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SPHERE(Spectro-Polarimetric High-contrast Exoplanet REsearch)

A Planet Finder Instrument for the VLTJeanJean--Luc Beuzit (PI), Markus Feldt (CoLuc Beuzit (PI), Markus Feldt (Co--PI),PI),

David Mouillet (PS), Pascal Puget (PM), Kjetil Dohlen (SE)David Mouillet (PS), Pascal Puget (PM), Kjetil Dohlen (SE)F. Wildi (AIT), T. Fusco, C. Petit (AO)F. Wildi (AIT), T. Fusco, C. Petit (AO)

and numerous participants from 12 European institutes !and numerous participants from 12 European institutes !

LAOG, MPIA, LAM, ONERA, LESIA, INAF, Geneva Observatory,LAOG, MPIA, LAM, ONERA, LESIA, INAF, Geneva Observatory,LUAN, ASTRON, ETHLUAN, ASTRON, ETH--Z, UvA, ESOZ, UvA, ESO

CoCo--IsIs: D. Mouillet (LAOG, Grenoble), T. Henning (MPIA, Heidelberg),: D. Mouillet (LAOG, Grenoble), T. Henning (MPIA, Heidelberg),C. Moutou (LAM, Marseille), A. Boccaletti (LESIA, Paris), S. UdryC. Moutou (LAM, Marseille), A. Boccaletti (LESIA, Paris), S. Udry

(Observatoire de Genève), M. Turrato (INAF, Padova), H.M. Schmid(Observatoire de Genève), M. Turrato (INAF, Padova), H.M. Schmid(ETH, Zurich), F. Vakili (LUAN, Nice), R. Waters (UvA, Amsterdam)(ETH, Zurich), F. Vakili (LUAN, Nice), R. Waters (UvA, Amsterdam)

Science objectivesHigh contrast imaging down to planetary massesInvestigate large target sample: statistics, variety ofstellar classes, evolutionary trendsComplete the accessible period windowFirst order characterization of the atmosphere (clouds,dust content, Methane, water absorption, effectivetemperature, radius, dust polarization)Understand the planetary system origins

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Science objectives

Radial Velocity

Large Surveys

HC & HAR Imaging

Lensing

Transits

StarsStars -- BDsBDs

BDsBDs -- PlanetsPlanets

High contrast detection capabilityHigh contrast detection capabilityExtreme AO (turbulence correction)Extreme AO (turbulence correction)

feed coronagraph with well corrected WFfeed coronagraph with well corrected WFSR ~ 90% in HSR ~ 90% in H--bandband

Coronagraphy (removal of diffraction pattern)Coronagraphy (removal of diffraction pattern)high dynamics at short separationshigh dynamics at short separations

Differential detection (removal of residual defects)Differential detection (removal of residual defects)calibration of non common path aberrationscalibration of non common path aberrationspupil and field stabilitypupil and field stabilitysmart post processing toolssmart post processing tools

High sensitivityHigh sensitivityoptimal correction up to V ~ 9optimal correction up to V ~ 9--1010

High level requirementsScientific requirementsScientific requirements

Gain up to 2 orders of magnitude in contrast as comparedGain up to 2 orders of magnitude in contrast as comparedto current instrumentationto current instrumentation

Reach short separations: 0.1’’Reach short separations: 0.1’’ –– 3” (13” (1-- 100AU)100AU)Survey a large number of targetsSurvey a large number of targets

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Common Path

Foreoptics

ExtremeAO

NIRCoronagraph

VisCoronagraph

ZIMPOL

IFS

IRDIS

High frequency AO correction (41x41 act.)High stability : image / pupil controlVisible – NIR Refraction correctionFoV = 12.5’’40x40 SH-WFS in visible1.2 KHz, RON < 1e-

Pupil apodisation,Focal masks: Lyot, A4Q, ALC.IR-TT sensor for fine entering

Coronagraphic imaging:Dual polarimetry, direct BB + NB.

= 0.5 – 0.9 µm,/2D @ 0.6 µm, FoV = 3.5”

0.95 – 1.35/1.65 µm/2D @ 0.95 µm,

Spectral resolution:R = 54 / 33FoV = 1.77”

0.95 – 2.32 µm; /2D @ 0.95 µmDifferential imaging: 2 wavelengths,R~30, FoV = 12.5’’Long Slit spectro: R~50 & 400Differential polarizationNasmyth platform, static bench,

Temperature control, cleanliness controlActive vibration control

Beam control(DM, TT, PTT,derotation)Pola controlCalibration

Concept overview

(i) modes and operations(i) modes and operations

11 ‘’ x 12.5’’

Astrometric accuracy: 0.5 – 2 mas(depending on SNR)

> 1.77 ‘’ (3’’)

10-6 (10-7) at 0.5”

5. 10-6 (5. 10-7) at 0.5”

Simultaneous use ofY-J band with IFSDual imaging in H

Multiplex advantage forfield and spectral rangeMutual support: falsealarm reduction, operation,calibrationImmediate companionearly classification

Combined useand advantagesof IRDIS/DBI

and IFS

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ImplementationImplementationCPICPI

IRDISIRDIS IFSIFS

ZIMPOLZIMPOL

ITTMITTM

PTTMPTTM

DMDM

DTTPDTTP

DTTSDTTS

WFSWFS

DeDe--rotatorrotator

VIS ADCVIS ADCNIR ADCNIR ADC

Focus 1Focus 1

Focus 2Focus 2

Focus 3Focus 3

Focus 4Focus 4

NIR coronoNIR corono

VIS coronoVIS corono

HWP2HWP2

HWP1HWP1

Polar CalPolar Cal

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NIR ADCNIR ADC

VIS ADCVIS ADC

WFSWFSDTTPDTTP

Focus 2Focus 2

FiltersFiltersSpatial filterSpatial filter

NIRNIRVISVIS

ZIMPOLZIMPOL

VISVIS

WFSWFS

IRDIFSIRDIFS

DTTSDTTSApodizerApodizer

AO systemCorrect for turbulence

provide a corrected area of 1.5-2 arcsec diameter60 nm rms on corrected modes => (90% SR in H for typical Paranal

conditions)Residual jitter smaller than ±3 (goal 1.5) mas rmsOptimal perf for V-mag GS < 9 (goal 10)Good correction (better than NAOS) for GS mag < 12 (goal 15)

To ensure system stabilityTo ensure system stabilityOptical axis wrt to coronagraphic deviceOptical axis wrt to coronagraphic device < 0.5 mas< 0.5 mas (goal 0.2)(goal 0.2)Beam shift on optical surfacesBeam shift on optical surfaces < 0.2% (goal 0.1) of the full pupil< 0.2% (goal 0.1) of the full pupil

diameterdiameterNon common path aberrations (down to coronagraph device)Non common path aberrations (down to coronagraph device) < 15 nm rms< 15 nm rms

To provide useful data for image postTo provide useful data for image post--processingprocessingStorage of WFS and control dataStorage of WFS and control dataEstimation of turbulence and system critical parametersEstimation of turbulence and system critical parametersMeasurement of IRDIS internal defects (differential aberrations)Measurement of IRDIS internal defects (differential aberrations)

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AO System

SPARTA: Standard Platformfor Adaptive optics RealTime Applications

SPHERE Deformable Mirror

CILAS piezoCILAS piezo--stack DMstack DMdelivered end 2007delivered end 2007Surface quality: 5nm rmsSurface quality: 5nm rms

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Fast Image Tip-tilt

“X” bandwidth is 700 Hz at“X” bandwidth is 700 Hz at --3dB3dBphase shift ofphase shift of --1515°° at 80Hzat 80Hz“Y” bandwidth is 891 Hz at“Y” bandwidth is 891 Hz at --3dB3dBphase shift ofphase shift of --1010°° at 80 Hzat 80 HzGoal 1000HzGoal 1000Hz

Freq Resp 2:1 CBFX.DAT

180deg

-20

Phase

kHz10.0110 Hz (Log)

Freq Resp 2:1 CBFY.DAT

Freq Resp 2:1 CBFY.DAT3

dB

-27

Mag (dB)

kHz10.0110 Hz (Log)

Freq Resp 2:1 CBFX.DAT

X:80.84093 Hz Y:165.1293 deg

X:80.84093 Hz Y:170.242 deg

X:891.8301 Hz Y:-3.277 dB

X:700.2723 Hz Y:-2.966 dB

prototypeprototype

1.2 kHz, CCD220-based wavefront sensorBenefits from the Opticon JRA1 reasearch program (EU funded)Benefits from the Opticon JRA1 reasearch program (EU funded)Common with the VLT AOCommon with the VLT AO--facilityfacility1. pixels, square 24 m2. 100% fill factor and 240x240 square grid array of pixels.3. low read noise of < 1 e-/pixel and goal of 0.1 e-/pixel.4. range of operating frame rates from 25 frames/s (fps) to 1200fps

NGC development (ESO)NGC development (ESO)Spatially Filtered SHSpatially Filtered SH

Optimization of theOptimization of thespatial filter sizespatial filter sizeStudy of BB impactStudy of BB impactWCOG : confirmation ofWCOG : confirmation ofthe gain in perfthe gain in perf(simulation &(simulation &experimentation)experimentation)

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Main components – RTCBased on SPARTA platformBased on SPARTA platform

Consortium specifications (+ algo)Consortium specifications (+ algo)ESO developmentESO development

Main featuresMain featuresvery small global delay (~ 1ms)very small global delay (~ 1ms)

+ large number of actuators+ large number of actuatorshybrid control lawhybrid control law

LQG (Kalman filter based) for TTLQG (Kalman filter based) for TTOMGI for higher modesOMGI for higher modes

additional features to deal with SAXO specificities (DTTS, PTTS)additional features to deal with SAXO specificities (DTTS, PTTS)

StatusStatusSpecifications OKSpecifications OKDevelopment:Development:

Various version (drops) available for SPHERE during SPARTA developmentVarious version (drops) available for SPHERE during SPARTA development=> optimization of the AIT period => reduction of risks and planning drifts.=> optimization of the AIT period => reduction of risks and planning drifts.First version to be delivered midFirst version to be delivered mid--July 2009July 2009

Main components – Aux. sensorsDifferential TipDifferential Tip--Tilt SensorTilt Sensor

IR camera located just beforeIR camera located just beforethe coronagraph maskthe coronagraph mask1 to 10 % of the IR flux for this sensor1 to 10 % of the IR flux for this sensorWCoG measurementWCoG measurementcontrol of a diff. tip tilt platecontrol of a diff. tip tilt plateclosed loop schemeclosed loop scheme –– 11--10 Hz10 Hzadditional capability: focus check between twoadditional capability: focus check between twoobservationsobservationsCould potentially be used to implement onCould potentially be used to implement on--line phaseline phasediversitydiversity

Pupil TipPupil Tip--Tilt SensorTilt SensorUse of SH data (subUse of SH data (sub--aperture. intensities)aperture. intensities)PTTM close to the entrance focal planePTTM close to the entrance focal planeClosed loop schemeClosed loop schemeFrame rate ~ 0.1 HzFrame rate ~ 0.1 HzResidual beam shift < 0.2 % of the full pupil diameterResidual beam shift < 0.2 % of the full pupil diameter

DTTSDTTSVisVis

WFSWFSRTCRTC

DM & TTMDM & TTM

DTTPDTTP

VIS/IRVIS/IR 1/99 %1/99 %

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CoronagraphsClassical Lyot coronagraph

Proven concept, existing on sky, no substrateLimited to external regions (> 0.5’’)

4Q phase mask Y, J, HWell studied, existing in NACO for narrow bandAllow to explore inner regions (down to /D)On-going R&D

Apodized pupil LyotOptimized for Y, J, H

Other concepts (modular design)New ideas like ZOG, Annular Grove Phase Mask, etc.

IRDIS, IFS and ZIMPOL have pupil imaging lenses

SPHERE A4Q focal plane mask prototype

18 µm diameter tungsten wires

Airy diameter in H band

18 µm diameter tungsten wires

Airy diameter in H band

close-up showing the tungstenwires placed to mask theedges of the wave plates

the complete assembled device

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A4Q Prototype

1,E-07

1,E-06

1,E-05

1,E-04

1,E-03

1,E-02

1,E-01

1,E+000 2 4 6 8 10 12 14

separation in lambda/D

PSF - YPSF - JPSF - H4QPM - Y4QPM - J4QPM - H

1,E-07

1,E-06

1,E-05

1,E-04

1,E-03

1,E-02

1,E-01

1,E+000 2 4 6 8 10 12 14

separation in lambda/D

PSF - H1PSF - H24QPM - H14QPM - H24QPM - H1-H2

H1

H2

H1-H2

Raw performance

Dual-bandperformance

ImplementationImplementationCPICPI

IRDISIRDIS IFSIFS

ZIMPOLZIMPOL

ITTMITTM

PTTMPTTM

DMDM

DTTPDTTP

DTTSDTTS

WFSWFS

DeDe--rotatorrotator

VIS ADCVIS ADCNIR ADCNIR ADC

Focus 1Focus 1

Focus 2Focus 2

Focus 3Focus 3

Focus 4Focus 4

NIR coronoNIR corono

VIS coronoVIS corono

HWP2HWP2

HWP1HWP1

Polar CalPolar Cal

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IRDIS dual beam imager

Old M0 star, 10 pc

10 MJ planet at 0.1"1 MJ planet at 0.2"

Young M0 star, 40 pc

ImplementationImplementationCPICPI

IRDISIRDIS IFSIFS

ZIMPOLZIMPOL

ITTMITTM

PTTMPTTM

DMDM

DTTPDTTP

DTTSDTTS

WFSWFS

DeDe--rotatorrotator

VIS ADCVIS ADCNIR ADCNIR ADC

Focus 1Focus 1

Focus 2Focus 2

Focus 3Focus 3

Focus 4Focus 4

NIR coronoNIR corono

VIS coronoVIS corono

HWP2HWP2

HWP1HWP1

Polar CalPolar Cal

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ZIMPOL performance

ImplementationImplementationCPICPI

IRDISIRDIS IFSIFS

ZIMPOLZIMPOL

ITTMITTM

PTTMPTTM

DMDM

DTTPDTTP

DTTSDTTS

WFSWFS

DeDe--rotatorrotator

VIS ADCVIS ADCNIR ADCNIR ADC

Focus 1Focus 1

Focus 2Focus 2

Focus 3Focus 3

Focus 4Focus 4

NIR coronoNIR corono

VIS coronoVIS corono

HWP2HWP2

HWP1HWP1

Polar CalPolar Cal

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Journées FOST/GRIL ExoJournées FOST/GRIL Exo--planètes 19planètes 19--20 D20 D

Principe et ordres de grandeursPrincipe et ordres de grandeursPerformance en forte évolutionPerformance en forte évolution

101066

101088

2000’s2000’s

2010’s2010’s

2020’s2020’s

~ all stars~ all stars

R <~ 12R <~ 12

R <~ 9R <~ 9

R <~ ?R <~ ?

ConclusionsVery challenging project !Now at manufacturing stageAt Paranal in early 2011Main science outputs by ~2015 for both:

Large surveys for statistical approaches, broad targetselectionIn-depth characterization of specific systems

Critical step before further exoplanet studies in theELT era for

Technological developmentSystem/calibration/operational experienceScientific preparation on the given available target sample

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Thank you !

NNactact-- FFsampsamp-- : the necessary trade: the necessary trade--offsoffs

•• NNactact

•• FFsampsamp

•• (WFS(WFS--im)im)

Corrected areaCorrected area NNactact

ContrastContrast

(profil(profil (N(Nactact))--8/3)8/3)

ContrastContrast (F(Fsampsamp))22

Noise effectsNoise effects --22

WFS spectral bandwidthWFS spectral bandwidthVIS detectorVIS detector

Gain in limit magGain in limit magcontrastcontrast

WFS FluxWFS Flux (N(Nactact))Loss in limit magLoss in limit mag

WFS FluxWFS Flux (F(Fsampsamp))--11

Loss in limit magLoss in limit mag

Chromatism effectsChromatism effectscontrastcontrast

GAINS LOSSESGAINS LOSSES

Complex tradeComplex trade--offs:offs: depends on scientific requirements (ultimate contrast,depends on scientific requirements (ultimate contrast,number of targets) and atmospheric conditionsnumber of targets) and atmospheric conditions

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SAXO error budget41x41 actuators => corrected area +/41x41 actuators => corrected area +/-- 0.82” in H0.82” in H“Simplified” Error budget (nm rms) for SAXO“Simplified” Error budget (nm rms) for SAXO

Telescope/instrument defectsTelescope/instrument defectsin the corrected area : static / quasiin the corrected area : static / quasi--static => fully corrected by AOstatic => fully corrected by AOhigh freq : no correctionhigh freq : no correction -- included in the global system error budgetincluded in the global system error budget

Error sources Low frequencies (nm) High frequencies (nm)

Seeing 0.65 0.85 0.65 0.85

total for atmospheric limitations 11 14 9 11

total for DM errors 11 (7) 13 (9) 52 63

Total for temporal errors 19 (15) 23 (18) - -

Total for residual aliasing error 20 (13) 32 (23) - -

Total for noise related errors 42 (35) 44 (36) - -

Total for mis-calibration errors 10 (5) 10 (5)

TOTAL for the AO main AO loop 54 (43) 62 (49) 52.8 64.0

41x41 act.41x41 act.

1.2 KHz1.2 KHz

Filtered SHFiltered SH--WFSWFS

EMCCD, WCoG,EMCCD, WCoG,BB WFSBB WFSNCPA comp.NCPA comp.

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