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Spectro-Polarimetric High-contrast Exoplanet Research A Planet Finder Instrument for the VLT Jean-Luc Beuzit (PI), Markus Feldt (Co-PI), David Mouillet.

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Presentation on theme: "Spectro-Polarimetric High-contrast Exoplanet Research A Planet Finder Instrument for the VLT Jean-Luc Beuzit (PI), Markus Feldt (Co-PI), David Mouillet."— Presentation transcript:

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 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 Radial Velocity Large Surveys HC & HAR Imaging μ Lensing Transits Stars - BDs BDs - Planets

4 SPHERE main targets Target classes for wide exoplanet search (several hundreds objects) Young nearby stars (5-50 Myr) (detection down to 0.5 M J ) 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 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, data reduction and handling) 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 Operation strategy

6 High contrast detection capability High contrast detection capability Extreme AO (turbulence correction) Extreme AO (turbulence correction) feed coronagraph with well corrected WF feed coronagraph with well corrected WF SR ~ 90% in H-band SR ~ 90% in H-band Coronagraphy (removal of diffraction pattern) Coronagraphy (removal of diffraction pattern) high dynamics at short separations high dynamics at short separations Differential detection (removal of residual defects) Differential detection (removal of residual defects) calibration of non common path aberrations calibration of non common path aberrations pupil and field stability pupil and field stability smart post processing tools smart post processing tools High Level Requirements Scientific requirements Scientific requirements Gain up to 2 orders of magnitude in contrast Gain 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 coverage spectral coverage

7 40x40 SH-WFS in visible 1.2 KHz, RON < 1e- ALC, 4QPMs, Lyot, Slits IR –TT sensor λ = 0.5 – 0.9 µm - FoV = – 1.65 µm FoV = – 2.32 µm - FoV = 12.5 Nasmyth platform, static bench, Temperature control, cleanliness control Active vibration control Concept overview Beam control DM, TTs

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

9 Instrument modes

10

11 (i) modes and operations 11 x 12.5 Astrometric accuracy: 0.5 – 2 mas (depending on SNR) (10 -7 ) at ( ) 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

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 GPI at Gemini South Macintosh et al. HiCIAO + SCExAO 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 !


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