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Infrared Multi-Object Spectrometer (IRMS)

Wavelength: 0.8-2.5 μm

Observing Modes: Imaging and Multi-slit Spectroscopy

Spacial Scales: 0.06"

Spectral Resolution: 5000

Field Size: 2.1' x 2.1'

Image Quality: NFIRAOS Wide-Field Mode

Filters: Z, J, H, K

Multiplex: Cryogenic configurable slit unit. Slit width: 0.16" up to 46 slits


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Principal Investigator:
Barham Mobasher (UC, Riverside)

Infrared Multi-object Spectrometer (IRMS)

The IRMS is a near diffraction-limited multi-slit near-infrared spectrometer and imager. It is modeled closely after the MOSFIRE instrument on the Keck Telescope and will be fed by the Narrow-Field Infrared Adaptive Optics System (NFIRAOS). See schematic of the instrument in the following figure. 

IRMS will provide near-infrared imaging and multi-object spectroscopy at Y (0.97–1.12 micron), J (1.15–1.35 micron), H (1.46–1.81 micron), and K (1.93–2.45 micron) bands. Operating with NFIRAOS on the TMT, it can be used as a near-diffraction-limited imager and multi-slit spectrograph with moderate resolution. It has a circular field-of-view (FoV) of 2.27 arcmin in imaging mode, and elliptical FoV of 2.0'x0.6' in spectroscopy mode. The spatial scale is 0.06" per pixel, or 0.08" per pixel in the dispersion direction. The spectral resolution R is 3270 for a 3 pixel or 0.24" wide slit, or R = 4660 for a 2 pixel or 0.16" wide slit. IRMS has a multiplex capability of up to 46 slits using a slit mask system on a cryogenic configurable slit unit. Each slit width can be adjusted arbitrarily, with minimum slit width of 0.16". The IRMS detector will be 2048x2048 Teledyne Technologies Hawaii-2RG with a long wavelength cut-off at 2.5 micron.



IRMS Science

The science areas that will be advanced with IRMS observations include, but are not limited to, the following: 

  • Planetary Astronomy: Searching for Exoplanets
  • Stellar Astronomy: Massive Stars and Young Star Clusters
  • Active Galactic Nuclei (AGN): Co-evolution of Black Holes and Galaxies
  • Inter-Galactic Medium (IGM): Interaction of IGM with Galaxies at High-z
  • High-Redshift Universe: Population III Stars, Cosmic Re-ionization and Nature of the High-z Galaxies

Using Adaptive Optics

NFIRAOS Wide Field Mode will deliver images to IRMS that will produce almost an order of magnitude gain in encircled energy within 160″ slits over the entire of 2′ diameter field. These IRMS performance estimates were generated by the TMT AO analyst Luc Gilles in 2010. The solid curves are performance predictions for atmospheric turbulence and WFS noise effects only. Please note that enclosed energies are plotted as a function of the full (not half) slit width. The dashed and dotted curves include the additional wavefront errors due to implementation effects based on two models. Notice that the dashed curves aren't that much different from the solid curves for a 160 mas slit width, although more work is needed to estimate the actual structure function for these implementation errors. 



Dotted: Errors have a white spatial frequency spectrum, and the impact on the enclosed energies is estimated using Marechel's approximation.  Dashed: Errors have a Kolmogorov spectrum, and the impact on the enclosed energies is estimated by multiplying the OTF by a transfer function in the spatial frequency domain.

IRMS Science Team

  • Bahram Mobasher (UC Riverside) - Instrument Scientist
  • Masayuki Akiyama (Tohoku University)
  • Lee Armus (Spitzer Science Center)
  • Adam Burgasser (UC San Diego)
  • Peter Capak (Spitzer Science Center)
  • Ian Crossfield (University of Arizona)
  • Mark Dickinson (NOAO)
  • Don Figer (Rochester Institute of Technology)
  • Mauro Giavalisco (UMass Amherst)
  • Nobunari Kashikawa (NAOJ)
  • Nick Konidaris (Caltech)
  • Jessica Lu (University of Hawaii)
  • Norio Narita (NAOJ)
  • Naveen Reddy (UC Riverside)
  • Mike Rich (UCLA)
  • Luc Simard (University of Victoria)
  • Vivian U (UC Riverside)
  • Toru Yamada (Tohoku University)


IRMS Technical Team

  • Coming soon...