b.delabre november 2003angra dos reis - brazil eso 2 nd generation instrumentation – optical...

November 2003November 2003 ANGRA DOS REIS - BRAZILANGRA DOS REIS - BRAZIL

B.DelabreB.Delabre

ESO 2ESO 2ndnd GENERATION INSTRUMENTATION – OPTICAL DESIGNS GENERATION INSTRUMENTATION – OPTICAL DESIGNS

ESO VLT SECOND GENERATIONESO VLT SECOND GENERATIONINSTRUMENTATIONINSTRUMENTATION

Optical designsOptical designs

ANGRA DOS REIS - BRAZILANGRA DOS REIS - BRAZILNovember 2003November 2003B.Delabre (ESO)B.Delabre (ESO)


B.DelabreB.Delabre


This presentation will show possible This presentation will show possible opticaloptical

designs for ESO second generation VLTdesigns for ESO second generation VLT

instrumentation.instrumentation.

All instruments are still in Phase A All instruments are still in Phase A studiesstudies


B.DelabreB.Delabre


List of VLT second generation List of VLT second generation instruments:instruments:

HAWK-IHAWK-I (IR imager) (IR imager) KMOSKMOS (multi-objects Integral field spectrograph) (multi-objects Integral field spectrograph) MUSEMUSE (visible integral field spectrograph) (visible integral field spectrograph) X-SHOOTERX-SHOOTER (Medium resolution echelle (Medium resolution echelle

spectrograph from 300-1800 nm)spectrograph from 300-1800 nm) Planet finderPlanet finder (not included in the presentation) (not included in the presentation)


B.DelabreB.Delabre


HAWK-I HAWK-I Large field Infrared ImagerLarge field Infrared Imager

Build by : ESO Build by : ESO PI : Alan Moorwood (ESO)PI : Alan Moorwood (ESO)


B.DelabreB.Delabre

ESO 2ESO 2ndnd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-IHAWK-I

CharacteristicsCharacteristics

Field of viewField of view 8.0 x 8.0 arc min or 8.5 x 8.5 arc min 8.0 x 8.0 arc min or 8.5 x 8.5 arc min

depending of the selected conceptdepending of the selected concept Wavelength rangeWavelength range 800 – 2500 nm 800 – 2500 nm ScaleScale 0.117 or 0.125 arc sec/pixel 0.117 or 0.125 arc sec/pixel F/NF/N F/3.8 or F/3.6 F/3.8 or F/3.6 DetectorDetector 4k x 4k (18µm pixel) 4k x 4k (18µm pixel) No spectroscopy availableNo spectroscopy available ( by design) ( by design)


B.DelabreB.Delabre

ESO 2ESO 2ndnd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I GENERATION INSTRUMENTATION – OPTICAL DESIGNS – HAWK-I

3 designs are considered :3 designs are considered :

- Compact dioptric design with small filters- Compact dioptric design with small filters

- Larger dioptric design with large filters- Larger dioptric design with large filters

- All reflective design with large filters- All reflective design with large filters


B.DelabreB.Delabre


DESIGN 1 DESIGN 1

Compact dioptric solutionCompact dioptric solution

8.5 x 8.5 arc min field8.5 x 8.5 arc min field


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08:42:11

Scale: 0.21 24-Jun-03

119.05 MM

LAYOUT

Folding mirror

Folding mirror

Detector4k x 4k

Cryostat

window

1 m1 m


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accessible pupilaccessible pupil possibility to use standard 2 inches filterspossibility to use standard 2 inches filters image quality comparable to pixel size for the entire fieldimage quality comparable to pixel size for the entire field distortion freedistortion free no ghost imagesno ghost images no very high incidence angles on the lenses to avoid no very high incidence angles on the lenses to avoid

extreme sensitivity to element tilts and decentrings, extreme sensitivity to element tilts and decentrings, even at the cost of an extra element.even at the cost of an extra element. all spherical surfaces.all spherical surfaces. comfortable back focal distancecomfortable back focal distanceThe thickness and material of the filter must be constantThe thickness and material of the filter must be constantHigh incidence angles on the filters do not permit an effective High incidence angles on the filters do not permit an effective

use ofuse ofNarrow band filtersNarrow band filters


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13:31:45

Scale: 0.54 ESO 18-Feb-03

46.30 MM

CaF2

STIM28

BaF2

ZnSe Filter

BaF2

ZnS

ZnS

ZnSe

Detector


B.DelabreB.Delabre


14:09:18

ESO 18-Feb-03

25.40 MM

Cold stop for J Band

14:07:59

ESO 18-Feb-03

25.40 MM

Cold stop for H Band

14:06:19

ESO 18-Feb-03

25.40 MM

Cold stop for K Band

Pupil aberrationsPupil aberrations

The cold stop isThe cold stop isattached to the filterattached to the filter


B.DelabreB.Delabre


13:14:56

0.000,0.000 DG 0.00, 0.00

0.000,.0167 DG 0.00, 0.17

0.000,.0333 DG 0.00, 0.33

0.000,.0500 DG 0.00, 0.50

0.000,.0667 DG 0.00, 0.67

0.000,.0833 DG 0.00, 0.83

0.000,0.100 DG 0.00, 1.00

FIELDPOSITION

DEFOCUSING 0.00000

.254E-01 MM

Box : 1 pixel

Spot diagramsSpot diagramsPolychromaticPolychromatic1000-2500nm1000-2500nm

Box = 1 pixelBox = 1 pixel


B.DelabreB.Delabre


13:14:56

0.000,0.000 DG 0.00, 0.00

0.000,.0167 DG 0.00, 0.17

0.000,.0333 DG 0.00, 0.33

0.000,.0500 DG 0.00, 0.50

0.000,.0667 DG 0.00, 0.67

0.000,.0833 DG 0.00, 0.83

0.000,0.100 DG 0.00, 1.00

FIELDPOSITION

DEFOCUSING 0.00000

.254E-01 MM

Box : 1 pixel

Spot diagramsSpot diagrams850 – 1000nm850 – 1000nm



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DESIGN 2 DESIGN 2

Large dioptric designLarge dioptric design



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This design has the following advantages with respect toThis design has the following advantages with respect to

the compact design :the compact design :

- Less optical elements (only 5 lenses)- Less optical elements (only 5 lenses)

- No restriction on filter material and thickness, two - No restriction on filter material and thickness, two filterfilter

wheels are accommodated in front of the detectorwheels are accommodated in front of the detector

- Cold stop outside the objective- Cold stop outside the objective

- Relaxed tolerances on lens centerings- Relaxed tolerances on lens centerings

- Narrow band filters can be used- Narrow band filters can be used


B.DelabreB.Delabre


15:56:36

Scale: 0.18 15-Sep-03

138.89 MM

detector4K x 4K

folding mirror

folding mirror

entrancewindow

coldstop

2 filterwheels

lens objectiv

1.2 m1.2 m


B.DelabreB.Delabre


16:13:53

0.000,0.000 DG 0.00, 0.00

0.000,.0167 DG 0.00, 0.17

0.000,.0333 DG 0.00, 0.33

0.000,.0500 DG 0.00, 0.50

0.000,.0667 DG 0.00, 0.67

0.000,.0833 DG 0.00, 0.83

0.000,0.100 DG 0.00, 1.00

FIELDPOSITION

DEFOCUSING 0.00000

.183E-01 MM

box : 1pixel (18 microns)

Spot diagramsSpot diagramsPolychromaticPolychromatic1000-2500nm1000-2500nm



B.DelabreB.Delabre


16:58:17

15-Sep-03

108.70 MM

K Band

16:57:20

15-Sep-03

108.70 MM

H Band

16:56:18

Scale: 0.23 15-Sep-03

108.70 MM

J Band Pupil for J bandPupil for J band

Pupil for H bandPupil for H bandPupil for K bandPupil for K band

The cold stop is adjustedThe cold stop is adjustedfor K band, vignetting willfor K band, vignetting will

occur for J and H occur for J and H


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DESIGN 3DESIGN 3

All reflective designAll reflective design



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Advantages of this designAdvantages of this design : : - Efficiency (93% without filter)- Efficiency (93% without filter)

- Relaxed centering tolerances- Relaxed centering tolerances

- Achromatic- Achromatic

- Problem of refractive indices at cryogenic temperature does not - Problem of refractive indices at cryogenic temperature does not existexist

Drawbacks of this designDrawbacks of this design : :

- - Large sizeLarge size

- Slightly reduced field of view- Slightly reduced field of view

- Distortion is not fully corrected (around 0.002 %)- Distortion is not fully corrected (around 0.002 %)


B.DelabreB.Delabre


15:55:49

Scale: 0.09 13-Oct-03

271.74 MM

NasmythFocus

EntranceWindow

SphericalMirror

FilterWheel

Detector4K x 4K

asphericalMirror

Mirror (cold stop)

aspherical

HAWK-I MIRROR SOLUTION

2.3 m2.3 m


B.DelabreB.Delabre


Axis 1.0 2.0 3.0 4.0 arc min Axis 1.0 2.0 3.0 4.0 arc min

4 arc min4 arc min 25 μm 25 25 μm 25 21 21 15 15 17 17

3 arc min3 arc min 25 25 24 24 20 20 13 13 13 13

2 arc min2 arc min 25 25 23 23 19 19 13 13 10 10

1 arc min1 arc min 24 24 22 22 18 18 13 13 10 10

Axis 21Axis 21 20 17 20 17 13 13 11 11

-1 arc min-1 arc min 18 18 17 17 15 15 12 12 12 12

-2 arc min-2 arc min 15 15 14 14 12 12 10 10 13 13

-3 arc min-3 arc min 11 11 10 10 9 9 10 10 14 14

-4 arc min-4 arc min 12 12 13 13 14 14 15 15 15 15

Image qualityImage quality80% geometrical energy (diameter)80% geometrical energy (diameter)


B.DelabreB.Delabre


08:16:59

16-Sep-03

200.00 MM

08:15:46

16-Sep-03

200.00 MM

14:47:47

31-Oct-03

200.00 MM

The 3 concepts are represented The 3 concepts are represented at the same scaleat the same scale


B.DelabreB.Delabre

ESO 2ESO 2ndnd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE

MUSEMUSE Visible integral field spectrographVisible integral field spectrograph

Built by external consortiums : Lyon- Cambridge – Durham – Leiden – Oxford – Built by external consortiums : Lyon- Cambridge – Durham – Leiden – Oxford – Postdam - ZurichPostdam - Zurich

PI : Roland Bacon (Lyon)PI : Roland Bacon (Lyon)


B.DelabreB.Delabre


Integral field spectrographIntegral field spectrograph

Spectral rangeSpectral range : 465 – 930 nm : 465 – 930 nmField of viewField of view : 1.0 x 1.0 arc min (low resolution mode) : 1.0 x 1.0 arc min (low resolution mode) 7.5 x 7.5 arc sec (high resolution mode)7.5 x 7.5 arc sec (high resolution mode)Spatial samplingSpatial sampling: 0.2 arc sec (low resolution mode): 0.2 arc sec (low resolution mode) 0.026 arc sec (high resolution mode)0.026 arc sec (high resolution mode)Spectral samplingSpectral sampling : 0.1 (LR) or 0.0125 (HR) arc sec/pixel : 0.1 (LR) or 0.0125 (HR) arc sec/pixelSpectrographsSpectrographs : 24 single mode spectrographs : 24 single mode spectrographs equipped with 4K x 4K CCDequipped with 4K x 4K CCD Resolving powerResolving power : R=3000 at 700 nm for 2 pixels resolving : R=3000 at 700 nm for 2 pixels resolving

elementelement

Possibility to operate with adaptive opticsPossibility to operate with adaptive optics


B.DelabreB.Delabre


Optical Optical benchbench

2 x 4 2 x 4 spectrographsspectrographs


AO moduleAO module


1000 mm1000 mm


B.DelabreB.Delabre



AOAOmodulemodule

Optical benchOptical bench

Calib

rati

on

Calib

rati

on A

dap

tor

flan

ge

Ad

ap

tor

flan

ge

1000 mm1000 mm


B.DelabreB.Delabre


SpectrographSpectrographcryostatcryostat Image slicersImage slicers

cryostatcryostat

cryostatcryostat

cryostatcryostat

SpectrographSpectrograph



Image slicersImage slicers



2100 mm2100 mm

400

mm

400

mm









1000 mm1000 mm

SPECTROGRAPH RACKS SPECTROGRAPH RACKS ((2 X 4 SPECTROGRAPHS)2 X 4 SPECTROGRAPHS)


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The fore opticsThe fore optics


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The fore optics consists ofThe fore optics consists of : :

- An optical relay to produce an image of the telescope focus - An optical relay to produce an image of the telescope focus on a field splitter (this optic has 2 magnifications)on a field splitter (this optic has 2 magnifications)

- An optical derotator- An optical derotator

- A field splitter which cut the field of view in 24 sub-fields- A field splitter which cut the field of view in 24 sub-fields

- 24 transfer optics to send the light to the spectrographs- 24 transfer optics to send the light to the spectrographs


B.DelabreB.Delabre


08:53:50

Scale: 0.20 03-Nov-03

125.00 MM

Adaptor Adaptor flangeflange

Nasmyth Nasmyth FocusFocus

DerotatorDerotator

F/25 focusF/25 focus

Field splitterField splitter

Large field (1.0 x 1.0 arc min)Large field (1.0 x 1.0 arc min)

1035 mm1035 mm

600

mm

600

mm

Optical relayOptical relay


B.DelabreB.Delabre


10:02:52

0.000,0.000 DG 0.00, 0.00

0.000,.0042 DG 0.00, 0.35

0.000,.0083 DG 0.00, 0.71

0.000,.0118 DG 0.00, 1.00

FIELDPOSITION

DEFOCUSING 0.00000

.992E-01 MM

15 arcsec

30 arcsec

43 arcsec

Circle = 0.1 arc secCircle = 0.1 arc sec

Large fieldLarge fieldSpot diagramsSpot diagrams

0.097 mm0.097 mm


B.DelabreB.Delabre

ESO 2ESO 2ndnd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE GENERATION INSTRUMENTATION – OPTICAL DESIGNS - MUSE09:14:08

Scale: 0.20 03-Nov-03

125.00 MM

Small field (7.5 X 7.5 arc sec)Small field (7.5 X 7.5 arc sec)

F/200F/200Field splitterField splitter

DerotatorDerotator Nasmyth focusNasmyth focus

Adaptor Adaptor FlangeFlange

ExchangeableExchangeablelenseslenses

Optical relayOptical relay


B.DelabreB.Delabre


10:14:36

0.000,0.000 DG 0.00, 0.00

0.000,.0005 DG 0.00, 0.35

0.000,.0010 DG 0.00, 0.71

0.000,.0015 DG 0.00, 1.00

FIELDPOSITION

DEFOCUSING 0.00000

.391 MM

1.875 arcsec

3.75 arcsec

5.3 arcsec

Circle = 0.05 arc secCircle = 0.05 arc sec

0.385 mm0.385 mm

Small fieldSmall fieldSpot diagramsSpot diagrams


B.DelabreB.Delabre


15:55:52

20-Oct-03

25.40 MM

MUSE DEROTATOR

203 mm203 mm


B.DelabreB.Delabre


08:53:50

Scale: 0.20 03-Nov-03

125.00 MM

Adaptor Adaptor flangeflange

Nasmyth Nasmyth FocusFocus

DerotatorDerotator

F/25 focusF/25 focus

Field splitterField splitter

Large fieldLarge field

1035 mm1035 mm

600

mm

600

mm

AdaptiveAdaptiveopticsoptics


CalibrationCalibration unitunit


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Field slicer and transfer optics Field slicer and transfer optics (developed at CRAL by B.Lanz)(developed at CRAL by B.Lanz)

The 1 x 1 arc min field of view is cut in 24 fields of 20 x 7.5 arc sec The 1 x 1 arc min field of view is cut in 24 fields of 20 x 7.5 arc sec

A transfer optic is used to send individually each field to an image A transfer optic is used to send individually each field to an image slicerslicer

This optic produces also an anamorphic magnification :This optic produces also an anamorphic magnification :

F/25 to F/104 (spatial)F/25 to F/104 (spatial)

F/25 to F/208 (spectral)F/25 to F/208 (spectral)


B.DelabreB.Delabre


Pupil elements

SlicingElements

(at telescopefocal plane)

Slit elements(at Pseudo-slit

plane)

InputPupil

(from telescope)

Exit Pupilplane

SPECTRO-GRAPH

TELESCOPE

The Image slicersThe Image slicers developed at CRALdeveloped at CRAL

by B.Lanz and F.Henaultby B.Lanz and F.Henault


B.DelabreB.Delabre


The SpectrographsThe Spectrographs


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A classical design will be too expensiveA classical design will be too expensive No glasses like CaF2 or FK54…. can be No glasses like CaF2 or FK54…. can be

afforded. Only glasses with a price similar afforded. Only glasses with a price similar (max x2.5) to BK7 should be used if (max x2.5) to BK7 should be used if possible.possible.

The spectrographs should be small to The spectrographs should be small to reduce cost, volume and weightreduce cost, volume and weight

No mechanical functions are permitted (no No mechanical functions are permitted (no refocusing and no exchange of dispersive refocusing and no exchange of dispersive elements)elements)

Design guidelines :Design guidelines :


B.DelabreB.Delabre


Detector 4K x 4K with 15 microns pixelsDetector 4K x 4K with 15 microns pixels Entrance F/N F/4.5 (slit direction)Entrance F/N F/4.5 (slit direction) F/9.0 (dispersion)F/9.0 (dispersion) Output F/N F/2.0 (slit direction)Output F/N F/2.0 (slit direction) F/4.0 (dispersion)F/4.0 (dispersion) Flat entrance slitFlat entrance slit Entrance pupil 3 m after the slitEntrance pupil 3 m after the slit Dispersive element : VPH 700 mm-1Dispersive element : VPH 700 mm-1 Pupil size 45 x 90 mmPupil size 45 x 90 mm Wavelength range 465 – 930 nmWavelength range 465 – 930 nm Estimated transmission around 0.85 without VPHEstimated transmission around 0.85 without VPH

Characteristics :Characteristics :


B.DelabreB.Delabre


No expensive glasses is equivalent to poor No expensive glasses is equivalent to poor chromatic correctionchromatic correction

Chromatism is compensated by a tilt of the field Chromatism is compensated by a tilt of the field lens and the detectorlens and the detector

The VPH is not operating in a perfect parallel The VPH is not operating in a perfect parallel beam. It has some contributions to the correction beam. It has some contributions to the correction of image qualityof image quality

No refocusing required for correction of No refocusing required for correction of temperature variation (the variation of focus temperature variation (the variation of focus position is 4 position is 4 µµm/m/°C°C for the current design) for the current design)

Exchanges of dispersive elements or spectral Exchanges of dispersive elements or spectral ranges are not possibleranges are not possible


B.DelabreB.Delabre


11:02:00

Scale: 0.23Position: 1

25-Jun-03

108.70 MM

slit

collimator

VPH

Camera

Cryostat windowand CCD

MUSE SPECTROGRAPH Dispersion plane

920 mm

920 mm


B.DelabreB.Delabre


11:06:37


25-Jun-03

XZ108.70 MM

MUSE SPECTROGRAPH Slit plane

collimator

VPH

camera


B.DelabreB.Delabre


465 nm 540 nm

07:48:01

0.000,0.000 DG 0.00, 0.00

-0.31,0.000 DG 0.24, 0.00

-0.61,0.000 DG 0.48, 0.00

-0.92,0.000 DG 0.72, 0.00

-1.28,0.000 DG 1.00, 0.00

FIELDPOSITION

DEFOCUSING 0.00000

.305E-01 MM

07:49:59

0.000,0.000 DG 0.00, 0.00

-0.31,0.000 DG 0.24, 0.00

-0.61,0.000 DG 0.48, 0.00

-0.92,0.000 DG 0.72, 0.00

-1.28,0.000 DG 1.00, 0.00

FIELDPOSITION

DEFOCUSING 0.00000

.305E-01 MM

Boxes are 2 x 2 pixelsBoxes are 2 x 2 pixels


B.DelabreB.Delabre


620 nm 698 nm

07:51:45

0.000,0.000 DG 0.00, 0.00

-0.31,0.000 DG 0.24, 0.00

-0.61,0.000 DG 0.48, 0.00

-0.92,0.000 DG 0.72, 0.00

-1.28,0.000 DG 1.00, 0.00

FIELDPOSITION

DEFOCUSING 0.00000

.305E-01 MM

07:53:03

0.000,0.000 DG 0.00, 0.00

-0.31,0.000 DG 0.24, 0.00

-0.61,0.000 DG 0.48, 0.00

-0.92,0.000 DG 0.72, 0.00

-1.28,0.000 DG 1.00, 0.00

FIELDPOSITION

DEFOCUSING 0.00000

.305E-01 MM


B.DelabreB.Delabre


775 nm 852 nm

08:02:54

0.000,0.000 DG 0.00, 0.00

-0.31,0.000 DG 0.24, 0.00

-0.61,0.000 DG 0.48, 0.00

-0.92,0.000 DG 0.72, 0.00

-1.28,0.000 DG 1.00, 0.00

FIELDPOSITION

DEFOCUSING 0.00000

.305E-01 MM

08:04:09

0.000,0.000 DG 0.00, 0.00

-0.31,0.000 DG 0.24, 0.00

-0.61,0.000 DG 0.48, 0.00

-0.92,0.000 DG 0.72, 0.00

-1.28,0.000 DG 1.00, 0.00

FIELDPOSITION

DEFOCUSING 0.00000

.305E-01 MM


B.DelabreB.Delabre


930 nm

08:05:24

0.000,0.000 DG 0.00, 0.00

-0.31,0.000 DG 0.24, 0.00

-0.61,0.000 DG 0.48, 0.00

-0.92,0.000 DG 0.72, 0.00

-1.28,0.000 DG 1.00, 0.00

FIELDPOSITION

DEFOCUSING 0.00000

.305E-01 MM


B.DelabreB.Delabre


WavWav

SlitSlit465465 540540 620620 698698 775775 852852 930930

6767mmmm

2121 1212 1414 1414 1212 99 2323

4848 2020 1616 1515 1313 1010 88 1414

3232 1515 1414 1212 1010 88 66 1515

1616 1414 1111 99 99 66 88 1515

axisaxis 1313 1010 88 1010 66 77 1616

Rms spot diametersRms spot diameters


B.DelabreB.Delabre


The collimator is made of 4 lenses in 3 groupsThe collimator is made of 4 lenses in 3 groups

The materials are BK7 (3 lenses) and PBH1 (1 lens)The materials are BK7 (3 lenses) and PBH1 (1 lens)

The field curvature is not corrected (the correction The field curvature is not corrected (the correction is done by a cylindrical surface on back side of is done by a cylindrical surface on back side of the cryostat window.the cryostat window.

CollimatorCollimator


B.DelabreB.Delabre


10:15:06

Scale: 0.32 22-May-03

78.125 MM

MUSE COLLIMATOR


B.DelabreB.Delabre


09:57:20

Scale: 0.28 22-May-03

89.29 MM

COMPENSATOR

MUSE COLLIMATOR TEST SETUP


B.DelabreB.Delabre

ESO 2ESO 2ndnd GENERATION INSTRUMENTATION – OPTICAL DESIGNS -MUSE GENERATION INSTRUMENTATION – OPTICAL DESIGNS -MUSE

The camera includes 5 lenses made of BK7-NaLF7-The camera includes 5 lenses made of BK7-NaLF7-BK7BK7

PbH1-PbH1. PbH1-PbH1.

The field lens is not included in the cameraThe field lens is not included in the camera

The CameraThe Camera


B.DelabreB.Delabre


14:59:25

Scale: 0.72 22-May-03

34.72 MM

MUSE CAMERA


B.DelabreB.Delabre


15:03:00

Scale: 0.67 22-May-03

37.31 MM

MUSE CAMERA TEST SETUP


B.DelabreB.Delabre


The field lens will also act as cryostat window. The field lens will also act as cryostat window.

A cylindrical surface on its back side will correct the A cylindrical surface on its back side will correct the field curvature of the slit and collimator.field curvature of the slit and collimator.

The lens is perpendicular to the CCDThe lens is perpendicular to the CCD

The full cryostat is decentered and tilted with The full cryostat is decentered and tilted with respect to the camera axisrespect to the camera axis

The field lensThe field lens


B.DelabreB.Delabre


09:35:01


02-Jun-03

XZ19.23 MM

CENTRAL THICKNESS 35 MM

MUSE FIELD LENS


B.DelabreB.Delabre


MUSE ADAPTIVE OPTICSMUSE ADAPTIVE OPTICS


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MUSE IS COMPATIBLE WITH 3 OPERATION MUSE IS COMPATIBLE WITH 3 OPERATION MODESMODES::

- WITHOUT ADAPTIVE OPTIC- WITHOUT ADAPTIVE OPTIC - TELESCOPE ADAPTIVE SECONDARY- TELESCOPE ADAPTIVE SECONDARY - MULTI-CONJUGATE ADAPTIVE OPTICS- MULTI-CONJUGATE ADAPTIVE OPTICS No major modification of MUSE are requested to change from No major modification of MUSE are requested to change from

one operation mode to another.one operation mode to another.


B.DelabreB.Delabre


TELESCOPE ADAPTIVE TELESCOPE ADAPTIVE SECONDARYSECONDARY

(ONE DEFORMABLE MIRROR)(ONE DEFORMABLE MIRROR)


B.DelabreB.Delabre


LGSs attached to telescope center piece rotate like LGSs attached to telescope center piece rotate like telescope pupil at Nasmythtelescope pupil at Nasmyth

1’ Scientific FOV rotates like Nasmyth field rotation1’ Scientific FOV rotates like Nasmyth field rotation Differential rotation between LGSs and scientific FOVDifferential rotation between LGSs and scientific FOV LGS focus varies from 80-180 kmLGS focus varies from 80-180 km LGS defocalisation @ Nasmyth varies from:LGS defocalisation @ Nasmyth varies from: 180-80mm 180-80mm At Nasmyth focal plane LGS footprint varies from: 12-At Nasmyth focal plane LGS footprint varies from: 12-

5mm5mm Nasmyth pixel scale is 582µm/”Nasmyth pixel scale is 582µm/” => LGS at 1’x√2/2+ half LGS foot-print ~70” off-axis=> LGS at 1’x√2/2+ half LGS foot-print ~70” off-axis FOV for LGS-WFS is >4” (spot elongation+3σ seeing)FOV for LGS-WFS is >4” (spot elongation+3σ seeing)


B.DelabreB.Delabre


Laser& NGS light passes through Plate 1Laser& NGS light passes through Plate 1 Plate 2 reflects only the LGS light toward Plate 1Plate 2 reflects only the LGS light toward Plate 1 Plate 2 translates along optical axis to compensate for LGS Plate 2 translates along optical axis to compensate for LGS

focusfocus Plate 1 has 4 small mirrors, located in the central obstruction of Plate 1 has 4 small mirrors, located in the central obstruction of

each laser beam to reflect the LGS light toward the WFSeach laser beam to reflect the LGS light toward the WFS Plate 1 rotates to compensate for LGS rotation and SH pupil Plate 1 rotates to compensate for LGS rotation and SH pupil

rotationrotation WFSs and Plate 1 rotate togetherWFSs and Plate 1 rotate together Plate 2 has a notch filter in the center ~1.5’ field to block the Plate 2 has a notch filter in the center ~1.5’ field to block the

scattered laser light and transmit the scientific fieldscattered laser light and transmit the scientific field Plate 2 has a dichroic slit in the reflective area to transmit the Plate 2 has a dichroic slit in the reflective area to transmit the

NGS toward MUSENGS toward MUSE Plate 2 rotates for the acquisition and tracking of the NGS in the Plate 2 rotates for the acquisition and tracking of the NGS in the

slitslit NGS field rotation is compensated with the 3’ derotatorNGS field rotation is compensated with the 3’ derotator


B.DelabreB.Delabre


LGS @ 80 km

Laser focal plane

LGS derotator table

LGS focus trackingMirror/dichroic

Scie

nti

fic

fiel

d

LGS reflected light

NGS light

LGS Pupil image

LGS collimator

NA

SM

YT

H F

OC

AL

PL

AN

E

Pla

te 1

Pla

te 2


B.DelabreB.Delabre


LGS @ 180 km

Laser focal plane

LGS focus trackingMirror/dichroic

Scie

nti

fic

fiel

d

LGS reflected light

NGS light

LGS derotator table

LGS Pupil image

LGS collimator

Pla

te 1

Pla

te 2


B.DelabreB.Delabre


LGS mirror

Notch filter

NGS acq. slit

Functions:

LGS mirror (at 70” off-axis)LGS focus correctionField stop for laser light (1.5’-3’)LGS dichroic/notch filter (0-1.5’)NGS selector & transmitter

Notch transmission (normal incidence)

0.01%

0.10%

1.00%

10.00%

100.00%

450 500 550 600 650 700 750 800 850 900 950

transmission

wav

elen

gth

(n

m)

Plate 2Plate 2


B.DelabreB.Delabre


Natural guideNatural guideStar areaStar area

LGSLGSbeambeam

ScientificScientificfieldfield

LGS at 160 kmLGS at 160 kmPlate 1Plate 1

Natural guideNatural guideStar areaStar area

LGSLGSbeambeam

ScientificScientificfieldfield

Plate 1Plate 1

LGS at 80 kmLGS at 80 km


B.DelabreB.Delabre


FoV 140”

Fast Read-OutCCD

PupilRe-

imagingLens

XY Table

LensletArray


B.DelabreB.Delabre


MULTI CONJUGATES ADAPTIVE MULTI CONJUGATES ADAPTIVE OPTICSOPTICS

(2 DEFORMABLE MIRRORS + TIP-TILT MIRROR)(2 DEFORMABLE MIRRORS + TIP-TILT MIRROR)


B.DelabreB.Delabre


OPTICAL COMPONENTSOPTICAL COMPONENTS

Ground layer deformable mirror : 180 mmGround layer deformable mirror : 180 mm8.5 km layer deformable mirror : 150 mm8.5 km layer deformable mirror : 150 mmTip-tilt mirror : 180 mmTip-tilt mirror : 180 mm3 lenses objective3 lenses objective1 total reflection prism1 total reflection prism1 pupil relay lens1 pupil relay lens2 folding mirrors2 folding mirrors


B.DelabreB.Delabre


The full system is located between the adaptor The full system is located between the adaptor flange and the Nasmyth focus (250 mm only are flange and the Nasmyth focus (250 mm only are available)available)

The image produced is identical and at the same The image produced is identical and at the same location than the original Nasmyth image in order location than the original Nasmyth image in order to operate MUSE with or without Adaptive Optics to operate MUSE with or without Adaptive Optics with no modification of the instrument.with no modification of the instrument.


B.DelabreB.Delabre


CharacteristicsCharacteristics

4 laser guide stars at 70 arc sec off 4 laser guide stars at 70 arc sec off axisaxis

3 arc min field of view for natural 3 arc min field of view for natural guide starguide star

Wavelength range 450 -1000 nmWavelength range 450 -1000 nm


B.DelabreB.Delabre


Scale: 0.08 13-Oct-03

XZ316.46 MM

Tip-tiltMirror

8.5 kmlayer

Groundlayer

NasmythFocus

Pupil relayLens

Objective(gamma=1)

FoldingMirror

MUSE Multi conjugate AO (front view)


B.DelabreB.Delabre


13-Oct-03

316.46 MM

MUSE Multi conjugate AO (side view)

Adaptor flange

8.5 kmlayer

Objective Focus (F/15)


B.DelabreB.Delabre



Natural Natural Guide starGuide star

Focus Focus CompensationCompensation

plateplate

WSWSdetectordetector

WSWSdetectordetector

DerotatorDerotator

PupilPupilReimagingReimaging

lenslens

Pupil Pupil Reimaging prismReimaging prism

Large fieldLarge fieldobjectiveobjective

rotates like the fieldrotates like the field

rotates like the pupilrotates like the pupil


B.DelabreB.Delabre


Multi-object integral Multi-object integral field spectrographfield spectrograph

for near IRfor near IR(1000-2500 nm)(1000-2500 nm)


B.DelabreB.Delabre


Another way of building multi-object integral Another way of building multi-object integral field spectrographsfield spectrographs

The selection of objects is a very critical problem in IR multi-object The selection of objects is a very critical problem in IR multi-object spectroscopy because it requires a lot of cryogenic functions.spectroscopy because it requires a lot of cryogenic functions.

Based on the concept of a KMOS study done for ESO, we have developed Based on the concept of a KMOS study done for ESO, we have developed the baseline of a new solution which could strongly improve the reliability the baseline of a new solution which could strongly improve the reliability of the instrument at the cost of a small increase of background (2 warm of the instrument at the cost of a small increase of background (2 warm mirrors).mirrors).


B.DelabreB.Delabre

ESO 2ESO 2ndnd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - KMOS GENERATION INSTRUMENTATION – OPTICAL DESIGNS - KMOS

Main features of the new conceptMain features of the new concept : :

- Object selection done at ambient - Object selection done at ambient temperature (only 2 warm reflections)temperature (only 2 warm reflections)

- Small optical derotator inside or outside - Small optical derotator inside or outside the cryostatthe cryostat

- The instrument doesn’t need to rotate- The instrument doesn’t need to rotate - The entrance window is small- The entrance window is small - Only two cryogenic functions (derotator - Only two cryogenic functions (derotator

and grating exchange mechanism)and grating exchange mechanism)


B.DelabreB.Delabre

ESO 2nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - KMOSESO 2nd GENERATION INSTRUMENTATION – OPTICAL DESIGNS - KMOS

THE OBJECT ACQUISITION THE OBJECT ACQUISITION

SYSTEMSYSTEM


B.DelabreB.Delabre


Field mirrors (1 x 1 arc min)Field mirrors (1 x 1 arc min)(36 mirrors )(36 mirrors )

Pupil mirrors Pupil mirrors (steering mirrors)(steering mirrors)

Telescope focal planeTelescope focal plane

TELESCOPETELESCOPE

TO TO DEROTATORDEROTATOR

Each field mirror images aEach field mirror images aPupil on its own steering mirrorPupil on its own steering mirror


B.DelabreB.Delabre


13:59:18

left field Scale: 0.15Positions: 1-4

06-Oct-03

166.67 MM

STEERING MIRRORSSTEERING MIRRORS

TELESCOPETELESCOPEFOCAL PLANEFOCAL PLANE

OPTICAL DEROTATOROPTICAL DEROTATOR

OBJECT SELECTIONOBJECT SELECTION

WARM PARTWARM PART

COLD PARTCOLD PART

Pseudo pupilPseudo pupil

to image slicersto image slicers

Field maskField mask


B.DelabreB.Delabre


Main advantages of this conceptMain advantages of this concept : :

- Steering mirrors are accessibleSteering mirrors are accessible- Field slicer can be exchanged to have flexibility for object selectionField slicer can be exchanged to have flexibility for object selection- Small entrance window for the cryostatSmall entrance window for the cryostat- The instrument does not rotate, requirement on flexure are much The instrument does not rotate, requirement on flexure are much

easier easier

to fulfill.to fulfill.- The spectrograph operates horizontal. Most of the lens mounting The spectrograph operates horizontal. Most of the lens mounting

problems disappear.problems disappear.- High reliability (only two cryogenic functions)High reliability (only two cryogenic functions)- Possibility to include a warm viewing system for object acquisition.Possibility to include a warm viewing system for object acquisition.


B.DelabreB.Delabre


THE IMAGE SLICERSTHE IMAGE SLICERS

This devices have been developed at the LAM in Marseille (France)This devices have been developed at the LAM in Marseille (France)

A presentation by Eric Prieto will be (or has been) given during this workshopA presentation by Eric Prieto will be (or has been) given during this workshop

All reflective slicers could also be used.All reflective slicers could also be used.


B.DelabreB.Delabre


13:59:18

left field Scale: 0.15Positions: 1-4

06-Oct-03

166.67 MM

14:43:26

Scale:0.16

Position: 1 23-Jul-03

156.25 MM

entrance

slits

pupil relay lens

folding

mirror

Collimator

Camera

Grating

(exchangeable)

Filter

wheel

Detector

KMOS-2 SPECTROGRAPH

Object selectionObject selectiondevicedevice

ImageImageslicersslicers



B.DelabreB.Delabre


THE SPECTROGRAPHTHE SPECTROGRAPH


B.DelabreB.Delabre


The following table summarizes the characteristics of the instrument:

Entrance F/N F/17 (spatial) F/34 (spectral)

Output F/N F/3.1 (spatial) F/6.2 (spectral)

Entrance field of view 2 slits of 400 mm separated by 200 mm

Detector 4K x 4K (18 µm pixel)

Pupil size (on the grating) 100 x 50 mm100 x 50 mm

Magnification 0.182

Scale (spatial) 0.150 arc sec / pixel

Scale (spectral) 0.075 arc sec / pixel

Entrance pupil position infinity

Slit curvature flat


B.DelabreB.Delabre


14:43:26


23-Jul-03

156.25 MM

entranceslits

pupil relay lens

folding

mirror

Collimator

Camera

Grating

(exchangeable)

Filterwheel

Detector

KMOS-2 SPECTROGRAPH


B.DelabreB.Delabre


Focal length: 1700 mm Pupil diameter: 100 mm Wavelength range: 1000 – 2500 nm Field of view: 200 x 400 mm

The CollimatorThe Collimator


B.DelabreB.Delabre


15:06:26


23-Jul-03

147.06 MM

KMOS-2 COLLIMATOR

Caf2Caf2 Baf2Baf2

IRG3IRG3

SilicaSilica


B.DelabreB.Delabre


J Band: 400 mm- 1 R=4070 (2 pixels) between 1060 and 1345 nmH Band: 300 mm- 1 R=4660 (2 pixels) between 1430 and 1800 nmK Band: 225 mm- 1 R=4340 (2 pixels) between 2000 and 2440 nm

List of gratingsList of gratings


B.DelabreB.Delabre


Focal length: 310 mm Pupil diameter: 100 mm Wavelength range: 1000 – 2500 nm Field of view: 74 x 74 mm

The CameraThe Camera


B.DelabreB.Delabre


09:53:04

Scale: 0.33 24-Jul-03

75.76 MM

KMOS-2 CAMERA

filterCaf2Caf2

Caf2Caf2

Irg3Irg3 SilicaSilica

SilicaSilica ZnSeZnSe

AsphericAspheric


B.DelabreB.Delabre


Image qualityImage quality : :

Image quality has been computed with a full circular pupil of Image quality has been computed with a full circular pupil of

100 x 100 mm. In fact the spectrograph has a nominal pupil 100 x 100 mm. In fact the spectrograph has a nominal pupil

of 100 x 50 mm.of 100 x 50 mm.

The full pupil of 100 x 100 mm allows to collect the light The full pupil of 100 x 100 mm allows to collect the light whichwhich

is diffracted by the slicers.is diffracted by the slicers.


B.DelabreB.Delabre


J Band

Wavelength 1060 nm 1130 nm 1200 nm 1275 nm 1345 nm

Positions -36.4 mm -27.4 mm -18.5 mm -9.0 mm -0.2 mm

Axis 35 35 26 24 15

100 mm 20 26 22 20 11

200 mm 19 28 26 25 19

80% geometrical energy diameter80% geometrical energy diameter


B.DelabreB.Delabre


H Band

Wavelength

1430 nm 1500 nm 1600 nm 1700 nm 1800 nm

Positions -35.9mm -29.0 mm -19.4 mm -9.9 mm -0.5 mm

Axis 23 32 26 21 19

100 mm 22 32 28 21 16

200 mm 23 26 23 12 8



B.DelabreB.Delabre


K Band

Wavelength

2000 nm 2100 nm 2200 nm 2320 nm 2440 nm

Positions -32.0 mm -24.6 mm -17.4 mm -8.9 mm -0.4 mm

Axis 13 17 20 23 28

100 mm 25 20 19 19 23

200 mm 22 27 14 12 12



B.DelabreB.Delabre


X - ShooterX - Shooter

Built by : Astron – Copenhagen Obs. – ESO - INAF - Obs Paris-Built by : Astron – Copenhagen Obs. – ESO - INAF - Obs Paris-Meudon Meudon PI’s : D. D’Odorico – F. Hammer - L. Kaper - R.Pallavicini – PI’s : D. D’Odorico – F. Hammer - L. Kaper - R.Pallavicini – P.K. RasmussenP.K. Rasmussen

Medium resolution Echelle spectrographMedium resolution Echelle spectrograph


B.DelabreB.Delabre

ESO 2ESO 2ndnd GENERATION INSTRUMENTATION – OPTICAL DESIGNS – X- GENERATION INSTRUMENTATION – OPTICAL DESIGNS – X-SHOOTERSHOOTER

Characteristics :Characteristics :

Instrument located at Cassegrain FocusInstrument located at Cassegrain Focus

Fore optics : light split in 3 channels by dichroic platesFore optics : light split in 3 channels by dichroic plates

3 optical relays F/13.6 to F/7.53 optical relays F/13.6 to F/7.5

2 of these relays include an ADC2 of these relays include an ADC

Spectrographs : 3 “UVES” type spectrographs – Echelle formatSpectrographs : 3 “UVES” type spectrographs – Echelle format

Blue 300 – 550 nmBlue 300 – 550 nm

Red 500 – 1000 nmRed 500 – 1000 nm

IR 1000 – 1800 nm (or 2500 ?)IR 1000 – 1800 nm (or 2500 ?)


B.DelabreB.Delabre


14:26:05

ESO 07-Nov-03

125.00 MM

14:29:26

Red channel 500 – 1000 nmRed channel 500 – 1000 nm

Blue channel 300 – 550 nmBlue channel 300 – 550 nm

TelescopeTelescopeFocusFocus

ADCADC

ADCADC

Red mirrorRed mirror

2nd dichroic2nd dichroic

11StSt dichroic dichroic

14:59:26

IR Channel 950-1800 nmIR Channel 950-1800 nm


B.DelabreB.Delabre


15:14:55

0.000,0.000 DG 0.00, 0.00

0.000,.0093 DG 0.00, 0.50

0.000,.0186 DG 0.00, 1.00

FIELDPOSITION

DEFOCUSING 0.00000

.147 MM

15:55:47

0.000,0.000 DG 0.00, 0.00

0.000,.0093 DG 0.00, 0.50

0.000,.0186 DG 0.00, 1.00

FIELDPOSITION

DEFOCUSING 0.00000

.147 MM

bb

15:13:33

0.000,0.000 DG 0.00, 0.00

0.000,.0093 DG 0.00, 0.50

0.000,.0186 DG 0.00, 1.00

FIELDPOSITION

DEFOCUSING 0.00000

.147 MM

PRESLIT OPTICS – SPOT DIAGRAMSPRESLIT OPTICS – SPOT DIAGRAMS

IR Channel 950-1800 nmIR Channel 950-1800 nm Red channel 500 – 1000 nmRed channel 500 – 1000 nm Blue channel 300 – 550 nmBlue channel 300 – 550 nm

AXISAXIS

5 ARCSEC5 ARCSEC

10 ARCSEC10 ARCSEC

Circle = 0.5 arcsecCircle = 0.5 arcsec


B.DelabreB.Delabre


Entrance F/N F/7.5

Output F/N F/2.7

Entrance field of view 11 arc sec (3.2 mm)

Detector 2K x 4K (15 µm pixel)

Pupil size 100 mm100 mm

Collimator focal length 750 mm

Camera focal length 270 mm

Scale (spatial) 0.14 arc sec/pixel

Resolving power 4500 (for 1 arc sec slit)

Order separation between 110 and 200 pixels

BLUE SpectrographBLUE Spectrograph


B.DelabreB.Delabre


16:06:40

Position: 7 05-Nov-03

200.00 MM

ParabolicParabolicmirrormirror

F/2.7 CameraF/2.7 Camera

60 deg silica60 deg silicaprismsprisms

180 mm-1 grating180 mm-1 gratingBlazed at 42 degBlazed at 42 deg

SlitSlit

2K x 4K2K x 4KCCDCCD

X-ShooterX-ShooterBlue spectrographBlue spectrograph

Folding mirrorFolding mirror


B.DelabreB.Delabre


ordersorders

1414

1616

19 19

2222

2424

551.5 551.5 nmnmX=-18.8 y=-8.1X=-18.8 y=-8.1

1111

541.3 nm541.3 nmX=-9.4 y=-9.3X=-9.4 y=-9.3

1414

531.1 nm531.1 nmX=-0.2 y=-9.4X=-0.2 y=-9.4

1515

522.2nm522.2nmX=7.7 y=-8.7X=7.7 y=-8.7

1212

513.4 513.4 nmnmX=15.2 y=-X=15.2 y=-7.37.3

99 480.2 nm480.2 nmX=-16.3 y=-5.4X=-16.3 y=-5.4

1616

472.5 nm472.5 nmX=-8.2 y=-6.1X=-8.2 y=-6.1

55

464.7 nm464.7 nmX=-0.1 y=-6.0X=-0.1 y=-6.0

55

457.9 nm457.9 nmX=6.7 y=-5.3X=6.7 y=-5.3

77

451.0 451.0 nmnmX=13.4 y=-X=13.4 y=-4.04.0

1313 402.2 nm 402.2 nm X=-13.5 y=0.0X=-13.5 y=0.0

1717

396.8 nm 396.8 nm X=-6.8 y=-02X=-6.8 y=-02

7 7

391.3 nm 391.3 nm X=-0.1 y=0.1X=-0.1 y=0.1

88

386.4 nm 386.4 nm X=5.7 y=0.8X=5.7 y=0.8

1010

381.5 381.5 nm nm X=11.4 X=11.4 y=2.0y=2.0

1212 346.0 nm346.0 nmX=-11.4 y=6.9X=-11.4 y=6.9

1414

342.0 nm342.0 nmX=-5.8 y=7.0X=-5.8 y=7.0

77

337.9 nm337.9 nmX=-0.0 y=7.5X=-0.0 y=7.5

1010

334.3 nm334.3 nmX=4.9 y=-8.3X=4.9 y=-8.3

1010

330.6 330.6 nmnmX=9.8 y=9.5X=9.8 y=9.5

99 316.5 nm316.5 nmX=-10.3 X=-10.3 y=12.51y=12.51

1414

313.2 nm313.2 nmX=-5.2 y=12.7X=-5.2 y=12.7

99

309.8 nm309.8 nmX=-0.1 y=13.4X=-0.1 y=13.4

1010

306.7 nm306.7 nmX=4.4 y=14.3X=4.4 y=14.3

1111

303.5 303.5 nmnmX=9.1 y=15.5X=9.1 y=15.5

88

80% geometrical energy (diameter)80% geometrical energy (diameter)

b.delabre november 2003angra dos reis - brazil eso 2 nd generation instrumentation – optical...

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