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KMOS Instrument Science Team Review Instrument overview

KMOS Instrument Science Team Review Instrument overview. Consortium Members. Universitäts-Sternwarte München MPI für Extraterrestrische Physik UK Astronomy Technology Centre University of Durham University of Oxford University of Bristol European Southern Observatory.

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KMOS Instrument Science Team Review Instrument overview

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  1. KMOS Instrument Science Team ReviewInstrument overview

  2. Consortium Members • Universitäts-Sternwarte München • MPI für Extraterrestrische Physik • UK Astronomy Technology Centre • University of Durham • University of Oxford • University of Bristol • European Southern Observatory KMOS IST meeting, ESO, 10tth May 2006

  3. Announcement of Opportunity Feb 2002 • 1.0-2.4 mm Cryogenic Multi-Object Spectrometer • “Key requirement is to optimize the scientific potential of the instrument, particularly for the study of the intermediate and high-z slices of our Universe. This should drive its field of view and multiplex capability.” KMOS IST meeting, ESO, 10tth May 2006

  4. Top Level Scientific Drivers • Investigate the physical processes which drive galaxy formation and evolution over redshift range 1<z<10. • Map the variations in star formation histories, spatially resolved star-formation properties, and merger rates • Obtain dynamical masses of well-defined samples of galaxies across a wide range of environments at a series of progressively earlier epochs KMOS IST meeting, ESO, 10tth May 2006

  5. Top Level Requirements • Spatially-resolved (3-D) spectroscopy • Multiplexed spectroscopic observations • Observations across the J, H, and K infrared atmospheric windows • Versatile capability to address new scientific problems KMOS IST meeting, ESO, 10tth May 2006

  6. Multiplex advantage KMOS IST meeting, ESO, 10tth May 2006

  7. Science Requirements KMOS IST meeting, ESO, 10tth May 2006

  8. Functional Requirements KMOS IST meeting, ESO, 10tth May 2006

  9. Design Principles • Develop baseline design to deliver optimal set of science requirements • Exploit proven technologies and the consortium knowledge base • Prototype key technologies and subsystems where appropriate • Investigate backup solutions to minimise risk and explore possible trade-off options • Strong systems engineering approach throughout KMOS IST meeting, ESO, 10tth May 2006

  10. Systems Architecture KMOS IST meeting, ESO, 10tth May 2006

  11. Systems Architecture KMOS IST meeting, ESO, 10tth May 2006

  12. KMOS IST meeting, ESO, 10tth May 2006

  13. KMOS IST meeting, ESO, 10tth May 2006

  14. End-to-end Optical Model KMOS IST meeting, ESO, 10tth May 2006

  15. Pickoff Module

  16. Pickoff Subsystem • Fused silica singlet and powered entrance window to produce a flat, telecentric 7`.2 diameter Nasmyth focal plane • 24 constant path-length mechanical pickoff arms driven by cryogenic stepper-motors patrolling in 2 planes to minimizes contention during object acquisition; integral cold stop to minimize thermal background • Calibration unit to provide the ability to verify and calibrate the end-to-end performance of the instrument • Cryogenic mechanisms have demonstrated high reliability and have been the subject of extensive technology tests KMOS IST meeting, ESO, 10tth May 2006

  17. KMOS IST meeting, ESO, 10tth May 2006

  18. KMOS IST meeting, ESO, 10tth May 2006

  19. Technology PrototypingI: Prototype Pickoff Arm KMOS IST meeting, ESO, 10tth May 2006

  20. KMOS IST meeting, ESO, 10tth May 2006

  21. KMOS IST meeting, ESO, 10tth May 2006

  22. KMOS IST meeting, ESO, 10tth May 2006

  23. KMOS IST meeting, ESO, 10tth May 2006

  24. Integral Field Units

  25. IFU Subsystem • 8 pickoff subfields combined to produce single output slit; each subfield re-imaged on to 14x14 element image slicer • Diamond-machined monolithic optics (Al) to eliminate thermal effects and minimize alignment errors • All reflective, gold-coated, achromatic design • Anamorphic magnification produces regular spatial sampling on sky (0.2 arcsec) with Nyquist sampling of spectra • Each of 3 IFU systems is identical KMOS IST meeting, ESO, 10tth May 2006

  26. KMOS IST meeting, ESO, 10tth May 2006

  27. Integral field unit Slicing mirror Pupil mirror 3 identical sets of 8 IFUS 4 foreoptics designs (aspheric) 24 identical image slicer assemblies Slit mirror KMOS IST meeting, ESO, 10tth May 2006

  28. Pupil mirror assembly KMOS IST meeting, ESO, 10tth May 2006

  29. Spectrographs

  30. Spectrograph Subsystem • Modular spectrograph subsystems (3) • Toroidal reflective collimator and 6-element transmissive achromatic camera • 6-position grating turret; optimized J,H,K gratings bands • Additional IZ grating included at PDR; two further ‘double band’ gratings to be considered during FDR • Single mechanism - stepper motor drive with index limit switch KMOS IST meeting, ESO, 10tth May 2006

  31. KMOS IST meeting, ESO, 10tth May 2006

  32. KMOS IST meeting, ESO, 10tth May 2006

  33. KMOS IST meeting, ESO, 10tth May 2006

  34. KMOS IST meeting, ESO, 10tth May 2006

  35. Calibration system

  36. Calibration lamps (Th)-Ar Tungsten (2) KMOS IST meeting, ESO, 10tth May 2006

  37. Calibration system KMOS IST meeting, ESO, 10tth May 2006

  38. Calibration system 0=0.96 0=0.98 Upper port Lower port KMOS IST meeting, ESO, 10tth May 2006

  39. Detector and mount

  40. Detector moduleHawaii RG2 arrays from Rockwell (2048x2048 pixels), results from Gert Finger KMOS IST meeting, ESO, 10tth May 2006

  41. KMOS IST meeting, ESO, 10tth May 2006

  42. KMOS IST meeting, ESO, 10tth May 2006

  43. Detector mount: ESO standard KMOS IST meeting, ESO, 10tth May 2006

  44. Detector mount KMOS IST meeting, ESO, 10tth May 2006

  45. More on the detector mounting NB focus mechanism for lab testing only. KMOS IST meeting, ESO, 10tth May 2006

  46. Status and Schedule • KMOS ESO STC approval Nov 2003 • Phase B start July 2004 • Preliminary Design Review May 2006 • Arms PDR, June 2006 • Final Design Review March 2007 • Optics and cryostat FDR, Q4 2006 • Prelim Acceptance Europe March 2010 KMOS IST meeting, ESO, 10tth May 2006

  47. Summary • KMOS will be the first cryogenic multiple-integral field spectrometer on an 8-m class telescope • It will be a challenging instrument to build but with lots of exciting scientific potential • At PDR we believe we have a robust design which meets all the top-level science requirements KMOS IST meeting, ESO, 10tth May 2006

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