The European Extremely Large Telescope (E-ELT) is a revolutionary scientific project for a 40m-class telescope that will allow us to address many of the most pressing unsolved questions about our Universe.
The E-ELT will be the largest optical/near-infrared telescope in the world and will gather 13 times more light than the largest optical telescopes existing today. The E-ELT will be able to correct for the atmospheric distortions (i.e., fully adaptive and diffraction-limited) from the start, providing images 16 times sharper than those from the Hubble Space Telescope. The E-ELT will vastly advance astrophysical knowledge by enabling detailed studies of planets around other stars, the first galaxies in the Universe, super-massive black holes, and the nature of the Universe’s dark sector.
The Giant Magellan Telescope will be one member of the next class of super giant earth-based telescopes that promises to revolutionize our view and understanding of the universe. Commissioning of the telescope is scheduled to begin in 2021.
The GMT has a unique design that offers several advantages. It is a segmented mirror telescope that employs seven of today’s largest stiff monolith mirrors as segments. Six off-axis 8.4 meter or 27-foot segments surround a central on-axis segment, forming a single optical surface 24.5 meters, or 80 feet, in diameter with a total collecting area of 368 square meters. The GMT will have a resolving power 10 times greater than the Hubble Space Telescope. The GMT project is the work of a distinguished international consortium of leading universities and science institutions.
The goal of the Large Synoptic Survey Telescope (LSST) project is to conduct a 10-year survey of the sky that will deliver a 200 petabyte set of images and data products that will address some of the most pressing questions about the structure and evolution of the universe and the objects in it.
The construction phase of the project will deliver the facilities needed to conduct the survey: a large-aperture, wide-field, optical imaging telescope, a giga-pixel camera, and a data management system.
KASI is building a network of wide-field photometric survey systems called Korea Microlensing Telescope Network (KMTNet), funded by the government of Korea, in the southern hemisphere (Chile, South Africa, and Australia).
The primary scientific goal of the KMTNet project is to discover extrasolar planets with the main focus on discovering earth-mass planets in habitable zone using gravitational microlensing technique. The purpose of having three telescopes in three different time zone is to have a 24-hour uninterrupted monitoring of the night sky sources in the southern hemisphere.
The CTA project is an initiative to build the next generation ground-based very high energy gamma-ray instrument. It will serve as an open observatory to a wide astrophysics community and will provide a deep insight into the non-thermal high-energy universe.
The design foresees a factor of 5-10 improvement in sensitivity in the current very high energy gamma ray domain of about 100 GeV to some 10 TeV, and an extension of the accessible energy range from well below 100 GeV to above 100 TeV.
CCAT will be a 25-meter telescope for submillimeter astronomy that will combine high sensitivity, a wide field of view, and a broad wavelength range to provide an unprecedented capability for deep, large-area, multicolor submillimeter surveys. Instrumentation will include bolometer cameras, direct detection spectrometers, and heterodyne receiver arrays.
QUIET is a Project for very sensitive CMB polarization measurements . It will have arrays of detectors at two frequencies: 91-element array at 90 GHz and a 19-element array at 40 GHz.
The Cosmology Large-Angular Scale Surveyor (CLASS) is an instrument designed to test the “inflation” theory of the first trillionth of a trillionth of a second of the universe. In the most compelling verions of Inflation, gravitational waves are generated in the first moments of the universe.
CLASS is designed to search for this pattern Polarization will be measured over very large regions of the sky with radiometers at 40 GHz, 90 GHz, and 150/220 GHz.
Following completion of observations with POLARBEAR-1, two more 3.5 meter diameter Huan Tran Telescopes will be deployed at UCSD’s James Ax Observatory. This project, known as the “Simons Array”, will include more than 20,000 “POLARBEAR-2 style detectors, cooled nearly to absolute zero. The Simons Array will provide an unmatched combination of mapping speed, frequency, and sky coverage.