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Llano de Chajnantor Observatory is the name for a group of astronomical observatories located at an altitude of over 4,800 m (15,700 ft) in the Atacama Desert of northern Chile. The site is in the Antofagasta Region approximately 50 kilometres (31 mi) east of the town of San Pedro de Atacama .
Llano de Chajnantor Observatory, Atacama Desert, Chile 6 m telescope located on Cerro Toco. Atacama Large Millimeter Array (ALMA) Llano de Chajnantor Observatory, Atacama Desert, Chile 35-950 GHz [51] 54 dishes with 12-m diameter and 12 dishes with 7 m diameter, sensitive to wavelengths between radio and infrared (submillimetre astronomy).
The array has been constructed on the 5,000 m (16,000 ft) elevation Chajnantor plateau – near the Llano de Chajnantor Observatory and the Atacama Pathfinder Experiment. This location was chosen for its high elevation and low humidity, factors which are crucial to reduce noise and decrease signal attenuation due to Earth's atmosphere. [1]
The Atacama Pathfinder Experiment (APEX) is a radio telescope 5,064 meters above sea level, at the Llano de Chajnantor Observatory in the Atacama Desert in northern Chile, 50 km east of San Pedro de Atacama built and operated by three European research institutes.
View looking northeast across the Llano de Chajnantor and the first two ALMA antennas in late 2009, with Cerro Chajnantor rising above at right. The Indian Astronomical Observatory stands at an altitude of 4,500 m (14,800 ft) on Mount Saraswati in Ladakh, India.
Puna de Atacama, San Antonio de los Cobres, Salta, Argentina Coordinates 24°11′31″S 66°28′29″W / 24.19206°S 66.47483°W / -24.19206; -66
The Cosmic Background Imager (or CBI) was a 13-element interferometer perched at an elevation of 5,080 metres (16,700 feet) at Llano de Chajnantor Observatory in the Chilean Andes. It started operations in 1999 to study the cosmic microwave background radiation and ran until 2008.
The Atacama B-Mode Search (ABS) was an experiment to test the theory of cosmic inflation and distinguish between inflationary models of the very early universe by making precise measurements of the polarization of the Cosmic Microwave Background (CMB).