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1Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
Direct Imaging of Extrasolar Planets
Overview of Ground & Space Programs
Anthony Boccaletti : Obs. Paris-Meudon
2Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
Outline
1. A brief introduction to the high contrast imaging problematic
2. A brief review of projects (talks to follow)
4. « Where » do we need to direct our effort
3Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
No longer a dream !
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2M1207 5 MJ 46 AU
GQ Lup 17 MJ 100 AU
AB Pic 14 MJ 248 AU
CHRX73 12 MJ 210 AU
HN Peg 16 MJ 795 AU
DH Tau 12 MJ 330 AU
RSX 1609 8 MJ 330 AU
Detection was made possible because :
- small mass ratios (contrast is lower)- young ages (planet is brighter)- large physical / angular separations
4Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
A few more last week …
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Fomalhaut < 3 MJ 120 AU
HR8799 b 5 MJ 46 AU
HR8799 c 12 MJ 330 AU
HR8799 d 8 MJ 330 AU
5Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
Problematic
Planets are faint and close ….
109 = 1 milliard
106 = 1 million
Reflected light Thermal emission
STOP !!!! … What about diffraction ???
6Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
Problematic
Stellar images are not point-like …
7Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
Solutions to reduce diffraction
Yes but … the Sun is an extended source
Stars are point sources => diffraction is much stronger
We need more performant stellar coronagraphs … to attenuate stars
We need BIG telescopes …
We need to attenuate the star
8Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
In Theory …
€
ψA = A.e iϕ
€
ψA = A
€
ϕ =0siPlan A:
Plan B:
€
ψB =ψ A ⇒ ψ A .M
Plan C:
€
ψC =ψ B =ψ A ⊗M ⇒ ψ A ⊗M( ).D
Plan D:
€
ψD =ψC = ψ A .M( )⊗D
10Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
Problematic (again)
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Instruments are not perfect …. unfortunately
Many defects :
- atmospheric turbulence for ground based telescopes- static (more or less) optical aberrations- variation of transmission- alignment- chromaticity- …
=> Limits the performance of coronagraphs
11Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
Solutions to reject speckles
Wavefront Correction :at focal plane - speckles minimization - Self Coherent Camera
Wavefront Calibration :Differential imaging
- spectral (SDI, SD)- angular (ADI)- polarimetric (PDI)
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JPL Testbed
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SCC simulation
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SDI, GeminiSDI, Gemini
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ADI, GeminiADI, Gemini
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SD, VLTSD, VLT
13Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
Planet Finders on 8m telescopes (2011)
European Consoritum, VLT
- Dual band NIR camera (YJHK)- NIR IFS (YJH)- Dual Polarisation VIS camera
eXtreme AO + coronagraphy + differential imaging
HiCIAOJapan, Subaru
- Dual band NIR camera- Dual polarisation NIR camera
HiCIAO + (in dev., 2010)- Focal Plane WF- coronagraph improvement- NIR IFS
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US, Gemini South
- NIR IFS (YJH)Focal Plane
Looking at Giant Planets in : - young associations of stars (10 Myrs <100pc) - stars with known planets (RV surveys)- stars of intermediate age (0.1-1 Gyr)- very nearby bright stars
14Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
MIRIEurope + US consortium5 - 28 m imager + IFU
MIRI imager has 4 coronagraphs
4QPM in 3 filters (10.6, 11.4, 15.5 m) => self luminous mature giants T > 300-400K (5 - 10AU, 10pc, 5Gyr)
Expected contrast : 104 - 105
- photometry (R=20)
James Webb Space Telescope (2014)
=11.40m
CSA responsabilty 1 - 5 m tunable filterwith coronagraphic capabilities(Spectral Deconvolution)- spectra (R=100)
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US instrument0.6 - 5 m imager
NIRCAM has 5 coronagraphs Optimized for several filters (F200, F480, …)
Good performance at 4.8mAt 2.2 m mature giants are too faint.
Expected contrast : 105 - 106
- photometry (R=10-20)
NIRCAM
MIRI
FGS - TFI
& SPICA
15Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
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Extremely Large Telescopes (2020)
objectives : - mature giants- irradiated planets
heritage of VIZIR & MIRI
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/D = 50masPhotometry + spectra
heritage of SPHERE / GPI / HiCIAO
/D = 10mas - Photometry + spectra
objectives : - young giants - mature giants, spectral characterization- Super Earth : detection + 1st order charac.
16Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
Future projects … in space
Extend spectroscopic characterization towards ;
- shorter wavelengths (<1 m)- lower masses (Super Earths, Earths)- shorter separations (< 1 AU)- older objects (1 - 5 Gyr)- more distant stars (> 100 pc)- …
17Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
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Single spacecraft (later than 2020)
Small Telescopes : 1.5 - 2m
- optical quality - efficient coronagraph - focal plane WFS and correction- differential imaging
3 studies in the US :- PECO- ACCESS => Probe Class (Decadal Survey)- EPIC- SEE-COAST => CV proposal
- spectra : 0.4 - 1.0 m (R>50)- polarimetry : 0.4 - 0.85 m
objectives :- explore diversity of planets- mature giants in the visible- Super Earths- target list : HARPS, ESPRESSO, GAIA, COROT, KEPLER, …
18Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
Two spacecrafts: towards tellurics
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External Occulter Fresnel imaging lens
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Occulter : 50 mTelescope : 4 mSeparation : 80 000 kmOptimize for Vis. and UV : 0.4 -1.1 mChromatic High throughput
Occulter : 50 mTelescope : 4 mSeparation : 80 000 kmOptimize for Vis. and UV : 0.4 -1.1 mChromatic High throughput
Lens : 3.6 mTelescope : 68 cmSeparation : 2.5 - 20 kmOptimize for Vis. and UV : 0.1 -1 mChromaticLow throughput
Lens : 3.6 mTelescope : 68 cmSeparation : 2.5 - 20 kmOptimize for Vis. and UV : 0.1 -1 mChromaticLow throughput
19Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
Timeline
SPACE
GROUND
Vis / MIR - old EGPs- Super Earths- EarthsJWST
NIR + MIR old / close EGPs
8m + XAOSPHERE / GPI / HiCIAONIRyoung / massive / close EGPs
30 - 40 m + XAOEPICS / PFINIR + MIRold EGPs / Super Earth
8m + AOVLT, Keck, GeminiNIR
4m + AOSilla, CFHNIR
Room for missions !
1995 2000 2011 2017-20202007 2014
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HSTVis
20Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
Mass vs. Wavelength coverage
1
10
100
1000
10000
0,1 0,2 0,4 0,6 0,8 1 1,2 1,6 1,8 2 2,2 2,5 3 5 10 15 20
lambda ( )m
Earth masses
SPHERE GPI
HiCIAO
EPICSEPICSPFIPFI
MIRI MIRISPICASPICANIRCAM
Spa
ce te
lesc
opes
Occulters
Spa
ce
Inte
rfer
o met
ry
10 MJ
1 MJ
10 M
1 M
21Molecules in the atmosphere of extrasolar planets, Paris, 19-21 nov. 2008
A few conclusions …
1. high contrast imaging allows to study molecules in the atmosphere of a wide variety of objects
2. see the talks of this afternoon for details
3. most instruments focused on EGPs in the NIR & MIR
4. There is a gap between EGPs and Earth-like planets spectrocopy
5. What’s next (short timescale) :- spectroscopy of EGPs in the visible
- Super Earths are numerous- MIR : space interferometry more promising (see talk this
afternoon)