Tmt night

Infrared Imaging Spectrograph (IRIS)


Integrated Field Spectrograph

Wavelength: 0.8-2.5 μm

Spectral resolution: 4000 to 8000

Spacial Scales: Lenslet:0.004", 0.009".      
Slicer: 0.025", 0.05"

Field Size:
@4mas: 0.064" x 0.512" (broadband) and
0.458" x 0.512" (narowband)
@9mas: 0.144" x 1.152" (broadband) and 1.008" x 1.152" (narrowband)
@25mas: 1.1" x 2.275"
@50mas: 2.2" x 4.55"

Filters: Broadband filters (Y, Z, J, H, K), Narrowband (5 % bandpass) filters, and specialized filters (< 1% bandpass)


0.8-2.5 μm

Spatial Scale: 0.004"

Field Size: 17.2" x 17.2"

Astrometry: Absolute accuracy 2 mas. Relative accuracy 30 μas

Filters: Broadband filters (Y, Z, J, H, K), Narrowband (5 % bandpass) filters, and specialized filters (< 1% bandpass)

Status: Preliminary Design Review - Second Stage


Documents and Tools


Pricipal Investigator
James Larkin (UCLA)

Project Scientist
Shelley Wright (UCSD)

Science Partners
UCLA; UC, Berkeley; UC, Irvine; Caltech/IPAC; Swinburne University; NRC-H; NAOJ; U of Hawaii; Stanford University; NAOC; Indian Institute of Science; Kyoto University; U of Florida

Infrared Imaging Spectrograph (IRIS)

IRIS is a first generation near-infrared (0.85-2.5 μm) instrument being designed to sample the diffraction limit of the Thirty Meter Telescope. IRIS will include an integral field spectrograph (R~4000) and imaging camera (17"x17"). Both the spectrograph and imager will take advantage of the high spatial resolution achieved with the Narrow-Field Infrared Adaptive Optics System (NFIRAOS) at four spatial scales (0.004", 0.009", 0.025", 0.05"). IRIS will achieve an angular resolution ten times better than images from the Hubble Space Telescope, and will be the highest angular resolution near-infrared instrument in the world. 

IRIS model external

External model of IRIS

IRIS IFS model

IRIS IFS model

Integrated Field Spectrograph

The purpose of an integral field spectrograph (IFS) is to acquire spectra over a two-dimensional area of the sky, where for each spatial location (or dissecting element) a spectrum is produced. IRIS is designed with two spatial sampling techniques, lenslet array and mirror slicer, to optimize the best quality spectra with both high throughput and low wavefront error. Both the lenslet array and slicer optics are fed into a single spectrograph, and share similar optics (i.e., TMAs, reimaging optics, gratings, filters, and detector). The lenslet array is used for the finest spatial resolutions (0.004", 0.009") and the mirror slicer is used for the coarsest spatial resolutions (0.025", 0.05"). When delivered, IRIS will have a fully packaged data reduction pipeline for real-time reductions during observations and final reductions for user astronomers.


IRIS imager model

IRIS imager model


The near-infared (0.8 - 2.5 μm) imager will have a spatial sampling of 0.004" per pixel with a total field of view of 17.2" x 17.2". The optical design has been optimized to achieve the lowest wavefront error (~30 nm) in order to sample the high spatial resolutions achieved from the adaptive optics system, NFIRAOS. The leading science cases for the imager require a high level of astrometric precision (e.g., Galactic Center, star forming regions,). The imager is expected to achieve an astrometric absolute accuracy of 2-4 mas and relative accuracy of 30 μas. 


Geometric configuration for the three wavefront sensor arms that can be positioned over the 2' field of view. The IRIS imager (red) is on-axis and the IFS (blue) is 18" off-axis

On-Instrument Wavefront Sensors (OIWFS)

IRIS will house low-order wavefront sensors (WFS) that will be used by NFIRAOS to monitor tip-tilt, astigmatism, and focus. IRIS will have three WFSs, which will sample stars as faint as J = 22 mag over a 2 arcminute field-of-view (FOV). The WFSs must be deployable over the entire FOV to maximize sky coverage, and allow for optimum AO correction (the best correction is obtained when the WFSs are deployed symmetrically about the science target). The figure below shows the geometric configuration of the three tip-tilt guide arms and the locations of the IRIS imager and spectrograph.



IRIS atmospheric dispersion

IRIS atmospheric dispersion

Atmospheric Dispersion Corrector (ADC)

One of the challenges of generating an instrument with high angular resolutions (0.004") is compensating for the dispersion that occurs within Earth's atmosphere. In order to counter this effect IRIS will house an atmospheric dispersion corrector (ADC) in front of IRIS science's dewar. It will use real-time knowledge of atmospheric conditions (temperature, pressure, humidity) and optical elements to correct for dispersion over varying observing elevations.


IRIS Science

The IRIS science team has generated a plethora of astronomical topics that IRIS will be capable of exploring.The combination of a large collecting area and unprecedented angular resolution will have a direct impact on a broad range of science programs that span topics as diverse as the search for extrasolar planets to studies of the first stars to illuminate the Universe.  Most intriguing, are the new discoveries that will likely be revealed by IRIS. As is stated in The Exploration of the Unknown by Kellermann el al. 2009, "The excitement of the next generation of astronomical facilities is not in the old questions which will be answered, but in the new questions that they will raise." With IRIS and TMT extending our current technology by orders of magnitude in sensitivity and angular resolution it has the promise of doing just that.

First Light: Identification and characterization of first light galaxies and population III stars.

Figure on the right is a simulation of a forming galaxy at z=12.5 and the expected hydrogen number density (Johnson, Greif, Bromm 2008). The dense gas (orange-white) just left of the center of the galaxy represents the formation of two Pop III stars. Overlaid on the figure is a 1"x3" field of view (3.6kpc x 10.8kpc), which is close to the FOV using IRIS's 0.025" slicer scale.
High-z Galaxy Dynamics and Morphologies:Studying galaxy formation and mass assembly over cosmic time (1 < z <5). Using optical emission lines (e.g., Hα, Hβ, [OIII]) to map 2D dynamics of galaxies during the peak epoch of star formation and AGN accretion.

The anticipated S/N ratios for Hα emission from four high-z galaxies as observed using the IRIS IFS 0.05" spatial sampling (see Law et al. 2006).
Metallicity Evolution and Gradients: Tracing metallicity over cosmic time (1 < z <5) using multiple optical emission lines to determine the chemical enrichment history. The IFS will be able to map metallicity gradients over individual high-z galaxies from different galactic components (i.e.,bulge, disk, outflows, and inflows.

The figure on the right is a [NII]/Hα ratio map of a z~1.6 galaxy from the Keck AO system, and shows high spatial concentration (yellow) of [NII]/Hα which shows the presence of a weak AGN within this star-forming dominated galaxy (Wright et al. 2009). IRIS will be essential for distinguishing between AGN and star forming emission from different regions of a galaxy.
Supermassive Black Holes: A study of AGN, black hole demographics and growth throughout cosmic history.

The left figure is of the MBH-σ relation plotted for measured black hole masses versus observed dispersions of late-type spirals and nuclear star clusters (Barth et al. 2009). There is a large phase-space regime that requires both higher sensitivity and angular resolution observations of low mass black holes (106 Msun) and high mass black holes (109 Msun). IRIS's finest scale (0.004") is very suitable for this study.
Local Galaxies and Stellar Populations: A study of stellar populations in galaxies from the local group to the Virgo cluster. IRIS with its high-angular resolution and sensitivity will be able to produce near-infrared spectra and images of individual stars in nearby galaxies, and will probe the chemical enrichment and formation histories for a range of Hubble types.

A one-degree image of the Virgo cluster (18 Mpc) from HST, with the lenticular galaxy at the center and other spiral galaxies on the outskirts. IRIS will be able to study each of these galaxies to an unprecedented image depth.
Dwarf Galaxies: A study of local dwarf galaxy's dynamical and chemical enrichment to probe the dark matter distribution and differing dark matter models (warm vs. cold).

On the left, the cumulative number of Milky Way satellite galaxies as a function of their observed cicular velocities (black points). These observations are compared to the Via Lactea N-body simulation of predicted number of satellites and how differing reionization epochs influences the expected satellite number distribution (Simon & Geha 2007).
Galactic Center: Studying the properties and conditions surrounding the supermassive black hole (SMBH) at the center of the Galaxy. The relative astrometric accuracy of 30 μas will allow measurements to better constrain MBH, test General Relativity, determine GC distance, and the stellar dynamical history. 

Right figure is of the current imaging capabilities of the central arcsecond sources from Keck-AO. The image on the right represents the depth and resolution that TMT and IRIS will provide (see UCLA Galactic Center).
Star Formation: Investigating star formation properties in star clusters: timescale of star formation and efficiencies, initial cluster mass funcion (ICMF), initial mass function, multiplicity and kinematics 

The figure on the left illustrates three clusters with varying masses (30Dor: 105 Msun, NGC3603: 104 Msun, Orion: 103Msun) which will be resolved with IRIS at distances up to 20 Mpc away.
Microlensing: Constraining models of stellar structure and evolution by determining precise stellar masses from astrometric microlensing. IRIS, with its high astrometric relative accuracy, will be able to fit mircolens light curves to accurately determine stellar masses for a range of stellar-types. 

On the right, a proper motion curve for a star over 5 years that has been lensed (solid curve) and without being lens (dashed lens) (Belukurov & Evans 2002).
Extrasolar Planets: The detection and characterization of extrasolar planets and planet forming environments.

On the left, an image of the first extrasolar multiple planet system ever directly-imaged, around the young star HR 8799 (Marois et al. 2008). The image is a near-infrared color composite of J, H, and K bands taken from both Keck and Gemini telescopes using adaptive optics. Each planet is respectively 70, 40, and 25 AU from the central star. A system such as HR 8799 would be easily studied using IRIS.
Solar System:The formation history of our solar system. Using near-infrared spectroscopy for compositional and dynamical studies of Kuiper Belt Objects (KBO) and transneptunian objects (TNOs).

Near infared spectra of Pluto and the TNO, 2005 FY9, show strong methane absorption in the figure on the right (Licandro et al. 2006).


IRIS Science Team

  • Shelley Wright (UCSD): Project Scientist, High-Redshift Universe
  • Maté Adamkovics (Berkeley): Solar System 
  • Aaron Barth (UCI): Black Holes and Bulges 
  • Joshua Bloom (Berkeley): Microlensing 
  • Pat Coté (HIA): Black Holes and Nuclear Star Clusters 
  • Will Clarkson (UCLA): Astrometry
  • Tim Davidge (HIA): Stellar Populations of Nearby Galaxies 
  • Tuan Do (UCI): IRIS Sensitvities, Galactic Center
  • Andrea Ghez (UCLA): Galactic Center and Star Clusters 
  • Miwa Goto (MPIA): Star Formation 
  • David Law (UCLA): High-Redshift Universe 
  • Nobunari Kashikawa (NAO): First Light Galaxies 
  • Bruce Macintosh (LLNL): Exoplanets
  • Shri Kulkarni (Caltech): Astrometry 
  • Jessica Lu (Caltech): Star Formation, Astrometry, and Galactic Center 
  • Hajime Sugai (Kyoto U): AGN, Starbursts and the Early Universe 
  • Jonathan Tan (Florida): Star Formation

IRIS Technical Team

  • James Larkin (UCLA): Principal investigator, IFS design lead
  • Anna Moore (Caltech): Co-principal investigator, Slicer design lead
  • Brian Bauman (UCSC): Optical designer
  • John Canfield (UCLA): Mechanical engineer
  • David Crampton (HIA): TMT Instrument Project manager
  • Alex Delacroix (Caltech): Mechannical engineer
  • Murray Fletcher (HIA): OIWFS team member
  • Masahiro Konishi (NAOJ): Imager team
  • David Loop (HIA): OIWFS design lead
  • Dae-Sik Moon (HIA): Science calibration unit lead`
  • Drew Phillips (UCSC): ADC design lead
  • Vladmir Reshetov (HIA): Mechanical engineer
  • Luc Simard (HIA): IRIS/NFIRAOS technical interface
  • Ryuji Suzuki (IfA): Imager optical design
  • Tomonori Usuda (NAOJ): Imager team