italy’s plans for moon exploration · moon exploration • in 2005, asi top management proposed...

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

ItalyItaly’’s s PlansPlans

forfor

MoonMoon ExplorationExploration

Sylvie EspinasseItalian

Space Agency

http://nssdc.gsfc.nasa.gov/imgcat/hires/a17_m_2444.gif


Italy’s Plans

for

Moon

Exploration

•

National Programme for robotic Exploration

•

Human Exploration


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.



•

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



• 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.



• The Programme

is

science

driven:

1.

Define the scientific objectives 2.

Identify the

key measurements and related

requirements to meet those objectives3.

Prioritise the objectives

Input for

technological

studies


Moon Origin and evolution

SCIENCE Requirements

THEMES Range

Sensitivity Coverage/resplution

SUB THEMES SCIENCE AND TECHNOLOGY OBJECTIVES

DETAILED SCIENCE OBJECTIVES

MEASUREMENTS

Value Unit Value Unit Value Unit

Map of Si, Al, Mg, Ca Fe, Na, O, C

X-Ray Spectra of highlands and Maria 0.5-

20 keV <200 eV

Global Coverage

1-10 Km at 100 Km altitude

Map of olivines/ pyroxenes

VIS-IR Spectra of highlands and Maria 0.3-5 μm 10 nm

Global Coverage


Moon global

composition

VIS-IR Spectra Maria

0.3-5 μm 10 nm

Regional Coverage


Magma Ocean Model

Mapping distribution and

relative abundance of mafic mineral and plagioclase

VIS-IR Spectra Maria samples

0.3-5 μm 10 nm

Local coverage

in situ X-Ray diffratometric

analysis Local coverage in situ

Raman spectra Local coverage in situ

Constrain Theories of the origin of

the lunar upper mantle

sampling composition of

different location of lunar maria

VIS-IR Spectra of

central peaks 0.3-5 μm 5 nm Local coverage < 100 m

origin and

evolutionglobal

composition

origin and evolution of Lunar Crust

composition of different crater central peaks


SUB THEME

S

SCIENCE AND TECHNOLOG

Y OBJECTIVES


SITE MEASUREMENTS Operative Sensitivity Operative Angular

resolutio

n

Spectral

resolutio

n

FoV

Range Temperature

Value Uni

tValue U

nitValue Un

it

CMB polarisati

on

Stokes’

parameter

maps,

Correlation

modesTo

minimise the instrumental

noise

and RF interferences, the experiment

should

be

located

in a shaded

crater

on the dark side of the Moon

Radiometers

with

InP

LNAs

(HEMT) using

OMT for

splitting

the two

orthogonal

polarisation

of the incoming

radiation. Cross-

polarisation

less

than

40/50 dB.

Pointi

ng10-100 GH

z<0.1 mK

sec1/2

20-30 K 1 arcmin@

100 GHZ for

CMB

20% >10e4 deg2

(E and B mode)

cosmological

models

verification, high frequency

polarisation

surveys.

Inflation

and primordial

quantum fluctuations, structure

formation, reionisation, cosmological

parameters, particle

physics.

and Scann

ing

and gravitati

onal

waves

mm and sub-

mm optics

and large

focal

plane

detector arrays. Interferometric

systems

Bolometer

arrays

using

OMT for

splitting

the two

orthogonal

polarisation

of the incoming

radiation.

100-

1000GH

z100 m

K

CMB Polarisation


Vegetation Monitoring

SCIENCE AND TECHNOLOGY OBJECTIVES DETAILED SCIENCE

OBJECTIVES Spectral range Spectral resolution

Sensitivity (minimum)

Spatial coverage and resolution

Temporal resolution

Carbon cycle; Net Primary Production

Leaf Area Index-LAI, FPAR, Light Use Efficiency and other related vegetation indices Global land cover Cover type and extent Desertification processes

400-2500 nm VIS 2 nm IR 20 nm programmable

12 bit Global; <1x1km2

From 1 h to daily

Typical reflectance spectrum of vegetation


Summary of the proposals

•

Observation of the Universe:γ rays-X rays >>> 4-9 experimentsUV-Vis-IR >>> 5-6 experimentsRadioastronomy and microwave >>> 4 experimentsFundamental physics and Particles >>> 10 experiments

Total: 29 experiments•

Earth Observation:Atmosphere >>> 4 experimentsOceans >>> 6 experimentsVegetation, biomasse >>> 9 experimentsRadiation Balance >>> 12 experimentsEarth SAR remote sensing >>> 5 experimentsGeoreferentiation >>> 5 experiments

Total: 41 experiments


… 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 capabilitiesPre-selection

Final DecisionInternational Collaboration

ROADMAP(we are here!)


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



•

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.



•

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

Geophysical packageKa-band

GradiometerStereo-cameraLaser altimeter

Geochemical packageMultispectral

camerasγ, X, UV and IR spectrometersRadio and radar measurement

2 mission configurations proposed: 1 or 2 orbiters



•

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


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


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


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.


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)


open sky viewmask positioning

coded mask in place

Pictorial view of 1 TIGRE module


UV-Visible-IR

• Five themes1.

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


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


Sun

Observations

Site

Polar zones,crater edge or

rim for continuous Sun observation


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.


Radioastronomy


Waves of frequency< 50-100 MHz

are distorted crossing theionosphere and this limitsthe maximum baseline ofan interferometer and thusthe angular resolution ofobservations (Θ > deg).

Radioastronomy


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?


Radioastronomy

•

Low Frequency Radioastronomy

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

•

Limitations due to plasmas: interplanetary medium & interstellar

medium >>> scattering of long wavelengths

calculation of the limitations on the maximum baseline and maximum resolution with frequency for a radio telescope based on the Moon;calculation of the confusion limit (probability that the point spread function of the radiotelescope is contributed by more than 1 radio source)calculation of the temporal broadening (smearing of transient signals)

>>> Capabilities of a Moon Radiotelescope


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.


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


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)


- Size

< 100 kg- Feasibility

: OK

- Huge

international interest- Robotics/Mobility- Science : Top Level (immediately) !!

Modular: Size

100-300 kg as

a second

step

Unique

!

Precursor

Experiment


1500 PARTICELLESCIENCE THEMES

High Energy Gamma Rays

Extremely High Energy High Energy Neutrinos

(a)

Extremely High Energy High Energy Neutrinos

(b)

High Energy Cosmic Rays

Gravitational waves (b)

Solar plasma properties (a)

Plasma interaction with planetary surface (b)

Gravitational waves (a)

Fundamental physics tests

Very

PromisingAAA Regolith Calorimeter

Interesting

Interesting

Promising

Promising

Interesting

Interesting

Interesting

Very

promisingAAA (Laser ranging, OAC)

Priority

1 Very

Promising

2 Promising

3 Interesting

Particles and Fundamental

Physics


Sito

Fundamental PhysicsVery-High Energy Acceleration ProcessesDiscovery of new particles

Detection of Gamma Rays by using the lunar regolith like a passive material to build an electromagnetic calorimeter to measure energy and direction of particles

Detector inside the lunar ground

Scintillator bars in the lunar ground within the holes of 20 mm in diameter, which distance between them is about 5 cm (or 10 cm). The hole depth is 10 cm for the first circumference (which radius is 10 cm), 20 cm for the second, 30 for the third etc. up

1 - 300 GeV

.--> energetic resolution 20%/Sqrt(E) --> angular resolution < 1 degree

Larger possible 10000 cm2 sr is the objective for one module can be realized in more that one site

Requirements Coverage/resolutionRange /sensitivity

SCIENCE AND TECHNOLOGY


MEASUREMENTS

High Energy

Gamma Rays:

using

the regolith

to

build

a multi ton EM calorimeter

on the Moon


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


Spatial

distribution of the scintillator

bars

on the lunar surface

(distance

between

bars: 7,5 cm, to

be

optimized)


Charged

part

of the e.m. showerinduced

by

10 GeV gammas

in the

regolithNegative

charges

are in greenand positive

in red

Side view

Front view


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.


•

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.

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


LLRA_20th LLRA_21st

ΔTPulse to Moon Pulse back to Earth Pulse to Moon Pulses back to Earth

T3 T2 T1time time

T3T1

T2

T3 < T2 < T1

ΔT

1 widened pulseback to Earth

3 pulses back to Earth

Matrix array of 10x10tightly-spaced retro-reflectors

(~30cm x 30cm)

Sparse array of 8 retro-reflectors(~100m x 100m)


Deviation from 1/r2

force-law (Yukawa potential, α−λ

plane)


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


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



–

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!



•

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


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


Science Objectives Atmospheric chemistry Clouds properties Weather Systems

Detailed Science Objectives

Aerosols Optical

Properties

Trace gases content (O3

,NOx

,SO2

,CO)

Radiative & Microphysical

properties

Tropical cyclones, tornadoes, weather

fronts and depression

Spectral Range 0.4 –

3.0 µm< 10 @ VIS

µm< 20 @ NIR

nm

0.2 –

3.0 µm< 0.2 nm

0.6 –

0.8 µm< 0.15

µm

[ 1.5 –

4.5 ]< 0.5

54, 118, 425, 183, 380

5 –

14 µm> 0.5

µm

SensitivitySNR or NEDT

> 200 @VIS>100@NIR

>1000@ [UV-VIS]>50@NIR

> 0.50.25 (for 1.6 μm)

0.35 @ 300 (for 3.9 μm)

0.75 @ 250 (for 5-8μm)0.25 @ 300 (for >8

μm)

Spatial Coverage And

Resolution

250 x 250 m2

@VIS500 x 500 m2

@NIR

10x20 km2

5x10 km2 3x3 km2 3x3 km2

Temporal resolution 1 hour 30 min

1 hour 15 min 15 min

Main optical parameters for the definition of the optical system

for atmospheric observations.


•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.

TACS Trace

gases, Aerosols, and Clouds

Spectrometer


Constraints:Overall

Mass budget: 110 (TBC) KgOverall

Volume budget: 1 x 1 x 1.8

(TBC) m^3

TACS Trace

gases, Aerosols, and Clouds

Spectrometer

Scientific objectives:1.

Atmosphere

-

Trace

Gases2.

Ocean

Observation

(SST) Mass Budget: 88 (TBC) Kg

(Config. A -

worst

case)Including:1.

spectrometer

(30Kg);2.

electronics

(15 Kg)3.

robotic

support, including

optics

(43Kg)

Max power: (not

including

robotic

support)

a.

in operative conditions: 200 (TBC) Wb. in stand-by

conditions: 30 WTelescope

mounted

on a robotic

(earth

scanning) support

structure

+

Further

data:


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 61.7B 2x2 0.18 42.4C 3x3 0.1 39.8D 5x5 0.1 38

VISIOO VIS Imager

for

Oceans

Observation


φφAA φφBB/C/D/C/D φφEEOrbiterOrbiter

20082008 20102010 20122012 20142014 20162016 20182018

φφAA φφBB/C/D/C/D φφEELander (geochemistry, geophysics)Lander (geochemistry, geophysics)

PrePre--φφAA

Landing site Landing site determinationdetermination

PrePre--φφAA

Radio Radio TelescopeTelescope

PrePre--φφAAMoonCalMoonCal

PrePre--φφAALLRLLR

PrePre--φφAATIGRETIGRE

Draft

φφAA φφBB/C/D/C/D φφEERadiotelescopeRadiotelescope ? LLR?? LLR?

http://nssdc.gsfc.nasa.gov/imgcat/hires/a17_m_2444.gif


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.


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.


FLECS FLexible

and Expandable Commercial Structure

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.


FLECS FLexible

and Expandable Commercial Structure


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.


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

italy’s plans for moon exploration · moon exploration • in 2005, asi top management proposed...

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