1. KMOS Instrument Science Team Review Instrument overview

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

3. KMOS IST meeting, ESO, 10 tth May 2006 Announcement of Opportunity Feb 2002 1.0-2.4  m Cryogenic Multi-Object Spectrometer 1.0-2.4  m 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.” “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.”

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

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

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

7. KMOS IST meeting, ESO, 10 tth May 2006 Science Requirements RequirementEssential Requirements PDR Status Throughput ( REQ 3.5.1) J>20%, H>30%, K>30%J>30%, H>35%, K>35% Wavelength coverage (REQ 3.5.5) 1.05 to 2.5 μm 0.8 to 2.5  m Spectral Resolution (REQ 3.5.19) R>3200,3800,3000 (J,H,K)R=3500,3900,3700 Number of IFUs (REQ 3.5.14) 24 Extent of each IFU (REQ 3.5.10) 2.8 x 2.8 sq. arc seconds Spatial Sampling (REQ 3.5.11) 0.2 arc seconds Patrol field (REQ 3.5.9) 5’x 5’ field7.2 arcmin diameter field Close packing of IFUs (REQ 3.5.15) ≥3 within 1 sq arcmin Closest approach of IFUs (REQ 3.5.16) 2 target fields separated by 6 arcsec 2 target fields separated by 6 arcsec, plus the ability to assemble 24 IFUs into mapping configuration

8. KMOS IST meeting, ESO, 10 tth May 2006 Functional Requirements Requirement Baseline Design Flat-field accuracy <1% of night sky Instrumental Profile <5% deviation in the FWHM of line profiles at constant wavelength Array stability <1% of the night sky Cosmetic quality <3% of pixels are unstable Observing efficiency 70% Acquisition ±0.5 sampling element

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

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

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

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

14. End-to-end Optical Model

15. Pickoff Module

16. KMOS IST meeting, ESO, 10 tth May 2006 Pickoff Subsystem Fused silica singlet and powered entrance window to produce a flat, telecentric 7`.2 diameter Nasmyth focal plane 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 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 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 Cryogenic mechanisms have demonstrated high reliability and have been the subject of extensive technology tests

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

19. Technology Prototyping I: Prototype Pickoff Arm

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

24. Integral Field Units

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

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

27. Integral field unit Slicing mirror Pupil mirror Slit mirror 3 identical sets of 8 IFUS 4 foreoptics designs (aspheric) 24 identical image slicer assemblies

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

29. Spectrographs

30. KMOS IST meeting, ESO, 10 tth May 2006 Spectrograph Subsystem Modular spectrograph subsystems (3) Modular spectrograph subsystems (3) Toroidal reflective collimator and 6-element transmissive achromatic camera Toroidal reflective collimator and 6-element transmissive achromatic camera 6-position grating turret; optimized J,H,K gratings bands 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 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 Single mechanism - stepper motor drive with index limit switch

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

35. Calibration system

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

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

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

39. Detector and mount

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

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

43. Detector mount: ESO standard

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

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

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

47. KMOS IST meeting, ESO, 10 tth May 2006 SummarySummary KMOS will be the first cryogenic multiple- integral field spectrometer on an 8-m class telescope 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 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 At PDR we believe we have a robust design which meets all the top-level science requirements