1. KMOS operations and performance Presentation to the KMOS ESO IST, 10 th May 2006

2. KMOS IST meeting, ESO, 10 tth May 2006 KMOS operations Observation preparation Observation preparation Configuring the arms Configuring the arms Sky subtraction options Sky subtraction options During the observations During the observations Source acquisition Source acquisition Observation of calibration stars Observation of calibration stars After the observations After the observations Daytime calibration Daytime calibration Post processing steps Post processing steps

3. KMOS IST meeting, ESO, 10 tth May 2006 Setting the requirements Performance requirements are specified Performance requirements are specified Essential Essential the design must be meet these requirements and is verified against them the design must be meet these requirements and is verified against them Optimal Optimal Achieving these represents a significant scientific gain and our goal is for the design to meet these Achieving these represents a significant scientific gain and our goal is for the design to meet these Desirable Desirable to be met if can be met with minimal impact on the design/cost/schedule to be met if can be met with minimal impact on the design/cost/schedule Not all requirements have multiple levels Not all requirements have multiple levels

4. KMOS IST meeting, ESO, 10 tth May 2006 General operations principles Building on experience with NIR IFU instruments within the consortium Building on experience with NIR IFU instruments within the consortium SINFONI, GNIRS, UIST SINFONI, GNIRS, UIST Building on ESO experience with the aim of producing an operational model compliant with ESO standards and practice Building on ESO experience with the aim of producing an operational model compliant with ESO standards and practice

5. Preparation of the observations Performance information Configuration of the arms Sky subtraction mode

6. KMOS IST meeting, ESO, 10 tth May 2006 Req 3.5.1: Throughput Req 3.5.1: Throughput

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

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

10. Req 3.5.2: Instrument thermal background Design follows best practice of light tight croystat, use of baffling. Design follows best practice of light tight croystat, use of baffling.

11. KMOS IST meeting, ESO, 10 tth May 2006 Sensitivity model

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

13. KMOS IST meeting, ESO, 10 tth May 2006 Arm configuration 24 arms ( req 3.5.12 ) are configured within 7.2’ field (req 3.5.9) using KARMA 24 arms ( req 3.5.12 ) are configured within 7.2’ field (req 3.5.9) using KARMA Fields of view Fields of view 2.8arcsec x 2.8arcsec IFU fields (Req 3.5.10) 2.8arcsec x 2.8arcsec IFU fields (Req 3.5.10) 0.2arcsec in both spatial directions (Req 3.5.9) 0.2arcsec in both spatial directions (Req 3.5.9) Anamorphic magnification in the IFUs Anamorphic magnification in the IFUs

14. KMOS IST meeting, ESO, 10 tth May 2006 Arm configuration Arms are configured using KARMA Arms are configured using KARMA Automatic configuration based on rules and optional manual configuration Automatic configuration based on rules and optional manual configuration Input catalogue: Input catalogue: source positions with priority source positions with priority Band 1 – highest priority, must be observed Band 1 – highest priority, must be observed Band 2 – reduced priority, should be selected over a Band 3 object Band 2 – reduced priority, should be selected over a Band 3 object Band 3 – lowest priority, could be deselected with little loss to the programme. Band 3 – lowest priority, could be deselected with little loss to the programme.

15. KMOS IST meeting, ESO, 10 tth May 2006 Arm configuration Input catalogue: Input catalogue: Positions of objects with priority Positions of objects with priority Positions of reference stars for acquisition Positions of reference stars for acquisition Position of guide star Position of guide star Optional positions for sky with priority Optional positions for sky with priority Optional positions of bright stars to avoid Optional positions of bright stars to avoid Input image: Input image: Required Required Not used to derive object positions Not used to derive object positions Used to identify sky positions Used to identify sky positions

16. KMOS IST meeting, ESO, 10 tth May 2006 Arm configuration Set of rules Set of rules No collisions between arms No collisions between arms Never violated Never violated Closest approach includes margin for atmospheric refraction Closest approach includes margin for atmospheric refraction No vignetting No vignetting May be violated, flag set in the file header May be violated, flag set in the file header Will avoid bright objects (K<12) hitting an arm Will avoid bright objects (K<12) hitting an arm May be overridden in ‘manual’ mode May be overridden in ‘manual’ mode

17. KMOS IST meeting, ESO, 10 tth May 2006 Requirements on arm positioning Req 3.5.15: Close packing of target fields Req 3.5.15: Close packing of target fields ≥ 10 fields within 1arcminute ≥ 10 fields within 1arcminute Req 3.5.16: Simultaneous observations of close packed fields Req 3.5.16: Simultaneous observations of close packed fields ≥ 3 fields within more than one 1arcminute field ≥ 3 fields within more than one 1arcminute field ≥ 10 fields within more than one 1arcminute field, within a restricted patrol field ≥ 10 fields within more than one 1arcminute field, within a restricted patrol field

18. KMOS IST meeting, ESO, 10 tth May 2006 Access to clusters

19. KMOS IST meeting, ESO, 10 tth May 2006 Requirements on arm positioning Req 3.5.17: Closest approach of target fields Req 3.5.17: Closest approach of target fields 12 pairs of two target fields within 6arcsec edge-to-edge 12 pairs of two target fields within 6arcsec edge-to-edge Best seen in the mapping mode Best seen in the mapping mode

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

22. Fixed arm configurations For observations of the calibration source For observations of the calibration source For observations of calibration stars For observations of calibration stars For mapping mode For mapping mode

23. KMOS IST meeting, ESO, 10 tth May 2006 Mapping mode (req 3.5.16) Arms set to a regular grid on the sky Arms set to a regular grid on the sky Single configuration, fixed by arm mech. design Single configuration, fixed by arm mech. design Telescope offsets to execute a jitter pattern Telescope offsets to execute a jitter pattern 0.75 square arcmin in 16 moves 0.75 square arcmin in 16 moves TBD whether available in service mode TBD whether available in service mode

24. KMOS IST meeting, ESO, 10 tth May 2006 Sky subtraction modes Four modes of sky subtraction provided for in the PDR design Four modes of sky subtraction provided for in the PDR design Experience from other instruments being brought to bear Experience from other instruments being brought to bear Flexibility to explore the most efficient options during commissioning Flexibility to explore the most efficient options during commissioning Sky subtraction mode impacts the flat- field requirements Sky subtraction mode impacts the flat- field requirements

25. KMOS IST meeting, ESO, 10 tth May 2006 Sky Subtraction: Offsetting Objects Single set of objects is offset between arms Single set of objects is offset between arms 50% of time spent on source; 50% on sky 50% of time spent on source; 50% on sky Object and sky observed along same optical path/same pixels Object and sky observed along same optical path/same pixels Flat-field accuracy requirements ~1% Flat-field accuracy requirements ~1%

26. KMOS IST meeting, ESO, 10 tth May 2006 Sky subtraction: Offset frames Object is offset between arms Object is offset between arms Observing objects in the ‘offset’ beam improves efficiency, but may be hard to achieve in real sources? Observing objects in the ‘offset’ beam improves efficiency, but may be hard to achieve in real sources? Object and sky observed along same optical path/same pixels Object and sky observed along same optical path/same pixels Flat-field accuracy requirements ~1% Flat-field accuracy requirements ~1%

27. KMOS IST meeting, ESO, 10 tth May 2006 Sky Subtraction: Source fields Sky signal obtained from the periphery of the IFU fields Sky signal obtained from the periphery of the IFU fields Highly efficient Highly efficient Flat-field accuracy requirements ~0.1% Flat-field accuracy requirements ~0.1% Achieved through a combination of flat-field observation and scaling OH lines Achieved through a combination of flat-field observation and scaling OH lines

28. KMOS IST meeting, ESO, 10 tth May 2006 Subtraction: Sky arms Arms not assigned to objects are used to observe sky Arms not assigned to objects are used to observe sky Requirements on flat- fielding are that sky signal must be calibrated to 0.1% Requirements on flat- fielding are that sky signal must be calibrated to 0.1% Achieved through combination of flat-field and post-processing Achieved through combination of flat-field and post-processing

29. KMOS IST meeting, ESO, 10 tth May 2006 Other configurable parameters Exposure time Exposure time Time to reach the background limit TBD, but around 600s Time to reach the background limit TBD, but around 600s Non-destructive read-out will be standard Non-destructive read-out will be standard Spectrometer Spectrometer User selected wavelength band User selected wavelength band The same grating and appropriate filter selected for all three spectrographs The same grating and appropriate filter selected for all three spectrographs Achromatic spectrograph, so no focus Achromatic spectrograph, so no focus

30. KMOS IST meeting, ESO, 10 tth May 2006 Spectroscopic modes Req 3.5.5: Total wavelength coverage At PDR, four options: IZ, J, H, K At PDR, four options: IZ, J, H, K Extension to 0.8um is optimal requirement Extension to 0.8um is optimal requirement i.e. coatings, IQ etc are acceptable i.e. coatings, IQ etc are acceptable Requires additional IZ grating and filter, discussed later….. Requires additional IZ grating and filter, discussed later….. Additional, broader coverage (JH/HK) gratings with lower R TBD during FDR phase (req 3.5.20) Additional, broader coverage (JH/HK) gratings with lower R TBD during FDR phase (req 3.5.20)

31. KMOS IST meeting, ESO, 10 tth May 2006 Spectroscopic modes 3.5.21: Wavelength multiplex advantage ‘Optimal’ requirement and initial KMOS concept to configure 3 spectrometers with different gratings, different DITs ‘Optimal’ requirement and initial KMOS concept to configure 3 spectrometers with different gratings, different DITs Opted for single detector controller, therefore different DITs not possible Opted for single detector controller, therefore different DITs not possible Multi-grating option not implemented Multi-grating option not implemented

32. KMOS IST meeting, ESO, 10 tth May 2006 3.5.19: Spectral resolving power Spectral resolving power secondary to wavelength coverage IZ:0.8-1.05um; J:1.05-1.37um; H:1.45-1.85um; K:1.95-2.50um

33. During the observations Source acquisiton Calibration stars

34. KMOS IST meeting, ESO, 10 tth May 2006 Observational efficiency Req 3.5.8: Desirable requirement for >85% efficiency in one hour gives 9minute budget Req 3.5.8: Desirable requirement for >85% efficiency in one hour gives 9minute budget Instrument configured during 6min telescope preset Instrument configured during 6min telescope preset Predicted 1min for observations of reference objects during acquisition. Budget ~3min. Predicted 1min for observations of reference objects during acquisition. Budget ~3min. Additional ~1min required if reconfiguring arms for different science targets Additional ~1min required if reconfiguring arms for different science targets

35. KMOS IST meeting, ESO, 10 tth May 2006 On loading the arm configuration Arm positions recalculated for the airmass at the start of observations Arm positions recalculated for the airmass at the start of observations In the case of a failed arm, the requested rotation of the field is altered until the allocation of arms to high priority targets is optimised In the case of a failed arm, the requested rotation of the field is altered until the allocation of arms to high priority targets is optimised

36. KMOS IST meeting, ESO, 10 tth May 2006 Arm failure and related responses Impact of an arm failure Impact of an arm failure 1/24 loss of efficiency measured simply by non-availability of an arm 1/24 loss of efficiency measured simply by non-availability of an arm Thoughtful arm design has ensured that one arm does not block others Thoughtful arm design has ensured that one arm does not block others Modelling with KARMA suggests ~1 objects no longer accessible in ‘standard’ clusters. Modelling with KARMA suggests ~1 objects no longer accessible in ‘standard’ clusters. Can be improved by reselecting rotation Can be improved by reselecting rotation

37. KMOS IST meeting, ESO, 10 tth May 2006 Acquisition with KMOS Acquisition to ±(0.5,0.5) spatial elements Acquisition to ±(0.5,0.5) spatial elements Repeat positioning to <±0.2arcsecs Repeat positioning to <±0.2arcsecs

38. KMOS IST meeting, ESO, 10 tth May 2006 Acquisition Steps Configure KMOS during telescope preset Configure KMOS during telescope preset For three bright reference sources or for science field For three bright reference sources or for science field Acquire guide star Acquire guide star Targets should be acquired now Targets should be acquired now Observe, determine centroids Observe, determine centroids Apply systematic offset as required Apply systematic offset as required Ignore small (<~0.2arcsec) random offsets Ignore small (<~0.2arcsec) random offsets If sources are not seen, start a different OB If sources are not seen, start a different OB

39. KMOS IST meeting, ESO, 10 tth May 2006 Acquisition with KMOS In visitor mode only (req 3.5.11) In visitor mode only (req 3.5.11) Small (< 1 field) adjustments of arms subject to rules Small (< 1 field) adjustments of arms subject to rules

40. KMOS IST meeting, ESO, 10 tth May 2006 What changes during the observations? Nothing Nothing No movement of the arms No movement of the arms Not for sky positions Not for sky positions Not for atmospheric refraction Not for atmospheric refraction No flexure compensation No flexure compensation Not for spectroscopic shifts Not for spectroscopic shifts Not for image movements/flexure Not for image movements/flexure NB: change from Phase A concept NB: change from Phase A concept

41. KMOS IST meeting, ESO, 10 tth May 2006 More on Spectral flexure Sources Sources Flexure of the pseudo-slit relative to the spectrograph Flexure of the pseudo-slit relative to the spectrograph Flexure of the detector+mount relative to slit Flexure of the detector+mount relative to slit Flexure of the grating Flexure of the grating Design has flexure within acceptable limits (req 3.5.23: <0.2pixels) Design has flexure within acceptable limits (req 3.5.23: <0.2pixels) If as-built flexure is unacceptable, calibrate with OH lines If as-built flexure is unacceptable, calibrate with OH lines Technique developed on SINFONI Technique developed on SINFONI

42. KMOS IST meeting, ESO, 10 tth May 2006 SINFONI OH wave cal

43. KMOS IST meeting, ESO, 10 tth May 2006 More on image movement Sources Sources Bulk motion of the instrument relative to the Nasmyth flange Bulk motion of the instrument relative to the Nasmyth flange Relative movements of the arms Relative movements of the arms Relative motions of the arms cannot be compensated Relative motions of the arms cannot be compensated Arm design meets the requirements on flexure Arm design meets the requirements on flexure NB not a peculiarity of the arms NB not a peculiarity of the arms

44. KMOS IST meeting, ESO, 10 tth May 2006 More on image movement Bulk motion of the cryostat Bulk motion of the cryostat Produces shifts in the images Produces shifts in the images Blind co-addition of images will result in combined PSF of 0.49arcsec over 1 hour in 0.4arcsec seeing Blind co-addition of images will result in combined PSF of 0.49arcsec over 1 hour in 0.4arcsec seeing Compensated by post-processing of images Compensated by post-processing of images BUT NB this does not include detector cross-talk and assumes ZD>10degrees BUT NB this does not include detector cross-talk and assumes ZD>10degrees Produces a shift of the spectral lines in conditions of the best seeing Produces a shift of the spectral lines in conditions of the best seeing 5% increase in line width 5% increase in line width ±0.23pixels movement of the centroid ±0.23pixels movement of the centroid NB this does not affect subtraction of sky lines NB this does not affect subtraction of sky lines

45. KMOS IST meeting, ESO, 10 tth May 2006 Observation of calibration stars Fixed arm configuration Fixed arm configuration Telluric standard from one arm Telluric standard from one arm Option to repeat once per spectrograph Option to repeat once per spectrograph Three arms deployed into the field Three arms deployed into the field offset telescope offset telescope Flux calibration Flux calibration Via the telluric standard or a flux standard Via the telluric standard or a flux standard Relative throughput of arms scaled from sky background Relative throughput of arms scaled from sky background

46. After the observations Daytime calibration Post processing steps

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

48. KMOS IST meeting, ESO, 10 tth May 2006 Calibration lamps Dedicated calibration unit containing Dedicated calibration unit containing Two tungsten lamps for flat fielding (one plus spare) Two tungsten lamps for flat fielding (one plus spare) One argon lamp for wavelength calibration One argon lamp for wavelength calibration

49. KMOS IST meeting, ESO, 10 tth May 2006Flat-fieldingFlat-fielding Continuum source in the calunit Continuum source in the calunit Provide spatially+spectrally smooth field Provide spatially+spectrally smooth field Modelled spatial uniformity: Modelled spatial uniformity: Few-% (possibly better…..) Few-% (possibly better…..) Sphere to be built and tested during FDR phase Sphere to be built and tested during FDR phase To remove vignetting function, flat-field on sky with arms in deployed position To remove vignetting function, flat-field on sky with arms in deployed position Twilight flats provided for, but not routine Twilight flats provided for, but not routine

50. KMOS IST meeting, ESO, 10 tth May 2006 Wavelength calibration Argon arc lamp expected to provide wavelength calibration to <0.1pixel (±2.5kms -1 ) Argon arc lamp expected to provide wavelength calibration to <0.1pixel (±2.5kms -1 ) req 3.5.24 on wavelength scale accuracy met req 3.5.24 on wavelength scale accuracy met Requirement (3.5.22) on velocity precision of ±10kms -1 met Requirement (3.5.22) on velocity precision of ±10kms -1 met Including allowance for predicted movement of the centroid in best seeing Including allowance for predicted movement of the centroid in best seeing

51. KMOS IST meeting, ESO, 10 tth May 2006 Image reconstruction: in the lab Spatial calibration established in the lab Spatial calibration established in the lab Spectral curvature Spectral curvature Offsets of the IFU slitlets Offsets of the IFU slitlets

52. KMOS IST meeting, ESO, 10 tth May 2006 Image reconstruction: in the lab Test facility for use in integration lab Test facility for use in integration lab Slit mask projects to the focal plane and can be observed by each IFU in turn Slit mask projects to the focal plane and can be observed by each IFU in turn

53. KMOS IST meeting, ESO, 10 tth May 2006 Image reconstruction: on telescope Spatial calibration established most efficiently in the lab Spatial calibration established most efficiently in the lab Changes within and IFU not expected Changes within and IFU not expected Would be as result of movements of monolithic mirrors Would be as result of movements of monolithic mirrors Flexures may cause shift of the long slit (from 8 IFUs) relative to detector Flexures may cause shift of the long slit (from 8 IFUs) relative to detector Detectable from flat-field Detectable from flat-field Would not affect the reconstructed image Would not affect the reconstructed image

54. KMOS IST meeting, ESO, 10 tth May 2006 Image recon n : on the telescope No access to the front of the instrument No access to the front of the instrument Can verify image reconstruction from calunit Can verify image reconstruction from calunit Observations of the edges of the slitlets Observations of the edges of the slitlets Observations of the arc lines Observations of the arc lines Or spatial offsets measured from a star Or spatial offsets measured from a star

55. KMOS IST meeting, ESO, 10 tth May 2006 Data pipeline Philosophy Philosophy Bringing in SINFONI experience Bringing in SINFONI experience Minimise interpolations Minimise interpolations Single set of routines for Quick-look, on-line pipeline, off-line pipeline Single set of routines for Quick-look, on-line pipeline, off-line pipeline IFU is the ‘unit’ of reduction IFU is the ‘unit’ of reduction

56. KMOS IST meeting, ESO, 10 tth May 2006 Data pipeline

57. KMOS IST meeting, ESO, 10 tth May 2006 Data pipeline: OH sky subtraction Discussed to be added Discussed to be added Scaling OH lines, in particular Scaling OH lines, in particular

58. KMOS IST meeting, ESO, 10 tth May 2006 Data pipeline: OH sky subtraction

59. KMOS IST meeting, ESO, 10 tth May 2006 Summary Science Requirements RequirementEssential Requirements PDR Prediction 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 map configuration

60. IZ grating trade-offs

61. KMOS IST meeting, ESO, 10 tth May 2006 Performance gains KMOS offers high throughput at >0.8um KMOS offers high throughput at >0.8um Low background Low background OH lines an order of magnitude fainter than JHK OH lines an order of magnitude fainter than JHK At R=3500, 85% of band free of lines At R=3500, 85% of band free of lines

62. KMOS IST meeting, ESO, 10 tth May 2006 Performance, R=3500

63. KMOS IST meeting, ESO, 10 tth May 2006 Comparison with existing facilities In future, X-shooter with R~4-7000 single IFU In future, X-shooter with R~4-7000 single IFU

64. KMOS IST meeting, ESO, 10 tth May 2006 Technical issues Coatings and optics Coatings and optics Philosophy is to take what we get Philosophy is to take what we get Optimised for JHK, perform well at IZ Optimised for JHK, perform well at IZ For IZ we require: For IZ we require: One additional grating - selected One additional grating - selected One additional blocking filter - selected One additional blocking filter - selected

65. KMOS IST meeting, ESO, 10 tth May 2006 Technical issues Grating turret Grating turret Can accommodate 3 additional gratings Can accommodate 3 additional gratings Does not increase in size Does not increase in size Weight limit still OK Weight limit still OK IZ grating selected IZ grating selected Filter wheels Filter wheels Can accommodate the additional filter with no change in size Can accommodate the additional filter with no change in size Filter selected Filter selected

66. KMOS IST meeting, ESO, 10 tth May 2006 Resource issues Grating and filter will need installed, tested and paid for Grating and filter will need installed, tested and paid for 3 x Z band gratings = £ 30K 3 x Z band gratings = £ 30K 3 x Z band filters=£ 8K 3 x Z band filters=£ 8K Alignment of filters=£ 3K (0.05 FTE) Alignment of filters=£ 3K (0.05 FTE) Alignments of gratings=£ 3K (0.05 FTE) Alignments of gratings=£ 3K (0.05 FTE) Factory Calibrations etc=£ 6K (0.1 FTE) Factory Calibrations etc=£ 6K (0.1 FTE) Total = £50K Total = £50K Additional time required in testing Additional time required in testing ~1 month ~1 month