Exo-planets Direct Imaging
A New for Exoplanet ImagingGal Chauvin
- IPAG/CNRS - Institute of Planetology & Astrophysics of
Grenoble/France
GAIA-ESF Workshop November, 5th 2012, Torino
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)
. Prsentation: GCh, IPAG, member of the VLT/SPHERE consortium.
Purpose: In the context of GAIA, I will show why imaging is
important for our understanding of exoplanetary systems, their
properties & formation. Entering a new era with the 2nd
gerenation of planet imager instrument. highlight the synergy btw
Imaging and GAIA 1OutlineA New Era for Exoplanet ImagingI-
Introduction: Why Imaging?II- Techniques & StrategyIII-
Results: What can we learn?IV A New Era: VLT/SPHERE GAIA-ESF
Workshop November, 5th 2012, Torino1. Specifity of imaging in
comparison with other Planet Hunting Techniques2. briefly introduce
technical challenge, limitations & strategy3. Results, some
illustrations of results obtained at IPAG4. Finally, why we are
entering a new era with the new generation of planet imagers2I-
IntroductionPlanet Hunting Techniqueshttp://exoplanet.eu/
Radial Velocity . Indirect technique: Doppler shift (Targets:
quiet stars; activity)
. Orbital & Physical properties: > Mp.sin(i), P, e, a,
& 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
. Radial Velocity technique, indirect, successfull with more
than 800 EGPsRepresented here in a diagra showing their masses as a
function of smaEnable the determinatoin of the Planet orbital
properties and the minimum massSpin-Orbit, Architacture &
Dynamics, also access telluric masses and explore the presence of
super-Earths in HZStatistics: Occurrence 10-30%, depedence on host
properties
I- IntroductionPlanet Hunting Techniqueshttp://exoplanet.eu/
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. Transit observations, very close-in planets . Access radius,
inclination, true mass and density, . Planetary interiors. CoRot
& Kepler results: multiple systems, architecture &
stability.. Transmission/emission spectroscopy. Composition, T-P
profile, circulation & evaporating atmosphere. I-
IntroductionPlanet Hunting Techniqueshttp://exoplanet.eu/
-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, , T0 (1-5 AU) Bean
et al. 07, 08; Benedict et al. 02, 10 Muterspaugh et al. 10;
Sozzetti et al. 10
micro-lensing, based on 1 grav. event Sensitive down to telluric
planets (1-5AU); Problems for follow-up (distant targets)AND
Astrometry, mainly used for the characterization of know planets
detected in RV: i, true mass, more sensitive at long periods >
But should soon provide several thousands of new planetary systems
with GAIA up to 5-10 AU. I- IntroductionPlanet Hunting
Techniqueshttp://exoplanet.eu/
Direct Imaging . Direct technique: Planets photons(Targets:
young & nearby stars)
. Orbital & Physical properties: > L, a , e, i, , T0 >
Giant planets at wide orbits (>10 AU) > Multiple:
Architecture & Stability > Planet disk connection Chauvin et
al. 05, 10; Lafrenire 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...
Janson et al. 10; Bonnefoy et al. 09, 12 . In this context imaging
is unique:. To probe the propeteries of the our regions of
planetary systems. Access the luminosity and enable spectroscopy of
non-strongly irradieted giant planets. But also offer the
possibility to study young systems (not sensitive to activity),
dynamical evolution of planeatry systems and the connection btw
recently formed giant planets and the circumstellar environment.
OutlineA New Era for Exoplanet ImagingI- Introduction: Why
Imaging?II- Techniques & StrategyIII- Results: What can we
learn?IV A New Era: VLT/SPHERE GAIA-ESF Workshop November, 5th
2012, Torino2. Now what about the observing challenge, the
limiations and the strategy to image ginat
planets?7Detect/characterize something faint, angularly close to
something bright.Imaging: an observing challenge!II- Strategy High
image quality - High angular resolution, PSF Stability- Calibration
of static aberrations
Stellar Halo Brightness - Halo attenuation/PSF subtraction -
Speckle noise Intrinsic companion faintness - Long overall
observations;
HIP95270 (Tuc-Hor)VLT/NaCo H, 10 by 10
(?)
(?)
. The observing challenge: to detect sth faint angularly cose
sth bright. to get relative photometry, astrometry and possibly
start getting a spectral characterization of the object. For this
you need to deal with various important issues1. High image
quality, HAR, stable PSF2. Stellar Halo attenuation, PSF
subtraction and residual Speckle noise3. Faintness of the
companion, overall long exposures
Dedicated Instrumentation
High Angular Resolution Space telescope 10m-telescopes + AO
system
VLT/NACO
Gemini S/NKeckSubaru/HiCIAOHST
LBT/ArizonaII- StrategyHAR:. Space. Ground-based Telescope to
compensate for the atmosphere turbulence Adaptive optics (recover
diffraction-limit resolution) Impressive evolutionHigh Angular
Resolution
II- Strategy. In that context, development in instrumentation,
larger mirrors and faster and more complex AO system have clearly
shown an impressive evolution over the past decade . This is well
illustrated by the AO images of the GQ Lupi companion detected by
Neuhauser et al. In 2005 was hardly distinguishable in 1995 from a
speckle pattern with the first ESO AO system Come-On+ . GPI, SPHERE
>1000 actuatorsThe art of PSF subtraction 1 (i.e 19AU@19pc)Field
Rotation
II- StrategyVLT/NaCoHigh Contrast at inner angles Main
limitation ( 200 AU Closer PMCs:- A4V-A5V massive primaries- q <
0.005 ; = 8 - 120 AU- CS Disk signatures IV- Key results
2M1207 DH Tau AB Pic SCR1845 CHXR 73GQ Lup1RXJS609CT ChaGJ
758Ref: Chauvin et al. 04; Itoh et al. 05; Chauvin et al. 05;
Biller et al. 05; Luhman et al. 06; Thalmann et al. 09; Lafrenire
et al. 08; Neuhauser et al. 05; Schmidt et al. 09; Lagrange et al.
10; Kalas et al. 08; Marois et al. 08,10...Familys portrait.
Planetary mass companions have been imaged and characterized . 2
classes: first detections of wide PMCs around GKM dwarfs: low-q
and/or large phys. sep More recently, detection of closer PMCs
around massive stars: high-q and phys sep 8 115 AU and a connection
with the presence of disk signatureOuter Giant Planet
PopulationPhysics of Giant PlanetsOccurrence &
FormationArchitecture & StabilityStatistical properties
(occurrence, planetary host dependency, disk properties)Formation
Theories: CA, GI or CFAstrometry & Disk/Planet Orbits,
dynamical interactions, resonances & long-term evolution
Photometry & SpectroscopyAtmosphere & physical
propertiesIV- Key results. All these recents
results/detection/non-detection teach us about:1/ Physics of the
Giant Planet Population at Wide Orbits: Luminosity & SED
(composition, clouds coverage)2/ Architecture, orbita properties
and stability3/ Occurrence & Formation mechanisms via thei
statistical properties Physics of Giant PlanetsIV- Key
resultsCompanion nature?
Planet Single-band photometry Stellar properties: d & age
Evolutionary models (Luminosity - Mass). Pictoris b, J = 10.6+-0.3
mag,. 12 Myr @ 19.3 pc,. Mass = 7 8 Mjup (Hot-Startmodels)
> However, uncertainties in the model predictions >
Dependence: formation mechanisms , gas accretion shock &
initial conditions
VLT/NaCo ADI imagingField Rotation
Bonnefoy et al. 12Marley et al. 07; Mordasini et al. 12 .
Reminder: for all imaged planets we observed the planets
luminosity. The mass in infered from evol. Model predictions, that
depens on the initial conditions, formation mechanisms, accretion
shock during the formation.. Combination of RV + Imaging or
Astrometry + Imaging > Mass Luminosity diagram to calibrate the
modelsPhysical propertiesIV- Key resultsAtmosphere
Planets SED Stellar properties: d & age Synthetic-Grid of
spectra
Atmospheric properties
Pic b, Teff = 1650 +- 150K, log(g) = 4.00.5, FeH = 0.00.5, R =
1.3+-0.2 RJup> dusty clouds (L-type)
. Radiative transfert code . Dusty Cloud Formation/Sedim. . Mol.
opacity / Non-eq Chem. Bonnefoy et al. 12. Determination of the
spectral properties.. Use of atmophere model predictions to
describe the physical & chemical process at work.. In the
context of Bpic b, low-gravity atmosphere (~early-L). Presence of
dusty clouds and patch. We are currently a new spectroscopic
classification of cool and low-gravity atmopsheres (young T
dwarfs), . implication of low-gravity conditions on the
atmosphereic properties (HR8799bcde an no CH4 presence at Teff =
1000K). IV- Key results
Nov 2003Oct 2009500 mas
N
E
Imaging Exoplanets revolution Lagrange et al. 09, 10Bonnefoy et
al. 10, Quanz et al. 10Orbital Properties & Architecture
Discovery: Nov 2003 L = 7.7 mag, sep = 300 +- 15 mas Monitoring
campaign: 2008 - now Recovery: Oct. 2009 VLT/NaCo ADI
imagingL-band, Pic b. Focus on orbital properties and the planetary
system architecture. Detection/Recovery: first direct imaging of
exoplanets revolution. Follow-up to constrain orbital properties
IV- Key resultsN
E
Imaging Exoplanets revolution Chauvin et al. 12Orbital
Properties & Architecture Discovery: Nov 2003 . L = 7.7 mag,
sep = 300 +- 15 mas Monitoring campaign: 2008 - nowRecovery: Oct.
2009Astrometric follow-up . VLT/NaCo monitoring 2003 - 2012
. Follow-up to constrain orbital properties with various epochs
btw 2003, 2008 and 2012.. MCMC analysis to derive the most probable
orbital parameters (similar studies for hr8799bcde, Soummer et al.;
Esposito et al.,)
IV- Key results
Constraining the orbitOrbital Properties & Architecture MCMC
Orbital fitting Pic b, P = 17 - 21 yrs a = 8 - 10 AU e < 0.17 i
= 88.5 +- 1.5 deg = 212.5 +- 1.5 deg Chauvin et al. 12 N
E
. MCMC analysis to derive the most probable orbital parameters
(similar studies for hr8799bcde, Soummer et al.; Esposito et al.,).
8-10 AU (parameter space where CA is still efficient), Low-ecc, big
omega compatible with the planet being in the warp component of the
Bpic disk
IV- Key resultsConstraining the orbitOrbital Properties &
Architecture Planet Disk connection. main disk, up to 20 (1000 AU),
PAMD = 209.5+-0.3deg . Pic b PA Pic b = 212.0+-1.3o
> Pic b in the disks warp, Lagrange et al. 12N
E
N
E
2
Main diskWarp. Planet Disk simultaneous characterization
unambiguously confirm that the planet is not in the MD, more likely
in the warp component, being responsible for the warp formation,
clear planet disk interaction. . In the context of imaged planets,
Bpi b planet is the most favorable one for a formatio by CA (8
AU).
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
IV- Key resultsCrida et al. 09; Scharf & Menou 09CA
LimitFormation & Evolution. Another way to explore the possible
origins of the imaged giant planets is to plot them as a function
of sma with the predictions of plabetary formation mechanisms.
Blue: low-q PMCs. Red: high-q with CS disks presence. Only Bpicb,
hr8799d, e? CA, need alternative mechanisms at wide orbits or evoke
dynamical evolution (outward migration or planet plnaet
interactions). BUT, clearly the next step now is to image more of
these systems to derive the statitstical properties of the
poulation of giant planets at wide orbits. > systematic
searches
OutlineA New Era for Exoplanet ImagingI- Introduction: Why
Imaging?II- Techniques & StrategyIII- Results: What can we
learn?IV A New Era: VLT/SPHERE GAIA-ESF Workshop November, 5th
2012, Torino4. SPHERE
26Upcoming 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 starsV- A New Era V- A New Era SPHERE
concept
ZIMPOLIRDISIFSFoVSq 3.5 (instantaneous)Up to 4 radius (mosaic)Sq
11Sq 1.77Spectral Range0.5 0.9 m0.95 2.32 m0.95 1.35/1.65 mSpectral
informationBB, NBBB, NBSlit spectro: 50/40050 / 30Linear
PolarisationSimultaneous on same detector, x 2 arms,
exchangeableSimultaneous dual beam, exchangeablexCoronography: no
/4Q / Lyot
Rotation at Nasmyth:Pupil-stab. (instrument fixed wrt
tel.)Field-stab (slit spectro, long DIT)No rotation: minimize
crosstalk) 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 /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
SPHERE InstrumentsV- A New Era Observing with SPHERESPHERE
Timeline,Fall 12, Tests @IPAGMarch 13PAE April 13ShippingMay 13
Integration @ParanalJuly & Dec 13First Light &
Commissioning phase 1, 2 & 3March 14CfP 94, offered to the ESO
community- All offered mode fully supported/documented, -
Calibration & data reduction pipelineGTO (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
GAIASPHEREELT-PCSGAIAhttp://exoplanet.eu/Mesa et al. 11Kasper et
al. 10Lattanzi & Sozzetti 10V- A New Era Synergy with GAIAGAIAs
planetary systems About 10 000 EGPs with GAIA for (d < 200 pc, V
< 13) stars. Marginal overlap with SPHERE- favorable cases (very
nearby), GAIA > planets orbital phase - Follow-up for
Photometric/Spectroscopic characterization> but, will have to
wait for ELT-(IFU & PCS) for systematic study Outer regions of
GAIAs 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, TorinoIV- Key
resultsMass determination& related uncertainties
Cold startHot start Planet photometry & spectroscopy Stellar
properties: d & age Evolutionary model predictions .
not-calibrated at young ages. Role of initial conditions Hot-start
(Baraffe et al. 03; Burrows et al. 03) Cold start Core Accretion
(Marley et al. 07; Fortney et al. 08)Hot startPhysical properties.
For that aspect: a first issue to keep in mind is that for all
discovered PMC we use A Mass Luminosity relation based a/ planet
photometry & spectroscopyb/ star propertiesc/ Evol Model
Predictions (not well calibrated and importance of Initial
Conditions and Formation)IV- Key resultsMass determination&
related uncertainties
Cold startHot start Planet photometry & spectroscopy Stellar
properties: d & age Evolutionary model predictions .
not-calibrated at young ages. Role of initial conditions Hot-start
(Baraffe et al. 03; Burrows et al. 03) Cold start Core Accretion
(Marley et al. 07; Fortney et al. 08)Hot start Pic b7-8
MJupPhysical properties. For that aspect: a first issue to keep in
mind is that for all discovered PMC we use A Mass Luminosity
relation based a/ planet photometry & spectroscopyb/ star
propertiesc/ Evol Model Predictions (not well calibrated and
importance of Initial Conditions and Formation)IV- Key resultsN
E
Constraining the orbit (MCMC Orbital fitting)Orbital Properties
& Architecture
. Use of all detection around various stars a,d null detection
to constraint the Frequency of GP at all orbitsIV- Key results500
mas
N
E
Disk-Planet connection
Orbital Properties & ArchitectureLagrange et al. (12) 2
Oct 2009N
E
Imaging the inner disk of 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 . Where is the planet? . Use of all detection
around various stars a,d null detection to constraint the Frequency
of GP at all orbitsIV- Key resultsNov 2003Oct 2009500 mas
N
E
Disk-Planet connection
Orbital Properties & ArchitectureOct 2009N
E
2
Imaging the inner disk of 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 . Where is the planet? Lagrange et al.
(12)WarpMain disk. Use of all detection around various stars a,d
null detection to constraint the Frequency of GP at all orbitsIV-
Key resultsNov 2003Oct 2009500 mas
N
E
Disk-Planet connection
Orbital Properties & Architecture
Oct 2009N
E
2
Imaging the inner disk of 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 . Planets position angle: PAb = 212.0+-1.3
deg> Probably not in the main disk, but in the warp> Inner
warped disk sculpted by the planet: (Mb < 20 Mjup ) Lagrange et
al. (12)Main diskWarp. Use of all detection around various stars
a,d null detection to constraint the Frequency of GP at all
orbits