Science Workshop, Toulouse, March 18-19, 2009

MUSEMUSEEtat d’avancementEtat d’avancement

Atelier : « Les galaxies à z>3 dans la perspective de MUSE »

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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)

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CRALProject OfficeSlicerSpectrographIntegration

LATTElectronicsControl SoftwareForeOptics

NOVA (Leiden)AO interfaceASSIST (AOF)

ETHSpectrograph Procurment

AIPCalibration UnitData Reduction Software

AIGSplitting & Relay OpticsMain Structure

ESODetector SystemGALACSI

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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

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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

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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

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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

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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

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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 ?

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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?

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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

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Total ThrougputTotal Througput

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Throughput Throughput ComparisonComparison

- Expected MUSE WFM- Xshooter- FORS2- VIMOS-IFU- FLAMES-IFU

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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

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Spatial PSF in WFMSpatial PSF in WFM

MedianUpper quartileLower quartile

Cn² profile

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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

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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%

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Slicer prototypeSlicer prototype

Winlight ISS prototype, full slicer January 2008

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VPHG KOSI prototypeVPHG KOSI prototype

VPHG prototype delivered the 09/10/08

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Science grade EEV Science grade EEV CCDCCD

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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

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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

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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.