GAIA-ESF Workshop – November, 5th 2012, Torino
A New for Exoplanet Imaging
Gaël Chauvin
- IPAG/CNRS Institute of Planetology & Astrophysics of Grenoble/France
Collaborations: J.-L. Beuzit, A.M. Lagrange, D. Mouillet, J. Rameau & P.
Delorme (IPAG/Fr); S. Desidera, D. Mesa & R. Gratton (Oss. Padova/It); A.
Boccaletti, R. Galicher, D. Rouan & P. Baudoz (LESIA/Fr); D. Apai (Uv.
Arizona/US); M. Meyer, S. Quanz & M. Reggianni (ETHZ)/Swi); M. Bonnefoy,
W. Brandner & C. Mordasini (MPIA/Ger); C. Moutou, A. Zurlo & A. Vigan
(LAM/Fr); J. Girard, C. Dumas, , J. Milli, D. Mawet & M. Kasper (ESO); S.
Udry, J. Hagelberg (Geneva/Swi)…
Outline
A New Era for Exoplanet Imaging
I- Introduction: Why Imaging?
II- Techniques & Strategy
III- Results: What can we learn?
IV – A New Era: VLT/SPHERE
GAIA-ESF Workshop – November, 5th 2012, Torino
I- Introduction
Planet Hunting Techniques
 Radial Velocity
. Indirect technique: Doppler shift
(Targets: quiet stars; activity)
. Orbital & Physical properties:
> Mp.sin(i), P, e, a, ω & T0
> Spin-Orbit Alignment
> Architecture & Stability
> exo-Earths & Habitable Zone
Dumusque et al. 12; Triaud et al. 11
. Statistics: more than 800 exoplanets
> Occurrence down to Super-Earths
> Planetary host: Fe/H & binarity
De Sousa et al. 11; Udry & Santos 07
http://exoplanet.eu/
I- Introduction
Planet Hunting Techniques
 Transit
. (In)direct technique: 1ary/2ary eclipse.
(Targets: quiet stars; activity; crowded fields)
. Orbital & Physical properties:
> R*/Rp, Mp, P, a, i, T0
> Planetary Interiors
> Multiple: Architecture & Stability
> Circumbinary planets
Leger et al. 09; Doyle et al. 11; Balatha et al. 12
. Transmission/emission spectroscopy
> Composition (H20, CO, NaI, KI... Haze)
> Vertical T-P structure, atmospheric
circulation & evaporation
Swain et al. 08; Knutson et al. 09; Desert et al. 12
http://exoplanet.eu/
I- Introduction
Planet Hunting Techniques
 μ-lensing
. Indirect technique: Unique Rel. Event
(Targets: Crowded fields; probability)
. Orbital & Physical properties:
> Mp, M*, d, P, a (1-5 AU)
> Super-Earths
. Free-floating, wide orbit planets?
Gould et al. 06; Cassan et al. 12
 Astrometry
. Indirect technique: Reflex motion
(Targets: Nearby stars)
. Orbital & Physical properties:
> Mp, P, i, e, a, ω, T0 (1-5 AU)
http://exoplanet.eu/
Bean et al. 07, 08; Benedict et al. 02, 10
Muterspaugh et al. 10; Sozzetti et al. 10
I- Introduction
Planet Hunting Techniques
 Direct Imaging
. Direct technique: Planet’s photons
(Targets: young & nearby stars)
. Orbital & Physical properties:
> L, a , e, i, ω, T0
> Giant planets at wide orbits (>10 AU)
> Multiple: Architecture & Stability
> Planet – disk connection
Chauvin et al. 05, 10; Lafrenière et al. 07
Soummer et al. 11; Vigan et al. 12
. High-contrast spectroscopy
> Non-strongly irradiated EGPs
> Low-gravity, composition, non-LTE
chemistry, cloud coverage...
http://exoplanet.eu/
Janson et al. 10; Bonnefoy et al. 09, 12
Outline
A New Era for Exoplanet Imaging
I- Introduction: Why Imaging?
II- Techniques & Strategy
III- Results: What can we learn?
IV – A New Era: VLT/SPHERE
GAIA-ESF Workshop – November, 5th 2012, Torino
II- Strategy
Imaging: an observing challenge!
Detect/characterize something faint,
angularly close to something bright.
 High image quality
- High angular resolution, PSF Stability
- Calibration of static aberrations
HIP95270 (Tuc-Hor)
VLT/NaCo H, 10” by 10”
 Stellar Halo Brightness
- Halo attenuation/PSF subtraction
- Speckle noise
 Intrinsic companion faintness
- Long overall observations;
(?)
(?)
II- Strategy
Dedicated Instrumentation
High Angular Resolution
 Space telescope
 10m-telescopes + AO system
HST
Gemini S/N
VLT/NACO
LBT/Arizona
Subaru/HiCIAO
Keck
II- Strategy
Impressive evolution
High Angular Resolution
 Adaptive optics (recover diffraction-limit resolution)
II- Strategy
The art of PSF subtraction
High Contrast at inner angles
 Main limitation (<1.0-2.0’’): Atmospheric & instrumental speckles
 Coronagraphy
- Occulting and Lyot-pupil mask
- 4QP Mask, Boccaletti et al. 08
- new: PIAAC, ALC, APC & Vortex
 Differential Imaging
- Polarimetric (PDI)
- Spectral (SDI), Close et al. 05
- Angular (ADI), Marois et al. 06
 Post-processing tools
- LOCI, Lafrenière et al. 07
- ANDROMEDA, Mugnier et al. 10
- KLIP/PCA, Soummer et al. 12
Field Rotation
VLT/NaCo
1“ (i.e 19AU@19pc)
II- Strategy
The art of PSF subtraction
High Contrast at inner angles
 Main limitation (<1.0-2.0’’): Atmospheric & instrumental speckles
 Coronagraphy
- Occulting and Lyot-pupil mask
- 4QP Mask, Boccaletti et al. 08
- new: PIAAC, ALC, APC & Vortex
 Differential Imaging
- Polarimetric (PDI)
- Spectral (SDI), Close et al. 05
- Angular (ADI), Marois et al. 06
 Post-processing tools
- LOCI, Lafrenière et al. 07
- ANDROMEDA, Mugnier et al. 10
- KLIP/PCA, Soummer et al. 12
Field Rotation
VLT/NaCo
1“ (i.e 19AU@19pc)
II- Strategy
Detection Performances
High Contrast at inner angles
 Coronagraphy or SAT-Imaging
combined with ADI, SDI (or PDI)
 Improved performances
Detection
Limits: 0.1-2.0”
inside
the IWAs:
H-band
Detection Limits:
Obs. Tobs
Time=~10min
H-band;
60-90 min
Star, H = 5-6
Star, H = 5-6
Down to ΔH = 14.0 @1.0”
(d = 30 pc)
II- Strategy
Detection Performances
High Contrast at inner angles
 Coronagraphy or SAT-Imaging
combined with ADI, SDI (or PDI)
 Improved performances
Detection
Limits: 0.1-2.0”
inside
the IWAs:
H-band
Detection Limits:
Obs. Tobs
Time=~10min
H-band;
60-90 min
Star, H = 5-6
Star, H = 5-6
Down to ΔH = 14.0 @1.0”
(d = 30 pc)
d = 30 pc, 10 Myr
COND03 Evol. Models
Baraffe et al. 03
II- Strategy
Optimized Samples
Young, nearby stars
 Age < 200 Myr
. Young, nearby associations
 Distance < 100 pc
. access small sma,
. enhanced sensitivity
 Spectral Types: AFGKM
. AF: More massive EGPs?
. M: favorable contrast
 V-band < 10.0 – 12.0
. AO-Full Performance limitation
> All observed by GAIA
NaCo Large Program’s sample,
preparatory mission to SPHERE (Chauvin et al. 10)
Outline
A New Era for Exoplanet Imaging
I- Introduction: Why Imaging?
II- Techniques & Strategy
III- Results: What can we learn?
IV – A New Era: VLT/SPHERE
GAIA-ESF Workshop – November, 5th 2012, Torino
IV- Key results
Family’s portrait
2M1207
DH Tau
AB Pic
SCR1845
CHXR 73
GJ 758
CT Cha
1RXJS609
GQ Lup
 Wide orbit PMCs:
- low mass KM stars
- q = 0.02 – 0.2 or Δ > 200 AU
 Closer PMCs:
- A4V-A5V massive primaries
- q < 0.005 ; Δ = 8 - 120 AU
- CS Disk signatures
Fomalhaut
Hr8799
Beta Pic
Ref: Chauvin et al. 04; Itoh et al. 05; Chauvin et al. 05; Biller et al. 05; Luhman et al. 06; Thalmann et al. 09;
Lafrenière et al. 08; Neuhauser et al. 05; Schmidt et al. 09; Lagrange et al. 10; Kalas et al. 08; Marois et al. 08,10...
IV- Key results
Outer Giant Planet Population
Architecture & Stability
Physics of Giant Planets
Photometry & Spectroscopy
Atmosphere
& physical properties
Astrometry & Disk/Planet
Orbits, dynamical interactions,
resonances & long-term evolution
Occurrence & Formation
Statistical properties (occurrence,
planetary host dependency, disk
properties)
Formation Theories: CA, GI or CF
IV- Key results
Physics of Giant Planets
Companion nature?
 Planet Single-band photometry
 Stellar properties: d & age
 Evolutionary models (Luminosity - Mass)
. β Pictoris b, ΔJ = 10.6+-0.3 mag,
. 12 Myr @ 19.3 pc,
. Mass = 7 – 8 Mjup (“Hot-Start”models)
> However, uncertainties in the model predictions
> Dependence: formation mechanisms , gas
accretion shock & initial conditions
Marley et al. 07; Mordasini et al. 12
Field Rotation
VLT/NaCo ADI imaging
Bonnefoy et al. 12
IV- Key results
Physical properties
Atmosphere
 Planet’s SED
 Stellar properties: d & age
 Synthetic-Grid of spectra
. Radiative transfert code
. Dusty Cloud Formation/Sedim.
. Mol. opacity / Non-eq Chem.
 Atmospheric properties
β Pic b,
Teff = 1650 +- 150K, log(g) = 4.0±0.5,
FeH = 0.0±0.5, R = 1.3+-0.2 RJup
> dusty clouds (Lβ-type)
Bonnefoy et al. 12
IV- Key results
Orbital Properties & Architecture
Imaging Exoplanet’s revolution
 Discovery: Nov 2003
Nov 2003
Oct 2009
ΔL’ = 7.7 mag, sep = 300 +- 15 mas
 Monitoring campaign: 2008 - now
 Recovery: Oct. 2009
Lagrange et al. 09, 10
Bonnefoy et al. 10, Quanz et al. 10
N
VLT/NaCo ADI imaging
L’-band, β Pic b
500 mas
E
IV- Key results
Orbital Properties & Architecture
Imaging Exoplanet’s revolution
 Discovery: Nov 2003
. ΔL’ = 7.7 mag, sep = 300 +- 15 mas
 Monitoring campaign: 2008 - now
 Recovery: Oct. 2009
 Astrometric follow-up
. VLT/NaCo monitoring 2003 - 2012
Chauvin et al. 12
N
E
IV- Key results
Orbital Properties & Architecture
Constraining the orbit
 MCMC Orbital fitting
β Pic b,
P = 17 - 21 yrs
a = 8 - 10 AU
e < 0.17
i = 88.5 +- 1.5 deg
Ω = 212.5 +- 1.5 deg
Chauvin et al. 12
IV- Key results
Orbital Properties & Architecture
Constraining the orbit
Main disk
2“
Warp
 Planet – Disk connection
. main disk, up to 20’’ (1000 AU),
PAMD = 209.5+-0.3deg
. β Pic b
PAβ Pic b = 212.0+-1.3o
> β Pic b in the disk’s warp, Lagrange et al. 12
N
E
IV- Key results
Formation & Evolution
 In-situ Core Accretion does not work at > 20-30 AU
> Core or Disk fragmentation ?
Dodson –Robinson et al. 09; Boley et al. 09
> Inner limit to the Core or Disk fragmentation?
 Dynamical evolution & stability
> outward migration (corotation torque), planet scattering & resonances
Crida et al. 09; Scharf & Menou 09
Outline
A New Era for Exoplanet Imaging
I- Introduction: Why Imaging?
II- Techniques & Strategy
III- Results: What can we learn?
IV – A New Era: VLT/SPHERE
GAIA-ESF Workshop – November, 5th 2012, Torino
V- A New Era
Upcoming instruments (mid-2013),
 GPI,
Gemini Planet Finder (MacIntosh et al. 08)
- Fast-high order adaptive optics system
- Interferometric wave front sensing for static aberrations
- NIR-IFU + Apodized pupil Lyot coronagraph
 VLT/SPHERE (Beuzit et al. 08)
- SAXO, Extreme AO system (ITTM-DM and DTTS, PTTS)
- NIR (YJHK): IRDIS (Dual imaging Spectrograph) and IFU 3D-spectroscopy
- VIS: ZIMPOL (Imaging Polarimeter)
- Coronagraphs: Classical Lyot, A4P and ALC
- GTO of 260 nights; 200 devoted to survey 300 nearby stars
V- A New Era
SPHERE concept
V- A New Era
SPHERE Instruments
ZIMPOL
IRDIS
IFS
FoV
Sq 3.5’’
Sq 11’’
Sq 1.77’’
Spectral Range
0.5 – 0.9 μm
0.95 – 2.32 μm
0.95 – 1.35/1.65 μm
Spectral
information
BB, NB
BB, NB
50 / 30
Slit spectro: 50/400
Linear
Polarisation
Simultaneous on same
Simultaneous dual
(instantaneous)
Up to 4’’ radius (mosaic)
detector, x 2 arms,
exchangeable
Coronography: no /4Q / Lyot
Rotation at Nasmyth:
Pupil-stab. (instrument fixed wrt tel.)
Field-stab (slit spectro, long DIT…)
No rotation: minimize crosstalk…)
beam, exchangeable
x
AO sensitivity for high contrast:
R=9.5 for NIR; R=9 for R; R=7.8 for whole VIS
Separation with improved contrast:
2 - 20 λ/D, ie 30-300 mas in R, or 80 – 800 mas in H
Mode switching: not VIS and NIR in same night
V- A New Era
Observing with SPHERE
SPHERE Timeline,
•
•
•
•
•
•
Fall 12,
March 13
April 13
May 13
July & Dec 13
March 14
Tests @IPAG
PAE
Shipping
Integration @Paranal
First Light & Commissioning phase 1, 2 & 3
CfP 94, offered to the ESO community
- All offered mode fully supported/documented,
- Calibration & data reduction pipeline
• GTO (260 nights over 3 - 5 yrs; 26-40 nights/semester)
> NIRSUR: SPHERE Giant Planet Search (200 nights)
- 400-600 stars observed (Age < 1 Gyr; SpT: AFGKM; < 100-150 pc)
- Occurrence & properties of the giant planet population at wide orbits (> 10 AU)
V- A New Era
Synergy with GAIA
V- A New Era
Synergy with GAIA
SPHERE
GAIA
ELT-PCS
http://exoplanet.eu/
Mesa et al. 11
Kasper et al. 10
Lattanzi & Sozzetti 10
V- A New Era
Synergy with GAIA
GAIA’s planetary systems
 About 10 000 EGPs with GAIA for (d < 200 pc, V < 13) stars.
 Marginal overlap with SPHERE
- favorable cases (very nearby), GAIA > planet’s orbital phase
- Follow-up for Photometric/Spectroscopic characterization
> but, will have to wait for ELT-(IFU & PCS) for systematic study
 Outer regions of GAIA’s planetary systems
- Could help to constrain GAIA astrometric solutions (long-periods)
- Outer planets detection & characterization in synergy with GAIA
> Architecture, Dynamical evolution, Stability & Formation
To conclude: GAIA will provide a rich list of targets for Imaging surveys
Thank You!
GAIA-ESF Workshop – November, 5th 2012, Torino
IV- Key results
Physical properties
Mass determination
& related uncertainties
 Planet photometry & spectroscopy
 Stellar properties: d & age
 Evolutionary model predictions
. not-calibrated at young ages
. Role of initial conditions
“Hot-start”
Hot start
(Baraffe et al. 03; Burrows et al. 03)
“Cold start” – Core Accretion
(Marley et al. 07; Fortney et al. 08)
Cold start
IV- Key results
Physical properties
Mass determination
& related uncertainties
 Planet photometry & spectroscopy
 Stellar properties: d & age
 Evolutionary model predictions
. not-calibrated at young ages
. Role of initial conditions
“Hot-start”
β Pic b
7-8 MJup
Hot start
(Baraffe et al. 03; Burrows et al. 03)
“Cold start” – Core Accretion
(Marley et al. 07; Fortney et al. 08)
Cold start
IV- Key results
Orbital Properties & Architecture
Constraining the orbit (MCMC Orbital fitting)
N
E
IV- Key results
Orbital Properties & Architecture
Disk-Planet connection
2“
 Imaging the inner disk of β Pictoris
Lagrange et al. (12)
. the main disk, up to 20’’ (1000 AU), PAMD = 209.5+-0.3deg
. The warp-component, 0 – 5’’ (0 – 100 AU), PAW = 212.5 deg
N
. Where is the planet?
500 mas
E
IV- Key results
Orbital Properties & Architecture
Disk-Planet connection
Nov 2003
Main disk
2“
Oct 2009
Warp
 Imaging the inner disk of β Pictoris
Lagrange et al. (12)
. the main disk, up to 20’’ (1000 AU), PAMD = 209.5+-0.3deg
. The warp-component, 0 – 5’’ (0 – 100 AU), PAW = 212.5 deg
N
. Where is the planet?
500 mas
E
IV- Key results
Orbital Properties & Architecture
Disk-Planet connection
Nov 2003
Main disk
2“
Oct 2009
Warp
 Imaging the inner disk of β Pictoris
. the main disk, up to 20’’ (1000 AU), PAMD = 209.5+-0.3deg
. The warp-component, 0 – 5’’ (0 – 100 AU), PAW = 212.5 deg
N
. Planet’s position angle: PAb = 212.0+-1.3 deg
> Probably not in the main disk, but in the warp…500 mas
> Inner warped disk sculpted by the planet: (Mb < 20 Mjup )
Lagrange et al. (12)
E