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VLTI Tutorial VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, Garching

VLTI Tutorial

The VLTI conceptual design

VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, Garching

VLTI 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, Garching

The Final VLTI Array Layout

4 UT's as 'trapezoidal' as

possible (wind shadow, ground quality) ♦Baselines 47 - 130m

1.5 milli arcsec

30 Stationsfor AT's

♦Baselines 8 - 200m

1 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 room

All 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, Garching

The VLTI Optical Layout

VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, Garching

The '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, Garching

Telescope Optical Design

Intermediate Focusbelow M4:

♦Various artificial light sourcesfor calibration & alignment

Intermediate pupilimage on

M8: ♦Deformable mirrorfor MACAO

CoudeFocus:

♦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, Garching

Relay Optics

VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, Garching

Relay 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 towards

M12 in DL Tunnel

Location for STRAP/

MACAO Wave Front

Sensor

VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, Garching

The Delay Lines

VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, Garching

The 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: <15W

Variable Curvature Mirror

(VCM) ♦re-image pupil inside the

Laboratory

♦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, Garching

Transfer Optics

VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, Garching

Transfer 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, Garching

Beam Make-up

STRAP (Tip-Tilt)

or

MACAO (Adaptive Optics

FINITO (Fringe Tracker)

VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, Garching

STRAP (Tip-Tilt)

Quad-celldetector with APDat telescope Coude focus

Pure 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 0

0.10.20.30.40.5

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, Garching

MACAO (Adaptive Optics)

X-Y Tableallows reference source

different from target A mustfor UTin K-band (AMBER). Gain in coherent flux≈100

60 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, Garching

MACAO performance

667k
266k
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 00.6

0.40.8

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, Garching

FINITO (Fringe Tracker)

VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, Garching

The VLTI Laboratory

High thermal stability; limited access, low power dissipation

Telescope Exit Pupil re-imagedinto instruments

Optical design for up to 8 beams(4 UTs with dual feed) 5 m VINCI PRIMA FSU M16 MIDI MIDI

Visitor

Instrument

PRIMA DDLs Beam

Compressors

SwitchyardAMBER

DL I DL II

DL III

DL IV

VLTI Laboratory

ZOPD Ref.

FSU

Telescope Exit Pupil

Delay Line Tunnel

VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, Garching

Inside 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, Garching

VLTI Tutorial

The VLTI

selected critical technical aspects VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, Garching

VLTI Error Budget

LEGEND:

OPD VARIATION

A

CROSS PUPIL

OVERALL

OPD VARIATION

WITH TIME

POLARIZATION

EFFECTS

UNEQUAL BEAM

INTENSITIES

VLTI

INSTRUMENT

FRINGE TRACKER

A

DAPTIVE OPTICS

OPTICAL DESIGN

OPTICS

IMPERFETION

FINE IMAGE

TRACKER

A tmosphere

Internal seeing

Coating

Internal seeingFiguring errors

A lignment errors

Fringe 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 µm

With spatial filter

φ=17 airy radii

LINEAR

RETARDATION

Systematic visibility loss (%) Random visibility loss (%)Error source

Fringe sensor= Allocation to be extracted

from a closed loop analysis39.3 5.4 2.0

0.4 31.0 5

6.00.0 0.06 0.00.1 0.00.00.0

0.0 0.0

0.14

0.06.16

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 0.0

2.0 0.1?

VLTI INSTRUMENTS= Error sources not part of

this error budget

OPD 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 6,2

Fringe 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) < atmosphere

Wavelength 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, Garching

Unequal 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, Garching

Polarization 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, Garching

Polarization 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, Garching

VLTI Tutorial

Some results from on-going VLTI

commissioning VLTI Tutorial: VLTI Concept & technical aspects, B. Koehler, 20 November 2001, Garching

Measured micro-seismic vibration

OPD as measured with accelerometers

at the back of Transfer Opticsmirrors (M12, M16, Switchyard, Beam

Compressor)

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, Garching

OPD stability inside UT

Measured with high sensitive accelerometerson UT#1&3 Few improvementson sub-system identifiedand on-going

Overall stability excellent

M1 M2 M3 M4 M5 M6

Overview - Vibrations of subsystems

0.00.11.010.0100.0

All OFF

Air Co. in Power cabinet ON

(Alt+Az+Nasm.) LCU's ON

M2 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, Garching

Measured OPD spectrum

0 10 20 30
40
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
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