Transcript SPHERE – the high contrast challenge Markus Kasper, ESO ESO, 27 Nov 09

SPHERE – the high contrast challenge
Markus Kasper, ESO
ESO, 27 Nov 09
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Outline
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SPHERE project history
 The mission
 The concept
 Demonstrations
 Now and soon
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From the start…
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
 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
GJ 758, Thalmann et al 2009
HR 8799,etMarois
et27
alNov
2008
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Lagrange
al.ESO,
2009
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Science objectives
Stars - BDs
Large Surveys
BDs - Planets
Radial Velocity
HC & HAR Imaging
Transits
μ Lensing
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SPHERE features
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High contrast detection capability
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Characterization
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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)
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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Concept overview
Beam control
DM, TTs
Fore
optics
Common Path
40x40 SH-WFS in visible
1.2 KHz, RON < 1e-
Vis
Coronagraph
Extreme
AO
NIR
Coronagraph
ALC, 4QPMs, Lyot, Slits
IR –TT sensor
Nasmyth platform, static bench,
Temperature control, cleanliness control
Active vibration control
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λ = 0.5 – 0.9 µm - FoV = 3.5”
ZIMPOL
IFS
0.95 – 1.65 µm
FoV = 1.77”
IRDIS
0.95 – 2.32 µm - FoV = 12.5’’
SPHERE implementation
CPI
De-rotator HWP2
HWP1
ITTM
PTTM
Polar Cal
DM
NIR ADC
VIS ADC
DTTS
VIS corono
ZIMPOL
WFS
NIR corono
DTTP
IFS
IRDIS
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Spectral Differential Imaging
(SDI)
Lenzen paper
NACO, Close et al. 2003
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Angular Differential Imaging
(ADI)
NACO at Nasmyth of VLT (Alt-Az)
-> pupil and field rotate at different speeds
Standard:
Rotate NACO to stabilize field PA
New 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
Mordasini et al. (2009)
Nearby stars (<20 pc) ESO, 27 Nov 09
Young stars (<5 108 yrs)
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Science objectives
Stars - BDs
Large Surveys
BDs - Planets
Radial Velocity
HC & HAR Imaging
Transits
μ Lensing
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XAO with HOT
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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
Aller-Carpentier, proc. AO4ELT
100
95
90
85
SR (%)
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80
75
70
65
60
55
50
2
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6
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Star magnitude
10
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XAO coronagraphy
with HOT
Martinez et al., submitted to A&AL
Good agreement with
SPHERE simulations
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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
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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
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ASTRON, 16/17 Nov
200927
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 Review
Jan.-Dec. 2009: Procurement / Manufacturing
Oct. 2009 – June 2010: Sub-systems AIT
July 2010 – February 2011: Global system AIT
Feb.-March 2011: Preliminary Acceptance Europe
May-End 2011: Commissioning
Early 2012: Beginning of science operation
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Review Passed
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