European Southern Observatory European Southern Observatory © ESO 2005 Page 1 AO Department Leiden,...

Leiden, April 26th 2005Leiden, April 26th 2005

EuropeanSouthernObservatory


© ESO 2005© ESO 2005Page 1 AO DepartmentAO Department

MUSEMUSE

MMulti ulti UUnit nit SSpectroscopic pectroscopic EExplorerxplorer

AO assisted integral field spectrographAO assisted integral field spectrograph

Developed by a consortium led by:Developed by a consortium led by: CRAL-Lyon (R.Bacon, PI)CRAL-Lyon (R.Bacon, PI)

Contributions of:Contributions of:Durham, Leiden, LAOMP, ETH, AIP, ESODurham, Leiden, LAOMP, ETH, AIP, ESO

Schedule:Schedule:CDR: 2004CDR: 2004Kick off: Jan 2005Kick off: Jan 2005Commissioning: 2011Commissioning: 2011





Science objectiveScience objective

3D Ultra Deep Field: 10-19 erg s-1 cm-2 80x1 hours integration80x1 hours integration

Faint Ly a emitters; Progenitors of Milky Way ? Star Formation History at Z>4 Development of dark matter halos Link between Lya emitters and High Res. QSO absorption

Physiscs of high Z galaxies from resolved spectroscopy

Kinematics, population, cluster, outflows, merger... In (nearby) galaxies

Stars: massive spectroscopy of crowded regions, Origin of bipolar stellar outflows and shock waves

SERENDIPITY





MUSE RequirementsMUSE Requirements Spectrometer resolution R~3000Spectrometer resolution R~3000 Wavelength range: 0.465Wavelength range: 0.465μμm-0.93 m-0.93 μμmm 300 x 300 spatial resolution elements (spaxels)300 x 300 spatial resolution elements (spaxels) High efficiencyHigh efficiency

Shutter open timeShutter open time Throughput, > 0.24 Throughput, > 0.24

2 observing modes: Wide Field Mode and Narrow Field Mode2 observing modes: Wide Field Mode and Narrow Field Mode

Observing modeObserving mode WFM (GLAO)WFM (GLAO) NFM (LTAO)NFM (LTAO)

FoVFoV 1’x1’1’x1’ 7.5”x7.5”7.5”x7.5”

Spatial SamplingSpatial Sampling 0.2x0.2 arcsec^20.2x0.2 arcsec^2 25x25mas^225x25mas^2

Spatial resolutionSpatial resolution 0.3-0.4 arcsec.0.3-0.4 arcsec. 30-50 mas30-50 masAO “performance”AO “performance” 2 x EE increase @ 2 x EE increase @

750nm 750nm Strehl 0.05 (0.1) @ 650nmStrehl 0.05 (0.1) @ 650nm

Sky coverage:Sky coverage: 70% @ Gal. pole70% @ Gal. pole TT reference: Science objectTT reference: Science object

AO “on time”AO “on time” 70%-ile70%-ile --





MUSE Instrument conceptMUSE Instrument concept

MCAOfocal plane

Enlarger/Anamorphoser Field-splitter

Split focal plane

Image slicer

Spectrometerpseudo-

entrance slit

CollimatorCamera

CCDplane

Dispersing element

Spectrometer

Sub-FoV

24 Spectrometers IFUs

4k x 4k Detectors

402.653.184 pixel





MUSE FacilityMUSE Facility

©© I. Lewis, I. Lewis, OxfordOxford

VLT-Nasmyth VLT-Nasmyth platform size: platform size: 5mx4m5mx4m

Max load: Max load: 8.000Kg8.000Kg





GALACSIGALACSI

Ground Atmospheric Layer Adaptive

Corrector for Spectroscopic Imaging

Ground Atmospheric Layer Adaptive

Corrector for Spectroscopic Imaging Located Nasmyth focus of UT4Located Nasmyth focus of UT4 Developed and build by ESO AO dept.Developed and build by ESO AO dept. 4 Na-LGS, 1’(WFM) and 15”(NFM) off axis4 Na-LGS, 1’(WFM) and 15”(NFM) off axis 1 NGS1 NGStartar within 45”<r<120” (WFM) > 17.5mag (R) within 45”<r<120” (WFM) > 17.5mag (R) 1 NGS1 NGSsourcesource (extended) on axis >15mag (goal 16mag J-K (extended) on axis >15mag (goal 16mag J-K

band)band) Baseline: VLT-Deformable M2 is the DMBaseline: VLT-Deformable M2 is the DM Test bed (incl. M2 ?) developed and build by LeidenTest bed (incl. M2 ?) developed and build by Leiden





GLACSI RequirementsGLACSI Requirements

Transmission: 92% average, 80% minimum (WFM)Transmission: 92% average, 80% minimum (WFM) AO operations in 70%-ile of the atmospheric conditions at 30AO operations in 70%-ile of the atmospheric conditions at 30° off zenith° off zenith

0.6” to 1.1” seeing @ 500nm0.6” to 1.1” seeing @ 500nm

Light pollution of science field:Light pollution of science field: @ 589nm @ 589nm ±20nm (goal 10nm) < brightest sky line, e.g. <±20nm (goal 10nm) < brightest sky line, e.g. <600 photons/s/sq”600 photons/s/sq” Outside the Na notch<10ph/Angstrom/hour/sq arc sec.Outside the Na notch<10ph/Angstrom/hour/sq arc sec.

“ “No” NGS within the Science field, scattered light!No” NGS within the Science field, scattered light!

Sky coverage > 70% at the galactic poleSky coverage > 70% at the galactic pole Long integration time (80x1h)Long integration time (80x1h)

High temporal instrument stabilityHigh temporal instrument stability

AO residual Image motion <50mas within 1h (WFM) TBCAO residual Image motion <50mas within 1h (WFM) TBC AO residual Image motion <10mas within 1h (NFM) TBC AO residual Image motion <10mas within 1h (NFM) TBC AO Setup time < 5 minAO Setup time < 5 min





GALACSI Optical layout (WFM)GALACSI Optical layout (WFM)

Reimaging lens F/4.0

Field separator

Nasm

yth

Adap

tor

flang

e

4’ Field selector

VisibleTT

Sensor

1’ Optics free Scientific Field

CALIBRATIONMIRROR

LGS WFS

LGS WFS

LGS Focus compensation

LGS pick upLGS pick upExchangeable unit for NFMExchangeable unit for NFM

500 mm BFD500 mm BFD

180mm defocused Laser beam

1.45 arc min

Hole

FIELD SEPARATORTransmits 589nmReflects visible light

4 a

rc m

in





Functional requirementsFunctional requirements

Matching between SH WFS and DSMMatching between SH WFS and DSM co rotate to the pupilco rotate to the pupil

LGS mounted to the telescopeLGS mounted to the telescope Field rotation with the speed of the pupil rotation Field rotation with the speed of the pupil rotation

GALACSI needs to co-rotate to the pupil GALACSI needs to co-rotate to the pupil At Nasmyth the pupil rotation is equal to the altitude motion of At Nasmyth the pupil rotation is equal to the altitude motion of

the telescopethe telescope operational range: 0operational range: 0°° to 60 to 60° Zenith distance° Zenith distance Most probable case: 5Most probable case: 5° to 45°, e.g. ± 20° instrument motion P-V° to 45°, e.g. ± 20° instrument motion P-V Low rate, < 15Low rate, < 15°/hour°/hour Helps to achieve the image stability requirementHelps to achieve the image stability requirement

NGS rotates with the fieldNGS rotates with the field Field selector (rotating with the pupil) needs to follow the field Field selector (rotating with the pupil) needs to follow the field

rotation - pupil rotation (WFM)rotation - pupil rotation (WFM)





GALACSI-MUSE InstrumentGALACSI-MUSE Instrument

MUSE Spectrographs

GA

LA

CS

IG

LA

O/S

CA

O

Fie

ld s

plit

ter

De

-ro

tato

r…

Nasmith platform

VL

Y-N

asm

yth

ro

tato

r

GALACSI is mounted to the Nasmyth rotator

Muse is on the Nasmyth Platform

Field de-rotation for Muse

Problem: Rotator wobble Platform wobble Flexure of GALACSI Temperature effects Residual alignment

errors, Field de rotator

wobble …

Causes differential image motion between the GALACSI and MUSE Instrument

metrology is required





MUSE focal plane

CCD camera focal plane

CCDfieldCCDfield MetrologyMetrology

Reimaging lens F/4.0

Nasm

yth

Adap

tor

flan

ge

4’ Field selector

VisibleTT

Sensor

LGS WFS

LGS WFS

LGS Focus compensation

Point source mounted at MUSE focal plane imaged to a CCD camera inside GALACSIde-rotator moves spot on the CCD

4 sources on MUSEAveraging of 4 centroids gives the “rotation free” position of the field center

Lateral motion of Muse, the de-rotator or GALACSY can be measured and corrected by offsetting the NGS Field selector.

MUSEfield

De-rotator field

4 Point sources





Opto-mechanical implementationOpto-mechanical implementation





Beam from the telescope

Field Splitter

Field Selector Assembly (turntable + goniometer stage)4 LGS pick up

Mirrors for WFM/NFM

VIS T/T sensor240x240 L3 CCD

4 LGS WFSs32x32 subap.240x240 L3 CCD

IR T/T sensorMetrology pick up mirror

Metrology CCD camera

Calibration/acquisition mirror

Acquisition CDD camera

AO Calibration sources





Field Selector TrackingField Selector Tracking

Visible Tip Tilt Sensor Field of View

4 a

rc m

in

Hole1.45 arc min

Field selector field: Diameter 4 arc min with 1.45 arc min holeField selector field: Diameter 4 arc min with 1.45 arc min hole NGS moves on a circular traceNGS moves on a circular trace

Speed: Field rotation + Pupil rotationSpeed: Field rotation + Pupil rotation Worst case: Meridian crossing close to zenith Worst case: Meridian crossing close to zenith

(180(180° rotation within 2 minutes ° rotation within 2 minutes 2mm/s 2mm/s))

Tracking accuracy >> Image stabilityTracking accuracy >> Image stability ~15~15μμm position accuracy during the motion in the entire fieldm position accuracy during the motion in the entire field

Offset requests from the MetrologyOffset requests from the Metrology





4.5

5

5.5

6

6.5

x 106

-100 -80 -60 -40 -20 0 20 40 60 80 100-100

-80

-60

-40

-20

0

20

40

60

80

100

field position ["]

fie

ld p

os

itio

n [

"]

LGS, pointing:60", z=15

LGS light pollutionLGS light pollution

Science fieldScience field Small if the LGSs are launched at the side of the telescopeSmall if the LGSs are launched at the side of the telescope Severe if launched from M2:Severe if launched from M2:

Background: ~ 10e7 photons/s/sqarcsec.Background: ~ 10e7 photons/s/sqarcsec. Permitted background in the science field after a Notch filter Permitted background in the science field after a Notch filter

600 Photons/s/sqarcsec.600 Photons/s/sqarcsec.Notch filter with attenuation ~ 5e5 required Notch filter with attenuation ~ 5e5 required

0

1

2

3

4

5

6

7

-400 -300 -200 -100 0 100 200 300 400

-400

-300

-200

-100

0

100

200

300

400

field position ["]

field

pos

ition

["]

1 LGS 330" off axis,

0

1

2

3

4

5

6

7

320 325 330 335 340 345 350

-20

-15

-10

-5

0

5

10

15

20

field position ["]

field

pos

ition

["]

1 LGS 330" off axis,

5.5

6

6.5

7

7.5

x 106

-100 -80 -60 -40 -20 0 20 40 60 80 100-100

-80

-60

-40

-20

0

20

40

60

80

100

field position ["]

fie

ld p

os

itio

n [

"]


5

6

7

8

9

10

x 106

-100 -80 -60 -40 -20 0 20 40 60 80 100-100

-80

-60

-40

-20

0

20

40

60

80

100

field position ["]

fie

ld p

os

itio

n [

"]


5

5.5

6

6.5

7

7.5

8

8.5

x 106

-100 -80 -60 -40 -20 0 20 40 60 80 100-100

-80

-60

-40

-20

0

20

40

60

80

100

field position ["]

fie

ld p

os

itio

n [

"]


5

5.5

6

6.5

7

7.5

x 106

-100 -80 -60 -40 -20 0 20 40 60 80 100-100

-80

-60

-40

-20

0

20

40

60

80

100

field position ["]

fie

ld p

os

itio

n [

"]






Fratricide effect

-80 -60 -40 -20 0 20 40 60 80

-80

-60

-40

-20

0

20

40

60

80

field position ["]

field

pos

ition

["]

View of 1 subap. "Big WFS"

WFS #1

WFS #4

WFS #3

WFS #2

Simulated for large fieldWFS cut a fraction of the field4 LGSLaunch beh. M2Pointing 60“ off axisSub aperture position (0, -1) [m]

WFS Not present if the LGSs are

launched at the side of the telescope but Spot elongation!

Severe if launched from M2: Some sub apertures “look

trough” the launch beam of one of the lasers and are completely blinded

How many and in which conditions as well as the Impact to WF reconstruction is to be analyzed





RTCRTC

MUSE RTC MUSE RTC architecture based architecture based on ESO RTC on ESO RTC platform (SPARTA)platform (SPARTA)

FPGA for slope FPGA for slope calculation (pipeline)calculation (pipeline)

G4 processor G4 processor boards for the boards for the reconstruction on reconstruction on VME busVME bus

Fro nt-EndAc q uisitio n

C PU

C PU

C PU C PU

C C D C o ntro lle r

192x192 a c tive a re a

C PU

C PU

C PU C PU



C PU

C PU

C PU C PU



C PU

C PU

C PU C PU


256x256 d e te c to r


CPU

CPU

CPU

CPU

CPU

CPU

CPU

CPU

Tip /Tilt Se nso r De fo rm a b le M irro r

100/1000 Ethe rne tLC U




VM E64x

CPU

CPU

CPU

CPU

CPU

CPU

CPU

CPU

Rec

ons

truc

tion

CPU

CPU

CPU

CPU

Co

ntro

l

Sta tistic s





GALACSI ScheduleGALACSI Schedule

CDR: Mar.2004CDR: Mar.2004Trade off review: Oct. 2005Trade off review: Oct. 2005

Interface definitionInterface definitionLGS launch positionLGS launch positionDSM feasibility / approvalDSM feasibility / approval

PDR: July 06PDR: July 06FDR: July 07FDR: July 07 Integration and testing stand alone/ Integration and testing stand alone/

with DSMwith DSMGALACSI PAE: March 2010GALACSI PAE: March 2010GALACSI Commissioning: Oct. 2010GALACSI Commissioning: Oct. 2010

European Southern Observatory European Southern Observatory © ESO 2005 Page 1 AO Department Leiden,...

Documents

Transcript of European Southern Observatory European Southern Observatory © ESO 2005 Page 1 AO Department Leiden,...