KMOS Instrument Science Team Review Instrument overview

KMOS Instrument Science Team Review

Instrument overview

KMOS IST meetingKMOS IST meeting, , ESO, 10ESO, 10tthtth May 2006 May 2006

Consortium MembersConsortium MembersConsortium MembersConsortium Members• Universitäts-Sternwarte München Universitäts-Sternwarte München • MPI für Extraterrestrische MPI für Extraterrestrische

PhysikPhysik• 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 ObservatoryEuropean Southern Observatory


Announcement of Announcement of OpportunityOpportunity Feb 2002 Feb 2002

Announcement of Announcement of OpportunityOpportunity Feb 2002 Feb 2002

• 1.0-2.4 1.0-2.4 m Cryogenic Multi-Object m Cryogenic Multi-Object SpectrometerSpectrometer

• ““Key requirement is to optimize the scientific Key requirement is to optimize the scientific potential of the instrument, particularly for the potential of the instrument, particularly for the study of the intermediate and high-z slices of study of the intermediate and high-z slices of our Universe. This should drive its field of view our Universe. This should drive its field of view and multiplex capability.”and multiplex capability.”


Top Level Scientific Top Level Scientific DriversDrivers

Top Level Scientific Top Level Scientific DriversDrivers

• Investigate the physical processes Investigate the physical processes which drive galaxy formation and which drive galaxy formation and evolution over redshift range 1<z<10.evolution over redshift range 1<z<10.

• Map the variations in star formation Map the variations in star formation histories, spatially resolved star-histories, spatially resolved star-formation properties, and merger ratesformation properties, and merger rates

• Obtain dynamical masses of well-Obtain dynamical masses of well-defined samples of galaxies across a defined samples of galaxies across a wide range of environments at a series wide range of environments at a series of progressively earlier epochsof progressively earlier epochs


Top Level RequirementsTop Level RequirementsTop Level RequirementsTop Level Requirements

• Spatially-resolved (3-D) Spatially-resolved (3-D) spectroscopyspectroscopy

• Multiplexed spectroscopic Multiplexed spectroscopic observationsobservations

• Observations across the Observations across the JJ, , HH, and , and K K infrared atmospheric windowsinfrared atmospheric windows

• Versatile capability to address Versatile capability to address new scientific problemsnew scientific problems


Multiplex advantageMultiplex advantageMultiplex advantageMultiplex advantage


Science RequirementsScience RequirementsScience RequirementsScience RequirementsRequirement Essential

RequirementsPDR 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 2.5m

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 24

Extent of each IFU (REQ 3.5.10)

2.8 x 2.8 sq. arc seconds 2.8 x 2.8 sq. arc seconds

Spatial Sampling (REQ 3.5.11)

0.2 arc seconds 0.2 arc seconds

Patrol field (REQ 3.5.9)

5’x 5’ field 7.2 arcmin diameter field

Close packing of IFUs (REQ 3.5.15)

≥3 within 1 sq arcmin ≥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


Functional RequirementsFunctional RequirementsFunctional RequirementsFunctional RequirementsRequirementRequirement Baseline DesignBaseline Design

Flat-field accuracyFlat-field accuracy <1% of night sky<1% of night sky

Instrumental ProfileInstrumental Profile<5% deviation in the FWHM <5% deviation in the FWHM

of line profiles at of line profiles at constant wavelengthconstant wavelength

Array stabilityArray stability <1% of the night sky<1% of the night sky

Cosmetic qualityCosmetic quality <3% of pixels are unstable<3% of pixels are unstable

Observing efficiencyObserving efficiency 70%70%

AcquisitionAcquisition ±0.5 sampling element±0.5 sampling element


Design PrinciplesDesign PrinciplesDesign PrinciplesDesign Principles• Develop baseline design to deliver optimal Develop baseline design to deliver optimal set of science requirementsset of science requirements

• Exploit proven technologies and the Exploit proven technologies and the consortium knowledge baseconsortium knowledge base

• Prototype key technologies and subsystems Prototype key technologies and subsystems where appropriatewhere appropriate

• Investigate backup solutions to minimise Investigate backup solutions to minimise risk and explore possible trade-off risk and explore possible trade-off optionsoptions

• Strong systems engineering approach Strong systems engineering approach throughoutthroughout


Systems ArchitectureSystems ArchitectureSystems ArchitectureSystems Architecture


End-to-end Optical End-to-end Optical ModelModel

End-to-end Optical End-to-end Optical ModelModel

Pickoff ModulePickoff Module


Pickoff SubsystemPickoff SubsystemPickoff SubsystemPickoff Subsystem• Fused silica singlet and powered entrance window to Fused silica singlet and powered entrance window to produce a flat, telecentric 7`.2 diameter Nasmyth produce a flat, telecentric 7`.2 diameter Nasmyth focal planefocal plane

• 24 constant path-length mechanical pickoff arms 24 constant path-length mechanical pickoff arms driven by cryogenic stepper-motors patrolling in 2 driven by cryogenic stepper-motors patrolling in 2 planes to minimizes contention during object planes to minimizes contention during object acquisition; integral cold stop to minimize thermal acquisition; integral cold stop to minimize thermal backgroundbackground

• Calibration unit to provide the ability to verify Calibration unit to provide the ability to verify and calibrate the end-to-end performance of the and calibrate the end-to-end performance of the instrumentinstrument

• Cryogenic mechanisms have demonstrated high Cryogenic mechanisms have demonstrated high reliability and have been the subject of extensive reliability and have been the subject of extensive technology teststechnology tests


Technology PrototypingTechnology PrototypingI: Prototype Pickoff ArmI: Prototype Pickoff Arm Technology PrototypingTechnology PrototypingI: Prototype Pickoff ArmI: Prototype Pickoff Arm

Integral Field Units


IFU SubsystemIFU SubsystemIFU SubsystemIFU Subsystem• 8 pickoff subfields combined to produce 8 pickoff subfields combined to produce single output slit; each subfield re-single output slit; each subfield re-imaged on to 14x14 element image slicerimaged on to 14x14 element image slicer

• Diamond-machined monolithic optics (Al) Diamond-machined monolithic optics (Al) to eliminate thermal effects and to eliminate thermal effects and minimize alignment errors minimize alignment errors

• All reflective, gold-coated, achromatic All reflective, gold-coated, achromatic designdesign

• Anamorphic magnification produces Anamorphic magnification produces regular spatial sampling on sky (0.2 regular spatial sampling on sky (0.2 arcsec) with Nyquist sampling of spectraarcsec) with Nyquist sampling of spectra

• Each of 3 IFU systems is identicalEach of 3 IFU systems is identical


Integral field Integral field unitunit

Integral field Integral field unitunit

Slicing mirror

Pupil mirror

Slit mirror

3 identical sets of 8 IFUS4 foreoptics designs (aspheric)24 identical image slicer assemblies


Pupil mirror assemblyPupil mirror assemblyPupil mirror assemblyPupil mirror assembly

Spectrographs


Spectrograph SubsystemSpectrograph SubsystemSpectrograph SubsystemSpectrograph Subsystem• Modular spectrograph subsystems (3)Modular spectrograph subsystems (3)• Toroidal reflective collimator and 6-Toroidal reflective collimator and 6-element transmissive achromatic element transmissive achromatic cameracamera

• 6-position grating turret; optimized 6-position grating turret; optimized J,H,K gratings bandsJ,H,K gratings bands

• Additional IZ grating included at Additional IZ grating included at PDR; two further ‘double band’ PDR; two further ‘double band’ gratings to be considered during FDRgratings to be considered during FDR

• Single mechanism - stepper motor Single mechanism - stepper motor drive with index limit switch drive with index limit switch


100.00 MM

All spherical lenses

Torroidal collimator mirror

Flat fold mirror (slit below)

X

Y

ZnSe Fused Silica

ESF03 CaF2

ESF03 CaF2

Calibration system


Calibration lampsCalibration lampsCalibration lampsCalibration lamps

(Th)-Ar

Tungsten (2)


Calibration systemCalibration systemCalibration systemCalibration system


Calibration systemCalibration systemCalibration systemCalibration system

0=0.96

0=0.98

Upper port Lower port

Detector and mount


Detector moduleDetector moduleHawaii RG2 arrays from Rockwell (2048x2048 Hawaii RG2 arrays from Rockwell (2048x2048

pixels), results from Gert Fingerpixels), results from Gert Finger

Detector moduleDetector moduleHawaii RG2 arrays from Rockwell (2048x2048 Hawaii RG2 arrays from Rockwell (2048x2048

pixels), results from Gert Fingerpixels), results from Gert Finger


Detector mount: ESO Detector mount: ESO standardstandard

Detector mount: ESO Detector mount: ESO standardstandard


Detector mountDetector mountDetector mountDetector mount


More on the detector mounting NB focus mechanism for lab testing only.


Status and ScheduleStatus and ScheduleStatus and ScheduleStatus and Schedule

• KMOS ESO STC approval Nov 2003KMOS ESO STC approval Nov 2003• Phase B start July 2004Phase B start July 2004• Preliminary Design Review May 2006Preliminary Design Review May 2006

• Arms PDR, June 2006Arms PDR, June 2006• Final Design Review March 2007Final Design Review March 2007

• Optics and cryostat FDR, Q4 2006Optics and cryostat FDR, Q4 2006• Prelim Acceptance Europe March Prelim Acceptance Europe March 2010 2010


SummarySummarySummarySummary

• KMOS will be the first cryogenic KMOS will be the first cryogenic multiple-integral field spectrometer on multiple-integral field spectrometer on an 8-m class telescopean 8-m class telescope

• It will be a challenging instrument to It will be a challenging instrument to build but with lots of exciting build but with lots of exciting scientific potentialscientific potential

• At PDR we believe we have a robust At PDR we believe we have a robust design which meets all the top-level design which meets all the top-level science requirementsscience requirements

KMOS Instrument Science Team Review Instrument overview

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