Spectro-Polarimetric High-contrast Exoplanet Research

A Planet Finder Instrument for the VLT

Jean-Luc Beuzit (PI), Markus Feldt (Co-PI), Jean-Luc Beuzit (PI), Markus Feldt (Co-PI), David Mouillet (PS), Pascal Puget (PM), Kjetil Dohlen (SE)David Mouillet (PS), Pascal Puget (PM), Kjetil Dohlen (SE)

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

LAOG, MPIA, LAM, ONERA, LESIA, INAF, Geneva Observatory,

LUAN, ASTRON, ETH-Z, UvA, ESO

Co-IsCo-Is: D. Mouillet (LAOG, Grenoble), T. Henning (MPIA, Heidelberg), C. : D. Mouillet (LAOG, Grenoble), T. Henning (MPIA, Heidelberg), C. Moutou (LAM, Marseille), A. Boccaletti (LESIA, Paris), S. Udry 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 objectives High contrast imaging down to planetary masses Investigate large target sample: statistics, variety of

stellar classes, evolutionary trends Complete the accessible mass/period diagram First order characterization of the atmospheres

(clouds, dust content, methane, water absorption, effective temperature, radius, dust polarization)

Understand the formation of planetary systems

Science objectives

Radial Velocity

Large Surveys

HC & HAR Imaging

μ Lensing

Transits

Stars - BDsStars - BDs

BDs - PlanetsBDs - Planets

SPHERE main targets

Target classes for wide exoplanet search (several hundreds objects) Young nearby stars (5-50 Myr) (detection down to 0.5 MJ) Young active F-K stars (0.1 – 1 Gyr) Late type stars Known planetary systems (from other techniques) Closest stars (< 6 pc)

Selection of individual targets Known (proto)planetary disks: physics, evolution, dynamics Variety of selected high contrast targets: YSO gas

environment, evolved stars, Solar System objects

Survey of a few hundreds stars is desirable Survey of a few hundreds stars is desirable

Statistical approach needed (frequency)Statistical approach needed (frequency)

More efficient use of instrument (operation, calibration, More efficient use of instrument (operation, calibration,

data reduction and handling)data reduction and handling)

Follow-up observations for characterization

A few hundred nights required over several years 260 GTO nights already approved

Additional surveys/programs to be discussed

Operation strategy

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

feed coronagraph with well corrected WFfeed coronagraph with well corrected WF SR ~ 90% in H-bandSR ~ 90% in H-band

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

Differential detection (removal of residual Differential detection (removal of residual

defects)defects) calibration of non common path aberrationscalibration of non common path aberrations pupil and field stabilitypupil and field stability smart post processing toolssmart post processing tools

High Level Requirements

Scientific requirementsScientific requirements Gain up to 2 orders of magnitude in contrastGain up to 2 orders of magnitude in contrast Reach short separations: 0.1’’ – 3” (1- 100AU)Reach short separations: 0.1’’ – 3” (1- 100AU) Survey a large number of targets (V<10)Survey a large number of targets (V<10) spectral coveragespectral coverage

40x40 SH-WFS in visible1.2 KHz, RON < 1e-

ALC, 4QPMs, Lyot, SlitsIR –TT sensor

λ = 0.5 – 0.9 µm - FoV = 3.5”

0.95 – 1.65 µm FoV = 1.77”

0.95 – 2.32 µm - FoV = 12.5’’

Nasmyth platform, static bench, Temperature control, cleanliness control Active vibration control

Concept overview

Beam control DM, TTs

Actual design

CPICPI

IRDISIRDISIFSIFS

ZIMPOLZIMPOL

ITTMITTM

PTTMPTTM

DMDM

DTTPDTTP

DTTSDTTS

WFSWFS

De-rotatorDe-rotator

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

Instrument modes

Science module

Modes Motivation / specificities

Dual Band I maging (DBI )

• Baseline planet det ect ion capabilit y

• High cont r ast imaging

• Complet e NI R spect r al r ange cover age, opt imized f or J and H

• Wide simult aneous FoV (>11")

Long slit spect r oscopy • Simult aneous low r esolut ion Yt o Ks spect r um

• Medium r esolut ion spect r oscopy

Classical imaging • Complet e set of wide and medium band f ilt er s

• Wide FoV (>11")

I RDI S

Dual Polar izat ion imaging (DPI ) • Spect r al complement ar it y wit h ZI MPOL

• Lar ger simult aneous FoV (>3")

I FS I maging spect r oscopy in Y t o J

• Higher cont r ast per f or mance goal • I nt er nal mult iplex advant age wit h mor e

spect r al channels t han DBI , mor e r obust t o

unexpect ed spect r al f eat ur es

• Mult iplex advant age when simult aneous wit h I RDI S

Ver y accur at e r elat ive polar imet r y • Det ect ion of ver y f aint r ef lect ed light (down t o

t he level of inner planet s) ZI MPOL

Classical imaging

• High St r ehl, high angular r esolut ion

• Complet e set of wide, medium and nar r ow band

f ilt er s

Instrument modes

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

11 ‘’ x 12.5’’

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

1.77 ‘’

10-6 (10-7) at 0.5”

5. 10-6 (5. 10-7) at 0.5”

Simultaneous use of Y-J band with IFS Dual imaging in H

Multiplex advantage for field and spectral range

Mutual support: false alarm reduction, operation, calibration

Immediate companion early classification

Combined use and

advantages of IRDIS/DBI and

IFS

IRDIS / IFS performances

ZIMPOL performance

Project Schedule

we started in May 2001 we started in May 2001 ……December 2008: Final Design ReviewDecember 2008: Final Design ReviewJan.-Dec. 2009: Procurement / ManufacturingJan.-Dec. 2009: Procurement / ManufacturingOct. 2009 – June 2010: Sub-systems AITOct. 2009 – June 2010: Sub-systems AITJuly 2010 – February 2010: Global system AITJuly 2010 – February 2010: Global system AITFeb.-March 2011: Preliminary Acceptance EuropeFeb.-March 2011: Preliminary Acceptance EuropeMay-Oct. 2011: Commissioning runs (3 runs)May-Oct. 2011: Commissioning runs (3 runs)Early 2012: Beginning of science operationEarly 2012: Beginning of science operation

Other Instruments

GPI at Gemini SouthGPI at Gemini SouthMacintosh et al. Macintosh et al.

HiCIAO + SCExAO HiCIAO + SCExAO

at Subaruat SubaruTamura et al. & Guyon et alTamura et al. & Guyon et al

Summary Very challenging project ! Now at manufacturing stage At Paranal in early 2011 Main science outputs by ~2015 for both:

Large surveys for statistical approaches, broad target selection

In-depth characterization of specific systems Critical step before further exoplanet studies in

the ELT era for Technological development System/calibration/operational experience Scientific preparation on the given available target

sample

Thank you !Thank you !