World Library  
Flag as Inappropriate
Email this Article

Atacama Large Millimeter Array

Atacama Large Millimeter/submillimeter Array
ALMA logo
Organisation Multi-national
Location(s) Llano de Chajnantor Observatory
Atacama Desert, Chile
Altitude 5,058.7 m (16,597 ft)
Telescope style at least 50 12-m (39 ft) reflectors connected by fiber-optic cables
Website Official ALMA site
Official NRAO ALMA site
Official ESO ALMA site
Official NAOJ ALMA site

The Atacama Large Millimeter/submillimeter Array (ALMA) is an astronomical interferometer of radio telescopes in the Atacama desert of northern Chile. Since a high and dry site is crucial to millimeter wavelength operations, the array has been constructed on the Chajnantor plateau at 5,000 meters altitude, near Llano de Chajnantor Observatory and Atacama Pathfinder Experiment. Consisting of 66 12-meter (39 ft), and 7-meter (23 ft) diameter radio telescopes observing at millimeter and submillimeter wavelengths, ALMA is expected to provide insight on star birth during the early universe and detailed imaging of local star and planet formation.

ALMA is an international partnership among Europe, the United States, Canada, East Asia and the Republic of Chile. Costing about US$1.4 billion, it is the most expensive ground-based telescope in operation.[1][2] ALMA began scientific observations in the second half of 2011 and the first images were released to the press on 3 October 2011. The array has been fully operational since March 2013.[3][4]


  • Overview 1
    • History 1.1
  • Funding 2
  • Assembly 3
    • Transporting antennas to the site 3.1
  • Scientific results 4
    • Images from initial testing 4.1
    • Comet studies 4.2
    • Planetary formation 4.3
  • Global collaboration 5
  • ALMA regional centre (ARC) 6
  • Project detail 7
    • Atacama Compact Array 7.1
  • Work stoppage 8
  • Project timeline 9
  • Videos and gallery 10
  • See also 11
  • References 12
  • External links 13


The first two ALMA antennas linked together as an interferometer
The ALMA correlator

The initial ALMA array will be composed of 66 high-precision antennas, and operate at wavelengths of 0.3 to 9.6 mm. The array will have much higher sensitivity and higher resolution than existing submillimeter telescopes such as the single-dish James Clerk Maxwell Telescope or existing interferometer networks such as the Submillimeter Array or the Institut de Radio Astronomie Millimétrique (IRAM) Plateau de Bure facility.

The antennas can be moved across the desert plateau over distances from 150 m to 16 km, which will give ALMA a powerful variable "zoom", similar in its concept to that employed at the Very Large Array (VLA) site in New Mexico, United States.

The high sensitivity is mainly achieved through the large numbers of telescopes that will make up the array.

The telescopes are provided by the European, North American and East Asian partners of ALMA. The American and European partners have each placed orders for twenty-five 12-meter diameter antennas, that will compose the main array. East Asia is contributing 16 antennas (four 12-meter diameter and twelve 7-meter diameter antennas) in the form of the Atacama Compact Array (ACA), which is also part of the enhanced ALMA.

By using smaller antennas than the main ALMA array, larger fields of view can be imaged at a given frequency using ACA. Moving the antennas closer together will enable the imaging of sources of larger angular extent. The ACA will work together with the main array in order to enhance the latter's wide-field imaging capability.


On 4 March 2011, ten Antennas are installed at Chajnantor.

ALMA has its conceptual roots in three astronomical projects — the Millimeter Array (MMA) of the United States, the Large Southern Array (LSA) of Europe, and the Large Millimeter Array (LMA) of Japan.

The first step toward the creation of what would become ALMA came in 1997, when the NRAO (National Radio Astronomy Observatory) and the ESO (European Southern Observatory) agreed to pursue a common project that merged the MMA and LSA. The merged array combined the sensitivity of the LSA with the frequency coverage and superior site of the MMA. ESO and NRAO worked together in technical, science, and management groups to define and organize a joint project between the two observatories with participation by Canada and Spain (the latter became a member of ESO later).

A series of resolutions and agreements led to the choice of "Atacama Large Millimeter Array", or ALMA, as the name of the new array in March 1999 and the signing of the ALMA Agreement on February 25, 2003, between the North American and European parties. ("Alma" means "soul" in Spanish and "learned" or "knowledgeable" in Arabic.) Following mutual discussions over several years, the ALMA Project received a proposal from the NAOJ (National Astronomical Observatory of Japan) whereby Japan would provide the ACA (Atacama Compact Array) and three additional receiver bands for the large array, to form Enhanced ALMA. Further discussions between ALMA and NAOJ led to the signing of a high-level agreement on September 14, 2004 that makes Japan an official participant in Enhanced ALMA, to be known as the Atacama Large Millimeter/submillimeter Array. A groundbreaking ceremony was held on November 6, 2003 and the ALMA logo was unveiled.[5]

During an early stage of the planning of ALMA, it was decided to employ ALMA antennas designed and constructed by known companies in North America, Europe and Japan, rather than using one single design. This was mainly for political reasons. Although very different approaches have been chosen by the providers, each of the antenna designs appears to be able to meet ALMA's stringent requirements.


ALMA was initially a 50-50 collaboration between the National Radio Astronomy Observatory and European Southern Observatory (ESO) and later extended with the help of the other Japanese, Taiwanese, and Chilean partners.[6] ALMA is the largest and most expensive ground-based astronomical project, costing between US$1.4 and 1.5 billion.[1][7] (However, various space astronomy projects including Hubble Space Telescope, JWST and several major planet probes have cost considerably more).



The complex was built primarily by European, U.S., Japanese and Canadian companies and universities. Three prototype antennas have undergone evaluation at the Very Large Array site in New Mexico since 2002.

General Dynamics C4 Systems and its SATCOM Technologies division was contracted by Associated Universities, Inc. to provide twenty-five of the 12m antennas,[8] while European manufacturer Thales Alenia Space provided the other twenty-five principal antennas[9] (in the largest-ever European industrial contract in ground-based astronomy). The first antenna was delivered in 2008, the last in 2011.

Progress at the ALMA Operations Support Facility - a panoramic view.

Transporting antennas to the site

Transporting the 115 tonne antennas from the Operations Support Facility at 2900 m altitude to the site at 5000 m presented enormous challenges; as portrayed in the television documentary Monster Moves: Mountain Mission.[10] The solution chosen was to use two custom 28-wheel self-loading heavy haulers. The vehicles were made by Scheuerle Fahrzeugfabrik in Germany and were 10 m wide, 20 m long and 6 m high, weighing 130 tonnes. They were powered by twin turbocharged 500 kW Diesel engines.

The transporters, which featured a driver's seat designed to accommodate an oxygen tank to aid breathing the thin high-altitude air, placed the antennas precisely at the site. The first vehicle was completed and tested in July 2007.[11] Both transporters were delivered to the ALMA Operations Support Facility (OSF) in Chile on February 15, 2008.

On July 7, 2008 an ALMA transporter moved an antenna for the first time, from inside the antenna assembly building (Site Erection Facility) to a pad outside the building for testing (holographic surface measurements). The antenna was of the North American VertexRSI design.[12]

During Fall, 2009 the first three antennas were transported one-by-one to the Array Operations Site. At the end of 2009, a team of ALMA astronomers and engineers successfully linked three of the observatory's advanced antennas at the 5,000-metre (16,000 ft) elevation observing site thus finishing the first stage of assembly and integration of the fledgling array. Linking three antennas to work in unison for the first time allowed the ALMA team to correct errors that can arise when only two antennas are used, thus paving the way for precise, high-resolution imaging. With this key step, commissioning of the instrument began January 22, 2010.

On July 28, 2011, the first European antenna for ALMA arrived at the Chajnantor plateau, 5000 meters above sea level, to join 15 antennas already in place from the other international partners. This was the number of antennas specified for ALMA to begin its first science observations, and was therefore an important milestone for the project.[13] In October 2012, 43 of the 66 antennas had been set up.

Scientific results

Images from initial testing

Antennae Galaxies composite of ALMA and Hubble observations

By the summer of 2011 sufficient telescopes were operational during the extensive program of testing prior to the Early Science phase for the first images to be captured.[14] These early images give a first glimpse of the potential of the new array that will produce much better quality images in the future as the scale of the array continues to increase.

The target of the observation was a pair of colliding galaxies with dramatically distorted shapes, known as the Antennae Galaxies. Although ALMA did not observe the entire galaxy merger, the result is the best submillimeter-wavelength image ever made of the Antennae Galaxies, showing the clouds of dense cold gas from which new stars form, which cannot be seen using visible light.

Comet studies

On 11 August 2014, astronomers released studies, using the Atacama Large Millimeter/submillimeter Array (ALMA) for the first time, that detailed the distribution of HCN, HNC, H2CO, and dust inside the comae of comets C/2012 F6 (Lemmon) and C/2012 S1 (ISON).[15][16]

Planetary formation

An image of the protoplanetary disk surrounding Hl Tauri (a very young T Tauri star[17] in the constellation Taurus) was made public in 2014, showing a series of concentric bright rings separated by gaps, indicating protoplanet formation. As of 2014, most theories did not expect planetary formation in such a young (100,000-1,000,000 years) system, so the new data spurred renewed theories of protoplanetary development. One theory suggests that the faster accretion rate might be due to the complex magnetic field of the protoplanetary disk.[18]

Global collaboration

The future ALMA array on Chajnantor (artist's rendering)

The Atacama Large Millimeter/submillimeter Array (ALMA), an international astronomy facility, is a partnership of Europe, North America and East Asia in cooperation with the Republic of Chile. ALMA is funded in Europe by the European Southern Observatory (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 of Japan (NINS) 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.

ALMA regional centre (ARC)

The ALMA regional centre (ARC) has been designed as an interface between user communities of the major contributors of the ALMA project and the JAO. Activates for operating the ARC have also divided into the three main regions involved (Europe, North America and East Asia). The European ARC (led by ESO) has been further subdivided into ARC-nodes [19] located across Europe in Bonn-Bochum-Cologne, Bologna, Ondřejov, Onsala, IRAM (Grenoble), Leiden and JBCA (Manchester).

The core purpose of the ARC is to assist the user community with the preparation of observing proposals, ensure observing programs meet their scientific goals efficiently, run a help-desk for submitting proposals and observing programs, delivering the data to principal investigators, maintenance of the ALMA data archive, assistance with the calibration of data and providing user feedback.[20]

Project detail

A starry night at the ALMA site.
2012 ALMA Video Compilation Released[21]
  • At least 50 antennas of 12 m diameter located at an elevation of 5,000 m at Llano de Chajnantor Observatory, enhanced by a compact array of 4 x 12 m and 12 x 7 m antennas (consortium currently considering to build 50 or 64 [3][4])
  • Imaging instrument in all atmospheric windows between 350 μm and 10 mm
  • Array configurations from approximately 150 m to 14 km
  • Spatial resolution of 10 milliarcseconds (10−7 radians), 10 times better than the Very Large Array (VLA) and 5 times better than the Hubble Space Telescope, but still considerably lower than the resolution achieved with optical and infrared interferometers.
  • The ability to image sources arcminutes to degrees across at one arcsecond resolution
  • Velocity resolution under 50 m/s
  • Faster and more flexible imaging instrument than the Very Large Array
  • Largest and most sensitive instrument in the world at millimeter and submillimeter wavelengths
  • Point source detection sensitivity 20 times better than the Very Large Array
  • Data Reduction system will be CASA (Common Astronomy Software Applications) which is a new software package based on AIPS++

Atacama Compact Array

The Atacama Compact Array

The Atacama Compact Array, ACA, is a subset of 16 closely separated antennas that will greatly improve ALMA’s ability to study celestial objects with a large angular size, such as molecular clouds and nearby galaxies. The antennas forming the Atacama Compact Array, four 12-meter antennas and twelve 7-meter antennas, were produced and delivered by Japan. In 2013 the Atacama Compact Array was named the Morita Array after Professor Koh-ichiro Morita, a member of the Japanese ALMA team and designer of the ACA, who died on 7 May 2012 in Santiago.[22]

Work stoppage

In August 2013, workers at the world’s largest radio telescope went on strike to demand better pay and working conditions. This is one of the first strikes to affect an astronomical observatory. The work stoppage began after the Observatory failed to reach an agreement with the workers' union.[23][24][25][26] After 17 days an agreement was reached providing for reduced schedules and higher pay for work done at high altitude.[27][28]

Project timeline

The final ALMA antenna.[29]
Date Activity
1995 ESO/NRAO/NAOJ joint site testing with Chile.
May 1998 Start of Phase 1 (Design & Development).
June 1999 European/U.S. Memorandum of Understanding for Design & Development.
February 2003 Final European / North American Agreement, with 50% of funding from ESO, and 50% of funding shared between USA and Canada.
April 2003 Testing of first prototype antenna begins at the ALMA Test Facility (ATF) site in Socorro, New Mexico.
November 2003 Groundbreaking ceremony at ALMA site.
September 2004 European, North American & Japanese draft agreement, with Japan providing new extensions to ALMA.
October 2004 Opening of Joint ALMA office, Santiago, Chile.
September 2005 Taiwan joins the ALMA Project through Japan.
July 2006 European, North American & Japanese amend agreement on the Enhanced ALMA.
April 2007 Arrival of first antenna in Chile.
February 2008 Arrival of the two ALMA transporters in Chile.
July 2008 First antenna movement with a transporter.
December 2008 Acceptance of the first ALMA antenna.
May 2009 First interferometry with two antennas at the Operations Support Facility (OSF).
September 2009 First move of an ALMA antenna to Chajnantor.
November 2009 Phase closure with three antennas at Chajnantor.
2010 Call for shared-risk Early Science proposals.
2011 September Start of Early Science Cycle 0. Sixteen 12-m antennas in the 12-m Array.
2013 January Start of Early Science Cycle 1. Thirty-two 12-m antennas in the 12-m Array.
2013 March 13 ALMA Inauguration.
2014 June Start of Early Science Cycle 2. Thirty-four 12-m antennas in the 12-m Array, nine 7-m antennas in the 7-m Array, and two 12-m antennas in the TP Array.

Videos and gallery

See also

Looking over to the ALMA site from APEX.
ALMA Site.
A Digital Highway to ALMA.[30]


  1. ^ a b "ALMA Inauguration Heralds New Era of Discovery". ESO - European Southern Observatory. 13 March 2013. Retrieved 29 April 2014. 
  2. ^ Romero, Simon (7 April 2012). "At the End of the Earth, Seeking Clues to the Universe". New York Times. Retrieved 8 April 2012. 
  3. ^ "Alma telescope: Ribbon cut on astronomical giant". BBC. Retrieved 13 March 2013. 
  4. ^ Spie (2014). "Pierre Cox plenary: ALMA Update". SPIE Newsroom.  
  5. ^ Alejandro Peredo. "Ground breaking ceremony for the Atacama Large Millimeter Array (ALMA)". Retrieved 15 November 2014. 
  6. ^ ALMA Partners
  7. ^ Chile's ALMA probes for origins of universe, Associated Press
  8. ^ GD - 2005
  9. ^ ESO - 2005
  10. ^ "Monster Moves, Season 5, Episode 6: Mountain Mission". Retrieved 17 March 2012. 
  11. ^ "Giant truck set for sky-high task". BBC News. 30 July 2007. Retrieved 31 July 2007. 
  12. ^ July 2008 NRAO ALMA newsletter article by Dr. Al Wootten
  13. ^ "European ALMA antenna brings total on Chajnantor to 16". ESO Organisation Release. 28 July 2011. Retrieved 29 July 2011. 
  14. ^ "ALMA Open its Eyes". ALMA Press Release. 3 October 2011. Retrieved 4 October 2011. 
  15. ^ Zubritsky, Elizabeth; Neal-Jones, Nancy (11 August 2014). "RELEASE 14-038 - NASA’s 3-D Study of Comets Reveals Chemical Factory at Work".  
  16. ^ Cordiner, M.A.; et al. (11 August 2014). "Mapping the Release of Volatiles in the Inner Comae of Comets C/2012 F6 (Lemmon) and C/2012 S1 (ISON) Using the Atacama Large Millimeter/submillimeter Array".  
  17. ^ Weintraub, David A.; Kastner, Joel H.; Whitney, Barbara A. (October 1995). "In Search of HL Tauri". The Astrophysical Journal Letters 452: L141–L145.  
  18. ^ Stephens, Ian W.; Looney, Leslie W.; Kwon, Woojin; Fernández-López, Manuel; Hughes, A. Meredith; et al. (October 2014). "Spatially resolved magnetic field structure in the disk of a T Tauri star".  
  19. ^ "ARC-nodes". Retrieved 15 November 2014. 
  20. ^ "ALMA regional centre". Retrieved 15 November 2014. 
  21. ^ "New 2012 ALMA Video Compilation Released". ESO Press Release. Retrieved 13 February 2013. 
  22. ^ "ALMA Compact Array Completed and Named After Japanese Astronomer". ESO Announcement. Retrieved 8 May 2013. 
  23. ^ Alejandro Peredo. "ALMA Observatory Statement". Retrieved 15 November 2014. 
  24. ^ Washington Post
  25. ^ "BBC News". BBC News. Retrieved 15 November 2014. 
  26. ^ "Huffington Post:". Retrieved 15 November 2014. 
  27. ^ "ALMA resumes operations after end of workers’ strike". Retrieved 11 May 2015. 
  28. ^ "17-Day ALMA Strike Ends in Resolution". Sky & Telescope. Retrieved 11 May 2015. 
  29. ^ "Final Antenna Delivered to ALMA". ESO Press Release. Retrieved 2 October 2013. 
  30. ^ "A Digital Highway to ALMA". ESO Press Release. Retrieved 13 February 2013. 

External links

  • Official ALMA site
  • NRAO ALMA site
  • UK ALMA site
  • ESO ALMA site
  • ALMA site by NAOJ
  • ALMA Antennas Collect First Data, ", 17 November 2009.
  • How the Huge ALMA Radio Telescope Works (Infographic),, 12 March 2013.
  • Into Deep Space: The Birth of the Alma Observatory
  • An optical system design for the Atacama Large Millimeter Array SPIE Newsroom, 5 June 2014.
  • CBS News' "60 Minutes" program, original broadcast on 9 March 2014, rebroadcast on 27 July 2014. Bob Simon is the correspondent. Michael Gavshon and David Levine, producers.

This article was sourced from Creative Commons Attribution-ShareAlike License; additional terms may apply. World Heritage Encyclopedia content is assembled from numerous content providers, Open Access Publishing, and in compliance with The Fair Access to Science and Technology Research Act (FASTR), Wikimedia Foundation, Inc., Public Library of Science, The Encyclopedia of Life, Open Book Publishers (OBP), PubMed, U.S. National Library of Medicine, National Center for Biotechnology Information, U.S. National Library of Medicine, National Institutes of Health (NIH), U.S. Department of Health & Human Services, and, which sources content from all federal, state, local, tribal, and territorial government publication portals (.gov, .mil, .edu). Funding for and content contributors is made possible from the U.S. Congress, E-Government Act of 2002.
Crowd sourced content that is contributed to World Heritage Encyclopedia is peer reviewed and edited by our editorial staff to ensure quality scholarly research articles.
By using this site, you agree to the Terms of Use and Privacy Policy. World Heritage Encyclopedia™ is a registered trademark of the World Public Library Association, a non-profit organization.

Copyright © World Library Foundation. All rights reserved. eBooks from Project Gutenberg are sponsored by the World Library Foundation,
a 501c(4) Member's Support Non-Profit Organization, and is NOT affiliated with any governmental agency or department.