IRIS Overview

Yutaka Hayano
ATC/TMT-J, NAOJ

2015/09/14-16

GOPIRA Symposium 20151IRIS Technical TeamJames Larkin (UCLA), PI, Lenslet IFS
Luc Simard, Brent Ellerbroek
Anna Moore (CIT), Co-PI, PM, Slicer IFS
TMT Instrumentation management
Shelley Wright (UCSD), PS, Pipeline and Gratings
James Wincentsen (CIT), PE
Jennifer Dunn (NRC-H), Co-I, OIWFS, NFIRAOS interface
Yutaka Hayano, Ryuji Suzuki (NAOJ), Co-I’s, Imager
Kai Zhang (NIAOT, 南京天文光学技術研究所), Co-I, Image slicer IFS
Engineers at COO, NRC-H, NAOJ, UCLA, UCSC–––––

Mechanical - Alex Delacroix, Bob Weber (COO), Ramunas Wierzbicki, Vlad Reshetov (NRCH), John Canfield, Eric Wang (UCLA), Yoshiyuki Obuchi, Bungo Ikenoue, Sakae Saito,
Fumihiro Uraguchi (NAOJ),
Optics- David Anderson, John Pazder, Jenny Atwood (NRC-H), Renate Kupke, Drew Phillips(UCSC), Toshihiro Tsuzuki (NAOJ)
S/W –Jason Weiss, Chris Johnson, Ji Man Sohn (UCLA), Bob Wooff (NRC-H), ReedRiddle(COO)
Detectors – Roger Smith (COO)
EE – Kris Caputa (NRC-H), Ken Magnone (UCLA)

Shaojie Chen, Elliot Meyer, University of Toronto, Grating trade study@TMT, NFIRAOS: Lianqi Wang, Corinne Boyer, Pete Byrnes, Glen Herriot, Matthias
Schoek and the IRIS astrometry team and many many more…
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IRIS Capabilities
Diffraction limited integral field spectrograph and imager to work with TMT AO system(NFIRAOS)–––

Wavelength Range 0.84-2.4 microns
Wavefront Error < 30 nm for fine scales
High Order Atmospheric Dispersion Correction

On-Instrument deployable wavefront sensors (OIWFS).
––Three sensors (one including focus) to measure tip/tilt, focus and distortion across field.
Work in near infrared to gain from NFIRAOS AO correction

Spectrograph––Spectral Resolution ~ 4000 (8000 and other modes)
IFS with Four Plate Scales (0.004, 0.009, 0.025, 0.050 arcsec per sample)

Imager–––34 arcsec field of view (2x2 grid of H4RG detectors)
0.004 arcsec plate scale
Parallel observations with IFS (share filter)

NSCU calibration system internal to NFIRAOS led by Moon and Simard.

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GOPIRA Symposium 20153NFIRAOS with IRIS

ImagerSpectrograph2015/09/14-16	

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Full Instrument•OIWFS•Support•Structure•Imager•Spectrograph2015/09/14-16

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IRIS focal plane

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OIWFS(On Instrument Wavefront Sensor)
Separate chamber cooled to -30C.
Can be mounted to NFIRAOS
through support structure with“dummy” IRIS top plate.
Different detectors, motors,sensors, etc…
But goals still include commoncontrollers and software.
– Galil motor controllers

Prototype probe arm is mature.
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Science Dewar
Dewar has two halves– Imager, SpectrographIn baseline system, cold structure
hangs from dewar lid with G10cylinder.

•Imager– Spectrograph cold structure mounts tobottom of Imager optical plate.

Cooling systems are tee’d to eachhalf so they run in parallel.

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•Spectrograph9Imager Dewar
Imager is assembled
and tested as a unit at
NAOJ.

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Imager optics
Double TMA Layout	
NFIRAOS	  focal	  plane	“C” means conic surface	

TMA	  camera	
Entrance	  window	
C	C	TMA	  collimator	

C	C	

1010 mm	

C	C	Pupil	  	  (95	  mm	  dia.)	
H4RG	  detectors	
1890 mm	

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Packaging
Three stairs structure design	
Entrance window	Collimator mirrors	Filter wheel	

Fold mirror	

ADC stage	
Detectors	

Camera TMA	

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Spectrographs
Spectrographs are jointly assembled andtested by UCLA and Caltech.

Lenslet Channel(Green)Camera TMA(Green)IFS Structure(Gold)
Slicer Channel(Blue)

Grating Turret(Purple) 13Spectrograph Modes
Slicer
– 1.125”x2.2” @ 0.025” scale– 2.25”x4.4” @ 0.050” scale
45 x 88 x 1600(λ) elements– R=4000 – 20% bandpasses

Additional narrow field,
high resolution modes areplanned.

Lenslet– 0.45”x0.51” @ 0.004” scale– 1.01”x1.15” @ 0.009” scale
112 x 128 x 500(λ) elements

Low resolution mode(R~500) may be possible
with double-pass prisms– R=4000 – 5% bandpasses

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Order of Integration
LensletSpecSlicer
SpecImager

OIWFS

HybridSpec

NFIRAOSTMTNFIRAOS+ OIWFS
ScienceDewar
NFIRAOS+ IRIS
Final AIV

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IRIS AIV Flow Overview•Nasmyth Clean Tent Assembly Area
(Location TBD)•NFIRAOS
Integration•NFIRAOS
Deintegration•Standalone Mode•in Nasmyth Clean Tent

•Prepare for Shipment toMauna Kea

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IRIS schedule – based on
March 2015 TMT schedule
Light Preliminary Design Phase - Current
Final Design Phase starts – Jan 2016
Fab Phase starts - July 2017
Major subsystems complete - June 2020–––OIWFS integration in Victoria
Imager and top of dewar integration at NAOJ
Spectrograph and bottom of dewar integration in California

OIWFS begins Integration with NFIRAOS in Victoria: July 2020
–Small camera mounts to bottom of dewar lid

Imager and spectrograph integrate in California: July 2020
Combine Science Dewar, OIWFS and NFIRAOS: July 2021
AIV at TMT: Start in early 2022
Technical Commissioning: May-July 2023 -> After Jan 2024?
Science commissioning: Oct 2023-Jan 2024 -> After March 2024?
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