Spectro-Polarimetric High-contrast Exoplanet Research
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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 (PS), Pascal Puget (PM), Kjetil Dohlen (SE) and numerous participants from 12 European institutes !

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Spectro-Polarimetric High-contrast Exoplanet Research A Planet Finder Instrument for the VLT

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Spectro polarimetric high contrast exoplanet research a planet finder instrument for the vlt

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)


Science objectives

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 objectives1

Science objectives

Stars - BDs

Large Surveys

BDs - Planets

Radial Velocity

HC & HAR Imaging

Transits

μ Lensing


Sphere main targets

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


Spectro polarimetric high contrast exoplanet research a planet finder instrument for the vlt

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


Spectro polarimetric high contrast exoplanet research a planet finder instrument for the vlt

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


Concept overview

Beam control DM, TTs

40x40 SH-WFS in visible

1.2 KHz, RON < 1e-

λ = 0.5 – 0.9 µm - FoV = 3.5”

0.95 – 1.65 µm

FoV = 1.77”

ALC, 4QPMs, Lyot, Slits

IR –TT sensor

0.95 – 2.32 µm - FoV = 12.5’’

Nasmyth platform, static bench,

Temperature control, cleanliness control

Active vibration control

Concept overview


Actual design

Actual design

CPI

Focus 1

HWP2

De-rotator

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


Instrument modes1

Instrument modes


Combined use and advantages of irdis dbi and ifs

Combined use and advantages of IRDIS/DBI and IFS

(i) modes and operations

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

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

IRDIS / IFS performances


Zimpol performance

ZIMPOL performance


Project schedule

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

Other Instruments

  • GPI at Gemini South

    Macintosh et al.

  • HiCIAO + SCExAO

    at Subaru

    Tamura et al. & Guyon et al


Summary

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 !


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