Transcript 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.

KMOS Instrument Science
Team Review
Instrument overview
Consortium Members
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Universitäts-Sternwarte München
MPI für Extraterrestrische Physik
UK Astronomy Technology Centre
University of Durham
University of Oxford
University of Bristol
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European Southern Observatory
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KMOS IST meeting, ESO, 10tth May 2006
Announcement of Opportunity
Feb 2002
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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
Top Level Scientific Drivers
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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
Top Level Requirements
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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
Multiplex advantage
KMOS IST meeting, ESO, 10tth May 2006
Science Requirements
Requirement
Essential
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 2.5mm
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
KMOS IST meeting, ESO, 10tth 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
KMOS IST meeting, ESO, 10tth May 2006
Design Principles
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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
Systems Architecture
KMOS IST meeting, ESO, 10tth May 2006
Systems Architecture
KMOS IST meeting, ESO, 10tth May 2006
KMOS IST meeting, ESO, 10tth May 2006
KMOS IST meeting, ESO, 10tth May 2006
End-to-end Optical Model
KMOS IST meeting, ESO, 10tth May 2006
Pickoff Module
Pickoff Subsystem
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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
KMOS IST meeting, ESO, 10tth May 2006
KMOS IST meeting, ESO, 10tth May 2006
Technology Prototyping
I: Prototype Pickoff Arm
KMOS IST meeting, ESO, 10tth May 2006
KMOS IST meeting, ESO, 10tth May 2006
KMOS IST meeting, ESO, 10tth May 2006
KMOS IST meeting, ESO, 10tth May 2006
KMOS IST meeting, ESO, 10tth May 2006
Integral Field Units
IFU Subsystem
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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
KMOS IST meeting, ESO, 10tth May 2006
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
Pupil mirror assembly
KMOS IST meeting, ESO, 10tth May 2006
Spectrographs
Spectrograph Subsystem
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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
All spherical
lenses
ZnSe
Fused Silica
ESF03
CaF2
CaF2
ESF03
Torroidal
collimator mirror
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Flat fold mirror
(slit below)
100.00
MM
X
KMOS IST meeting, ESO, 10tth May 2006
KMOS IST meeting, ESO, 10tth May 2006
KMOS IST meeting, ESO, 10tth May 2006
KMOS IST meeting, ESO, 10tth May 2006
Calibration system
Calibration lamps
(Th)-Ar
Tungsten
(2)
KMOS IST meeting, ESO, 10tth May 2006
Calibration system
KMOS IST meeting, ESO, 10tth May 2006
Calibration system
0=0.96
0=0.98
Upper port
Lower port
KMOS IST meeting, ESO, 10tth May 2006
Detector and mount
Detector module
Hawaii RG2 arrays from Rockwell (2048x2048 pixels),
results from Gert Finger
KMOS IST meeting, ESO, 10tth May 2006
KMOS IST meeting, ESO, 10tth May 2006
KMOS IST meeting, ESO, 10tth May 2006
Detector mount: ESO standard
KMOS IST meeting, ESO, 10tth May 2006
Detector mount
KMOS IST meeting, ESO, 10tth May 2006
More on the detector mounting
NB focus mechanism for lab testing
only.
KMOS IST meeting, ESO, 10tth May 2006
Status and Schedule
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KMOS ESO STC approval Nov 2003
Phase B start July 2004
Preliminary Design Review May 2006
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Final Design Review March 2007
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Arms PDR, June 2006
Optics and cryostat FDR, Q4 2006
Prelim Acceptance Europe March 2010
KMOS IST meeting, ESO, 10tth May 2006
Summary
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KMOS will be the first cryogenic multipleintegral 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