AO4ELT, Paris, 23 June 2009 EPICS, exoplanet imaging with the E-ELT Markus Kasper, Jean-Luc Beuzit, Christophe Verinaud, Emmanuel Aller- Carpentier, Pierre

AO4ELT, Paris, 23 June 2009

EPICS, exoplanet imaging with the E-ELTEPICS, exoplanet imaging with the E-ELT

Markus Kasper, Jean-Luc Beuzit, Christophe Verinaud, Emmanuel Aller-Markus Kasper, Jean-Luc Beuzit, Christophe Verinaud, Emmanuel Aller-Carpentier, Pierre Baudoz, Anthony Boccaletti, Mariangela Bonavita, Carpentier, Pierre Baudoz, Anthony Boccaletti, Mariangela Bonavita,

Kjetil Dohlen,Kjetil Dohlen, Raffaele G. Gratton, Norbert Hubin, Florian Kerber, Visa Raffaele G. Gratton, Norbert Hubin, Florian Kerber, Visa Korkiaskoski, Patrice Martinez, Patrick Rabou, Ronald Roelfsema, Korkiaskoski, Patrice Martinez, Patrick Rabou, Ronald Roelfsema, Hans Hans

Martin Schmid, Niranjan Thatte, Lars Venema, Martin Schmid, Niranjan Thatte, Lars Venema, Natalia YaitskovaNatalia Yaitskova

ESO, LAOG, LESIA, FIZEAU, Osservatorio Astronomico di Padova, ESO, LAOG, LESIA, FIZEAU, Osservatorio Astronomico di Padova, ASTRON, ETH Zürich, University of Oxford, LAMASTRON, ETH Zürich, University of Oxford, LAM, NOVA, NOVA

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Outline

Science goals (6s) Instrument and AO concept (12s) Science Output prediction (4s)

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Exoplanets observations early 2009Exoplanets observations early 2009

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~ 300 Exoplanets detected, >80% by radial velocities, mostly gas giants, a dozen Neptunes and a handful of Super-Earths

Constraints on Mass function, orbit distribution, metallicity

Some spectral information from transiting planets

Spectrum of HD 209458b Richardson et al., Nature 445, 2007

33HR 8799, Marois et al 2008 Beta Pic, Lagrange et al 2009


(Some) open issues(Some) open issues

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Planet formation (core accretion vs gravitational disk instability)

Planet evolution (accretion shock vs spherical contraction / “hot start”)

Orbit architecture (Where do planets form?, role of migration and scattering)

Abundance of low-mass and rocky planets Giant planet atmospheres

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Object Class 1, young & self-lumObject Class 1, young & self-lumPlanet formationPlanet formation

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in star forming regions or young associations

Requirements:• High spat. resolution of ~30 mas (3 AU at 100 pc, snow line for G-star )• Moderate contrast ~10-6

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Object Class 2, within ~20 pcObject Class 2, within ~20 pcOrbit architecture, low-mass planet abundance Orbit architecture, low-mass planet abundance

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~500 stars from Paranal ± 30 deg, ~60-70% M-dwarfs

Requirements

• High contrasts~10-9 at 250 mas (Jupiter at 20pc)

• + spatial resolution ~10-8 at 40 mas (Gl 581d,~8 M)

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AO4ELT, Paris, 23 June 2009 77

Object Class 3, already known onesObject Class 3, already known onesPlanet evolution and atmospheresPlanet evolution and atmospheres

discovered by RV, 8-m direct imaging (SPHERE, GPI) or astrometric methods (GAIA, PRIMA)

SPHERE discovery space

GAIA discovery space

From ESO/ESA WG report

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Contrast requirements summaryContrast requirements summary

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Concept

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Concept: Achieve very high contrast

Highest contrast observations require multiple correction stages to correct for

1. Atmospheric turbulence2. Diffraction Pattern3. Quasi-static instrumental

aberrations

XAO

Visible diffraction suppression

Diff. Pol.

IFS

Coherence-based concept?

XAO, S~90% Diffraction + staticaberration correction

Speckle Calibration,Differential Methods

Contrast ~ 10-3-10-4 Contrast ~ 10-6 Contrast ~ 10-9

x 1000 !

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NIR diffraction suppression


XAO concept

Main parameters (baseline)

Serial SCAOM4 / internal WFS, XAO

XAO: roof PWS at 825 nm, 3 kHz

200x200 actuators (20 cm pupil spacing)

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RTC requirements:Efficient algorithms studied outside EPICS phase-A

Numerical simulation, see poster of Visa Korkiakoski

AO + coro

1e-6

1e-7


High Order Testbench (HOT)Demonstrate XAO / high contrast concepts

Developed at ESO in collaboration with Arcetri and Durham Univ. Turb. simulator, 32x32 DM, SHS, PWS, coronagraphy, NIR camera H-band Strehl ratios ~90% in 0.5 seeing (SPIE 2008, Esposito et al.

& Aller-Carpentier et al. ) correcting 8-m aperture for ~600 modes

2 4 6 8 10 1250

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60

65

70

75

80

85

90

95

100

Star magnitude

SR

(%

)

See poster of Aller-Carpentier


HOT: XAO with APL coronagraph

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700K object next to K0 star• Good agreement with SPHERE simulations

• Additional gain by quasi-static speckle calibration (SDI, ADI)


HOT speckle stability

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0 + 6hrs +30 hrs


Correction of quasi-static WFE incl. segments piston

Standard WFE specs ok for most optics (near pupil)

DM “cleans” its control area from speckles Need: measure static aberrations some nm level at science

wavelength through residual turbulence (PD or Speckle Nulling)

Concept to be demonstrated FP7 funded exp. (FFREE@LAOG and HOT)

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HOT: Segments piston and correction of quasi-static WFE

0.05

0.1

0.15

0.2

0.25

0.3

0.05

0.1

0.15

0.2

0.25

0.3

With segmentation

HOT pupil with DM and segmentation


Residual PSF calibration

Getting from systematic PSF residuals (10-6-10-7) to 10-8-10-9

Spectral Devonvolution (Sparks&Ford, Thatte et al.), Trade-off: spectral bandwidth vs inner working angle, IFS (baseline Y-H)

Multi-band spectral or polarimetric differential imaging for smallest separation, needs planet “feature” (e.g. CH4 band, or polarization) IFS and differential polarimeter (600-900 nm)

Coherence based methods (speckles interfere with Airy Pattern, a planet does not) Self-Coherent camera (see talk by P. Baudoz)

Angular Differential Imaging (ADI) All

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Example: Spectral DeconvolutionExample: Spectral Deconvolution

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Speckle chromaticity and Fresnel

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20 nm rms at 10x Talbot

20 nm rms in pupil plane

SD needs “smooth” speckle spectrum-> near-pupil optics


End-2-end analysis

Apodizer only leads to improved final contrastAPLCApodizer


E-ELT WFE requirements

Segment alignment (PTT) < 36 nm rmsSegment figuring < 50 nm rmsSegment high orders < 50 nm rmsM2-5, f>50 cycles/pupil < 30 nm rms Roughness < 5 nm rms


Baseline Concept

All optics near the pupil planeminimize amplitude errors and speckle irregular chromaticity


Detection rates, MC simulation

23232323


Predicted Science Output

MC simulations planet population with orbit and mass

distribution from e.g. Mordasini (2007) Model planet brightness (thermal,

reflected, albedo, phase angle,…) Match statistics with RV results

Contrast model Analytical AO model incl.

realistic error budget Spectral deconvolution No diffraction or static WFE Y-H, 10% throughput, 4h obs

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Detection rates, nearby+young stars

Mordasini et al. 2007

Contrast requirements

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Predicted EPICS outputPredicted EPICS output

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Target Target classclass

# targets# targets Self-Self-luminous luminous planetsplanets

Giant Giant planetsplanets

NeptunesNeptunes Rocky Rocky planetsplanets

1. Young 1. Young starsstars

688 ~100 (~100) Dozens Very few (?)

2. Nearby 2. Nearby starsstars

512 Dozen ~100 Dozens Dozen

3. Stars 3. Stars w. planetsw. planets

>100 Some >100 >Dozen >2

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SummarySummary

EPICS is the NIR E-ELT instrument for Exoplanet research

Phase-A to study concept, demonstrate feasibility by prototyping, provide feedback to E-ELT and come up with a development plan

Conclusion of Phase-A early 2010 Exploits E-ELT capabilities (spatial resolution and

collecting power) in order to greatly advance Exoplanet research (discovery and characterization)

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Documents

AO4ELT, Paris, 23 June 2009 EPICS, exoplanet imaging with the E-ELT Markus Kasper, Jean-Luc Beuzit, Christophe Verinaud, Emmanuel Aller- Carpentier, Pierre