List of instrument concepts proposed for further study in the instrument white papers.
High-Resolution Optical Spectrometer (HROS)
- R=25,000 to 100,000 (50,000 to ≥90,000)
- Multiplex ≤100 (Single object)
InfraRed Multi-slit Spectrometer (IRMS)
- 0.95-2.45µm, R=3270-4660 and Y,J,H,K imaging
- 2.05x2.05 sq arcmin, 0.060 arcsec/pixel, AO with NFIRAOS
- >80% EE in 0.12” by 0.16”, 46 adjustable 2.43 arcsec slits
Multi-IFU imaging spectrometer (IRMOS)
- 0.84-2.4µm (0.8-2.5µm)
- R=4000-10,000, full Y,J,H or K bands at 4000 (2000-10,000)
- 2' patrol field (>2'), >10 IFUs, 0.5"@0.012"/spaxel, 1.06"@0.025", 2.1"@0.05 (3"x3"@0.05")
- >50% EE in 0.05", overall efficiency 40% (>30%)
bMICHI - mid-IR AO Fed spectrometer imager IFU (MIRES)
- 3-14µm (8-18µm)
- R~600 long slit with polarimetry, 100,000-120,000 (5000-100,000)
- R~1000 N-band IFU, 2x5 0.035" spaxels
- 24.4"-28.1" FOV imager (10"), 0.012"/pixel@L,M, 0.028"/pixel@N (0.17") with polarimetry
Planetary System Instrument (PSI)
- 0.6-5.3µm (1-2.5µm) with coronograph
- Contrast ~10-8 @ 1–2λ/D
- R=50-5000 IFU/imager with polarimetry (≤100)
Multi-fiber High-resolution NIR spectometer (MODHIS)
- 0.95-2.5µm, fed by NFIRAOS
- R~100,000, 30 cm/s velocity precision
- Multiplex ~25 over 2"-5" with 0.1"x0.1" mini-IFUs@ 0.02" sampling
Astronomical Rapid Imager and Spectropolarimetric Explorer (ARISE)
- 0.31-4.8µm simultaneous, R>15000
- 5' FOV imaging @0.1"/pixel in u, g', r', i', z', J, H, K, L', M'
- 10 Hz full frame, 100 Hz windowed
- 1.1-4.8µm polarimetry
- 0.31-1µm IFU
Near-IR AO-fed Echelle Spectrometer (NIRES)
- 1-5µm, AO with NFIRAOS
- R~20,000 for 1-2.5µm, R~100,000 for 3-5µm
- Simultaneous 1.5µm@R>20,000
- >20% throughput
The TMT observatory is designed to support a wide range of different forms of facility class instrumentation. An original suite of instrument concepts was developed and the observatory design was developed around them (see listing of instrument requirements in the TMT Science Requirements Document - SRD). These longstanding ideas for instruments have continued to evolve and new instrument concepts are being actively developed (see a present list on the left). Currently the main instruments planned for operation at first-light are WFOS and IRIS. Any other facility-instruments planned afterwards are part of the “next-generation” suite of instruments. The prioritization for future instrument capabilities and the resulting strategy or sequence for instrument development is based on community exploration.
To support the exploration of future instrument ideas an extensive investigation of the ability of the observatory to support polarimetric observing modes was carried out. The science limitiations and abilities were explored and it was determined that there are many potential science programs that could be carried out if suitable polarimetric instrumentation is developed even though the fundamental polarimetric precision with TMT is affected by the three mirror design.
Community explorations were formally started in September, 2017 with a call for TMT Instrumentation White Papers (deadline for submission was March 21, 2018). In addition, the 2017 TMT Science Forum, held in Mysore, India, was dedicated to forming the teams to kick off the concept studies for the next generation of TMT instruments. Some of these teams have existed and been active over the previous few years and their specific instrument concepts were explored at the 2017 TMT Science Forum:
An outcome of the 2017 Forum was to respond to the call for White Papers on TMT next generation instrumentation, which will lead to launching feasibilities studies (subject to availability of funding) later in 2018 for all concepts ranked as top-priority by the TMT Science Advisory Committee. The list on the left includes a mix of well established instrument concepts as well as several more novel but exciting concepts.