TMT is the largest telescope project to be built at Mauna Kea, Hawaii. Countries to be contributing for this project are the USA ( NASA ), India ( ISRO ), Japan ( NAOJ ), China ( NAOC ), and Universities of Canada. The project's estimated cost would be around 1.3 billion and all the countries will contribute for this and will have benefits for future space missions.
Features
As information collected from www.tmt.org, the instruments used in this observatory are:
HROS (High-Resolution Optical Spectrometer)
A single-object, seeing-limited, high-resolution (R = 50000 for 1 arc sec slit) optical-UV Echelle spectrograph in the heritage of HIRES at Keck and UVES at the VLT.
IRMOS (Infrared Multi object Spectrometer)
designed to use multi-object adaptive optics (MOAO) techniques over a 5 arcmin field of regard to feed up to 20 deployable IFUs.
MIRES (Mid-Infrared Echelle Spectrometer)
Is a diffraction-limited, high-resolution (5000 < R < 100000) spectrometer and imager operating at 8 – 18 µm. It will employ a separate AO system optimized for the mid-infrared.
NIRES (Near-Infrared Echelle Spectrometer)
Fed by NFIRAOS, NIRES is a diffraction-limited highresolution (20 000 < R < 100 000) spectrometer covering 1 – 2.4 µm simultaneously. It is a scientific descendant of NIRSPEC at Keck and CRIRES at the VLT.
PFI (Planet Formation Instrument)
an extreme AO high contrast exoplanet imager with spectroscopic (R ≤ 100) capability. The first generation system will obtain 106 (goal: 107) contrasts while the second generation requirement is 108(goal: 109) in H-band for R < 8 mag. PFI is intended to be deployed after GPI at Gemini and SPHERE at the VLT so that lessons learned from those pathfinder high-contrast imagers can be fed back into PFI. Indeed, there is a large overlap between the GPI and PFI development teams.
WIRC (Wide Field InfraRed Camera)
a moderate field near infrared imager configuration fed by NFIRAOS to provide near diffraction-limited images through a variety of filters with high photometric and astrometric accuracy. WIRC is expected to deliver Nyquist sampled images (λ/2D = 0.004 arcsec) over a 30 arcsec diameter field-of-view with wavelength coverage 0.8 – 2.5 µm (goal: 0.6 – 5 µm).
This observatory can be used for tests for the standard model of particle physics. The tests and researches for the Higgs Boson can be conducted here, at Hawaii. From this observatory, formations of galaxies and universe can be studied and their characteristics can be observed. Using the speed of light, from this observatory, we can see distances of 13 billion light years so we can see how galaxies evolved. We can also find other terrestrial planets, where life can exist.
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See the following video from You tube what this project looks like:
Article By - M. Santosh
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