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MUSE Etat d’avancement. Atelier : « Les galaxies à z>3 dans la perspective de MUSE ». Organisation. AIP Calibration Unit Data Reduction Software. NOVA (Leiden) AO interface ASSIST (AOF). AIG Splitting & Relay Optics Main Structure. CRAL Project Office Slicer Spectrograph - PowerPoint PPT Presentation
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Science Workshop, Toulouse, March 18-19, 2009
MUSEMUSEEtat d’avancementEtat d’avancement
Atelier : « Les galaxies à z>3 dans la perspective de MUSE »
p.2
OrganisationOrganisationPrincipal
Investigator R. Bacon (Lyon)
Executive Board (coIs)T. Contini (Toulouse),
S. Dreizler (Göttingen), B. Guiderdoni (Lyon),
S. Lilly (Zurich),M. Steinmetz (Potsdam)
J. Schaye (NOVA)
Project ManagerP. Caillier
(Lyon)
Local PMLyon
A. Remillieux
Local PMGöttingenH. Nicklas
Local PMNOVA
R. Stuik
Local PMPotsdamM. Roth
Local PMESO
G. Rupprecht
InstrumentScientist
L. Wisotzki(Potsdam)
Science TeamJ. Blaizot (Lyon)
J. Brinchmann (NOVA)T. Contini (Toulouse)M. Carollo (Zurich)
S. Dreizler (Göttingen)E. Emsellem (Lyon) M. Franx (NOVA)
B. Guiderdoni (Lyon)W. Kollatschny (Göttingen)
S. Lilly (Zurich)R. Pello (Toulouse)M. Roth (Potsdam)J. Schaye (NOVA)
E. Slezak (Nice/Lyon)G. Soucail (Toulouse)
M. Steinmetz (Potsdam)P. Weilbacher (Potsdam)
L. Wisotzki (Potsdam)H. Wozniak (Lyon)
Science TeamAssociates
R. McDermid (NOVA)
Deputy IST. Contini (Toulouse)
Software PMA. Pécontal
(Lyon)
System Engineer M. Loupias
(Lyon)
Local PMToulouse
S. Brau-Nogué
ESO ResponsibleL. Pasquini
Project Assurance Manager
L. Capoani(Lyon)
p.3
CRALProject OfficeSlicerSpectrographIntegration
LATTElectronicsControl SoftwareForeOptics
NOVA (Leiden)AO interfaceASSIST (AOF)
ETHSpectrograph Procurment
AIPCalibration UnitData Reduction Software
AIGSplitting & Relay OpticsMain Structure
ESODetector SystemGALACSI
p.4
Get everything!– Eliminates pre-imaging– Eliminates pre-
selection– Observe only once– Attack multiple science
topics simultaneously– Large discovery space
for serendipitous sources
Spectroscopic Surveys - Spectroscopic Surveys - IFUIFU
UDF
UDF
UDF
p.5
Very Top Level Very Top Level RequirementsRequirements
IFU Large field of view (for an IFU) Large simultaneous spectral range Medium spectral resolution
– Emission line profiles– Avoid OH lines in the red
High spatial resolution High throughput Red sensitive Very stable, capable of very long integration Minimum number of modes (WFM/NFM) WFM is a priority wrt NFM
p.6
Instrument OverviewInstrument OverviewFocus Nasmyth B UT4
Deformable Secondary Mirror
1170 actuators
Laser guide stars 4 x 20-25 Watts
Instrument Integral Field Spectrograph
Number of IFU units 24
Detectors 4k x 4k Deep depletion CCD
Simultaneous Wavelength Range
480 – 930 nm (nominal)465 – 930 nm (extended)
Resolving Power 1750@465nm – 3750@930nm
Datacube Size 1570 MB
p.7
Wide Field ModeWide Field Mode
Field of View 1x1 arcmin2
Spatial Sampling 0.2x0.2 arcsec2
Spectra/Exposure 90,000
Sky Coverage in AO 70% @ galactice pole99% @ galactic equator
AO Energy gain wrt seeing
x2
p.8
Narrow Field ModeNarrow Field Mode
Field of View 7.5x7.5 arcsec2
Spatial Sampling 25x25 milliarcsec2
Spectra/Exposure 90,000
Spatial resolution 5-10% Strehl Ratio @ 650nm10%-20% Strehl Ratio @ 850nm
p.9
Top Level ChallengesTop Level Challenges
Cost/Performance– Is it feasible to build 24 high performance IFUs within the
budget ? Weight/Volume
– How to fit MUSE in the restricted Nasmyth volume and weight budget ?
MAIT/Schedule– Is it feasible to manufacture, integrate and test MUSE in
a reasonable time scale ? Data reduction & analysis
– Is it feasible to reduce the data ?– Will the end user be able to analyze it ?
Adaptive Optics Facility– Is it feasible to build and operate the AO facility in time
for MUSE and with the requested efficiency ?
p.10
2005 2006 2007
KOJan.
OPDRJuly
FDRMar.
Design Phase
PDRJuly
2008
PlanningPlanning
2009 2010 2011 2012
MAIT Phase
IFU MIASept.
PAEJuly (12
IFU)
PACJuly
S/S MIADec.
OFDRDec.
2001 2002 2003
ESOCall for Idea CDR
Pre-Phase A & Phase A
Council Approval
2004
KO phase A
Commissioning
24 IFUNov?
p.11
MUSE Facility PlanningMUSE Facility Planning
2011 2012 2013 2014
PAEJuly
PACJuly
MU
SE
with
out A
Oco
mm
issionin
g
2011 2012 2013 2014
PAEDec
PACSep
Com
missio
nin
gw
ith A
O
MUSE
GALACSI
ScienceStart
GA
LAC
SI
Com
missio
nin
g
p.12
p.13
p.14
Total ThrougputTotal Througput
p.15
Throughput Throughput ComparisonComparison
- Expected MUSE WFM- Xshooter- FORS2- VIMOS-IFU- FLAMES-IFU
p.16
Spatial PSF in WFMSpatial PSF in WFM
Dimm seeing: 1.1 arcsec 0.65 arcsec
465 nm930 nm
---- Non AO WFM AO median Cn² profile
p.17
Spatial PSF in WFMSpatial PSF in WFM
MedianUpper quartileLower quartile
Cn² profile
p.18
Deep field limiting Deep field limiting magnitudemagnitude
• 80x1 hour integration time• Spatially and spectrally unresolved source • S/N = 5 by spectral element (R=3000)• Valid outside OH lines
p.19
Noise RegimeNoise Regime
() Object Sky Dark Current Readout
4807.0% 74.4% 4.6% 14.0%
500 6.5% 77.0% 4.1% 12.4%
630 5.1% 84.6% 2.5% 7.8%
7005.0% 85.5% 2.4% 7.1%
8004.9% 85.8% 2.3% 7.0%
9307.5% 71.2% 5.3% 16.0%
p.20
Slicer prototypeSlicer prototype
Winlight ISS prototype, full slicer January 2008
p.21
VPHG KOSI prototypeVPHG KOSI prototype
VPHG prototype delivered the 09/10/08
p.22
Science grade EEV Science grade EEV CCDCCD
p.23
MAITMAITImage
DissectorArray
Spectro-graph
VPH Grating
CCD
Derotator
Field Splitter & Separator
Main Structure
Image Slicer
Focusing Mirrors Array
Spectrograph
Detector Vessel
Detector Head Alignment
Foreoptics
Field Splitter & Separator
Main Structure
Vaccuum & Cryogeny System
Relay Optics
Foreoptics Extension
IFU
MUSE standalone
Instrument Sofware
Control Electronics
Calibration Unit
Main Structure
AIP CU
LATT FO
IAG IMS
CRAL IFU
ESO
MUSEIntegration
Hall
Subsystem AIT
Industrial Contract
System AIT
Cryostats
Relay Optics
IAG SRO
LATT ICE
Instrument Main
StructureCabinets
Vacuum Cryogenic
System
FO Extension
Beam
Relay Optics
IFU
Global TestsPAE
CalibrationUnit
ForeOpticsField Splitter & Separator
x24Instrument Software
x24
p.24
MUSE Integration MUSE Integration HallHall
p.25
Data ReductionData Reduction
Data Volume– 10 to 190 Gb science raw data/night– 10 to 100 Gb calibration raw data/24
hours
Pipeline design– Propagate estimated noise variance – One one resampling step
p.26
ConclusionConclusionPerformance Type
Milestone IndicatorsWFM Lim I Flux 80hWFM Spatial ResolutionNFM Strehl Ratio @ 650 nm
MarginsThroughputWFM IQ
Dreamed Phase A2.7-4.2 10-19 erg.s-1.cm-2
0.3-0.5 arcsec5-10%
Designed
PDR2.6-4.2 10-19 erg.s-1.cm-2
0.33-0.52 arcsec4-9%
14-17%24-40%
FDR2.4-3.9 10-19 erg.s-1.cm-2
0.3-0.5 arcsec11%
17-4-8%41-24%
Build PAE
Real Comm.