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Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 1Page 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
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 2Page 2 AO DepartmentAO Department
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
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 3Page 3 AO DepartmentAO Department
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 --
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 4Page 4 AO DepartmentAO Department
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
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 5Page 5 AO DepartmentAO Department
MUSE FacilityMUSE Facility
©© I. Lewis, I. Lewis, OxfordOxford
VLT-Nasmyth VLT-Nasmyth platform size: platform size: 5mx4m5mx4m
Max load: Max load: 8.000Kg8.000Kg
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 6Page 6 AO DepartmentAO Department
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
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 7Page 7 AO DepartmentAO Department
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
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 8Page 8 AO DepartmentAO Department
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
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 9Page 9 AO DepartmentAO Department
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)
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 10Page 10 AO DepartmentAO Department
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
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 11Page 11 AO DepartmentAO Department
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
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 12Page 12 AO DepartmentAO Department
Opto-mechanical implementationOpto-mechanical implementation
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 13Page 13 AO DepartmentAO Department
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
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 14Page 14 AO DepartmentAO Department
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 15Page 15 AO DepartmentAO Department
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
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 16Page 16 AO DepartmentAO Department
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 [
"]
LGS, pointing:60", z=0
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 [
"]
LGS, pointing:60", z=60
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 [
"]
LGS, pointing:60", z=45
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 [
"]
LGS, pointing:60", z=30
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 17Page 17 AO DepartmentAO Department
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
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 18Page 18 AO DepartmentAO Department
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 C D C o ntro lle r
192x192 a c tive a re a
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 C D C o ntro lle r
256x256 d e te c to r
192x192 a c tive a re a
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
256x256 d e te c to r
256x256 d e te c to r
256x256 d e te c to r
VM E64x
CPU
CPU
CPU
CPU
CPU
CPU
CPU
CPU
Rec
ons
truc
tion
CPU
CPU
CPU
CPU
Co
ntro
l
Sta tistic s
Leiden, April 26th 2005Leiden, April 26th 2005
EuropeanSouthernObservatory
EuropeanSouthernObservatory
© ESO 2005© ESO 2005Page 19Page 19 AO DepartmentAO Department
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