Atacama Large Millimeter Array
|Location||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.12 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 2013.34
- 1 Overview
- 2 Funding
- 3 Assembly
- 4 Scientific results
- 5 Global collaboration
- 6 ALMA regional centre (ARC)
- 7 Project detail
- 8 Work stoppage
- 9 Project timeline
- 10 Videos and gallery
- 11 See also
- 12 References
- 13 External links
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.
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.17
- European Southern Observatory and the European Regional Support Centre
- National Science Foundation via the National Radio Astronomy Observatory and the North American ALMA Science Center
- National Research Council of Canada
- National Astronomical Observatory of Japan (NAOJ) under the National Institutes of Natural Sciences (NINS)
- ALMA-Taiwan at the Academia Sinica Institute of Astronomy & Astrophysics (ASIAA)
- Republic of Chile
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 antennas9 (in the largest-ever European industrial contract in ground-based astronomy). The first antenna was delivered in 2008, the last in 2011.
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.
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.
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).1516
An image of the protoplanetary disk surrounding Hl Tauri (a very young T Tauri star17 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[update], 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
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.
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
- 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 )
- 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++
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 suddenly passed away on 7 May 2012 in Santiago.22
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.23242526 After 17 days an agreement was reached providing for reduced schedules and higher pay for work done at high altitude.2728
|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.|
Video compilation showing various aspects of ALMA.
This artist's rendering of the ALMA array on the Chajnantor plateau shows how, as an interferometer, ALMA acts like a single telescope with a diameter as large as the distance between its individual antennas (represented by the blue circle).
A talk on the Atacama Large Millimeter/submillimeter Array (ALMA), by Leonardo Testi.
This video clip shows the distinguished guests, including the President of Chile, Sebastián Piñera, arriving at the ALMA Operations Support Facility (OSF), located at an altitude of 2900 meters in the Atacama Desert in Chile for the inauguration of the giant telescope. The guests are shown with one of the giant ALMA transporters as well as other components.
Share the excitement of the inauguration ceremony and contemplate the breathtaking images from ALMA itself and views of its unique environment in the Atacama Desert.
This 16-minute video presents the history of ALMA from the origins of the project several decades ago to the recent first science results. (in HD)
This video begins near the ground of the Chajnantor Plateau, at 5000 meters altitude in the Chilean Andes. The video camera being used is mounted to a hexacopter and as it begins its ascent we get a magnificent view of the 58 antennae that make up the Atacama Large Millimeter/submillimeter Array.
Time-lapse video at the ALMA Array Operations Site (AOS).
On 30 September 2013 the final ALMA antenna was handed over to the ALMA Observatory. This video shows the antenna being moved on the giant transporter called "Otto". The 12-meter-diameter dish was manufactured by the European AEM Consortium and also marks the successful delivery of a total of 25 European antennas — the largest ESO contract so far.
ALMA 2012 relocation compilation.
The final antenna for the project is here seen arriving to the high site at the observatory, 5000 meters above sea level.
ALMA antenna moves.
|Wikimedia Commons has media related to Atacama Large Millimeter Array.|
- Atacama Pathfinder Experiment (APEX), single dish submillimeter telescope built on a modified ALMA prototype antenna
- Atacama Submillimeter Telescope Experiment
- CARMA a sensitive millimeter-wave array operated by a consortium including Caltech, University of California Berkeley, University of Illinois, University of Maryland and University of Chicago
- Cosmic Background Imager a 13 element interferometer operating in Llano de Chajnantor since 1999.
- IRAM 30 Meter Telescope (Pico Veleta, Spain), the largest millimetric telescope in the world, operated by IRAM
- James Clerk Maxwell Telescope The most sensitive existing submillimeter telescope
- Plateau de Bure Interferometer, one of the most successful existing millimeter-wave arrays, operated by IRAM
- List of observatories
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- ALMA Partners
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- "ALMA Open its Eyes". ALMA Press Release. 3 October 2011. Retrieved 4 October 2011.
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- 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". The Astrophysical Journal 792 (1). doi:10.1088/2041-8205/792/1/L2. Retrieved 12 August 2014.
- Weintraub, David A.; Kastner, Joel H.; Whitney, Barbara A. (October 1995). "In Search of HL Tauri". The Astrophysical Journal Letters 452: L141–L145. Bibcode:1995ApJ...452L.141W. doi:10.1086/309720.
- 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". Nature 514 (7524): 597–599. arXiv:1409.2878. Bibcode:2014Natur.514..597S. doi:10.1038/nature13850.
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- Alejandro Peredo. "ALMA Observatory Statement". Retrieved 15 November 2014.
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- Official ALMA site
- NRAO ALMA site
- UK ALMA site
- ESO ALMA site
- ALMA site by NAOJ
- ALMA Antennas Collect First Data, "bbc.co.uk, 17 November 2009.
- How the Huge ALMA Radio Telescope Works (Infographic), Space.com, 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.
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