Spectro-Polarimetric High-contrast Exoplanet Research A Planet Finder Instrument for the VLT Jean-Luc Beuzit (PI), Markus Feldt (Co-PI), David Mouillet (PS), Pascal Puget (PM), Kjetil Dohlen (SE) and numerous participants from 12 European institutes ! LAOG, MPIA, LAM, ONERA, LESIA, INAF, Geneva Observatory, LUAN, ASTRON, ETH-Z, UvA, ESO Co-Is: D. Mouillet (LAOG, Grenoble), T. Henning (MPIA, Heidelberg), C. Moutou (LAM, Marseille), A. Boccaletti (LESIA, Paris), S. Udry (Observatoire de Genève), M. Turrato (INAF, Padova), H.M. Schmid (ETH, Zurich), F. Vakili (LUAN, Nice), R. Waters (UvA, Amsterdam)

Understand the formation of planetary systems 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 Large Surveys Radial Velocity HC & HAR Imaging Stars - BDs Large Surveys BDs - Planets Radial Velocity HC & HAR Imaging Transits μ Lensing

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

Operation strategy Survey of a few hundreds stars is desirable Statistical approach needed (frequency) More efficient use of instrument (operation, calibration, 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

High Level Requirements Scientific requirements Gain up to 2 orders of magnitude in contrast Reach short separations: 0.1’’ – 3” (1- 100AU) Survey a large number of targets (V<10) spectral coverage High contrast detection capability Extreme AO (turbulence correction) feed coronagraph with well corrected WF SR ~ 90% in H-band Coronagraphy (removal of diffraction pattern) high dynamics at short separations Differential detection (removal of residual defects) calibration of non common path aberrations pupil and field stability smart post processing tools Pushing the high contrast detection capability based on past experience (known concept with analyzed limits and improved properties ) and a dedicated instrument Room for further improvement and tests (with potentially relaxed schedule, general specs (field, spectral domain,…)

Concept overview Beam control DM, TTs λ = 0.5 – 0.9 µm - FoV = 3.5” 40x40 SH-WFS in visible 1.2 KHz, RON < 1e- 0.95 – 1.65 µm FoV = 1.77” Nasmyth platform, static bench, Temperature control, cleanliness control Active vibration control ALC, 4QPMs, Lyot, Slits IR –TT sensor 0.95 – 2.32 µm - FoV = 12.5’’

Actual design CPI ZIMPOL IFS IRDIS ITTM PTTM DM DTTS WFS DTTP Focus 1 De-rotator HWP2 ITTM HWP1 PTTM Polar Cal Focus 2 DM Focus 4 NIR ADC VIS ADC DTTS VIS corono Focus 3 ZIMPOL WFS NIR corono DTTP IFS IRDIS

Instrument modes

Instrument modes

Combined use and advantages of IRDIS/DBI and IFS (i) modes and operations Combined use and advantages of IRDIS/DBI and IFS Astrometric accuracy: 0.5 – 2 mas (depending on SNR) 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 A preciser 10-6 (10-7) at 0.5” 1.77 ‘’ 5. 10-6 (5. 10-7) at 0.5” 11 ‘’ x 12.5’’

IRDIS / IFS performances

ZIMPOL performance

Project Schedule we started in May 2001 … December 2008: Final Design Review Jan.-Dec. 2009: Procurement / Manufacturing Oct. 2009 – June 2010: Sub-systems AIT July 2010 – February 2010: Global system AIT Feb.-March 2011: Preliminary Acceptance Europe May-Oct. 2011: Commissioning runs (3 runs) Early 2012: Beginning of science operation

Other Instruments GPI at Gemini South HiCIAO + SCExAO at Subaru Macintosh et al. HiCIAO + SCExAO at Subaru Tamura 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 !