Large Telescopes

Región de Antofagasta. Chajnantor Plateau

ALMA is an interferometer that consists of a giant array of 12-m antennas (the 12-m array), with baselines up to 16 km, and an additional compact array of 7-m and 12-m antennas to greatly enhance ALMA’s ability to image extended targets, it observes at wavelengths in the range 3 mm to 400 μm (84 to 720 GHz).

CBI is an instrument designed to make images of the CMB radiation and to measure its statistical properties on angular scales from 5 arcmin to one degree. It is a 13-element interferometer mounted on a 6 meter platform operating in ten 1-GHz frequency bands from 26 GHz to 36 GHz.

APEX is a 12-m diameter telescope, operating at millimetre and submillimetre wavelengths — between infrared light and radio waves. Submillimetre astronomy opens a window into the cold, dusty and distant Universe, but the faint signals from space are heavily absorbed by water vapour in the Earth’s atmosphere.

This is the pilot telescope for the TAO Project. Is a1.0-m infrared telescope located at an altitude of 5640 m.

Región de Antofagasta. Cerro Toco

The ACT is a custom 6-m telescope . The goals of the project are to study how the universe began, what it is made of, and how it evolved to its current state. For that ACT observes simultaneously in three frequency bands centered on 148 GHz, 218 GHz, and 277 GHz.

The Huan Tran Telescope has 3.5-m in diameter. The Polarbear instrument is a state of the art fusion of optics and silicon. Virtually every component was designed for the sole purpose of producing a high fidelity map of CMB polarization.

Región de Antofagasta. Pampa la Bola

ASTE is a project to operate a high precision 10-m submillimeter telescope. One of its major goals is to explore the southern sky with waves up to 900 GHz

Equipped with a 4 m submillimeter telescope, NANTEN2 is used to survey the southern sky in molecular and atomic spectral lines between 110 and 880 GHz (2.6 mm to 350 micron wavelength)

Región de Antofagasta. Cerro Paranal

The VLT is composed by four Unit Telescopes (UTs) of 8.2-m diameter that operate individually using a large collection of instruments. The VLT offers also the possibility of combining the light from the four UTs to work as an interferometer (VLTI). In addition to the 8.2-m diameter telescopes the VLTI is complemented by four Auxiliary Telescopes (AT) of 1.8-m diameter to improve its imaging capabilities.

VISTA works at near-infrared wavelengths and its main mirror is 4.1-m across. At the heart of the telescope is a three-tone camera with 16 state-of-the-art infrared-sensitive detectors.

The VST  is the largest telescope in the world designed for surveying the sky in visible light. It has a 2.6-m mirror and a 268-megapixel camera called OmegaCAM.

Región de Atacama. Cerro Las Campanas

The Magellan Telescopes are 6.5-m twins called Baade and Clay. The Baade telescope hosts the following instruments: The Inamori Magellan Areal Camera and Spectrograph (IMACS), the FourStar wide field near-infrared camera and the FIRE (Folded port InfraRed Echellette) spectrograph. The Clay Telescope hosts: The Magellan Inamori Kyocera Echelle (MIKE), the MagE (Magellan Echellette) Spectrograph, the Low Dispersion Survey Spectrograph (LDSS-3), and a large mosaic CCD camera with a 24′ x 24′ field-of-view (Megacam).

The Irénée du Pont is a 2.5-m telescope. It was designed to have an exceptionally wide field for direct photography

The Henrietta Swope is a 1.0-m reflector telescope. It has a 4kx4k direct ccd camera.

Región de Coquimbo. Cerro Tololo

The wide field of the Blanco telescope, uses instruments such as: Dark Energy Camera (DECam), a high-performance wide-field CCD with 520 Mpix; The Infrared Side Port Imager (ISPI); COSMOS imager and spectrograph; and The Hydra multi-object spectrograph

he SMARTS consortium operates the 1.5-m, 1.3-m, 1.0-m and 0.9-m telescopes on Cerro Tololo. The 1.5-m hosts CHIRON , a highly stable fiber-fed cross-dispersed echelle spectrometer. The 1.3-m hosts A Novel Dual Imaging CAMera (ANDICAM) that takes simultaneous optical and infrared data. The 1.0-m hosts  Y4KCam an optical CCD optimized for wide-field broad-band imaging. The 0.9-m hosts 2KCCD.

LCOGT has three 1.0-m telescopes as part of their international network that also includes sites in: Haleakala, McDonald Observatory, Teide Observatory, Sutherland, Ali Observatory and Siding Spring.

Región de Coquimbo. Cerro Pachón

Gemini South is a  8.1-m diameter telescope with a twin on the summit of  Mauna Kea. Each telescope has a suite of instruments covering the optical and ground-accessible infrared wavelength regions. Several instruments are simultaneously mounted at the Cassegrain focus, giving the observatory great flexibility in adapting to changing weather conditions, observing multiple programs requiring different instruments in one night, and making time-critical measurements including responding within minutes to notifications to observe rapid transients such as gamma-ray bursts.

SOAR Telescope is a 4.1 meter aperture telescope designed to work from the atmospheric cut-off in the blue (320 nm) to the near infrared, with excellent optical image quality, The telescope uses active optics on its primary and secondary mirrors.

Región de Coquimbo. Cerro La Silla

It is an optical and near-infrared telescope that hosts the High Accuracy Radial velocity Planet Searcher (HARPS) that is dedicated to the discovery of extrasolar planets. It is a fiber-fed high resolution echelle spectrograph.

The NTT is a 3.58-m Richey-Chretien telescope which pioneered the use of active optics. The telescope and its enclosure had a revolutionary design for optimal image quality.

It is an optical and near-infrared telescope that hosts three instruments: the 67-million pixel Wide Field Imager; GROND, the Gamma-Ray Burst Optical/Near-Infrared Detector,; and the high-resolution spectrograph, FEROS, used to make detailed studies of stars.

t is operated by the Geneva Observatory, Université de Genève (Switzerland). It is used in conjunction with the CORALIE spectrograph to conduct high precision radial velocity measurements principally to search for large exoplanets.

The Danish telescope is a spectrographic telescope that is equipped with the Danish Faint Object Spectrograph and Camera spectrograph.

This 1971 telescope hosts a new large camera to conduct a southern hemisphere search for new Pluto-sized dwarf planets and supernovae: the LaSilla–QUEST Variability survey. The camera is a mosaic of 112 CCDs, with a total of 160 million pixels, covering the full field of view of the telescope.

This 1-m photometric telescope is used by a collaboration between the Bochum and UCN-Antofagasta universities.