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
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)
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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
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Science objectives
Radial Velocity
Large Surveys
HC & HAR Imaging
μ Lensing
Transits
Stars - BDsStars - BDs
BDs - PlanetsBDs - Planets
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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
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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
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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
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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
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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
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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
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Instrument modes
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(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
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IRDIS / IFS performances
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ZIMPOL performance
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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
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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
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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
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Thank you !Thank you !