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MUSE Etat d’avancement

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

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  1. MUSEEtat d’avancement Atelier : « Les galaxies à z>3 dans la perspective de MUSE » Science Workshop, Toulouse, March 18-19, 2009

  2. Organisation

  3. 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

  4. 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

  5. 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

  6. Instrument Overview

  7. Wide Field Mode

  8. Narrow Field Mode

  9. 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 ?

  10. 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)

  11. 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

  12. Total Througput

  13. ThroughputComparison - Expected MUSE WFM - Xshooter - FORS2 - VIMOS-IFU - FLAMES-IFU

  14. Spatial PSF in WFM ---- Non AO WFM AO median Cn² profile 465 nm 930 nm Dimm seeing: 1.1 arcsec 0.65 arcsec

  15. Spatial PSF in WFM Cn² profile Median Upper quartile Lower quartile

  16. Deepfieldlimiting magnitude • 80x1 hour integration time • Spatially and spectrally unresolved source • S/N = 5 by spectral element (R=3000) • Valid outside OH lines

  17. Noise Regime

  18. Slicer prototype Winlight ISS prototype, full slicer January 2008

  19. VPHG KOSI prototype • VPHG prototype delivered the 09/10/08

  20. Science grade EEV CCD

  21. MAIT x24

  22. MUSE Integration Hall

  23. 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

  24. Conclusion

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