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Eric Pantin,
Jean Schneider, A. Boccaletti, P. Baudoz, R. Galicher, R. Gratton,
D. Stam et al.
Polarimetry and spectral imaging
of mature Jupiter and super-Earth
with SEE-COAST
SEE-COAST UCF Orlando 2
Direct
imaging
Complementarity of techniques
SPECTRA & POLARIZATION
DATA
Transi
t
SEE-COAST UCF Orlando 3
Space-based
Ground-based
1995 2000 2011 2017-20202010 >2025-30
We are here
Ground/space complementarity
SEE-COAST UCF Orlando 4
Space-based
Ground-based
1995 2000 2011 2017-2020 >2025-30
8m + OA
VLT, Keck,
Gemini
4m + OA
Silla, CFH
We are here
2010
Ground/space complementarity
HST
SEE-COAST UCF Orlando 5
Space-based
Ground-based
1995 2000 2011 2017-2020 >2025-30
We are here
2010
8m + XAO
SPHERE / GPI / HICIAO
NIR : EGPs young/massive/nearby
Ground/space complementarity
8m + OA
VLT, Keck,
Gemini
4m + OA
Silla, CFH
HST
SEE-COAST UCF Orlando 6
Space-based
Ground-based
1995 2000 2011 2017-2020 >2025-30
We are here
2010
Ground/space complementarity
8m + OA
VLT, Keck,
Gemini
4m + OA
Silla, CFH
HST
30/42m + XAO
EPICS, METIS etc with ELTs
NIR : EGPs intermediate
Old + Super-Earth ?
8m + XAO
SPHERE / GPI / HICIAO
NIR : EGPs young/massive/nearby
SEE-COAST UCF Orlando 7
Space-based
Ground-based
1995 2000 2011 2017-2020
JWST
NIR + MIR:
Old EGPs>2025-30
We are here
2010
SPICA MIR:
Old EGPs
Ground/space complementarity
8m + OA
VLT, Keck,
Gemini
4m + OA
Silla, CFH
HST
30/42m + XAO
EPICS, METIS etc with ELTs
NIR : EGPs intermediate
Old + Super-Earth ?
8m + XAO
SPHERE / GPI / HICIAO
NIR : EGPs young/massive/nearby
SEE-COAST UCF Orlando 8
Space-based
Ground-based
1995 2000 2011 2017-2020
Darwin/TPF-I
MIR: Earth
TPF-C
Vis: Earth
>2025-30
We are here
?
?
2010
JWST
NIR + MIR:
Old EGPs
SPICA MIR:
Old EGPs
Ground/space complementarity
8m + OA
VLT, Keck,
Gemini
4m + OA
Silla, CFH
HST
30/42m + XAO
EPICS, METIS, etc with ELTs
NIR : EGPs intermediate
Old + Super-Earth ?
8m + XAO
SPHERE / GPI / HICIAO
NIR : EGPs young/massive/nearby
SEE-COAST UCF Orlando 9
Space-based
Ground-based
1995 2000 2011 2017-2020 >2025-30
Visible light
Old giants & super-Earths
We are here
?
?
2010
JWST
NIR + MIR:
Old EGPs
SPICA MIR:
Old EGPs Darwin/TPF-I
MIR: Earth
TPF-C
Vis: Earth
?
?Ground/space complementarity
8m + OA
VLT, Keck,
Gemini
4m + OA
Silla, CFH
HST
30/42m + XAO
EPICS, METIS, etc with ELTs
NIR : EGPs intermediate
Old + Super-Earth ?
8m + XAO
SPHERE / GPI / HICIAO
NIR : EGPs young/massive/nearby
Opportunity for space
projects
SEE-COAST UCF Orlando 10
Space-based
Ground-based
1995 2000 2011 2017-2020 >2025-30
We are here
?
?
2010
JWST
NIR + MIR:
Old EGPs
SPICA MIR:
Old EGPs Darwin/TPF-I
MIR: Earth
TPF-C
Vis: Earth
?
?
SEE COAST Vis/NIR
Old Jupiter + Super Earth
Ground/space complementarity
8m + OA
VLT, Keck,
Gemini
4m + OA
Silla, CFH
HST
30/42m + XAO
EPICS, PFI, etc with ELTs
NIR : EGPs intermediate
Old + Super-Earth ?
8m + XAO
SPHERE / GPI / HICIAO
NIR : EGPs young/massive/nearby
SEE-COAST UCF Orlando 11
What SEE-COAST will characterize :
What's expected :
Exo-zodiacal and debris disk
Mature Jupiter (>1 Gyr)
And unexpected objects !Stay open-minded (cf. hot Jupiter in 1995)
Brighter
Atmosphere, climate
Variations, habitability
Super
Earth
Around nearby star
-
SEE-COAST UCF Orlando 13
Polarimetry : physical informationsJupiter-like planet - Stam et al. 2005
Spectrum
Polarization
Earth-like planet - Stam et al. 2008
cloud
vegetation
oceanA=0
A=1
SEE-COAST UCF Orlando
- Spectral time variation=> variation of temperature
=> surface properties
0.45 m
0.75 m
- Polarimetric time variation => surface properties
Cloud free Earth from 0.65 to 0.9 m
50° Phase angle
130°90°
• Spectroscopy• Polarimetry• Variability
SEE-COAST UCF Orlando 17
How many detections ?
1e-9
1e-10
Requirements : 10-10 contrast Small inner working angles
SEE-COAST UCF Orlando 18
Hyperbolic secondary mirror 4,85m long
Parabolic primary mirror
Two folding
mirrors
Focal plane Submitted in 2007 to
ESA Cosmic Vision
SEE-COAST proposed to ESA Cosmic VisionParameter Value
Entrance pupil diameter D > 1.5m
Angular resolution 70 mas @ 0.6 m
Contrast (after speckle subtraction) @ 2 /D
< 10-9
Contrast (after speckle subtraction) @ 4 /D
< 10-10
Orbit for 6 months visibility, high thermal stability
L2 Lagrangian
SEE-COAST UCF Orlando
1) Coronagraphy2) Wavefront control (a few nm rms from science image)
3) Polarization+Spectral Differential imaging
SEE-COAST : optical concept
1) visible light channel (0.4-0.85 m): 2 polarimetric arms
2) Near-IR channel (0.85-1.25 m): no polarimetry
SEE-COAST UCF Orlando 20
Main component I: Achromatic Coronagraph
Laboratory "planet"
Contrast : 6.7 10- 9
at 4.5/D= 20%
Visible lightBaudoz et al. 2007, 08
Multi-stage four quadrant
phase mask coronagraph
SEE-COAST UCF Orlando 21
Main component II: Wavefront correction
Speckle nulling
in a limited FOV
with a DM (JPL, Trauger
& Traub, 07)
2 stages WFS: 1st stage : Classical WFS+DM (~1 nm rms residuals) 2nd stage : Phase correction in coronagraphic image : wavefront error
reduced by 100, spurious speckles by a factor 10 000 (speckles nulling).
2 DMs concept is preferred (and envisioned)
SEE-COAST UCF Orlando 22
Main component III :
Integral Field Spectrometer (R=40-80)
Field position
Wavelength
SEE-COAST UCF Orlando 23
Main component IV :
Reject efficiently spurious star speckles
1) differential polarimetry
Field position
Wavelength
2) spectral deconvolution (aberrations scale with )
Wavelength
3) Self-coherent method (Baudoz, 07)
SEE-COAST UCF Orlando
SummarySEE COAST requires :
High contrast : ≈ 10-10 AND small IWA : ≈ 2 /D
SEE COAST can get :
low res spectra of mature giants < 20pc (< 8 - 10 AU)
colors of a few mature Super Earths < 10pc (< 4 - 5 AU)
possibly Earths around the nearest star ( Cen)
low res spectra of self luminous planets (extension to near IR)
SEE COAST is :
Compatible with general astrophysics (pushing to UV, wide field ?)
Compatible with transit spectroscopy
additional targets (unresolved planets) & complements IR transit characterization programs
Next steps in the project :
refine some science cases and simulations (statistical analysis)
elaborate optical design with industrial partners (Astrium) + derive tolerances
technological developments in coronagraphy and wavefront control
get prepared for next COSMIC VISION proposal (2010)
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