What is ALMA?
High on the Chajnantor plateau in the Chilean Andes, the European Southern Observatory (ESO), together with its international partners, is building 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 will be composed of 66 high-precision antennas, spread over distances of up to 16 kilometres. This global collaboration is the largest ground-based astronomical project in existence.
What is submillimetre astronomy?
Light at these wavelengths comes from vast cold clouds in interstellar space, at temperatures only a few tens of degrees above absolute zero, and from some of the earliest and most distant galaxies in the Universe. Astronomers can use it to study the chemical and physical conditions in molecular clouds — the dense regions of gas and dust where new stars are being born. Often these regions of the Universe are dark and obscured in visible light, but they shine brightly in the millimetre and submillimetre part of the spectrum.
Why build ALMA in the high Andes?
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 5000-m high plateau at Chajnantor, one of the highest astronomical observatory sites on Earth.
The ALMA site, some 50 km 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 m higher than the observatories on Mauna Kea, and 2400 m higher than the VLT on Cerro Paranal.
A Tour at the Chajnantor Plateau
Click on the image to take a Virtual Tour in and nearby Chajnantor.
ALMACam LIVE AOS.
ALMACam LIVE OSF.
To visit the ALMA Site, please see Media Visits
Why is ALMA an interferometer?
ALMA will be a single telescope of revolutionary design, composed initially of 66 high-precision antennas, and operating at wavelengths of 0.32 to 3.6 mm. Its main 12-metre array will have fifty antennas, 12 metres in diameter, acting together as a single telescope — an interferometer. An additional compact array of four 12-metre and twelve 7-metre antennas will complement this. The 66 ALMA antennas can be arranged in different configurations, where the maximum distance between antennas can vary from 150 metres to 16 kilometres, which will give ALMA a powerful variable “zoom”. It will be able to probe the Universe at millimetre and submillimetre wavelengths with unprecedented sensitivity and resolution, with a vision up to ten times sharper than the Hubble Space Telescope, and complementing images made with the VLT Interferometer.
Science with ALMA
ALMA is the most powerful telescope for observing the cool Universe — molecular gas and dust as well as the relic radiation of the Big Bang. ALMA will study the building blocks of stars, planetary systems, galaxies and life itself. By providing scientists with detailed images of stars and planets being born in gas clouds near our Solar System, and detecting distant galaxies forming at the edge of the observable Universe, which we see as they were roughly ten billion years ago, it will let astronomers address some of the deepest questions of our cosmic origins.
ALMA's construction will be completed in 2013, but early scientific observations with a partial array began in 2011. See press release eso1137 for more information.
The ALMA project is a partnership of Europe, North America and East Asia in cooperation with the Republic of Chile. ALMA is funded in Europe by ESO, in North America by the U.S. National Science Foundation (NSF) in cooperation with the National Research Council of Canada (NRC) and the National Science Council of Taiwan (NSC) and in East Asia by the National Institutes of Natural Sciences (NINS) of Japan in cooperation with the Academia Sinica (AS) in Taiwan. ALMA construction and operations are led on behalf of Europe by ESO, on behalf of North America by the National Radio Astronomy Observatory (NRAO), which is managed by Associated Universities, Inc. (AUI) and on behalf of East Asia by the National Astronomical Observatory of Japan (NAOJ). The Joint ALMA Observatory (JAO) provides the unified leadership and management of the construction, commissioning and operation of ALMA.
Star formation, molecular clouds, early Universe.
More about the ALMA Observatory
- ALMA Antennas
- ALMA Transporters
- ALMA and Interferometry
- More interesting facts are available on the FAQs page
- Read more about this observatory on the ALMA Handout in PDF format
- Images taken with ALMA
- Images of ALMA
- More ALMA Image Archive and ALMA Video Archive are available in the ESO multimedia archive
- For scientists: for more detailed information, please visit our technical pages
- Visit the ALMA Observatory website
- ESO press releases with results from ALMA
The ALMA Planetarium Show
"In search of our Cosmic Origins" is an inspiring show, introducing ALMA, the largest astronomical project in existence. Read more at the Cosmic Origins website.
Download this trailer in other formats from the Video Archive.
|Name:||Atacama Large Millimeter/submillimeter Array|
|Altitude:||4576 to 5044m (most above 5000 m)|
|Type:||Sub-millimeter interferometer antenna array|
|Diameter. Primary M1:||54 x 12.0 m (AEM, Vertex, and MELCO) and 12 x 7.0 m (MELCO)|
|Material. Primary M1:||CFRP and Aluminium (12-metre),
Steel and Aluminium (7-metre)
|Diameter. Secondary M2:||0.75 m (for 12-metre antennas);
0.457 m (for 7-metre antennas)
|Material. Secondary M2:||Aluminium|
|First Light date:||30 September 2011|
|Interferometry:||Baselines from 150 m to 16 km|
Stars form in dense clouds of the interstellar medium, but even in these densest regions the pressure is comparable to the most tenuous vacuum created in a laboratory on Earth. In these clouds, the temperatures are below -200 degrees Celsius.
ALMA is located in the southern hemisphere, but it is close enough to the Equator to be able to observe 73% of the northern sky, and 87% of the sky overall.
When astronomers combine the light waves from two telescopes using the principle of interferometry, they can very precisely determine the direction of an object in space. Your ears work in a similar way to localise sounds, by comparing the sound received at the left and right ears.
The skies over the ESO sites in Chile are so dark that on a clear moonless night it is possible to see your shadow cast by the light of the Milky Way alone.
There is an Earth-mass of alcohol near the centre of our Milky Way. However, most of it is methanol, and it is diluted 1:1000 with water. Telescopes observing at millimetre and submillimetre wavelengths, like APEX and soon ALMA, are used to detect many other molecules in space.
The two ALMA transporters each weigh 132.5 tonnes and have twin engines each rated at 500 kW each (at sea level). This gives a total of about 1400 horsepower, and is equivalent to about 20 "Smart Fortwo" cars.
ALMA on Google Maps