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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

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muse etat d avancement

MUSEEtat d’avancement

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

Science Workshop, Toulouse, March 18-19, 2009

slide3

AIP

Calibration Unit

Data Reduction Software

NOVA (Leiden)

AO interface

ASSIST (AOF)

AIG

Splitting & Relay Optics

Main Structure

CRAL

Project Office

Slicer

Spectrograph

Integration

ESO

Detector System

GALACSI

LATT

Electronics

Control Software

ForeOptics

ETH

Spectrograph Procurment

spectroscopic surveys ifu
Get everything!

Eliminates pre-imaging

Eliminates pre-selection

Observe only once

Attack multiple science topics simultaneously

Large discovery space for serendipitous sources

UDF

UDF

UDF

Spectroscopic Surveys - IFU
very top level requirements
Very Top LevelRequirements
  • 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 prioritywrt NFM
top level challenges
Top 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 ?
slide10

Planning

Pre-Phase A & Phase A

2001

2002

2003

2004

ESO

Call for Idea

KO phase A

Council Approval

CDR

Design Phase

2005

2006

2007

2008

OPDR

July

KO

Jan.

PDR

July

OFDR

Dec.

MAIT Phase

Commissioning

2009

2010

2011

2012

IFU MIA

Sept.

S/S MIA

Dec.

PAC

July

FDR

Mar.

24 IFU

Nov?

PAE

July (12 IFU)

slide11

MUSE Facility Planning

2011

2012

2013

2014

MUSE

PAE

July

PAC

July

MUSE

without AO

commissioning

Science

Start

Commissioning

with AO

2011

2012

2013

2014

GALACSI

PAE

Dec

PAC

Sep

GALACSI

Commissioning

throughput comparison
ThroughputComparison

- Expected MUSE WFM

- Xshooter

- FORS2

- VIMOS-IFU

- FLAMES-IFU

spatial psf in wfm
Spatial PSF in WFM

---- Non AO

WFM AO median Cn² profile

465 nm

930 nm

Dimm seeing: 1.1 arcsec 0.65 arcsec

spatial psf in wfm1
Spatial PSF in WFM

Cn² profile

Median

Upper quartile

Lower quartile

deep field limiting magnitude
Deepfieldlimiting magnitude
  • 80x1 hour integration time
  • Spatially and spectrally unresolved source
  • S/N = 5 by spectral element (R=3000)
  • Valid outside OH lines
slicer prototype
Slicer prototype

Winlight ISS prototype, full slicer January 2008

vphg kosi prototype
VPHG KOSI prototype
  • VPHG prototype delivered the 09/10/08
slide23
MAIT

x24

data reduction
Data 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