The Wide Field Optical Spectrometer (WFOS) will provide near-ultraviolet and optical (0.3 – 1.0 μm wavelength) imaging and spectroscopy over a more than 40 square arcminute field-of-view. Using precision cut focal plane masks, WFOS will enable long-slit observations of single objects as well as short-slit observations of hundreds of objects simultaneously. WFOS will use natural (uncorrected) seeing images.
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 (TMT). 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.
The IRMS is a near diffraction-limited multi-slit near-infrared spectrometer and imager. As one of the first-light instruments on the TMT, 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.
The first light Adaptive Optics (AO) architecture for the TMT has been defined to provide near-diffraction-limited wavefront quality and high sky coverage in the near infra-red (IR) for the first TMT science instruments IRIS and IRMS. Design, fabrication and prototyping activities of the TMT first light AO systems and their components in Canada, China, France, and in the US are currently on schedule.