|
High on the Chajnantor plateau in the Chilean Andes, the European Southern Observatory (ESO), together with its international partners, is operating the Atacama Large Millimeter/submillimeter Array (ALMA) – a state-of-the-art telescope to study light from some of the coldest objects in the Universe. This light has wavelengths of around a millimetre, between infrared light and radio waves, and is therefore known as millimetre and submillimetre radiation. ALMA comprises 66 high-precision antennas, spread over distances of up to 16 kilometers (10 miles). This global collaboration is the largest ground-based astronomical project in existence.
Millimetre and submillimetre radiation opens a window into the enigmatic cold Universe, but the signals from space are heavily absorbed by water vapour in the Earth’s atmosphere. Telescopes for this kind of astronomy must be built on high, dry sites, such as the 5,000-meter (17,000-feet) high plateau at Chajnantor, one of the highest astronomical observatory sites on Earth.
The ALMA site, some 50 kilometers (31 miles) east of San Pedro de Atacama in northern Chile, is in one of the driest places on Earth. Astronomers find unsurpassed conditions for observing, but they must operate a frontier observatory under very difficult conditions. Chajnantor is more than 750 meters (2,500 feet) higher than the observatories on Mauna Kea, and 2,400 meters (7,900 feet) higher than the VLT on Cerro Paranal. More…, how does ALMA works? and about the facilities.
Special thanks to David Rabanus, the director Pierre Cox and his assistant Daphne Elliott-Patterson for organizing my 2014 visit.
Please also visit the ESO Ultra HD Expedition blog by my friends Babak Tafreshi and Christoph Malin.
Click on thumbnails for a larger version
|
|
Français
Llano de Chajnantor ALMA Observatory, Chile
', 'A climb of the Purico volcano at 5,300 meters (17,400 feet) was mandatory to take this picture of the ALMA antennas from a distance of about 5 kimometers (2.7 miles). A few of the 66 12-meter antennas and Array Operations Site (AOS) are visible.', 'en', 1);)
', 'A climb of the Purico volcano at 5,300 meters (17,400 feet) was mandatory to take this picture of the ALMA antennas from a distance of about 5 kimometers (2.7 miles). The 66 12-meter antennas and Array Operations Site (AOS) are visible.', 'en', 1);)
 is a 10-meter antenna built as a preprototype for ALMA.<br>The ASTE was deployed to its site on Pampa La Bola, near Cerro Chajnantor and the Llano de Chajnantor Observatory. The antenna shows excellent performance including a surface accuracy of 19µm (0.00075 inches) r.m.s.. The telescope is remotely controllable from multiple sites through satellite connections and the Internet. It is operated by the National Astronomical Observatory of Japan and the University of Tokyo, Nagoya University, and Osaka Prefecture University, in cooperation with the Universidad de Chile.', 'en', 1);)
;)
;)
;)
, a six-meter telescope designed to make high-resolution, microwave-wavelength surveys of the sky in order to study the Cosmic Microwave Background Radiation (CMB). At an altitude of 5,190 meters (17,030 feet), it’s one of the highest permanent, ground-based telescopes in the world.', 'en', 1);)
;)
;)
 technical building started in October 2005 and the outer shell was completed by mid 2006. Inside construction work was completed in summer 2007. Human operations at the AOS will be limited to an absolute minimum, due to the high altitude at 5,000 meters (16,500 feet). The AOS technical building houses the receiving end of the back end and the correlator, ALMA’s brain. It is basically a supercomputer designed especially for ALMA whose only purpose is to take the signals coming from its manifold antennas and to combine them, in order to generate astronomic data for subsequent analysis. The correlator multiplies the signals from the various antennas and saves the data to files known as Visibilities, which contain all the information necessary to form a 2-D image of the region of the sky observed (in addition to providing spectral information, that is, the capacity to form simultaneous images at thousands of consecutive frequencies). The process of passing from the Visibilities to a scientific image requires a number of calibration and reduction stages for which a specialized data reduction program has been devised. Digitized signals received from the radio telescopes are processed here and further transmitted to the data storage facilities located at the Operations Support Facility (OSF).', 'en', 1);)
;)
;)
Guest Book
