Aerial view of the Observatory
|Location||Arecibo, Puerto Rico|
|Wavelength||electromagnetic spectrum: (3.00 cm to 1.00 meter)|
|Built||Completed in 1963|
|Telescope style||spherical reflector|
|Diameter||1,000 ft (300 m)|
|Collecting area||73,000 square meters (790,000 sq ft)|
|Mounting||semi-transit telescope: fixed primary with secondary (Gregorian reflector) and a delay-line feed, each of which moves on tracks to point to different parts of the sky.|
National Astronomy and Ionosphere Center
|Area||118 acres (480,000 m2)|
|Architect||Gordon, William E; Kavanaugh, T.C.|
|NRHP Reference #||07000525|
|Added to NRHP||September 23, 2008|
The Arecibo Observatory is a radio telescope in the municipality of Arecibo, Puerto Rico. This observatory is operated by SRI International, USRA and UMET, under cooperative agreement with the National Science Foundation (NSF). This observatory is also called the National Astronomy and Ionosphere Center, although "NAIC" refers to both the observatory and the staff that operates it. From its construction in the 1960s until 2011, the observatory was managed by Cornell University.
The Observatory's 1,000 ft (305 m) radio telescope is the world's largest single-aperture telescope. It is used in three major areas of research: radio astronomy, atmospheric science, and radar astronomy. Scientists who want to use the Arecibo Telescope submit proposals that are evaluated by an independent scientific board.
The Radio Telescope has made appearances in motion picture and television productions, gaining more recognition in 1999 when it began to collect data for the SETI@home project. It has been listed on the American National Register of Historic Places beginning in 2008. It was the featured listing in the National Park Service's weekly list of October 3, 2008. The Center was named in IEEE Milestone in 2001. It has a visitors center that is open part time.
- 1 General information
- 2 Design and architecture
- 3 Research and discoveries
- 4 SETI / METI
- 5 Other uses
- 6 Funding concerns
- 7 Ángel Ramos Foundation Visitor Center
- 8 List of directors
- 9 In popular culture
- 10 See also
- 11 References
- 12 Further reading
- 13 External links
The main collecting dish is 1,000 ft (305 m) in diameter, constructed inside the depression left by a karst sinkhole. It contains the largest curved focusing dish on Earth, giving Arecibo the largest electromagnetic-wave-gathering capacity. The dish surface is made of 38,778 perforated aluminum panels, each about 3 by 6 feet (1 by 2 m), supported by a mesh of steel cables. The ground underneath is accessible and supports shade-tolerant vegetation.
The Radio Telescope is a spherical reflector, not a parabolic reflector. To aim the device, the receiver is moved to intercept signals reflected from different directions by the spherical dish surface. A parabolic mirror would have varying astigmatism when the receiver is off the focal point, but the error of a spherical mirror is the same in every direction.
The receiver is on a 900-ton platform suspended 150 m (500 ft) above the dish by 18 cables running from three reinforced concrete towers, one 110 m (365 ft) high and the other two 80 m (265 ft) high, placing their tops at the same elevation. The platform has a 93-meter-long rotating, bow-shaped track, called the azimuth arm, carrying the receiving antennas and secondary and tertiary reflectors. This allows the Telescope to observe any region of the sky in a forty-degree cone of visibility about the local zenith (between −1 and 38 degrees of declination). Puerto Rico's location near the Northern Tropic allows Arecibo to view the planets in the Solar System over the Northern half of their orbit. The round trip light time to objects beyond Saturn is longer than the 2.6 hour time that the telescope can track a celestial position, preventing radar observations of more distant objects.
Design and architecture
The origins of the Arecibo Observatory trace to late 1950s efforts to develop anti-ballistic missile (ABM) defences as part of the newly formed ARPA's ABM umbrella-effort, Project Defender. Even at this early stage it was clear that the use of radar decoys would be a serious problems at the long ranges needed to successfully attack a warhead, ranges on the order of 1,000 miles (1,600 km).
Among the many Defender projects were several studies based on the concept that a re-entering nuclear warhead would cause unique physical fingerprints while still in the upper atmosphere. It was known that hot, high-speed objects caused ionization of the atmosphere that created radar returns, and it appeared that a warhead's signature would be different enough from decoys that a detector could pick out the warhead directly, or alternately, provide additional information that would allow the operators to focus a conventional tracking radar on the single return from the warhead.
Although the concept appeared to offer a solution to the tracking problem, there was almost no information on either the physics of re-entry or a strong understanding of the normal composition of the upper layers of the ionosphere. ARPA began to address both simultaneously; to better understand the radar returns from a warhead a number of radars were build on Kwajalein Atoll, while another effort started with the dual-purpose of understanding the ionosphere's F-layer while also producing a general purpose scientific radio observatory.
The Arecibo Telescope was built between mid-1960 and November 1963 and designed by William E. Gordon of Cornell University, who intended to use it to study Earth's ionosphere. Originally, a fixed parabolic reflector was envisioned, pointing in a fixed direction with a 150 m (500 ft) tower to hold equipment at the focus. This design would have limited its use in other research areas, such as radar astronomy, radio astronomy and atmospheric science, which require the ability to point at different positions in the sky and track those positions for an extended period as the Earth rotates. Ward Low of the Advanced Research Projects Agency (ARPA) pointed out this flaw and put Gordon in touch with the Air Force Cambridge Research Laboratory (AFCRL) in Boston, Massachusetts, where one group headed by Phil Blacksmith was working on spherical reflectors and another group was studying the propagation of radio waves in and through the upper atmosphere. Cornell University proposed the project to ARPA in mid-1958 and a contract was signed between the AFCRL and the University in November 1959. Cornell University and Zachary Sears published a request for proposals (RFP) asking for a design to support a feed moving along a spherical surface 435 feet (133 m) above the stationary reflector. The RFP suggested a tripod or a tower in the center to support the feed. On the day the project for the design and construction of the antenna was announced at Cornell University, Gordon had also envisioned a 435 ft (133 m) tower centered in the 1,000 ft (300 m) reflector to support the feed.
George Doundoulakis, who directed research at General Bronze Corporation in Garden City, New York, along with Zachary Sears, who directed Internal Design at Digital B & E Corporation, New York, received the RFP from Cornell University for the antenna design and studied the idea of suspending the feed with his brother, Helias Doundoulakis, a civil engineer. George Doundoulakis identified the problem that a tower or tripod would have presented around the center, (the most important area of the reflector), and devised a better approach by suspending the feed. He presented his proposal to Cornell for a doughnut truss suspended by four cables from four towers above the reflector, having along its edge a rail track for the azimuthal feed's positioning. A second truss, in the form of an arc, or arch, was to be suspended below, which would rotate on the rails through 360 degrees. The arc also had rails on which the unit supporting the feed would move for the feed's elevational positioning. A counter-weight would move symmetrically opposite to the feed for stability and, if a hurricane struck, the entire feed could be raised and lowered. Helias Doundoulakis designed the cable suspension system which was finally adopted. Although the present configuration is substantially the same as the original drawings by George and Helias, (though with three towers instead of the original four), the U.S. Patent office granted Helias a patent, for the brothers' innovative idea. William J. Casey, who later became the director of the Central Intelligence Agency under President Ronald Reagan, was also an assignee on the patent.
Construction began in mid-1960, with the official opening on November 1, 1963. As the primary dish is spherical, its focus is along a line rather than at a single point (as would be the case for a parabolic reflector). As a result, complicated line feeds were implemented to carry out observations. Each line feed covered a narrow frequency band (2–5% of the center frequency of the band); a limited number of line feeds could be used at any one time, limiting the telescope's flexibility.
Since then, the Arecibo Telescope has been upgraded several times. Initially, when the maximum expected operating frequency was about 500 MHz, the surface consisted of half-inch galvanized wire mesh laid directly on the support cables. In 1974, a high-precision surface consisting of 40,000 of individually adjustable aluminum panels replaced the old wire mesh, and the highest usable frequency was raised to approximately 5000 MHz. A Gregorian reflector system was installed in 1997, incorporating secondary and tertiary reflectors to focus radio waves at a single point. This allowed the installation of a suite of receivers, covering the entire 1–10 GHz range, that could be easily moved to the focal point, giving Arecibo more flexibility. A metal screen was also installed around the perimeter to block the ground's thermal radiation from reaching the feed antennas. Finally, a more powerful 2400 MHz transmitter was added.
Research and discoveries
Many scientific discoveries have been made using the Arecibo Telescope. On April 7, 1964, shortly after it began operations, Gordon Pettengill's team used it to determine that the rotation rate of Mercury was not 88 days, as previously thought, but only 59 days. In 1968, the discovery of the periodicity of the Crab Pulsar (33 milliseconds) by Lovelace and others provided the first solid evidence that neutron stars exist. In 1974, Hulse and Taylor discovered the first binary pulsar PSR B1913+16, an accomplishment for which they later received the Nobel Prize in Physics. In 1982, the first millisecond pulsar, PSR B1937+21, was discovered by Donald C. Backer, Shrinivas Kulkarni, Carl Heiles, Michael Davis, and Miller Goss. This object spins 642 times per second, and until the discovery of PSR J1748-2446ad in 2005, was identified as the fastest-spinning pulsar.
In August 1989, the Observatory directly imaged an asteroid for the first time in history: 4769 Castalia. The following year, Polish astronomer Aleksander Wolszczan made the discovery of pulsar PSR B1257+12, which later led him to discover its three orbiting planets and possible comet. These were the first extrasolar planets discovered. In 1994, John Harmon used the Arecibo Radio Telescope to map the distribution of ice in the poles of Mercury.
In January 2008, detection of prebiotic molecules methanimine and hydrogen cyanide were reported from the Arecibo Observatory radio spectroscopy measurements of the distant starburst galaxy Arp 220.
SETI / METI
The Arecibo Message
In 1974, the Arecibo message, an attempt to communicate with potential extraterrestrial life, was transmitted from the radio telescope toward the globular cluster M13, about 25,000 light-years away. The 1,679 bit pattern of 1s and 0s defined a 23 by 73 pixel bitmap image that included numbers, stick figures, chemical formulas and a crude image of the Telescope itself.
The RuBisCo Stars
On November 7, 2009, as part of the 35th anniversary of the Drake/Sagan transmission to M13, the RuBisCO gene sequence was transmitted to three "nearby" stars: GJ 83.1, Teagarden's star SO 025300.5+165258 and Kappa Ceti (G5B). The project was by artist Joe Davis with support from Paul Gilster, the Arecibo Observatory, Cornell University and others.
Search for Extra-Terrestrial Intelligence (SETI), is a program focused on finding extraterrestrial "life" or advanced technologies that surpass terrestrial acquisitions. SETI aims to answer the eternal question: "Are we alone in the Universe?" by emitting a series of radio frequencies, (signaling waves in the electromagnetic spectrum), to penetrate Earth´s atmosphere, sending a signal to space and recording data of possible sounds or feedback received.
Arecibo is the source of data for the SETI@home and Astropulse distributed computing projects put forward by the Space Sciences Laboratory at the University of California, Berkeley and was used for the SETI Institute's Project Phoenix observations. The Einstein@Home distributed computing project has found more than 20 pulsars in Arecibo data.
Terrestrial aeronomy experiments at Arecibo have included the Coqui 2 experiment, supported by NASA. The Arecibo Telescope also has military intelligence uses, some of which include locating Soviet radar installations by detecting their signals bouncing off the Moon.
Limited amateur radio operations have occurred, using "moon bounce" or Earth–Moon–Earth communication, in which radio signals aimed at the Moon are reflected back to Earth. The first of these operations was on April 13–14, 1964, using the call KP4BPZ. A dozen or so two-way contacts were made on 144 and 432 MHz. On July 3 and July 24, 1965, KP4BPZ was again activated on 432 MHz, making approximately 30 contacts on 432 MHz during the limited time slots available. For these tests, a very wide-band instrumentation recorder captured a large segment of the receiving bandwidth, enabling later verification of other amateur station callsigns (obviously, not two-way contacts). From April 16–18, 2010, again, the Arecibo Amateur Radio Club KP4AO conducted moon-bounce activity using the antenna. On November 10, 2013, the KP4AO Arecibo Amateur Radio Club conducted a Fifty-Year Commemoration Activation, lasting 7 hours on 14.250 MHz SSB, without using the main dish antenna.
Since the early 1970s, the Arecibo Observatory has been supported by the NSF (National Science Foundation divisions of Astronomical Sciences and of Atmospheric Sciences) with incremental support by NASA, for the operation of the planetary radar. Between 2001 and 2006, NASA decreased, then eliminated, its support of the planetary radar, but restored and increased the funding in FY-2010.
A report by the NSF division of Astronomical Sciences, made public on November 3, 2006, recommended substantially decreased astronomy funding for the Arecibo Observatory, from $10.5 million in 2007 to $4.0 million in 2011. If other sources of money could not be obtained, the observatory would be forced to close. The report also advised that 80 percent of the observation time be allocated to the surveys already in progress, reducing available time for smaller programs.
Academics and researchers responded by organizing to protect and advocate for the Observatory. They established the Arecibo Science Advocacy Partnership (ASAP), to advance the scientific excellence of Arecibo Observatory research and to publicize its accomplishments in astronomy, aeronomy and planetary radar. ASAP's goals included mobilizing the existing broad base of support for Arecibo science within the fields it serves directly, the broad scientific community; provide a forum for the Arecibo research community and enhance communication within it; promote the potential of Arecibo for groundbreaking science; suggest paths that will maximize it into the foreseeable future, and showcase the broad impact and far-reaching implications of the science currently carried out with this unique instrument.
Contributions by the government of Puerto Rico may be one way to help fill the funding gap, but remain controversial and uncertain. At town hall meetings about the potential closure, Puerto Rican Senate President Kenneth McClintock announced an initial local appropriation of $3.0 million during fiscal year 2008 to fund a major maintenance project to restore the three pillars that support the antenna platform to their original condition, pending inclusion in the next bond issue. The bond authorization, with a $3.0 million appropriation, was approved by the Senate of Puerto Rico on November 14, 2007, on the first day of a special session called by Aníbal Acevedo Vilá. The Puerto Rico House of Representatives repeated this action on June 30, 2008. Puerto Rico's governor signed the measure into law in August 2008. These funds were made available during the second half of 2009.
In a letter published on September 19, 2007, José Enrique Serrano, a member of the U.S. House of Representatives Appropriations Committee, asked the National Science Foundation to keep Arecibo in operation.
Language similar to that of the letter of September 19 was included in the FY-2008 omnibus spending bill. In October 2007, Puerto Rico's then-Resident Commissioner, Luis Fortuño, along with Dana Rohrabacher, filed legislation to assure the continued operation of the famed Observatory. A similar bill was filed in the U.S. Senate in April 2008 by the Junior Senator from New York, Hillary Clinton.
Since the Arecibo observatory is owned by the Government of the United States, donations by private or corporate donors cannot be made. However, as a non-profit (501(c)(3)) "public charities" under US law, the operators, SRI International and Universidad Metropolitana, can accept contributions on behalf of the Arecibo Observatory.
In September 2007, in an open letter to researchers, the NSF clarified the status of the budget for NAIC, stating the present plan could hit the targeted budgetary revision. No mention of private funding was made. However, in the event that its budget target is not reached, it must be noted that the NSF is undertaking studies to mothball or demolish the Observatory to return it to its natural setting.
In November 2007, The Planetary Society urged the U.S. Congress to prevent the Arecibo Observatory from closing because of insufficient funding, since its radar contributes greatly to the accuracy of predictions of asteroid impacts on the Earth. The Planetary Society believes that continued operation of the observatory will reduce the cost of mitigation (that is, deflection of a near-Earth asteroid on collision to Earth), should that be necessary.
Also in November of that year The New York Times described the consequences of the budget cuts at the site. In July 2008, the British newspaper The Daily Telegraph reported that the funding crisis, due to federal budget cuts, was still very much alive.
The SETI@home program is using the telescope as a primary source for ET research. The program urges people to send a letter to their political representatives in support of full federal funding of the Observatory.
The NAIC received $3.1 million from the American Recovery and Reinvestment Act of 2009. This was used for basic maintenance and for a second, much smaller, antenna to be used for very long baseline interferometry, new Klystron amplifiers for the planetary radar system and student training. This allotment was an increase of about 30 percent over the FY-2009 budget. However, the FY-2010 funding request by NSF was cut by $1.2 million, (−12.5 percent), over the FY-2009 budget), in light of their continued plans to reduce funding.
The 2011 NSF budget was reduced by a further $1.6 million, −15 percent compared to 2010, with a further $1.0 million reduction projected by FY-2014. Beginning in FY-2010, NASA restored its historical support by contributing $2.0 million per year for planetary science, particularly the study of near-Earth objects, at Arecibo. NASA implemented this funding through its Near Earth Object Observations program.
Furthermore, in 2010 the NSF issued a call for new proposals for the management of NAIC beginning in FY-2012. On May 12, 2011, the agency informed Cornell University that, as of October 1, 2011, it would no longer be the operator of the NAIC and the Arecibo Observatory. At that time, Cornell transferred its operations to SRI International, along with two other managing partners, Universities Space Research Association and Universidad Metropolitana de Puerto Rico, with a number of other collaborators. Upon the award of the new cooperative agreement for NAIC management and operation, NSF also decertified NAIC as a Federally Funded Research and Development Center (FFRDC), with the stated goal of providing the NAIC with greater freedom to establish broader scientific partnerships and pursue funding opportunities for activities beyond the scope of those supported by NSF.
Ángel Ramos Foundation Visitor Center
Opened in 1997, the Ángel Ramos Foundation Visitor Center  features interactive exhibits and displays about the operations of the radio telescope, astronomy and atmospheric science. The center is named after the financial foundation that honors Ángel Ramos, the owner of the El Mundo newspaper and the founder of Telemundo. The Foundation provided half of the funds to build the Visitor Center, with the remainder received from private donations and Cornell University.
The Ángel Ramos Foundation Visitor Center, in collaboration with the Caribbean Astronomical Society, host a series of Astronomical Nights throughout the year, which feature diverse discussions regarding exoplanets, and astronomical phenomenons and discoveries (such as Comet ISON). The main purpose of the Center is to increase public interest in astronomy, the Arecibo Observatory's research successes and space endeavors.
The Visitor Center is open Wednesday - Sunday, on many holidays and during school breaks.The admission fee is $10.00 for adults, and $6.00 for seniors and children under 10.
List of directors
- 1960–1965, Dr. William E. Gordon (Ph.D., Cornell University)
- 1965–1966, Dr. John W. Findlay (Ph.D., University of Cambridge)
- 1966–1968, Dr. Frank Drake (Ph.D., Harvard University)
- 1968–1971, Dr. Gordon Pettengill (Ph.D., UC Berkeley)
- 1971–1973, Dr. Tor Hagfors (Ph.D., University of Oslo)
- 1973–1982, Dr. Harold D. Craft Jr. (Ph.D., Cornell University)
- 1982–1987, Dr. Donald B. Campbell (Ph.D., Cornell University)
- 1987–1988, Dr. Riccardo Giovanelli (Ph.D., University of Bologna)
- 1988–1992, Dr. Michael M. Davis (Ph.D., Leiden University)
- 1992–2003, Dr. Daniel R. Altschuler (es) (Ph.D., Brandeis University)
- 2003–2006, Dr. Sixto A. González (Ph.D., Utah State University)
- 2006–2007, Dr. Timothy L. Hankins (Ph.D., University of California at San Diego)
- 2007–2008, Dr. Robert B. Kerr (Ph.D., University of Michigan)
- 2008–2011, Dr. Michael C. Nolan (Ph.D., University of Arizona)
- 2011–present, Dr. Robert B. Kerr (Ph.D., University of Michigan)
In popular culture
- The Arecibo Observatory was featured on Cosmos: A Personal Voyage in Part 12 "Encyclopedia Galactica."
- Arecibo Observatory was used as a filming location in the climax of the James Bond movie GoldenEye (1995), and as a level in the accompanying Nintendo 64 video game GoldenEye 007.
- The film Contact (1997), based on the Carl Sagan 1985 novel of the same name, features Arecibo, where the main character uses the facility as part of a SETI project.
- Fox Mulder went to the Arecibo Observatory in The X-Files episode, "Little Green Men."
- The Observatory is featured in the film Species (1995), the James Gunn novel The Listeners (1972), the Robert J. Sawyer novel Rollback, the Mary Doria Russell novel The Sparrow and the film The Losers.
- A radio telescope based on the observatory is featured in Battlefield 4 on the multiplayer map "Rogue Transmission".
- "Arecibo" is the title of the first track of the album "[ Twentythree ]" by Carbon Based Lifeforms.
- National Astronomy and Ionospheric Center (Arecibo Observatory)
- Air Force Research Laboratory
- Five hundred meter Aperture Spherical Telescope
- Atacama Large Millimeter Array
- List of radio telescopes
- Sixto A. González, former director of the Arecibo Observatory (2003–2006)
- William E. Gordon, founder and first director of the Observatory (AIO 1963–1965)
- Tor Hagfors, former director of the Arecibo Observatory (1971–1973) and also of NAIC (October 1982 to September 1992).
- Helias Doundoulakis
- UPRM Planetarium
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- Daniel Fischer (2002). "A comet orbiting a pulsar?". The Cosmic Mirror (244).
- Harmon, J.K., M.A. Slade, R.A. Velez, A. Crespo, M.J. Dryer, and J.M. Johnson (1994). Radar Mapping of Mercury's Polar Anomalies. Nature. p. 369.
- Staff (15 January 2008). "Life's Ingredients Detected In Far Off Galaxy". ScienceDaily (ScienceDaily LLC). Archived from the original on April 21, 2008. Retrieved 2008-03-29.
[Article] Adapted from materials provided by Cornell University.
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- "Einstein@Home new discoveries and detections of known pulsars in the BRP4 search". Einstein@Home. August 27, 2012. Retrieved August 28, 2012.
- Steve Blank "Secret history of Silicon Valley" talk
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- Rick Weiss (9 September 2007). "Radio Telescope And Its Budget Hang in the Balance". The Washington Post (Arecibo, Puerto Rico: The Washington Post Company). p. A01. Retrieved 2008-07-08.
The cash crunch stems from an NSF "senior review" completed last November. Its $200 million astronomy division, increasingly committed to ambitious new projects, but long hobbled by flat Congressional budgets, was facing a deficit of at least $30 million by 2010.
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- Arecibo participated in 90 of the 111 asteroid radar observations in 2005–2007. See JPL's list of all asteroid radar observations.
- Chang, K., "A Hazy Future for a 'Jewel' of Space Instruments.", New York Times, November 20, 2007
- Jacqui Goddard, "Threat to world's most powerful radio telescope means we may not hear ET", Daily Telegraph, July 12, 2008
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- Entry into the National Register of Historic Places
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- Altschuler, Daniel R.; Salter, Christopher J. (2013). "The Arecibo Observatory: Fifty astronomical years". Physics Today 66 (11): 43. Bibcode:2013PhT....66k..43A. doi:10.1063/PT.3.2179.
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