1. 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)

2. 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

3. Science objectives Large Surveys Radial Velocity HC & HAR Imaging
Stars - BDs
Large Surveys
BDs - Planets
Radial Velocity
HC & HAR Imaging
Transits
μ Lensing

4. 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

5. 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

6. 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,…)

7. 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’’

8. 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

9. Instrument modes

10. Instrument modes

11. 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 ‘’
( ) at 0.5”
11 ‘’ x 12.5’’

12. IRDIS / IFS performances

13. ZIMPOL performance

14. Project Schedule we started in May 2001 …
December 2008: Final Design Review
Jan.-Dec. 2009: Procurement / Manufacturing
Oct – 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

15. Other Instruments GPI at Gemini South HiCIAO + SCExAO at Subaru
Macintosh et al.
HiCIAO + SCExAO
at Subaru
Tamura et al. & Guyon et al

16. 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

17. Thank you !