Italy's Plans for Moon Exploration

ItalyItaly’’ss PlansPlans forfor MoonMoon ExplorationExploration Sylvie Espinasse Italian Space Agency

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Italy’s Plans for Moon Exploration

• National Programme for robotic Exploration • Human Exploration

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 National Programme for Moon Exploration

• In 2005, ASI Top Management proposed to the government to elaborate a National Programme for Moon Exploration and this has been approved by the Italian government in 2006 as one of the main element of the National AeroSpace Plan 2006-2008.

• Last year ASI has issued an AO to carry out 13 studies, 3 for science and 10 for technologies to elaborate the national “Vision for Moon Exploration”, 16 studies have been awarded.

• These studies are now concluded, the roadmap will be available by the end of October for presentation to ASI Top Management.

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 National Programme for Moon Exploration

• Moon Science and Resources + Earth Observation + Observation of the Universe

>>> Scientific Objectives >>> Measurements >>> Requirements • PLs: Optical Remote sensing + High Energy + In-situ sensing + Microwave

>>> Mass, Power, Data Budget,… • Launcher + Transfer Module + Orbiter + Descent and Landing System + High Mobility Vehicle + Robotics

>>> Missions Scenarios • ASI >>> Roadmap

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 National Programme for Moon Exploration

• More than 60 industries and institutes among Prime Contractors and Sub-Cos were involved in the process. • Mainly all Italian space industries together (7 large Italian companies, 18 SMEs, 1 European non Italian company, 2 consortium for 6 SMEs). • For some SMEs, it was their first experience of working with ASI. • Academic institutions: 12 universities, CNR (3 institutes), INFN and INAF institutes involving more than 30 scientists for the study Moon science and resources, 35 for the study of observation of the Universe and 25 for the study of Earth observation. LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 National Programme for Moon Exploration

• The Programme is science driven: 1. Define the scientific objectives 2. Identify the key measurements and related requirements to meet those objectives 3. Prioritise the objectives

Input for technological studies

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Moon Origin and evolution

SCIENCE SUB THEMES SCIENCE AND DETAILED SCIENCE MEASUREMENTS Requirements Sensitivity Coverage/resplution TECHNOLOGY OBJECTIVES THEMES OBJECTIVES Range Value Unit Value Unit Value Unit

Global 1-10 Km Map of Si, Al, Mg, X-Ray Spectra of 0.5- Coverage at 100 Km Moon Ca Fe, Na, O, C highlands and Maria 20 keV <200 eV altitude global Global 1-10 Km composition Map of olivines/ VIS-IR Spectra of Coverage at 100 Km pyroxenes highlands and Maria 0.3-5 μm 10 nm altitude

Regional 1-10 Km Coverage at 100 Km altitude Mapping VIS-IR Spectra Magma distribution and Maria Ocean relative abundance Model of mafic mineral 0.3-5 μm 10 nm origin and plagioclase global and composition evolution Local coverage VIS-IR Spectra Constrain Maria samples Theories of sampling the origin of composition of 0.3-5 μm 10 nm in situ the lunar different location of X-Ray diffratometric Local upper lunar maria analysis coverage in situ mantle Local Raman spectra coverage in situ

VIS-IR Spectra of origin and composition of central peaks Local evolution of different crater 0.3-5 μm 5 nm coverage < 100 m Lunar Crust central peaks

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 CMB Polarisation

SUB SCIENCE AND DETAILED SITE MEASUREMENTS Operative Sensitivity Operative Angular Spectral FoV THEME TECHNOLOG SCIENCE resolutio resolutio S Y OBJECTIVES Range Temperature n n OBJECTIVES

Value Uni Value U Value Un

t nit it CMB Stokes’ Correlation To minimise Radiometers Pointi 10-100 GH <0.1 20-30 K 1 20% >10e4 2 polarisati parameter modes the with InP ng z mK arcmin@ deg 1/2 on maps, instrumental LNAs sec 100 noise and RF (HEMT) GHZ for (E and B cosmological Inflation and using OMT and interferences, CMB mode) models primordial the for splitting Scann verification, quantum ing experiment the two high frequency fluctuations, should be orthogonal polarisation structure located in a polarisation of surveys. formation, shaded crater the incoming reionisation, on the dark radiation. cosmological side of the Cross- parameters, Moon polarisation particle less than physics. 40/50 dB. and mm and sub- Bolometer 100- GH 100 m gravitati mm optics and arrays using 1000 z K onal large focal OMT for waves plane detector splitting the arrays. two Interferometric orthogonal systems polarisation of the incoming radiation.

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Vegetation Monitoring

SCIENCE AND Spatial TECHNOLOGY coverage OBJECTIVES DETAILED SCIENCE Spectral Sensitivity and Temporal OBJECTIVES Spectral range resolution (minimum) resolution resolution Carbon cycle; Net Leaf Area Index-LAI, FPAR, Light 400-2500 nm VIS 2 nm 12 bit Primary Production Use Efficiency and other related IR 20 nm Global; From 1 h to vegetation indices programmable <1x1km2 daily Global land cover Cover type and extent Desertification processes

Typical reflectance spectrum of vegetation

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Summary of the proposals

• Observation of the Universe: ¾ γ rays-X rays >>> 4-9 experiments ¾ UV-Vis-IR >>> 5-6 experiments ¾ Radioastronomy and microwave >>> 4 experiments ¾ Fundamental physics and Particles >>> 10 experiments Total: 29 experiments • Earth Observation: ¾ Atmosphere >>> 4 experiments ¾ Oceans >>> 6 experiments ¾ Vegetation, biomasse >>> 9 experiments ¾ Radiation Balance >>> 12 experiments ¾ Earth SAR remote sensing >>> 5 experiments ¾ Georeferentiation >>> 5 experiments Total: 41 experiments

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 … towards the roadmap

– Scientific objectives and requirements issued by the 3 scientific studies – Priorities – Technological studies:

• 15 yrs

• Italian capabilities : – VEGA launcher + electric propulsion / other launchers – Orbiter carrying 100 kg of scientific P/L in polar orbit 100 km x 100 km or 100 km x 20.000 km (1.061 / 606 days cruise) – Descent and Landing Module delivering 90-110kg of P/L at the Lunar surface (14 days P/L support for Power and TLC) – Robotics capabilities Pre-selection Final Decision International Collaboration (we are here!) ROADMAP LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Study of the Moon and its resources

• Phase 1 – Analysis of the main open questions – Definition of the scientific themes to be further investigated

– Critical review of the data available and identification of the new

measurements to be performed

• Phase 2 – Definition of the measurements requirements • Phase 3 – Definition of an exploration strategy taking into account the new missions planned >>> missions scenario

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Study of the Moon and its resources

• Despite the data sets available from previous missions, (mainly low resolution and partial coverage remote sensing data or samples from the equatorial zone), the origin, evolution and internal structure of the Moon are still a matter of debate. • Considering that the Moon evolution ended about 3.2 b.y.a., it should keep traces of the processes on-going at the early stages of the Solar System. • The future human presence and utilization of the Moon requires a better knowledge of its environment and hazards and of its resources .

High resolution imaging and spectrometry from orbit and then from in-situ measurements.

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Study of the Moon and its resources

• Remote sensing measurements: – High resolution imaging with global coverage >>> morphology – High spatial and spectral resolution spectrometry >>> mineralogical distribution

– Global coverage of the gravity field and rotational state – Characterization of the polar zones – Characterization of the regolith 2 mission configurations proposed: 1 or 2 orbiters

Geophysical package Geochemical package Ka-band Multispectral cameras Gradiometer Stereo-camera γ, X, UV and IR spectrometers Laser altimeter Radio and radar measurement

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Study of the Moon and its resources

• In-situ measurements : – Geophysical package: • Heat flux in “non explored” regions • Seismological network • Laser reflectors – Geochemical package: • Elemental and mineralogical composition of high latitude (> 60°) samples (e.g. anorthositic crust) • Volatile reservoirs and transport in permanently shadowed craters in polar areas • Characterization of the regolith (record of solar history) – Environmental package: • Dust • Radiation

• Trade-offs between horizontal and vertical mobility LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Observation of the Universe from the Moon

• This study took into account the characteristics of the Lunar environment and looked at those experiments that could be competitive w.r.t. Earth based telescopes or free flyers: – Absence of atmosphere >>> no screening, electromagnetic spectrum fully accessible for simultaneous observations in all

wavelengths

– Far side radio quiet – Environment thermally stable for the instruments (slow rotation) – Passive cooling of IR instruments in permanently shadowed sites (craters)

– Low seismicity >>> pointing accuracy for interferometers

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Observation of the Universe from the Moon

– Allows terrestrial-type mountings instead of satellite systems without the limitations of a free flyer (mass, power, observation time) and possibility of refurbishment – Allows large (large collecting areas) and stable structures through the utilization of light materials because of the low gravity

• But: – Thermal conditions (night/day variations; terminal crossing) – Power supply during night

– Dust as a radiation absorber and damaging element for mechanisms – No magnetic field >>> cosmic rays – Moonquakes

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 X-rays and γ-rays

• The observation of the Universe requires coordinated and simultaneous observations in different windows of the EM spectrum • A “High Energy Observatory” composed of 4 telescopes ranging from few keV to many GeV has been studied • These telescopes are: – transit instruments with no specific pointing requirements (the sources will drift in the FOV-transit mode) – located in the equatorial region (even coverage of the sky ) – near side (TLC) – 27 terrestrial days (one Lunar rotation) continuous observation (tbd) >>> Extensive deep surveys • Possibility to build the Observatory via a modular approach • The 4 telescopes are very large instruments, they cannot be sent to the Moon in just one flight unless a system like the one in the NASA “ESAS” study is available. • Relevant information on dust, micrometeorites, temperature excursions and total radiation impacts on these structures are needed.

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 TIGRE Timing Italian Gamma Ray Experiment

• Scientific objectives: – Detailed study of individual cycles of Quasi Periodic Oscillations (QPOs) in Galactic binaries – Survey of X-ray pulsars – Temporal variability and quasi-periodicity during the prompt phase of gamma-ray bursts – High resolution timing study of bursts from magnetars • Characteristics: – Energy Range: 1-20 keV Timing only - 1-10 keV Imaging and Timing – FoV: Timing only half sky, – Slit collimator 1° x 60° - Collimator and Mask: 60°x 60° – Time resolution 10 μs – Modular structure >>> Total Geometric Area: 100 modules of 1 m2 =100 m2

>>> Proposed to study a precursor (1 module)

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 mask positioning open sky view

coded mask in place

Pictorial view of 1 TIGRE module

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 UV-Visible-IR

• Five themes 1. Solar Observations: UV Gregorian Solar Telescope 1-2m class with spectro-polarimetry capabilities

2. Solar System Minor Bodies Detection (NEAs): a 2m class telescope with high spatial resolution capabilities

3. Wide FoV Telescope: a 4-8m class telescope with a high spatial resolution capability >>> Galactic astronomy

4. Mid-IR Telescope >>> Extragalactic astronomy and Cosmology

5. Interferometry for extremely high resolution: an array of 1-2m class telescopes interferometrically linked, possibly assisted by a coronograph, characterized by a large coverage of Fourier plane with km’s baseline

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Sun Observations

• A 1 to 2 m Gregorian Diffraction limited UltraViolet telescope for Solar Observations . • Aiming to explore magnetic tubes fluxes, their temporal evolution and interaction with other Solar features. • Spectro-polarimetry capability is essential

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Sun Observations Site

Polar zones, crater edge or rim for continuous Sun observation

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Sun Observations

• Preliminary estimations: 350kg, far too large for capabilities available but strong and interesting synergies with Earth observations and radiation balance (climate change, meteo, interaction Sun-Earth…) • 1° Moon base at the South Pole >>> to be further studied but on a longer term than 15 yrs.

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Radioastronomy

Waves of frequency < 50-100 MHz are distorted crossing the ionosphere and this limits the maximum baseline of an interferometer and thus the angular resolution of observations (Θ > deg).

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Radioastronomy

• Low frequency radio observations from the Moon: 1. What kind of low frequency radio observations can be performed from the Earth?

2. Is a Moon based array really unique for low frequency radio astrophysics?

3. What kind of physical limitations should still be considered in the case of a Moon based array?

4. What is the importance of low frequency radio astrophysics? Which are the most relevant science cases that can be addressed for the 1° time from the Moon? 5. What kind of array we need to address the main science cases?

6. Is it possible to have a scientifically well motivated precursor

experiment?

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Radioastronomy

• Low Frequency Radioastronomy from the Moon ¾ no limitations due to Earth ionosphere for low-frequency radio observations (Earth based radiotelescope > 15-30 MHz) ¾ no human interferences ¾ radio telescopes are large instrument, limited on free flyers ¾ the far side of the Moon is an ideal site for a radiotelescope

• Limitations due to plasmas: interplanetary medium & interstellar medium >>> scattering of long wavelengths ¾ calculation of the limitations on the maximum baseline and maximum resolution with frequency for a radio telescope based on the Moon; ¾ calculation of the confusion limit (probability that the point spread function of the radiotelescope is contributed by more than 1 radio source) ¾ calculation of the temporal broadening (smearing of transient signals)

¾ >>> Capabilities of a Moon Radiotelescope

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Radioastronomy

• At frequencies < 40MHz, Earth based observations are difficult or impossible (magnetosphere, ionosphere and human interferences) >>> Moon based arrays give the unique possibility: – to look at the Dark Ages – to adequately sample the process of magnetic field amplification in the large scale structure – to catch the most distant radio sources in the universe.

• Radio observations from the Moon should address the origin of the diffuse radio emission in galaxy clusters and the physics of radio galaxies and quasars, the structure of the diffuse galactic non-thermal background and of the galactic magnetic field. • Radio observations from the Moon should be sensitive to physical processes that are very rare at higher frequencies: electron-cyclotron masers, synchrotron circular polarisation,… >>>Deep and spatially resolved observations are needed and can be performed only by using large arrays with long 10-100km baselines.

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Moon Radiotelescope

• Observatory at 1-60 MHz on the far side of the Moon • Dipole Array with max baseline 15-100 km • Number of Array elements 10-300

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Precursor Experiment

• 10 Dipoles (Magnetic dipoles) (1kg, 1,5W including RAM) on Rovers • Far side • Orbiter for communications with Earth • Rovers move and refill batteries during Lunar day (14 days) • Observations during Lunar night (14 days) • Minimum baseline < 50 m – Maximum baseline 2-15 km • Rovers provide 5-6 dipole configurations within 3 months • Baselines 50-100m (initial) – ~ km (3 months) • Observations at LF = 5 MHz – 50 MHz • Max spatial resolution between 0.5 deg – 3 arcmin • Sensitivity between 2000Jy – 10Jy

• First sub-degree images of the Galaxy at LF • First spatially resolved spectroscopy of the Galaxy at LF • First survey of the sky at LF (galaxy + extragalactic)

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Precursor Experiment

- Size < 100 kg - Feasibility : OK - Huge international interest - Robotics/Mobility Unique ! - Science : Top Level (immediately) !!

Modular: Size 100-300 kg as a second step

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 1500 PARTICELLE SCIENCE THEMES Very Promising High Energy Gamma AAA Regolith Calorimeter Rays

Particles and Extremely High Energy High Energy Neutrinos Interesting Fundamental (a) Interesting Physics Extremely High Energy High Energy Neutrinos (b) Promising High Energy Cosmic Rays Promising Solar plasma properties (a) Priority Interesting Plasma interaction with planetary surface (b) 1 Very Promising Interesting Gravitational waves (a) 2 Promising Interesting Gravitational waves (b) 3 Interesting Very promising Fundamental physics LEAG Annual Meeting “Enablingtests Exploration: The Lunar OuAAAtpost and (Laser Beyond” ranging, OAC) Houston (Texas - USA) – October 1-5, 2007 High Energy Gamma Rays: using the regolith to build a multi ton

EM calorimeter on the Moon

SCIENCE AND DETAILED SCIENCE Sito MEASUREMENTS Requirements Coverage/resolution TECHNOLOGY OBJECTIVES Range /sensitivity Detection of Gamma Detector Scintillator bars in the lunar ground within 1 - 300 .--> energetic Larger possible Rays by using the lunar inside the the holes of 20 mm in diameter, which GeV resolution 10000 cm2 sr is the Fundamental Physics regolith like a passive lunar ground distance between them is about 5 cm (or 20%/Sqrt(E) objective for one module Very-High Energy material to build an 10 cm). The hole depth is 10 cm for the --> angular can be realized in more Acceleration Processes electromagnetic first circumference (which radius is 10 resolution that one site Discovery of new particles calorimeter to measure cm), 20 cm for the second, 30 for the < 1 degree energy and direction of third etc. up particles

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 MOONCAL: an EM calorimeter to study high energy photons and electrons (1-1.000Gev)

• The goal is to build a large area detector, with a capability of 2 orders of magnitude higher exposure than GLAST making use of the unique properties of the Moon as a laboratory. • The idea is to use the lunar regolith “as is” as converter and to read the signal emitted by the EM shower through scintillator bars planted in the regolith. • The experiment can be built as modular additions of a limited number of bars installed during each robotic mission. • Each mission could carry 30-50kg of bars to be installed, incrementing the area of collection and without carrying to the Moon any heavy material for the converter neither moving large quantities of regolith.

>>> ideal for a precursor

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Spatial distribution of the scintillator bars on the lunar surface (distance between bars: 7,5 cm, to be optimized)

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Side view

Front view Charged part of the e.m. shower induced by 10 GeV gammas in the regolith Negative charges are in green and positive in red

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 MoonLIGHT-R: 2° Generation Lunar Laser Ranging (LLR)

• The idea is to improve the classical lunar ranging results, using better retro-reflectors located over a larger area. The expected accuracy would be at least 1 and up to 3 orders of magnitude better than the current results, paving the way to very interesting measurements in the field of General Relativity and cosmologically motivated Unified Theories.

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 MoonLIGHT: MOON LASER INSTRUMENTATION FOR GENERAL RELATIVITY HIGH-ACCURACY TESTS C. Cantone, S. Dell’Agnello, G. O. Delle Monache, M. Garattini, N. Intaglietta Laboratori Nazionali di Frascati (LNF) dell’INFN, Frascati (Rome), ITALY R. Vittori Italian Air Force, Rome, ITALY

• From the abstract ……. – a proposal (to NASA) for improving by a factor 1000 or more the

accuracy of the current Lunar Laser Ranging (LLR) experiment (performed in the last 37 years using the retro-reflector arrays deployed on the Moon by the Apollo 11, 14 and 15 missions). Achieving such an improvement requires a modified thermal, optical and mechanical design of the retro-reflector array and detailed experimental tests. The new experiment will allow a rich program of accurate tests of General Relativity already with current laser ranging systems. A new Unified Theories beyond GR can also be tested (see Dvali et al 2003). This accuracy will get better and better as the performance of laser technologies improve over the next few decades, like they did relentlessly since the ‘60s.

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 3 pulses back to Earth

T3 < T2 < T1 ΔT T2 1 widened pulse back to Earth T1 T3

Matrix array of 10x10 Sparse array of 8 retro-reflectors tightly-spaced retro-reflectors (~100m x 100m) (~30cm x 30cm)

LLRA_20th LLRA_21st

ΔT T T T LEAG Annual Meeting “Enablingtime Exploration: The Lunar Outpost and Beyond”3 2 1 time Houston (Texas - USA) – October 1-5, 2007 Pulse to Moon Pulse back to Earth Pulse to Moon Pulses back to Earth Deviation from 1/r2 force-law (Yukawa potential, α−λ plane)

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Lunar Laser Ranging Experiment

1. General relativity high-accuracy tests (Equivalence Principle) (Observation of the Universe)

2. Moon librations, Moon internal structure, tides, Moon geophysics (Moon study)

3. Establishment of a selenocentric reference system tied with the Earth fixed one which is needed for Earth images taken from the Moon georeferentiation (Earth observation)

4. Navigation on the Moon (exploration)

>>> Huge international interest

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Earth Observation from the Moon

• This study is taking into account the characteristics of the Lunar environment:

– a global view of the Earth, providing a full disk view (sunlit half the time) – the capability to observe continuously the Earth disk for long periods – a global coverage (not continuous) with a single instrument – the possibility to increase the integration time – day-night observation of the same area (relevant for vegetation fluorescence monitoring) – a synoptic view and the opportunity to monitor the evolution of large spatial scale phenomena with larger FoVs than those offered by a constellation of satellites

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Earth Observation from the Moon

– the possibility to observe the same area at high picture rate, for long periods allowing the characterization of rapidly varying, large scale phenomena – the reduction of influence of intermittent clouds – the possibility to deploy larger, more complex instrumentation

• But: – Thermal conditions (night/day variations; terminal crossing) – Power supply during night

– Dust as a radiation absorber and damaging element for

mechanisms

– No magnetic field >>> cosmic rays – Reduction in signal intensity due to the distance

– … and of course maintenance, transport and installation!

LEAG Annual Meeting “Enabling Exploration: The Lunar Ou tpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Earth Observation from the Moon

• Analysis of the science that can be done only from the Moon or in a better way than that allowed from a satellite or a constellation of satellites, in particular: – phenomena and processes acting at global spatial scale and with a high variability both in space and time: • simultaneous observation of different point of the Earth to explore spatial correlation over wide areas (vegetation, oceans) • phenomena requiring continuous observation of the same area for a certain interval of time (weather systems) • global (or very large area) observation because of their impact on large areas (ozone distribution, global circulation) – phenomena not well localized in space and with slow frequency that can benefit from a continuous monitoring of large areas such as meteoroids impacts – monitoring of the Sun-Earth system: Spectral and Total Solar Irradiance variations>>> global climate change

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Earth Observation from the Moon Main Objectives

1. Earth atmosphere: monitoring weather systems, clouds (radiative, chemical and physical properties), aerosols and gases (atmospheric chemistry at global and local scale) 2. Oceans: a. Physical oceanography: mapping of marine currents; ocean circulation; oceanic front identification; Optical Oceanography, water masses characterization, Sea-ice melting and formation b. Marine ecosystem studies: pollution monitoring, coastal waters, marine biology 3. Vegetation monitoring: Global climate change; terrestrial carbon cycle; Resource management and sustainability, desertification, photosynthesis efficiency. 4. Earth radiation budget: Sun spectral variations monitoring, Earth monitoring, climatology, Earth-Sun interaction

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Science Atmospheric chemistry Clouds properties Weather Systems Objectives Tropical cyclones, Detailed Aerosols Radiative & Trace gases content tornadoes, weather Science Optical Microphysical (O ,NO ,SO ,CO) fronts and Objectives Properties 3 x 2 properties depression 0.6 – 0.8 µm < 0.15 µm 0.4 – 3.0 µm Spectral Range 0.2 – 3.0 µm 5 – 14 µm < 10 @ VIS µm [ 1.5 – 4.5 ] < 0.2 nm > 0.5 µm < 20 @ NIR nm < 0.5

54, 118, 425, 183, 380 > 0.5 Sensitivity > 200 @VIS >1000@ [UV-VIS] 0.25 (for 1.6 μm) 0.75 @ 250 (for 5-8μm) SNR or NEDT >100@NIR >50@NIR 0.35 @ 300 (for 3.9 μm) 0.25 @ 300 (for >8 μm)

Spatial 250 x 250 m2 Coverage @VIS 10x20 km2 3x3 km2 3x3 km2 And 500 x 500 m2 5x10 km2 Resolution @NIR

Temporal 30 min 1 hour 15 min 15 min resolution 1 hour

Main optical parameters for the definition of the optical system for atmospheric observations.

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 TACS Trace gases, Aerosols, and Clouds Spectrometer

•Hyperspectral imaging/scanning spectrometer specifically designed for atmospheric applications. •TACS has been tailored on the requirements for atmospheric studies,but it could be used for vegetation monitoring under the condition to extend the observation time. •Spectral range: 0.2-3 μm - Spectral resolution: 0.2 nm

It is composed by: 1.a telescope, accommodated on an Earthtracking/scanning,

2.a multi-grating spectrometer (to cope with the large waveband)

The focal plane array should have at least 1k x 1k square detectors, with sensitivity extending from UV to MIR . Power consumption : ~150 W.

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 TACS Trace gases, Aerosols, and Clouds Spectrometer

Scientific objectives: 1. Atmosphere - Trace Gases 2. Ocean Observation (SST) Mass Budget: 88 (TBC) Kg (Config. A - worst case) Including: Constraints: 1. spectrometer (30Kg);

Overall Mass budget: 110 (TBC) Kg 2. electronics (15 Kg) 3. robotic support, including optics (43Kg) Overall Volume budget: 1 x 1 x 1.8 (TBC) m^3 + Max power : (not including robotic support) Telescope mounted on a robotic (earth scanning) a. in operative conditions: 200 (TBC) W b. in stand-by conditions: 30 W support structure

Further data:

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 VISIOO VIS Imager for Oceans Observation

VISIOO is a 2 m long telescope on a robotic Earth scanning system

The instrument measures the emission and absorbance lines of the atmosphere, and the Earth surface reflectance in response of Sun illumination. VIS-NIR spectral range (from 0.38 to 1.06 μm) with a spectral resolution better than 2 nm.

Camera & electronics (18 Kg constant value), Optics, robotic support : Configuration Nadir resolution (Km2) Aperture diameter (m) Payload weight (Kg) A 1x1 0.5 61.7

B 2x2 0.18 42.4 C 3x3 0.1 39.8 LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” D 5x5Houston (Texas - USA) – October0.1 1-5, 2007 38 Draft

2008 2010 2012 2014 2016 2018 Orbiter φA φB/C/D φE Landing site determination Lander (geochemistry, geophysics) Pre-φA φA φB/C/D φE Radiotelescope ? LLR? φA φB/C/D φE Radio Telescope Pre-φA LLR Pre-φA

TIGRE Pre-φA

MoonCal Pre-φA LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 ESA Aurora Exploration Programme

• Even if the ESA Aurora Core Programme is essentially focussed on the robotic and on the long-term on the human exploration of Mars, it does not exclude that the mission to be selected for launch after the ExoMars mission (2013) could be a lunar mission: – 2 missions concepts have just been selected for phase A studies to be performed in preparation of the ESA 2008 Ministerial Council; – 1 is a lunar lander mission to test soft and precision landing and hazard avoidance technologies in preparation of Mars Sample Return.

• Italy is looking forward to the selection of the NEXT mission (precursor to Mars Sample Return to be launched in the 2016-2018 timeframe) at the next Ministerial Council in 2008.

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Human Exploration

• Utilization of the ISS as a test bed for human exploration beyond LEO: for example life support systems within the ESA Aurora Core Programme.

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 FLECS FLexible and Expandable Commercial Structure

¾ This is a national on-going programme (phase B): • Objectives: technological R&D to develop pressurized modules for orbiting structures, surface Lunar and Martian habitats with a small volume at launch and a large volume once deployed • Key technologies: – Thermal and pressure aspects, leakage, radiations, deployment (A/R), resistance to meteorites impacts, air contamination and monitoring. • ASI plans to realize a prototype and to make it fly on a small satellite or on ISS. Pursue activities on FLECS at national level or in the ESA context.

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 FLECS FLexible and Expandable Commercial Structure

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Transportation

• Participation to the development of a new space human transportation system for ISS and the Moon in the ESA context together with Russia (CSTS ). – EXPERT is a low cost ballistic test-bed for re-usable transportation and re-entry.

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007 Next steps

• The situation is now mature for decisions to be taken in the forthcoming months: – National programme of Moon Exploration: • which element(s)? • which collaboration(s)? – ESA 2008 Ministerial Council: • NEXT • CSTS • Other

LEAG Annual Meeting “Enabling Exploration: The Lunar Outpost and Beyond” Houston (Texas - USA) – October 1-5, 2007