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El programa de ciencias del espacio de

la ESA

Fabio Favata

European Space Agency

Astronomy and Fundamental Physics Missions Coordinator

A broad mission portfolio

• A long-term commitment to the excellence of European science

• A balanced program serving a broad community

• Present: operations

• Immediate future: implementation • Farther future: proposals and studies

(2)

SOHO CLUSTER XMM NEWTON HERSCHEL INTEGRAL HUYGENS MARS EXPRESS SMART 1 GAIA LISA JWST VENUS EXPRESS BEPI COLOMBO ROSETTA IL W S T im e → ISO HST ULYSSES CLUSTER II Solar B COROT µSCOPE Double Star LPF Akari Cosmic Vision 2015-2025 Robotic exploration SOLAR ORBITER PLANCK

Program “legs”

Missions in operation - solar-terrestrial

SOHO/ Cluster

(3)

SOHO: Staring at the Sun

(4)

Cluster: Studying how the solar wind affects the Earth

(5)

Missions in operation - planetary

Mars Express Rosetta Cassini/Huygens Venus Express

The Cassini S/C

(6)

Diving through Titan’s atmosphere

(7)

First Close-Up Image of a comet - ESA’s GIOTTO Mission March: 1986

Europe on Giotto

(8)

67P/CG on 9 March 2003

ESO La Silla, 3.6m+EFOSC2

N E Sun D A B C Sun r = 2.49AU 65000km

(9)

Mars Express

What is the age of this dune field?

On-going process

(10)

Traces of liquid water on Mars

Water vapour concentration

Methane on Mars: any relation with ancient life?

(11)

Venus express: why this uncontrolled greenhouse effect?

Missions in operation - astronomy

XMM-Newton Integral

(12)

HST

Launched 1990

HST

HST

• Multi-purpose observatory

– Optical, NIR, UV

• First (and only) serviceable astronomy mission

• ESA junior partner to NASA (15% nominal) • Very successful cooperation

(13)

XMM - NEWTON

launched 1999

XMM-Newton

XMM-Newton

• X-ray observatory

• ESA-only mission (NASA contribution to P/L)

• Open to worldwide scientific community • Most productive ESA astronomy mission

(14)

INTEGRAL Launched 2002

INTEGRAL

INTEGRAL

• Gamma-ray observatory • ESA-Russia cooperation (25% nominal) • Mixed observatory-PI model Spectrometer SPI Imager IBIS (coded mask)

X-ray monitor JEM-X (2x) (coded mask)

Optical monitor OMC

Imager IBIS (detector assy)

X-ray monitor JEM-X (2x) (detector assy)

(15)

COROT

Launched October 2006

• Asteroseismology of a number of bright stars and search for rocky planets.

• 27 cm off-axis telescope (2.8 x 2.8o FOV) in polar orbit. • ESA junior partner to CNES (ca. 5% level)

COROT

Missions in preparation

Herschel-Planck 2008 Lisa-Pathfinder 2010 JWST (NASA-ESA-CSA) 2013 Gaia 2011 Bepi-Colombo 2013 Solar Orbiter (ESA-NASA) 2015 Chandrayan (ISRO-ESA) 2008 Microscope (CNES-ESA) 2010 2007 2008 2010 2012 2006 2013 2005 2009 2011 2014 2015 2016 2017

(16)

Herschel

Launch 2008

The first space facility to completely cover the far infrared and sub-millimetre (57 - 670 mm) range

– large (3.5 m), low emissivity (~ 4%), passively cooled (< 90 K) telescope and 3 cryogenically cooled science instruments, >3.5 years operation

Unique and complementary

– for λ < 200 µm much larger (but warmer)

aperture than missions with cryogenically cooled telescopes (IRAS, ISO, SIRTF, Astro-F,…)

– larger colder aperture, better ‘site’, and more observing time than balloon- and airborne instruments (~1000 SOFIA flights per year)

– larger field of view than interferometers

Launch 2008

Imaging of the whole sky at wavelengths near the peak of the spectrum of the Cosmic Microwave Background Radiation Field (CMB), - with an instrument sensitivity Δ T/T~10-6

- an angular resolution ~5’ - wide frequency coverage, and - excellent rejection of systematic effects.

(17)

Method:

• astrometry, Hipparcos principles • two 1.4×0.5 m2 mirrors + CCDs

• continuous ‘revolving’ sky scanning • 5-year observations: 100 epochs per star Objectives:

• distances + motions for 109 stars

• 10-20 microarcsec at 15 mag • structure and evolution of Galaxy

Launch: 2011

GAIA

JWST

• 6-m class mirror (25 m2 area) • 18 segments made of Beryllium • Diffraction-limited at 2 µm • 0.6 - 28 micron wavelength range • 3 core instruments

– 0.6-5 µm wide field camera – 1-5 µm multi-objects spectrometer – 5-28 µm camera/spectrometer

• Large sunshade (about size of tennis court) folded to fit in launch shroud

• 5 year operations requirement and 10 year goal

(18)

Studying Mercury, the closest planet to the sun, with BepiColombo

(19)

ESA’s new long-term plan for

Space Science

Cosmic Vision 2015-2025 process

• Call for Science Themes in Spring 2004

• Responses analyzed by ESA’s advisory structure in July 2004

• Workshop with community in Paris in September 2004 (400 participants)

• Spring 2005 the Cosmic Vision Plan was presented to the community

• Plan should cover one decade, with 3 Calls for Missions planned

(20)

Four “Grand Themes” identified

(see ESA publication BR-247)

1. What are the conditions for life and planetary formation?

2. How does the Solar System work?

3. What are the fundamental laws of the Universe? 4. How did the Universe

originate and what is it made of?

1. What are the conditions for life and planetary formation?

• 1 Place the Solar System into the overall context of planetary formation, aiming at comparative planetology

• 1.1 From gas and dust to stars and planets • 1.2 From exo-planets to bio-markers

(21)

1. What are the conditions for life and planetary formation?

2. How does the Solar System work?

• 2.1 From the Sun to the edge of the Solar System

• 2.2 Gaseous giants and their moons • 2.3 The building blocks of the Solar

(22)

2. How does the Solar System work?

3. What are the fundamental laws of the Universe?

• 3.1 Explore the limits of contemporary physics

• 3.2 The gravitational wave Universe • 3.3 Matter under extreme conditions

(23)

3. What are the fundamental laws of the Universe?

4. How did the Universe originate and what is it made of?

• 4.1 The early Universe

• 4.2 The Universe taking shape • 4.3 The evolving violent Universe

(24)

4. How did the Universe originate and what is it made of?

Cosmic Vision process

• First “Call for Missions” issued in 1st Q 2007

• 50 proposals received by June 2007 deadline

• Selection process by scientific community during summer

(25)

Cosmic vision process for 1st slice

• 2 launch opportunities, for 2017/2018 • Currently planning 1 M (2017) plus 1 L

(2018) mission

– L cap ca. 650 M€, M cap ca. 300 M€ ESA cost – P/L funded separately by ESA member states – Other mixes of mission sizes possible

– Programmatics to be reviewed according to budget evolution

European Science Community

Solar System Working Group Fundamental Physics Advisory Group Astronomy Working Group Space Science Advisory Committee Membership of advisory bodies is determined by individual scientific standing Member States ESF Space Science Committee X-member ESA Executive DG, D/Sci A dv ic e (implementation) Science Programme Committee Recommendations (resource)

The ESA program is chosen by the Scientific Community

(26)

Cosmic Vision process for 1st slice

• Mission concepts have been selected for

assessment studies

• Further down-selection is planned in 2009 and 2011

• Assessment studies ongoing, to mid 2009

Selected concepts for the first slice of

the Cosmic Vision program

• L mission concepts

– Xeus (large collecting area X-ray observatory) – Laplace/Tandem (mission to the outer planets) – LISA (ex officio, gravitational wave observatory)

• All of them require significant technology development

• All of them are proposed to ESA as international collaborations

– Cooperation scheme still being refined, specially for XEUS

(27)

Selected concepts for the first slice of

the Cosmic Vision program

• M mission concepts

– Plato (planetary transits and asteroseismology) – Euclid (Dark energy)

– Marco Polo (NEO sample return) – Cross Scale (magnetospheric physics)

• Missions of opportunity

– Spica (contribution to JAXA MIR observatory)

• No significant development required

XEUS: Scientific objectives

• A large collecting area X-ray

observatory

• Some key scientific drivers

– Evolution of large scale Structure and nucleosynthesis

– Coeval growth of galaxies and supermassive black holes

– Matter under extreme conditions

Z= 0 Z= 2

(28)

XEUS: top level requirements

• To be used as drivers for the Assessment phase

– 5 m2 @ 1 keV, 2 m2 @ Fe K

– 0.1-15 keV band (XMM/Chandra-like)

– ≥ 5 arcsec spatial resolution (2 arcsec goal)

– Wide field imaging (≥ 7 arcmin, R ≥ 50)

– High-res, non-dispersive spectroscopy (≥ 0.6 arcmin, R ≥ 1000-3000 @ FeK)

– Possible options: polarimetry, high time resolution, enhanced hard X-ray response and instrumentation

XEUS: implementation concept

• 2 S/C in formation flying • Mirror S/C accommodates large X-ray telescope • Detector S/C accommodates focal plane instruments

(29)

LISA

• Mission to detect and observe gravitational waves and their sources

• Joint ESA/NASA mission • Technological challenges

– Interferometric measurements to picometer accuracy – Drag-free technology

– Low frequency stability

LISA

• 3 drag-free S/C in a heliocentric orbit trailing the Earth by 20° (50 million kilometers)

(30)

Laplace/Tandem

Euclid

• Dark Energy recognized as highest priority in astronomy for M missions

• Two proposals (Dune and Space) received, both highly ranked

• A novel mission concept (Euclid)

incorporating elements from both proposals is being studied

(31)

Euclid science goals

• Constrain Dark Energy equation of state combining WL and BAO

• Wide field imaging, NIR photometry, NIR spectroscopy

Euclid payload complement

• 1.2 m Korsch TMA • 3 focal plane instruments

• Visible imager, 0.2 arcsec PSF (FWHM, 8000 A), 0.5 deg sq FOV

• NIR imaging photometer, 0.3 arcsec PSF, 0.5 deg sq FOV, YJH bands

• NIR MOS spectrograph, 0.9-1.7 µm, 0.5

deg sq FOV, R = 400 – Innovative use of DMDs

• Passively cooled to 170 K (CCD) and 140 K (NIR)

• 600 kg P/L (300 kg focal plane)

NIS

VIS NIP

(32)

Plato: scientific objectives

• Provide the observational data to understand the evolution of stars and their planets

• High accuracy photometry of a large sample of relatively bright stars

– Transiting terrestrial planets & – Asteroseismology of the planet host

• Challenging requirements

– 100,000 bright (V<11) MS stars with noise < 3e-5 in 1 hr

– Monitoring for > 3 yr

– Wide field (> 500 sq deg), large area

Plato: payload

• 28 co-aligned telescopes with 10 cm pupils

• 4 CCDs per focal plane,

3854x3854 18 µm pixels

• 557 deg sq FOV

• 30 sec observing cadence • V=8-14 and V=4-8 dinamic

range

• L 2 orbit, S/C rotation every 3 months

(33)

SPICA: baseline mission

• Space Infrared telescope for Cosmology and Astrophysics

• JAXA-led mission

• Coverage of FIR-MIR (5-210 µm) with imaging,

spectroscopic and coronographic instruments • Two orders of magnitude more sensitive than

Herschel in FIR

• Higher spectral resolution than JWST in MIR (R=30 000)

SPICA: European contribution

• ESA will provide:

– Cryogenic telescope assembly – European SPICA ground segment

– SAFARI system engineering and management

• SAFARI instrument

– FIR imaging spectrometer

– Nationally funded, Europe/Canada – ESA managed

(34)

Marco Polo

(35)

CV study organization

• Establishment of science study team

– ESA appointed, chosen, funded

• Internal convergence phase

– ESA-internal, CDF

• Industrial system assessment study

– ESA-funded, two parallel contractors

• P/L assessment study

– Nationally funded, PI-run

CV2015: long-term technology

development activities

• A number of high priority science goals identified with low TRL

• Incompatible with programmatics for first CV2015 slice

• Will be subject to joint (ESA + national) technology activities, in view of future CV2015 Calls

(36)

CV2015: long-term technology

development activities

• Goals in astrophysics for longer-term

technology are

– Detection and characterization of terrestrial exo-planets

– Study of B-mode polarization of CMB – Far-IR interferometry

References

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