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SPHERE – the high contrast challengeSPHERE – the high contrast challenge
Markus Kasper, ESOMarkus Kasper, ESO
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Outline
SPHERE project history The mission The concept Demonstrations Now and soon
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From the start…
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2 Phase A studies led by MPIA and LAOG: 2003 –2004
Phase A review Dec 2004 Major Merger: 2005 – 2006
(consortium agreement issue 1, Dec 2006)
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SPHERE project structure
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VLT 2nd generation instrument for Exoplanets
Consortium: LAOG, LAM, LESIA, LUAN, MPIA, Padova University, Obs. Geneve, ETH Zuerich, ASTRON and ONERA
Passed FDR in Dec 2008, now in MAIT phase
Many critical components (DM+driver, WFS CCD, IR detectors, large common path optics) already in house
Commissioning and 1st light in summer 2011, in less than 2 years!!
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Possible exoplanets, directly imaged
55HR 8799, Marois et al 2008Lagrange et al. 2009
GJ 758, Thalmann et al 2009
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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 features High contrast detection capability
Contrast Gain up to 5 mag wrt current instrumentation (10-6-10-7) Extreme AO (SR ~ 90% in H-band) Coronagraphy at small inner working angles: 0.1 – 3 Spectral Differential imaging (IRDIS, IFS) Polarimetric Differential imaging (ZIMPOL)
Characterization Polarimetry (IRDIS, ZIMPOL) Medium resolution Long-Slit spectroscopy
(R~500 in range 0.95 – 2.32 microns, IRDIS) Low resolution spectroscopy (R~50, IFS, IRDIS)
Classical imaging at high Strehl ratios (IRDIS, ZIMPOL)
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The concept
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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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SPHERE implementation
CPICPI
IRDISIRDISIFSIFS
ZIMPOLZIMPOL
ITTMITTM
PTTMPTTM
DMDM
DTTPDTTP
DTTSDTTS
WFSWFS
De-rotatorDe-rotator
VIS ADCVIS ADCNIR ADCNIR ADC
NIR coronoNIR corono
VIS coronoVIS corono
HWP2HWP2
HWP1HWP1
Polar CalPolar Cal
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Spectral Differential Imaging (SDI)
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Lenzen paper
NACO, Close et al. 2003
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Angular Differential Imaging (ADI)
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NACO at Nasmyth of VLT (Alt-Az)-> pupil and field rotate at different speeds
Standard: Rotate NACO to stabilize field PANew option: Rotate NACO to stabilize pupil (and diffraction pattern and quasi-static speckles)
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Instrument modes
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IRDIS / IFS performances
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ZIMPOL performance
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Predicted Science Output
MC simulations (MESS, Bonavita et al.) Modeled planet population or extrapolated RV
distribution Model planet brightness (thermal, reflected,
albedo, phase angle,…) Match statistics with RV results
1616Young stars (<5 108 yrs)Nearby stars (<20 pc)
Mordasini et al. (2009)
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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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XAO with HOT Developed at ESO in collaboration with Arcetri and Durham Univ. H-band Strehl ratios ~90% in 0.5 seeing (SPIE 2008, Esposito et al.
& Aller-Carpentier et al. ) correcting 8-m aperture for ~600 modes
2 4 6 8 10 1250
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Star magnitude
SR
(%
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Aller-Carpentier, proc. AO4ELT
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XAO coronagraphy with HOT
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Good agreement with SPHERE simulations
Martinez et al., submitted to A&AL
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CP bench aka piano
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CP dampers
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CP mounts and stages
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Toric mirrors All toric finished TM1&TM2 in specs New TM3 started
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Cabinets and cooling systems
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Calibration sources
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CODE/HODM testing
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WFS
ASTRON, 16/17 Nov ASTRON, 16/17 Nov 200920092727
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OCAM with LA
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IFS
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Opto - mechanics Layout
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IFS camera
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IRDIS status: MFG Progress
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ZIMPOL
Mark Downing (ESO), Peter Steiner (ETH) and Charlotte installing eng.detector system
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ZIMPOL, 1st light
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Project Schedule
started in May 2001
Phase-A, Consortium selection, PDR…
December 2008: Final Design ReviewJan.-Dec. 2009: Procurement / ManufacturingOct. 2009 – June 2010: Sub-systems AITJuly 2010 – February 2011: Global system AITFeb.-March 2011: Preliminary Acceptance EuropeMay-End 2011: CommissioningEarly 2012: Beginning of science operation
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Review Passed
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