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VLTI Tutorial
The VLTI conceptual design
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingVLTI Concept...The birth
From a 16m telescope
(1980) ...nice dream, but no interferometry ... ...to a linear array of four 8m telescopes... (1988) ...the baby was born! ... ...the troubles could start! ... ...to a mature VLT Interferometer layout (1990) VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingThe Final VLTI Array Layout
4 UT's as 'trapezoidal' as
possible (wind shadow, ground quality) ♦Baselines 47 - 130m1.5 milli arcsec
30 Stationsfor AT's
♦Baselines 8 - 200m1 milli arcsec
Delay Line Tunnel(160 x 8m)
positioned to minimize path differences. Can house 8 DL's Central combining Lab(20 x 7m) with specific VLTI building/ control roomAll elements are located on an 8m grid
Light travelling undergroundfor high thermal stability (vacuumalternative not selectedfor cost reasons) VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingThe VLTI Optical Layout
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingThe 'Appetizers'
(2 Siderostats) ♦Installed early 2001 ♦Relocatable in day(s) ♦Primary: 0.4 m ♦Autoguiding only ♦Airy disk (in K): 1.1"The 'Workhorses'
(3 Auxiliary Tel.) ♦Relocatablein 3h ♦Primary: 1.8m ♦Fast Tip-Tilt ♦Limited Chopping ♦Airy (in K): 0.25"The telescope family
The 'Kings'
(4 Unit Tel.) ♦Fixed position! ♦Primary: 8 m ♦Adaptive Optics ♦Airy disk (in K): 0.06" VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingTelescope Optical Design
Intermediate Focusbelow M4:
♦Various artificial light sourcesfor calibration & alignmentIntermediate pupilimage on
M8: ♦Deformable mirrorfor MACAOCoudeFocus:
♦Fast Tip-tilt sensor(STRAP) and later Wave Front Sensor(MACAO) ♦TCCDfor Field acquisition ♦Field of View at Coude: 2 arcmin. (FoV 2 arcsec in laboratory) VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingRelay Optics
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingRelay Optics
'Grasping' the UT-photons ♦M9: large dichroic.»Reflects IR to VLTI
»transmits Visible to STRAP and later MACAO Curvature sensor.»Optimized for polarization.
The Relay Optics (M9, M10, M11) inside UT Coude room) ♦M10: convex spherical.»Re-image telescope pupil
(M2) in Tunnel center.»Articulated mount to
adjust lateral pupil position in Lab. ♦M11: off-axis parabola.»Collimates beam and send
it into light duct towardsM12 in DL Tunnel
Location for STRAP/
MACAO Wave Front
Sensor
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingThe Delay Lines
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingThe Delay Lines
The 'Paranal-Express'
♦Stroke: 60 m (120m in OPL) ♦Resolution: <5nm ♦Max. velocity: 0.5 m/s ♦Stability (jitter): <14nm rms ♦Power dissipation: <15WVariable Curvature Mirror
(VCM) ♦re-image pupil inside theLaboratory
♦mounted on piezo translator for fast OPD correction The first two Delay Lines (#I & II) inside the tunnel VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingTransfer Optics
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingTransfer Optics
The beam bending 'gadgets'
♦Very high optical qualityflats (λ/60 surf.) ♦Coating optimizedfor transmission and polarization(45°incidence) ♦Very stiff mountsand tables for immunity to μ-seismic noise ♦M12 eventually on robotic arm for automatic array reconfiguration ♦M16 on translation stages for beam switching inside lab. ♦Support future dual-feed (PRIMA)The M12 flat folding mirror
The M16 flat folding mirror
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingBeam Make-up
STRAP (Tip-Tilt)
orMACAO (Adaptive Optics
FINITO (Fringe Tracker)
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingSTRAP (Tip-Tilt)
Quad-celldetector with APDat telescope Coude focusPure tip-tilt correction is optimal when D/r
0 <4, i.e. UT/10μm (MIDI) or AT/2 μm (VINCI,AMBER, MIDI)Gain on Strehl up to 5.
Will be used on UT till MACAO is available
Will be resident on AT
10 11 12 13 14 15 16 17 18 00.10.20.30.40.5
AT lab results, diffr. limit at 2.2 microns = 0.255 arcsecUT lab results, diffr. limit at 10 microns=0.26 arcsec
Tilt loop residual rms angular jitter
NGS V-magnitude, K0 star
Diffr. limit units
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingMACAO (Adaptive Optics)
X-Y Tableallows reference source
different from target A mustfor UTin K-band (AMBER). Gain in coherent flux≈10060 elements Curvature Systemat telescope Coude
♦WaveFrontSensor using APD coupled with optical fibers ♦Bimorph Deformable Mirror on Tip-Tilt mount ♦vibrating membrane, ♦radial geometry micro-lenses, VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingMACAO performance
667k266k
106k
42.1k
16.8k 6.67k 2.66k 1.06k 421
00.10.20.30.40.50.60.70.80.91
0.65" seeing, magnitude 20.5 sky, 1" FoV, 250 dark current, including error budgetSpecifications
1.0Count/subaperture/second
Guide Star Magnitude
0.2 00.60.40.8
1816141210
0.65" @ 500 nm,
o ~4ms,V=20.5 sky background
Strehl Ratio at 2.2 μm
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingFINITO (Fringe Tracker)
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingThe VLTI Laboratory
High thermal stability; limited access, low power dissipationTelescope Exit Pupil re-imagedinto instruments
Optical design for up to 8 beams(4 UTs with dual feed) 5 m VINCI PRIMA FSU M16 MIDI MIDIVisitor
Instrument
PRIMA DDLs BeamCompressors
SwitchyardAMBER
DL I DL IIDL III
DL IVVLTI Laboratory
ZOPD Ref.
FSUTelescope Exit Pupil
Delay Line Tunnel
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingInside the Laboratory
The Beam Switchyard
The Beam Compressors
♦3-mirror design (compress 80 18 mm) ♦High optical qualityoff-axis parabolas (surface error 7 rms)LEONARDOReference sources
♦Laser andwhite-light sources ♦Light can be sent to any instrument or backwards to telescope ♦Provide reference axis for each beamand reference OPDbetween beams ♦Enable instrument to obtain fringes in 'autotest'VINCITest Instrument
♦Used for VLTI commissioning& later as referencefor performance tracking.Fringe Tracker FINITO
♦Co-phases (3 beams) to allow long exposures ♦mH<12 (UT) The Beam Compressors (3 mirrors each)The Switchyard &Leonardoreference source
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, Garching VINCI VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingVLTI Tutorial
The VLTI
selected critical technical aspects VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingVLTI Error Budget
LEGEND:
OPD VARIATION
ACROSS PUPIL
OVERALL
OPD VARIATION
WITH TIME
POLARIZATION
EFFECTS
UNEQUAL BEAM
INTENSITIES
VLTIINSTRUMENT
FRINGE TRACKER
ADAPTIVE OPTICS
OPTICAL DESIGN
OPTICS
IMPERFETION
FINE IMAGE
TRACKER
A tmosphereInternal seeing
Coating
Internal seeingFiguring errors
A lignment errorsFringe sensor
A ctuator (Delay Line)Control elect.
Wave Front Sensor
Deformable mirror
Control elect.
Fine Image Sensor
A ctuator (M16)Control elect.
LINEAR
RETARDATION
PARTIAL
POLARIZATION
ROTAT. OF FRAME
OF REFERENCE
ON AXIS
CO-PHASING MODE
UT with ADAPTIVE OPTICS
= 2.2 µmWith spatial filter
φ=17 airy radii
LINEAR
RETARDATION
Systematic visibility loss (%) Random visibility loss (%)Error sourceFringe sensor= Allocation to be extracted
from a closed loop analysis39.3 5.4 2.00.4 31.0 5
6.00.0 0.06 0.00.1 0.00.00.0
0.0 0.0
0.140.06.16
0.00.14 0.010.0 ? 0.0
2.0 0.4 ?
4.5?22.70.02 0.0 6.3 0.1 2.0 0.4 ?
0.1 0.0
4.2 0.02.0 0.1?
VLTI INSTRUMENTS= Error sources not part of
this error budgetOPD variation with time
(vibrations)OPD variation across pupil(optical quality)PolarizationUneq. beam intensitiesDetector resolution, etc.
Seeing: 0.66 arcsec (@ 0.5 µm)
t0: 10 msec (@ 0.6 µm)Mv: 11
Cn2: 10e-15 m-2/3
VISIBILITY LOSS: ΔV/V
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingOPD variation with time (Piston errors)
Error sources:
♦Atmosphere ♦Internal seeing ♦Vibration (wind, natural & man-made seismics, acoustics, pumps, etc.)Compensated (Partially) by fringe
tracking.00,10,20,30,40,50,60,70,80,91
0,2 0,8 1,4 2 2,6 3,2 3,8 4,4 5 5,6 6,2Fringe Phase (rad)
Normalised Fringe Intensity
Fringe pattern at time t
Fringe pattern at time t + dt
Resulting Fringe patern
Piston variation
Top Level requirement:
Instrumental errors (internal seeing & vibrations) < atmosphereWavelength 0.6 µm 2.2 µm Exposure time 10 msec 48 msec OPL requirement (each arm) in [nm] 21 75 Telescope (UT or AT, each) 14 50 Delay Line (each) 14 50 Beam Combiner 6 21 Transfer Optics 3 10 Internal Seeing 3 10
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingUnequal beam intensity
Visibility loss due to intensity mismatch:
Error sources:
♦Atmospheric scintillation (negligible) ♦Coatings (small) ♦For fiber-fed instrument (large):»Tip-tilt errors
»Instantaneous Strehl fluctuation
2121..21IIII VV
VINCI measure I1 & I2
(photometry channels) to correct for this effect. VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingPolarization Effects
Linear Retardation
♦Error sources: Coatings»Different coatings in the two arms
»Differential incidence angles (between arms)
»Differential coating characteristics (e.g. thickness of the protecting layer) ♦Can be very critical in Near IR/Visible and for multi-dielectric coatings (M9). VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingPolarization Effects
Rotation of polarization frame
♦Error sources: »Differential frame-of-reference/pupil rotation due to optical design and/or misalignment ♦Can be avoided by proper optical design and alignment. VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingVLTI Tutorial
Some results from on-going VLTI
commissioning VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingMeasured micro-seismic vibration
OPD as measured with accelerometers
at the back of Transfer Opticsmirrors (M12, M16, Switchyard, BeamCompressor)
Accelerometer on back of M12-G0 mirror
Error budget:
Wavelength VIS NIR TIRTransfer
Optics31045
VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingOPD stability inside UT
Measured with high sensitive accelerometerson UT#1&3 Few improvementson sub-system identifiedand on-goingOverall stability excellent
M1 M2 M3 M4 M5 M6Overview - Vibrations of subsystems
0.00.11.010.0100.0
All OFF
Air Co. in Power cabinet ON
(Alt+Az+Nasm.) LCU's ONM2 Unit LCU ON
Cassegrain Adaptor LCU ON
M1 Cell LCU ON
HBS ON
Cooling Pumps ON (Tube valve CLOSED)
Cooling Pumps ON +Tube valve OPEN
Azimuth Motor ON
Altitude Motor ON (Cable Wrap OFF)
Altitude Motor ON + Cable Wrap B ON
Altitude Motor ON + Cable Wrap A&B ON
Subsystems
Contrast Loss [%]
VISNIRTIR
Spec. VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, GarchingMeasured OPD spectrum
0 10 20 3040
50
60
70
-30-25-20-15-10 -5 05
101520
File: opd_vinci_on_sky
Time [sec]
OPD [um]
OPD as measured on a star
by VINCIwith Siderostats 10 -2 10 -1quotesdbs_dbs30.pdfusesText_36[PDF] télécharger compressor mac
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