors: Ehrenfreund, P.; Tuairisg, S. Ó.; Foing, B. H.;
Sonnentrucker, P.; Cami, J.
Bibliographic Code: 2001bbbb.conf..150E
Abstract
@--------------------------------------------------------------------
Title: "Organics" experiment on the International Space
Station
Authors: Ruiterkamp, Richard; Ehrenfreund, Pascale;
Foing, Bernard; Salama, Farid
Bibliographic Code: 2001ESASP.496..137R
Abstract
In this experiment, large organics will be exposed on a long duration
radiation facility on the International Space Station. The results of
this experiment will help us to identify specific carbonaceous molecules
in the interstellar medium (ISM) and to monitor their evolution and
possible incorporation into Solar System material. The results also
allow us to make predictions concerning the survival probabilities of
specific organic species in space.
@--------------------------------------------------------------------
Title: Exo-astrobiology with ESA space science missions
Authors: Foing, Bernard H.
Bibliographic Code: 2001ESASP.496..121F
Abstract
Key questions of astrobiology can be addressed by several space missions
from the ESA Science Horizons 2000 Programme, such as: How do solar and
stellar systems form? (with ISO, FIRST, SMART-1, Rosetta, Colombo,
Gaia). Geological evolution of terrestrial planets (with Living planet,
Mars-express, SMART-1, Bepi-Colombo to Mercury). Interstellar Complex
organic chemistry (with ISO, ISS/EXPOSE, FIRST, Rosetta). Co-evolution
of Earth-Moon, impacts life frustration (with SMART-1, Bepi-Colombo).
How to detect other solar systems and habitable zones (with space
photometry, COROT, Eddington, Gaia, IRSI-Darwin). Early Earth and
alternative environments (Huygens/Cassini and Mars-express). Signature
of biosphere, global biomarkers and photosynthesis evolution (living
Planet missions, Darwin). Water and exobiology on Mars (with orbiter
instruments and Beagle-2 lander on Mars-express). Study of biomarkers
and delivery of organics (with Mars-express and future missions). We
shall review the exo-astrobiology potential from these ESA missions.
@--------------------------------------------------------------------
Title: Outreach and Education from ESA's SMART-1 Mission to
the Moon
Authors: Heather, D. J.; Foing, B. H.; van Susante, P.;
Almeida, M.
Bibliographic Code: 2001LPI....32.1983H
Abstract
We present some of the possible outreach and education activities that
are being considered for use during ESA's SMART-1 mission to the Moon,
including 'adopt a crater', 'illuminating poles' and others. Packages
will be produced for all levels.
@--------------------------------------------------------------------
Title: Next Steps for International Lunar Exploration
Authors: Foing, B. H.; Duke, M.; Galimov, E.; Mizutani, H.;
Ilewg
Bibliographic Code: 2001LPI....32.1827F
Abstract
We report activities and recommendations from the conferences organised
by ILEWG International Lunar Exploration Working Group. This covers
science questions, technology, data exchange, resources utilisation, the
Moon as step to Mars and solar system exploration.
@--------------------------------------------------------------------
Title: ESA'S SMART-1 Mission to the Moon
Authors: Foing, B. H.; Heather, D.; Almeida, M.; Racca, G.;
Marini, A.; The SMART-1 Team
Bibliographic Code: 2001LPI....32.1787F
Abstract
ESA's SMART-1 technology mission is to be launched at the end of 2002,
to reach the Moon with Solar Electric Propulsion. Its visible
multicolour camera, near IR spectrometer, an X-ray spectrometer will
address current key questions of lunar and planetary science.
@--------------------------------------------------------------------
Title: Results and Recommendations from the International
Conference on the Exploration and Utilisation of the
Moon 4 (ICEUM4)
Authors: Foing, B. H.; Heather, D. J.; Duke, M.; Racca, G.;
Pieters, C.; Mizutani, H.; Galimov, E.;
Dunkin, S. K.; van Susante, P.; Frischauf, N.;
Almeida, M.; Participants, Iceum4
Bibliographic Code: 2001LPI....32.1712F
Abstract
We present here highlights and recommendations from the ILEWG organized
ICEUM4 meeting held in the Netherlands in July 2000
@--------------------------------------------------------------------
Title: Lunar Explorers Society: Goals And Activities
Authors: Foing, B.; Van Susante, P.; Almeida, M.; Heather, D.;
Duke, M.; Dunkin, S.; Lunar Explorers Society
Bibliographic Code: 2001EM&P...85..533F
Abstract
The Lunar Explorers Society (LUNEX) was founded by the participants of
the 4th International Conference on the Exploration and Utilisation of
the Moon (ICEUM4), held in July 2000 at the European Space Research and
Technology Centre (ESTEC) in The Netherlands. ICEUM4 was organised under
the auspices of the International Lunar Exploration Working Group
(ILEWG), and aimed to draw together people from diverse backgrounds with
a common interest in the exploration of the Moon. At the end of the
conference, a formal ICEUM4 Declaration was drawn up detailing the
recommendations of the participants for the future of lunar exploration.
LUNEX will be a society open to all Lunar Explorers and will aim to
promote research, exploration and outreach programmes that will work
towards the realisation of the goals outlined in the ICEUM4 Declaration.
Following ICEUM4, a core group of active LUNEX members was identified to
begin to shape the new-born society with guidance from ILEWG. A series
of task groups have been installed to address the key LUNEX issues, with
strong participation of young lunar explorers, and work is progressing
towards the first LUNEX activities, both at the level of the task groups
and to form national chapters. The first LUNEX convention will be held
in March 2001, starting in Paris with the opening session, then
continuing in Houston at the LPSC and closing in Nice during the
EGS-conference. Further information about the Lunar Explorers Society
can be found on our Website: http://www.lunarexplorers.org
@--------------------------------------------------------------------
Title: The Science Goals Of Esa's Smart-1 Mission To The
Moon
Authors: Foing, B. H.; Heather, D. J.; Almeida, M.;
Science Technology Working Team, Smart-1.
Bibliographic Code: 2001EM&P...85..523F
Abstract
SMART-1 will be Europe's first lunar mission and represents an important
step forwards in developing an international program of lunar
exploration. The spacecraft will be ready for launch in late 2002, and
is designed to test new technologies for use on future ESA cornerstone
missions. In this respect, SMART-1 will also play a vital role in
developing cutting edge technologies that could be a major part of the
future of lunar and planetary science. SMART-1 will carry three remote
sensing instruments that will be used during the mission's nominal six
months in lunar orbit. These instruments will return data that will be
relevant to a broad range of lunar studies, from bulk crustal
composition and theories of lunar origin/evolution to the search for
cold traps at the lunar poles and the mapping of potential lunar
resources. With a perilune near the lunar south pole, the South
Pole-Aitken Basin (SPA) is a prime target for studies using the SMART-1
suite of instruments.
@--------------------------------------------------------------------
Title: Smart-1: The First Time Of Europe To The Moon;
Wandering in the Earth-Moon Space
Authors: Racca, Giuseppe D.; Foing, Bernard H.;
Coradini, Marcello
Bibliographic Code: 2001EM&P...85..379R
Abstract
After 40 years from the first lunar missions, Europe has started for the
first time the development of a mission which has the Moon as a target.
SMART-1 will be the first Western-European mission to the Earth's
satellite. The primary objective of the mission is to flight test
technology innovation for the future scientific deep-space missions.
This paper describes the mission concept, the technology and the
scientific aspects.
@--------------------------------------------------------------------
Title: Highlights from ICEUM4, the 4th International
Conference on the Exploration and Utilisation of the
Moon
Authors: Foing, B. H.; Duke, M.; Galimov, E.; Mizutani, H.;
Pieters, C.; Racca, G.; Heather, D. J.;
Frischauf, N.; van Susante, P.; Almeida, M.
Bibliographic Code: 2001EM&P...85..133F
Abstract
The Fourth International Conference on the Exploration and Utilisation
of the Moon (ICEUM4) at ESTEC in July 2000 was organised by the
International Lunar Exploration Working Group (ILEWG) and ESA. The
conference had a broad content including future missions such as ESA's
SMART-1 mission and the Japanese Lunar-A and SELENE projects, technology
support for these missions, the recent advances in science of the Moon,
human development of the Moon, and public outreach. The proceedings of
the conference have been published as ESA Publication ESA SP-462 and an
official declaration from the conference has been constructed from
recommendations made by task groups set up at the conference. The
declaration will be used as a focus for the efforts of the Lunar
Explorers Society (LUNEX), which was founded during the meeting.
Progress will be reported at ICEUM5, to be held as part of the World
Space Congress in Houston in October 2002.
@--------------------------------------------------------------------
Title: Spectral Line Variability in the Circumstellar
Environment of the Classical T Tauri Star SU Aurigae
(CD-ROM Directory: contribs/oliveira)
Authors: Oliveira, J. M.; Foing, B. H.; Unruh, Y. C.
Bibliographic Code: 2001ASPC..223..539O
Abstract
@--------------------------------------------------------------------
Title: MUSICOS Observations of the Chromospherically Active
Binary Star EI Eridani
Authors: