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Adam Savage, Clonkeen College

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Irbene radio telescope, Inženieru Street, Ventspils, Latvia

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Irbene radio telescope, Inženieru Street, Ventspils, Latvia

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Irbene radio telescope, Inženieru Street, Ventspils, Latvia

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Adam Savage, Clonkeen College

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Radiobservatório de Itapetinga, Atibaia - State of São Paulo, Brazil

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Radiobservatório de Itapetinga, Atibaia - State of São Paulo, Brazil

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Radiobservatório de Itapetinga, Atibaia - State of São Paulo, Brazil

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Matthew Dutton, Clonkeen college

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Rádio Observatório Pierre Kauffman - ROI/INPE

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O ROI deu início a suas atividades no começo dos anos 70 com a instalação de um radiotelescópio de 1.2 m de diâmetro operando em 7GHz e totalmente dedicado a observações da atividade solar. Também fazia parte dos instrumentos de pesquisa do observatório um sistema para recepção de sinais de Very L…

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Large Millimeter Telescope, Parque Nacional Pico de Orizaba, Volcán Sierra Negra, Puebla, Mexico

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Large Millimeter Telescope, Parque Nacional Pico de Orizaba, Volcán Sierra Negra, Puebla, Mexico

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Large Millimeter Telescope, Parque Nacional Pico de Orizaba, Volcán Sierra Negra, Puebla, Mexico

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Matthew Dutton, Clonkeen college

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Large Millimeter Telescope

The Large Millimeter Telescope (or Gran Telescopio Milimétrico Alfonso Serrano) is the world´s largest single-dish steerable millimetre-wavelength telescope designed specifically for astronomical observations in the wavelength range of 0.85 - 4mm. This binational project between México and the United States of America represents the largest and most complex scientific instrument constructed in México. Situated on the summit of Volcán Sierra Negra at an altitude of 4600 meters, the LMT has begun its exploration of the physical processes that lead to the formation and evolution of planetary systems, stars, black-holes and galaxies thoughout the 13.7 billion year history of the Universe.

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LMT - Large Millimeter Telescope Alfonso Serrano

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Large Millimeter Telescope The Large Millimeter Telescope (or Gran Telescopio Milimétrico Alfonso Serrano) is the world´s largest single-dish steerable millimetre-wavelength telescope designed specifically for astronomical observations in the wavelength range of 0.85 - 4mm. This binational project between México and the United States of America represents the largest and most complex scientific instrument constructed in México.

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SKA South Africa, Baker Street, Rosebank, Johannesburg, South Africa

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SKA South Africa, Baker Street, Rosebank, Johannesburg, South Africa

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SKA South Africa, Baker Street, Rosebank, Johannesburg, South Africa

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http://eor.berkeley.edu/ - Luke Bailey

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Llano de Chajnantor Observatory, San Pedro de Atacama, Chile

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Llano de Chajnantor Observatory, San Pedro de Atacama, Chile

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Llano de Chajnantor Observatory, San Pedro de Atacama, Chile

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http://metsahovi.aalto.fi/en/
Stephen Harpur, Clonkeen College

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Metsähovi Radio Observatory | Aalto University

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Metsähovi Radio Observatory is the only astronomical radio observatory in Finland. Metsähovi’s main instrument is the 14-metre radio telescope, which is used around the clock, every day of the year. Its observational data is used, e.g., for studying active galaxies, the Sun, and the rotation of the…

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Manas Chedimala, Clonkeen College

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The escope with a diameter of 25 m. The telescope was completed in 1956. It is no longer in operation as of 2000. Since August of 2009, it is officially a national Dutch industrial heritage monument. Dwingeloo radio observatory (near Dwingeloo, m. Westerveld, in the northeastern Netherlands), is a single dish radio tel
The "C.A. Muller Radio Astronomy Station" foundation ("CAMRAS" for short), established on January 29, 2007, restored the telescope to working order, with the consent of ASTRON, the owner of the telescope. More information about CAMRAS can be found at [1].
Paul Boven (JIVE, CAMRAS), along with radio amateurs and amateur astronomers, currently use the telescope for several projects, one being EME (communications). EME, also known as moonbounce, allows for people on different places of Earth to communicate via the Moon. In this technique, radio wave signals are aimed at the Moon by one location, bounce off the Moon's surface, and are detected by an antenna at a different location on Earth.
The site of the Dwingeloo Radio Observatory also houses most of the staff of ASTRON, and a test site for LOFAR.
Two galaxies are named after this telescope: Dwingeloo 1 and Dwingeloo 2.

Available observing mode: single dish.

Frequencies used currently: the system is under massive technical upgrade and the operating frequencies will be listed soon.

Research programs: solar radio astronomy, galactic radio astronomy.

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The escope with a diameter of 25 m. The telescope was completed in 1956. It is no longer in operation as of 2000. Since August of 2009, it is officially a national Dutch industrial heritage monument. Dwingeloo radio observatory (near Dwingeloo, m. Westerveld, in the northeastern Netherlands), is a single dish radio tel The "C.A.

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Stockert Radio Telescope, Stockert Radio Telescope, Bad Münstereifel, Germany

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Stockert Radio Telescope, Stockert Radio Telescope, Bad Münstereifel, Germany

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Stockert Radio Telescope, Stockert Radio Telescope, Bad Münstereifel, Germany

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Manas Chedimala, Clonkeen College

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Stockert radio telescope with sage in the foreground.

The Stockert radio telescope was constructed in 1956, and the Förderverein Astropeiler Stockert took the opportunity to celebrate the fiftieth anniversary in 2006. In the years 1985/86 I worked as operator at the Stockert radio telescope. Even before that I had taken part in a student practical there. From this resulted two articles for the journal of the amateur astronomy society Volkssternwarte Bonn. During the research for one of these articles, Prof. Wolfgang Priester gave me a photocopy of a newspaper article of 1957; the staff of the Universitätssternwarte Bonn concocted this April Fool's prank in the year after construction.

All these articles are available in transcripts of their German originals:

During a visit to the area in August 1999, I found the Stockert surrounded by a golf course and the observatory grounds owned by some company. In the 1980s we had used the 25 metre dish to make sensitive final calibration measurements for a survey of 11 cm radio continuum radiation. After that programme was completed I suppose there was nothing else to do for the telescope. Attempts by a third party to create a golf course and to include the observatory grounds and buildings in it met with resistance from the villagers of Eschweiler. One argument was the wildlife in the grounds. I guess the observatory was sold separately to some company around the time the golf course became reality. I gather the company ran into financial trouble and in 2005 the grounds were sold to the NRW Stiftung (a trust of the Land Nordrhein-Westfalen). The telescopes are now in the care of the Förderverein Astropeiler Stockert.

See also

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Stockert radio telescope with sage in the foreground. The Stockert radio telescope was constructed in 1956, and the Förderverein Astropeiler Stockert took the opportunity to celebrate the fiftieth anniversary in 2006. In the years 1985/86 I worked as operator at the Stockert radio telescope. Even before that I had taken part in a student practical there.

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Adam O’Hara, Clonkeen College

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Dec 15, 2021: The ARO 2022A Call for Proposals for February 15, 2022 - June 15, 2022 has been released.

The Arizona Radio Observatory (ARO) currently operates two radio telescopes in southern Arizona: the new 12m Telescope (12m), which is an ALMA prototype antenna located 50 miles southwest of Tucson on Kitt Peak, and the Submillimeter Telescope (SMT) located on Mt. Graham in south eastern Arizona.

Combined,the two telescopes routinely cover the entire millimeter and submillimeter windows from about 4.6 mm to about 0.6 mm, and at the SMT observations can be made all the way to 0.3 mm with PI instruments.

The telescopes are operated around-the-clock for about 9 to 10 months per year for a combined 10,000 hours per observing season (about 1500 hours are dedicated to sub-mm wavelengths at the SMT).

The ARO offices are centrally located in the Steward Observatory building on the campus of the University of Arizona in Tucson Arizona.

ARO receives the bulk of operations funding from the State of Arizona and additional support comes from the National Science Foundation (NSF) for instrumentation development. Current NSF support includes Major Research Instrumentation (MRI) funding for Development of a State-of-the-Art Multiband Receiver for Arizona Radio Observatory's New ALMA Antenna (PI Ziurys; AST-1531366), Mid-Scale Innovations Program (MSIP) funding for The Event Horizon Telescope Experiment (PI Marrone; SV5-85009/AST- 1440254), a Faculty Early Career Development (CAREER) program grant for Mapping the Fuel for Star Formation Across Cosmic History (PI Marrone; AST-1653228), an Advanced Technologies and Instrumentation grant for Measuring Reionization and the Growth of Molecular Gas with TIME (PI Marrone; S455656/AST-1910598), and a Partnerships for International Research and Education (PIRE) award for Black Hole Astrophysics in the Era of Distributed Resources and Expertise (PI Psaltis; OISE-1743747).

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Dec 15, 2021: The ARO 2022A Call for Proposals for February 15, 2022 - June 15, 2022 has been released. The Arizona Radio Observatory (ARO) currently operates two radio telescopes in southern Arizona: the new 12m Telescope (12m), which is an ALMA prototype antenna located 50 miles southwest of Tucson on Kitt Peak, and the Submillimeter Telescope (SMT) located on Mt.

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Adam O’Hara, Clonkeen College

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Overview

Heritage Category:

Listed Building

List Entry Number:

1443087

Date first listed:

10-Jul-2017

Statutory Address:

Jodrell Bank, Lower Withington, Macclesfield, SK11 9DL

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Heritage Category:

Listed Building

List Entry Number:

1443087

Date first listed:

10-Jul-2017

Statutory Address 1:

Jodrell Bank, Lower Withington, Macclesfield, SK11 9DL

The scope of legal protection for listed buildings

This List entry helps identify the building designated at this address for its special architectural or historic interest.

Unless the List entry states otherwise, it includes both the structure itself and any object or structure fixed to it (whether inside or outside) as well as any object or structure within the curtilage of the building.

For these purposes, to be included within the curtilage of the building, the object or structure must have formed part of the land since before 1st July 1948.
Understanding list entries
Corrections and minor amendments

The scope of legal protection for listed buildings

This List entry helps identify the building designated at this address for its special architectural or historic interest.

Unless the List entry states otherwise, it includes both the structure itself and any object or structure fixed to it (whether inside or outside) as well as any object or structure within the curtilage of the building.

For these purposes, to be included within the curtilage of the building, the object or structure must have formed part of the land since before 1st July 1948.
Understanding list entries
Corrections and minor amendments

Location

Statutory Address:

Jodrell Bank, Lower Withington, Macclesfield, SK11 9DL

The building or site itself may lie within the boundary of more than one authority.

District:

Cheshire East (Unitary Authority)

National Grid Reference:

SJ7981570810

Summary

Radio telescope. Designed 1960, built 1962-1964 and constructed to designs by Sir Charles Husband of structural engineers Husband and Company of Sheffield to the requirements of Sir Bernard Lovell. Constructed by Arrol & Co. New, circular bowl surface mounted on top of the original elliptical bowl in 1987.

Reasons for Designation

The Mark II Telescope, Jodrell Bank Observatory, designed 1960, built 1962-66 and constructed to designs by Sir Charles Husband to the requirements of Sir Bernard Lovell, is listed at Grade I for the following principal reasons:

* Technological innovation: Husband designed a pre-stressed concrete mount for the reflector dish to improve on the rigidity and accuracy of the structural steel he had used for the Lovell Telescope, and as a more economic solution, the design of which he then used as the basis for the telescope at Goonhilly, Cornwall (Grade II*), built to receive the first live transatlantic television pictures from the Telstar satellite in 1962, the successful design then widely adopted in the development of international modern satellite communications. The Mark II Telescope was the first telescope in the world to be steered by a digital computer, the Ferranti Argus 104, one of the very first computers designed for real-time control;

* Historic interest: as an early, large-scale, fully steerable radio telescope and key component of the Jodrell Bank Observatory. One of the earliest planned sites for radio astronomy in the world, its construction enabled the development of scientific research through greater accuracy in observations both individually and in conjunction with the earlier Lovell Telescope (Mark I Telescope) to progress the technique of interferometry, a role it continues in a worldwide context to this day;

* Design interest: the bold concrete frame and striking elliptical reflector dish give the Mark II Telescope an impressive, sculptural appearance; together with the Lovell Telescope it has a dramatic visual quality which captures in physical form the excitement of radio astronomy at this pioneering site;

* Group value: the radio telescope has a strong functional and visual connection with the Lovell Telescope (Grade I), through the discipline of radio astronomy for which the Observatory has a long-standing international reputation.

History

The observatory at Jodrell Bank was one of the earliest planned sites for radio telescopes in the world. As such it had a pivotal role in the development of the new science of radio astronomy which was one of the first steps towards modern Astrophysics, revolutionising our understanding of the Universe. The site was first used for academic purposes in 1939 when the University of Manchester's Botany Department purchased three fields in the Cheshire countryside covering around 11 acres. The earliest use of the site for radio astronomy occurred in December 1945 when Bernard Lovell, who worked for the university's Physics Department, moved here to escape the radio interference that occurred in Manchester city centre. His first observations used ex-army radar equipment located at the south end of the site, close to two pre-existing botany huts. Subsequently his team expanded northwards with the continuing construction of more permanent buildings, aerials and telescopes. Jodrell Bank's status as a world-class centre of ongoing scientific research continues to this day with the construction of the global headquarters for the Square Kilometre Array project linking hundreds of telescopes and aerials in South Africa and Western Australia.

The Mark II Telescope was instigated in 1960 by discussions between Sir Bernard Lovell and Sir Charles Husband of structural engineers Husband and Co of Sheffield, who had previously designed the Mark I Telescope (since renamed the Lovell Radio Telescope), built in 1952-57. When approaching the design of this second telescope various issues were addressed. The idea of an oval (elliptical) reflector arose as a response to the design problems of constructing a very large reflector. Husband wanted to keep down the vertical size to avoid constructional and aerodynamic problems. He also preferred to construct the whole turntable of pre-stressed concrete rather than structural steel for reasons of rigidity and economy. It was intended as the prototype of a larger telescope, later referred to as the Mark IV, which was never constructed. Meanwhile, in 1960 the General Post Office asked Husband to build a radio telescope at Goonhilly, Cornwall, for transatlantic communication via the first active communication satellite, known as Telstar, with a summer 1962 deadline. Husband declared this impossible unless he was allowed to use the basic design for the Mark II Telescope, scaling the design so the bowl was circular with the diameter of the minor axis of the Mark II. It was subsequently built to the 1962 timescale and is recognised as the birthplace of satellite communication (Antenna No.1 at Goonhilly Satellite Earth Station listed Grade II*). Funding for the construction of the Mark II Telescope was requested on 19 December 1960, but the Research Council of the Department of Scientific and Industrial Research (RCDSI) did not pass this until December 1961.

The telescope was built on the site of the earlier 218ft Transit Telescope and was operational by summer 1964. It had a steel sheet paraboloidal reflecting bowl with an elliptical aperture of major axis 125ft (38.1m) and minor axis of 83ft 4in (25.4m). The focal length was 40ft (12.2m), the mounting was alt-azimuth with 420 degrees of travel in azimuth and 0 to 90 degrees in elevation. The drive was a Ward-Leonard system with digital computer control giving great accuracy of positioning. The Mark II was the first telescope in the world to be steered by digital computer. The computer used was the Ferranti Argus 104, which was one of the very first computers designed for real time control, with a storage capacity of 12 Kbytes.

A combination of greater surface accuracy of the bowl and the design of more precise control devices meant that the Mark II was able to observe higher frequency wave lengths in the 21cm band and shorter than the Mark I Telescope and thus complement it. As well as operating as a solo instrument, the telescope was intended to work as an interferometer with the Mark I Telescope (two or more telescopes that combine their signals to produce a resolution equivalent to that of a telescope of diameter equal to the largest separation between its individual telescopes). In 1971 the Mark II's computer was upgraded to an Argus 400 computer, also capable of carrying out data acquisition for the telescope's observing programs, with the original 104 transferred to the upgraded Mark I. During the 1970s the telescope worked in conjunction with the Mark III telescope (built to the same dimensions in 1966 at Wardle, Nantwich, Cheshire and intended to be portable but never moved). This work led to the development of the Multi Telescope Radio Linked Interferometer (MTRLI) and then Multi-Element Radio Linked Interferometer Network (MERLIN) arrays of which it is an integral part.

In 1974 a proposal was made to upgrade the Mark II to Mark IIA, by giving it a 100ft circular aperture which could be used on wavelengths down to 6mm. However, funding could not be secured.

In 1987 the bowl was upgraded with a circular surface of new aluminium panels mounted on top of the original steel surface. The new surface had an accuracy of 1/3mm and was set using a holographic technique. It was built in a collaborative project between Jodrell Bank and Racal Antennas and resulted in the telescope being able to observe at the 22GHz MERLIN frequency. In the late 1990s a new, more compact carousel for the receivers was installed in the aerial focus. The building was refurbished in 2014.

The Mark II Telescope continues in daily use with the majority of current observational time spent either on e-MERLIN (the upgraded MERLIN programme) or Very Long Baseline Interferometry (VBLI), joining radio telescopes around the world.

Details

Radio telescope. Designed 1960, built 1962-1964 and constructed to designs by Sir Charles Husband of structural engineers Husband and Company of Sheffield to the requirements of Sir Bernard Lovell. Constructed by Arrol & Co. New, circular bowl surface mounted on top of the original elliptical bowl in 1987.

MATERIALS: concrete, structural steel, welded steel sheet, with later aluminium panels (1987).

PLAN: circular, ground-floor base building containing roller track and alt-azimuth mount with rectangular engine room projecting on south-east side; concrete bracket on top of circular base building supporting an elliptical dish; rectangular first-floor room located between the base of the bracket; separate, small, engine room situated on the rotating structure of the telescope.

EXTERIOR: the base building, ground-floor engine room (known as the Ward Leonard Room), first-floor central room (known as the Turntable Lab) and telescope bracket are constructed of pre-stressed concrete. The buildings have flat concrete roofs, some covered in asphalt. All the windows have Georgian-wired glazing.The ground-floor engine room is known as the Ward Leonard Room after the Ward Leonard Motor Generator System which used to be the standard system for producing Direct Currant (DC) power for rotating the telescope. It is well-lit by large, metal-framed windows. In the centre of the north-west side is a small, square projecting room with windows in all three elevations. On both sides of this room are wide, full-height doorways with timber double doors, that to the right with a wicket door. The circular base building is lit by four horizontal, metal-framed windows. On the south side is a tall, wide, doorway with timber double doors. On the east side there is a flight of concrete steps with metal pipe handrails with diamond wiring infill leading up to the roof of the circular building on which the telescope bracket stands. It has a similar metal pipe railing (without the wiring infill) around the perimeter. The flat-roofed Turntable Lab has concrete braces across to the outward-leaning telescope bracket. The room is well-lit by tall, vertical windows with metal frames. There are wide, full-height doorways with timber double doors at the right-hand ends of both long elevations. Situated on the rotating structure of the telescope is a small engine room known as the Elevation Drive Cabin. It has a deep, concrete engine-bed base, and the walls and flat-roof are constructed of riveted steel panels with a sliding, steel-panel doorway on one side. The elliptical reflector bowl has a lattice-work, steel frame supported on the concrete bracket with concrete counter-weights to the rear. The elliptical, paraboloidal bowl is constructed of welded steel sheet with a major axis of 125ft (38.1m) and minor axis of 83ft 4in (25.4m). Overlaying this is the 1987, circular surface of aluminium panels. The aerial with a focal point of 40ft (12m) is supported by four lattice-work legs standing out from the edge of the bowl structure; the lower, right leg incorporates a narrow flight of steps to access the aerial focal point with a hanging flight of steps to allow access from the roof of the Elevation Drive Cabin.

INTERIOR: the Ward Leonard Room contains the original azimuth gearbox on a deep concrete engine bed, since modified. It bears a plaque for Crofts (engineers) Ltd, Bradford and is stamped 'AUG 30 62 3Hz'. It powers a vertical driveshaft, gear chain and cogs which move rollers to control the horizontal position of the alt-azimuth mount in the circular base building. On the east side of the gearbox are the two original motors of the control system for the telescope, now replaced by control cabinets along the south-west side of the room. The circular base building contains the alt-azimuth mount which sits on 54 steel rollers in a 12.8m (42ft) diameter on a concrete foundation block in a spoke chamber. There is a narrow walkway around the outside. The first-floor Turntable Lab contains a central, full-height, circular cabinet of riveted steel panels known as a 'twister' through which the telescope wires are threaded to prevent their tangling. The room also retains the original circular, enamelled light shades. It has a small, 500kg travelling crane above a trap door in the floor through which the alt-azimuth mount can be reached. The Elevation Drive Cabin contains a motor and gearbox which drives a vertical driveshaft which controls the vertical position of the telescope.

Sources

Books and journals
Lovell, Bernard, The Jodrell Bank Telescopes, (1985), 10-17
Pevsner, N, Hubbard, E (eds), The Buildings of England: Cheshire. Kelsall: Jodrell Bank, (1971), 249
'Manchester: a new facility in very high frequency bands' in New Scientist, (4 Jan 1962), 13
Other
Jodrell Bank Observatory Site Conservation Management Plan Site Gazetteer, December 2014 (final draft) Chris Blandford Associates.
Jodrell Bank Observatory, the University of Manchester, Conservation Management Plan, June 2016, Chris Blandford Associates

Legal

This building is listed under the Planning (Listed Buildings and Conservation Areas) Act 1990 as amended for its special architectural or historic interest.

End of official list entry

Print the official list entry

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Jodrell Bank Observatory: Mark II Telescope, Lower Withington - 1443087 | Historic England

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Overview Heritage Category: Listed Building List Entry Number: 1443087 Date first listed: 10-Jul-2017 Statutory Address: Jodrell Bank, Lower Withington, Macclesfield, SK11 9DL Search over 1 million photographs and drawings from the 1850s to the present day using our images archive.

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Mukilson Dheepson, Clonkeen College

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Mukilson Dheepson, Clonkeen College

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Kjell Henriksen Observatory, Svalbard and Jan Mayen

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Kjell Henriksen Observatory, Svalbard and Jan Mayen

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Kjell Henriksen Observatory, Svalbard and Jan Mayen

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Eoin Farrelly, Clonkeen College

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Algonquin Radio Observatory, Unorganized South Nipissing District, ON, Canada

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Shane O'Sullivan Clonkeen College

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Medicina Radio Observatory, Via Fiorentina, Medicina, Metropolitan City of Bologna, Italy

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Medicina Radio Observatory, Via Fiorentina, Medicina, Metropolitan City of Bologna, Italy

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Medicina Radio Observatory, Via Fiorentina, Medicina, Metropolitan City of Bologna, Italy

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Eoin Farrelly, Clonkeen College

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The Northern Cross is, currently, composed of two perpendicular arms that are 564 m long (East-West) and 640 m long (North-South) and it has a useable total surface area of 30000 m ². Thanks to this vast area the antenna is capable of detecting very weak radio sources.

The antenna observes "through" a 2.7 MHz wide window, centered at 408 MHz and it has been mainly used to effect high sensitivity sky surveys and, thus, to produce large radio-source catalogues, which have been and are still today of fundamental importance for astronomical research.

Furthermore the "Cross" has been used for pulsars research and for the spectrometric study of interstellar dust (emission line of ionized hydrogen and of ionized carbon). Currently the instrument is being converted and upgraded in order to meet the international SKA ( Square Kilometre Array) program requirements. The ultimate goal ia a next generation radiotelescope with a useable total surface area of 1 km ² area. The "Cross", in fact, represents an ideal test ground for SKA technologies and data acquisition systems.

The ( ÷ 23 GHz range. In single dish, it is mainly used for : H 32 m parabolic antenna is employed both for single dish observations and for interferometry.In interferometry it works together with the other European Very Long Baseline Interferometry Network) antennas, installed all over Europe, in order to produce very high resolution images, which are quite useful for detailed radio sources studies. The radiotelescope can receive radio signals within the 1.4 ₂O and methanol maser spectrometry, monitoring of extragalactic compact sources flux variability, galactic polarimetric surveys,studies of comets, extrasolar planet research, and radar monitoring of Near Earth Objects (in collaboration with the NASA) EVN

The astronomical interferometric observations are, also, used for geodynamic studies. The VLBI techniques, in fact, allow measurement of the distance between the various antennas with a millimetric degree of accuracy. It is therefore the most precise way of monitoring and studying the movements of the Earth's crust.

The Medicina observatory is, also, involved in the SETI ( Search for Extra Terrestrial Intelligence) project. The SETI project's goal is to analyze radio signals originating in space in search of an artificial signal, which would act as undeniable proof of the existence of another technologically advanced civilization in the universe This study, statistically, has very little chance of success, so it is conducted without interfering with the normal astronomical activities. The SETI instrument (SERENDIP IV) works in parallel with the 32 m antenna and automatically analyzes detected signals, 24 hours a day. In this manner, the SETI project can be conducted without requiring active observation time or dedicated personnel.

The Radioastronomy Institute, also, operates another 32 m antenna located in Noto (Sicily), and a third (64 m parabolic) antenna is now under construction near Cagliari (Sardinia).

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The Northern Cross is, currently, composed of two perpendicular arms that are 564 m long (East-West) and 640 m long (North-South) and it has a useable total surface area of 30000 m 2. Thanks to this vast area the antenna is capable of detecting very weak radio sources.

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Submillimeter Array, Mauna Kea Access Road, Hilo, HI, USA

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Submillimeter Array, Mauna Kea Access Road, Hilo, HI, USA

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Submillimeter Array, Mauna Kea Access Road, Hilo, HI, USA

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James Haskins, Clonkeen College

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Star formation is a complex process, beginning from cold clouds of gas and dust and ending with the diverse population of stars we observe in our galaxy and beyond. Studying that process requires many different types of astronomical observations to capture the composition, dynamics, and other properties of star-forming regions. While most researchers focus on certain aspects of these systems, the COordinated Molecular Probe Line Extinction Thermal Emission (COMPLETE) Survey of Star Forming Regions was an ambitious project designed to capture as much information as possible, using data from multiple observatories to accomplish the task. During the survey's data-collecting period, each of these observatories provided a different type of observation on three star-forming regions in the Milky Way, across the infrared, microwave, and radio part of the spectrum of light. COMPLETE was a collaboration between astronomers at the Center for Astrophysics | Harvard & Smithsonian and other universities around the world.

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Located near the summit of Maunakea on the Big Island of Hawaii, the Submillimeter Array (SMA) is one of the flagship observatories of the Center for Astrophysics | Harvard & Smithsonian.

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jamie maguire

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The South African MeerKAT radio telescope, situated 90 km outside the small Northern Cape town of Carnarvon, is a precursor to the Square Kilometre Array (SKA) telescope and will be integrated into the mid-frequency component of SKA Phase 1.

The MeerKAT telescope is an array of 64 interlinked receptors (a receptor is the complete antenna structure, with the main reflector, sub-reflector and all receivers, digitisers and other electronics installed).

The configuration (placement) of the receptors is determined by the science objectives of the telescope.

48 of the receptors are concentrated in the core area which is approximately 1 km in diameter.

The longest distance between any two receptors (the so-called maximum baseline) is 8 km.

Each MeerKAT receptor consists of three main components:

1. The antenna positioner, which is a steerable dish on a pedestal;

2. A set of radio receivers;

3. A set of associated digitisers.

The antenna positioner is made up of the 13.5 m effective diameter main reflector, and a 3.8 m diameter sub-reflector. In this design, referred to as an 'Offset Gregorian' optical layout, there are no struts in the way to block or interrupt incoming electromagnetic signals. This ensures excellent optical performance, sensitivity and imaging quality, as well as good rejection of unwanted radio frequency interference from orbiting satellites and terrestrial radio transmitters. It also enables the installation of multiple receiver systems in the primary and secondary focal areas, and provides a number of other operational advantages.

The combined surface accuracy of the two reflectors is extremely high with a deviation from the ideal shape being no more than 0.6 mm RMS (root mean square). The main reflector surface is made up of 40 aluminium panels mounted on a steel support framework.

This framework is mounted on top of a yoke, which is in turn mounted on top of a pedestal. The combined height of the pedestal and yoke is just over 8 m. The height of the total structure is 19.5 m, and it weighs 42 tons.

The pedestal houses the antenna's pointing control system.

Mounted at the top of the pedestal, beneath the yoke, are an azimuth drive and a geared azimuth bearing, which allow the main and sub-reflectors, together with the receiver indexer, to be rotated horizontally. The yoke houses the azimuth wrap, which guides all the cables when the antenna is rotated, and prevents them from becoming entangled or damaged. The structure allows an observation elevation range from 15 to 88 degrees, and an azimuth range from -185 degrees to +275 degrees, where north is at zero degrees.

The steerable antenna positioner can point the main reflector very accurately, to within 5 arcseconds (1.4 thousandths of a degree) under low-wind and night-time observing conditions, and to within 25 arcseconds (7 thousandths of a degree) during normal operational conditions.

How does MeerKAT work?

Electromagnetic waves from cosmic radio sources bounce off the main reflector, then off the sub-reflector, and are then focused in the feed horn, which is part of the receiver.

Each receptor can accommodate up to four receivers and digitisers mounted on the receiver indexer. The indexer is a rotating support structure that allows the appropriate receiver to be automatically moved into the antenna focus position, depending on the desired observation frequency.

The main function of the receiver is to capture the electromagnetic radiation and convert it to an voltage signal that is then amplified by cryogenic receivers that add very little noise to the signal. The first two receivers will be the L-Band and UHF Band Receivers.

Four digitisers will be mounted on the receiver indexer, close to the associated receivers. The function of the four digitisers is to convert the radio frequency (RF) voltage signal from the receiver into digital signals. This conversion is done by using an electronic component called an analogue to digital converter (ADC). The L-band digitiser samples at a rate of 1 712 million samples every second. (The amount of data that is generated by the digitiser for a receiver is equivalent to approximately 73 000 DVDs every day or almost 1 DVD per sec.)

Once the signal is converted to digital data, the digitiser sends this data via buried fibre optic cables to the correlator, which is situated inside the Karoo Array Processor Building (KAPB) at the Losberg site complex.

A total of 170 km of buried fibre cables connect the receptors to the KAPB, with the maximum length between the KAPB and a single antenna being 12 km.

The fibre cables run inside conduits buried 1 m below the ground for thermal stability.

At the KAPB, the signals undergo various stages of digital processing, such as correlation - which combines all the signals from all the receptors to form an image of the area of the sky to which the antennas are pointing - and beam-forming, which coherently adds the signals from all the receptors to form a number of narrow, high sensitivity beams used for pulsar science. The science data products are also archived at the KAPB with a portion of the science archive data moved off site via fibre connection and stored in Cape Town (with possibilities of reprocessing the data).

Time and frequency reference signals are distributed, via buried optical fibres, to every digitiser on every receptor, so that they are all synchronised to the same clock. This is important to properly align the signals from all receptors.

The control and monitoring system is responsible for monitoring the health of the telescope and for controlling it to do what the operators want it to do. A large number of internal sensors (more than 150 000) monitor everything from electronic component temperatures to weather conditions and power consumption.

The telescope was originally known as the Karoo Array Telescope (KAT) that would consist of 20 receptors. When the South African government increased the budget to allow the building of 64 receptors, the team re-named it "MeerKAT" - ie "more of KAT". The MeerKAT (scientific name Suricata suricatta) is also a much beloved small mammal that lives in the Karoo region.

# data[].attributes.attachment_link.description
The MeerKAT telescope is an array of 64 interlinked receptors (a receptor is the complete antenna structure, with the main reflector, sub-reflector and all receivers, digitisers and other electronics installed). The configuration (placement) of the receptors is determined by the science objectives of the telescope.

# data[].attributes.location_name
Very Long Baseline Array Telescope, East End Road, Christiansted, St. Croix, USVI

# data[].attributes.headline
Very Long Baseline Array Telescope, East End Road, Christiansted, St. Croix, USVI

# data[].attributes.subject
Very Long Baseline Array Telescope, East End Road, Christiansted, St. Croix, USVI

# data[].attributes.body
James Haskins, Clonkeen College

# data[].attributes.attachment_link.title
Very Long Baseline Array - National Radio Astronomy Observatory

# data[].attributes.attachment_link.description
The Very Long Baseline Array (VLBA) is ten radio telescopes stationed across 5,351 miles. It’s the world’s sharpest, dedicated telescope array.

# data[].attributes.location_name
Owens Valley Radio Observatory (OVRO), Big Pine, CA, USA

# data[].attributes.headline
Owens Valley Radio Observatory (OVRO), Big Pine, CA, USA

# data[].attributes.subject
Owens Valley Radio Observatory (OVRO), Big Pine, CA, USA

# data[].attributes.body
Matthew Duffin, Clonkeen College

# data[].attributes.attachment_link.description
The Owens Valley Radio Observatory (OVRO) is one of the largest university-operated radio observatories in the world. It is dedicated to research in radio astronomy and astrophysics, the training of the next generation of radio astronomers, the development of cutting-edge radio instrumentation. It is operated by the Astronomy department of the California Institute of Technology.

# data[].attributes.location_name
Mount Pleasant Radio Astronomy Observatory & Grote Reber Museum, Denholms Road, Cambridge Tasmânia, Austrália

# data[].attributes.headline
Mount Pleasant Radio Astronomy Observatory & Grote Reber Museum, Denholms Road, Cambridge Tasmânia, Austrália

# data[].attributes.subject
Mount Pleasant Radio Astronomy Observatory & Grote Reber Museum, Denholms Road, Cambridge Tasmânia, Austrália

# data[].attributes.location_name
Radiotelescópio de Arecibo, Puerto Rico 625, Arecibo, Porto Rico

# data[].attributes.headline
Radiotelescópio de Arecibo, Puerto Rico 625, Arecibo, Porto Rico

# data[].attributes.subject
Radiotelescópio de Arecibo, Puerto Rico 625, Arecibo, Porto Rico

# data[].attributes.attachment_link.readable_text
O Radiotelescópio de Arecibo ou Telescópio de Arecibo ou Observatório de Arecibo era um radiotelescópio refletor esférico de 305 m (1 000 pés) construído em um sumidouro natural no Observatório de Arecibo localizado perto de Arecibo, Porto Rico. Um receptor orientável montado por cabo e vários transmissores de radar para emitir sinais foram montados 150 m (492 pés) acima do prato. Concluído em novembro de 1963, o Telescópio de Arecibo foi o maior telescópio de abertura única do mundo por 53 anos, até ser superado em julho de 2016 pelo Telescópio Esférico de Abertura de Quinhentos metros ( FAST) em Guizhou, China.

O Telescópio Arecibo foi usado principalmente para pesquisas em radioastronomia, ciência atmosférica e astronomia de radar, bem como para programas de busca por inteligência extraterrestre ( SETI). Cientistas que desejam usar o observatório enviaram propostas que foram avaliadas por árbitros científicos independentes. A NASA também usou o telescópio para programas de detecção de objetos próximos à Terra. O observatório, financiado principalmente pela National Science Foundation (NSF) com apoio parcial da NASA, foi administrado pela Universidade Cornell desde sua conclusão em 1963 até 2011, após o que foi transferido para uma parceria liderada pela SRI International. Em 2018, um consórcio liderado pela University of Central Florida assumiu a operação da instalação.

O design único e futurista do telescópio levou a várias aparições em filmes, jogos e produções de televisão, como para a cena de luta clímax no filme de James Bond (1995). Ele está listado no Registro Nacional de Locais Históricos dos EUA desde 2008. O centro foi nomeado um marco do IEEE em 2001.

Desde 2006, a NSF reduziu seu compromisso de financiamento para o observatório, levando os acadêmicos a exigir apoio financeiro adicional para continuar seus programas. O telescópio foi danificado pelo furacão Maria em 2017 e foi afetado por terremotos em 2019 e 2020. Duas rupturas de cabo, uma em agosto de 2020 e a segunda em novembro de 2020, ameaçaram a integridade estrutural da estrutura de suporte da plataforma suspensa e danificaram a antena. Devido à incerteza sobre a resistência restante dos outros cabos que sustentam a estrutura suspensa e ao risco de colapso devido a novas falhas tornando os reparos perigosos, a NSF anunciou em 19 de novembro de 2020 que o telescópio seria desativado e desmontado, com o rádio telescópio e instalação LIDAR permanecendo operacionais. Antes que pudesse ser desativado, vários dos cabos de suporte restantes sofreram uma falha crítica e a estrutura de suporte, antena e conjunto de cúpula caíram na antena às 7h55, horário local, em 1 ° de dezembro, 2020, destruindo o telescópio.

Informações gerais

A principal estrutura do telescópio tinha a forma de uma calota esférica 1 000 pés (305 m) de diâmetro com um 869 pés (265 m) de raio de curvatura. A superfície da estrutura era feita de 38 778 painéis de alumínio perfurados, cada um com cerca de 3 por 7 pés (1 por 2 m), suportados por uma malha de cabos de aço.

O telescópio tinha três transmissores de radar, com potências isotrópicas irradiadas efetivas (EIRPs) de 22 TW (contínuo) a 2 380 MHz, 3,2 TW (pico de pulso) a 430 MHz, e 200 MW a 47 MHz, também como uma instalação de modificação ionosférica operando em 5,1 e 8 175 MHz.

A estrutura permanecia estacionária, enquanto os receptores e transmissores foram movidos para o ponto focal adequado do telescópio para mirar no alvo desejado. Como um espelho esférico, o foco do refletor está ao longo de uma linha ao invés de em um ponto. Como resultado, alimentações de linha complexas foram implementadas para realizar observações, com cada alimentação de linha cobrindo uma banda de frequência estreita medindo 10-45 MHz. Um número limitado de alimentações de linha pode ser usado a qualquer momento, limitando a flexibilidade do telescópio.

O receptor estava em uma plataforma de 820 toneladas (900 toneladas curtas) suspensa 150 m (492 pés) acima do prato por 18 cabos principais que corriam de três torres de concreto armado (seis cabos por torre), uma de 111 m (365 pés) de altura e as outras duas com 81 m (265 pés) de altura, colocando seus topos na mesma elevação. Cada cabo principal era um feixe de 160 fios de 8 cm (3,1 pol.) De diâmetro, com o feixe pintado e ar seco continuamente soprado para evitar a corrosão devido ao clima tropical úmido. A plataforma tinha uma pista giratória em forma de arco de 93 m (305 pés) de comprimento, carregando as antenas receptoras e refletores secundários e terciários. Isso permitiu ao telescópio observar qualquer região do céu em um cone de 40 graus de visibilidade sobre o zênite local (entre -1 e 38 graus de declinação). A localização de Porto Rico perto do Trópico Norte permitiu que o telescópio Arecibo visse os planetas do Sistema Solar na metade norte de sua órbita. O tempo de luz de ida e volta para objetos além de Saturno é maior do que o tempo de 2,6 horas que o telescópio poderia rastrear uma posição celestial, evitando observações de radar de objetos mais distantes.

Em 19 de novembro de 2020, a National Science Foundation (NSF) anunciou a desativação da antena parabólica do Observatório depois que os danos na instalação se tornaram muito perigosos para consertar.

Finalmente em 1 de dezembro de 2020, a plataforma de equipamentos do radiotelescópio desabou, caindo de uma altura de 140 metros e danificando o domo da antena.

Pesquisa e descobertas

Muitas descobertas científicas foram feitas com o observatório. Em 7 de abril de 1964, logo após seu início de operação, a equipe de Gordon Pettengill usou-o para determinar que o período de rotação de Mercúrio não era de 88 dias, como se pensava anteriormente, mas de apenas 59 dias. Em 1968, a descoberta da periodicidade do Pulsar do Caranguejo (33 milissegundos) por Richard VE Lovelace e outros forneceu a primeira evidência sólida de que estrelas de nêutrons existem. Em 1974, Hulse e Taylor descobriram o primeiro pulsar binário PSR B1913 + 16, uma realização pela qual receberam mais tarde o Prêmio Nobel de Física. Em 1982, o primeiro pulsar de milissegundo, PSR B1937+21, foi descoberto por Donald C. Backer, Shrinivas Kulkarni, Carl Heiles, Michael Davis e Miller Goss. Este objeto gira 642 vezes por segundo e, até a descoberta do PSR J1748-2446ad em 2005, foi identificado como o pulsar de rotação mais rápida.

Em 1980, Arecibo fez a primeira observação de radar de um cometa ao detectar com sucesso o cometa Encke. Em agosto de 1989, o observatório fotografou diretamente um asteróide pela primeira vez na história: 4769 Castalia. No ano seguinte, o astrônomo polonês Aleksander Wolszczan fez a descoberta do pulsar PSR B1257+12, que mais tarde o levou a descobrir seus três planetas em órbita. Estes foram os primeiros planetas extrasolares descobertos. Em 1994, John Harmon usou o Arecibo Radio Telescope para mapear a distribuição de gelo nas regiões polares de Mercúrio.

Em janeiro de 2008, a detecção de moléculas prebióticas metanimina e cianeto de hidrogênio foi relatada a partir de medições de espectroscopia de rádio do observatório da galáxia distante Arp 220 em uma explosão estelar.

De janeiro de 2010 a fevereiro de 2011, os astrônomos Matthew Route e Aleksander Wolszczan detectaram explosões de emissão de rádio da anã marrom T6.5 2MASS J10475385 + 2124234. Esta foi a primeira vez que a emissão de rádio foi detectada de uma anã T, que tem linhas de absorção de metano em sua atmosfera. É também a anã marrom mais fria (a uma temperatura de ~ 900 K) a partir da qual a emissão de rádio foi observada. As explosões de rádio altamente polarizadas e altamente energéticas indicaram que o objeto tem um campo magnético de força > 1,7 kG e atividade magnética semelhante ao planeta Júpiter e ao Sol.

A mensagem de Arecibo

Em 1974, a mensagem de Arecibo, uma tentativa de comunicação com vida extraterrestre em potencial, foi transmitida do radiotelescópio para o aglomerado globular Messier 13,, a cerca de 25 000 anos-luz de distância. O padrão de 1 679 bits de 1s e 0s definiu uma imagem de bitmap de 23 por 73 pixels que incluía números, bonecos, fórmulas químicas e uma imagem crua do telescópio.

Projetos SETI e METI

Busca por inteligência extraterrestre ( SETI) é a busca por vida extraterrestre ou tecnologias avançadas. O SETI tem como objetivo responder à pergunta "Estamos sozinhos no Universo?" escaneando os céus em busca de transmissões de civilizações inteligentes em outros lugares de nossa galáxia.

Em comparação, METI (mensagens para inteligência extraterrestre) refere-se à busca ativa pela transmissão de mensagens.

Arecibo é a fonte de dados para o SETI@home e Astropulse computação distribuída projetos apresentados pelo Laboratório de Ciências Espaciais na Universidade da Califórnia, Berkeley, e foi usado para observações do Projeto Phoenix do Instituto SETI. O projeto de computação distribuída Einstein@Home encontrou mais de 20 pulsares nos dados de Arecibo.

Outros usos

Experimentos de aeronomia terrestre em Arecibo incluíram o experimento Coqui 2, apoiado pela NASA O telescópio também tinha originalmente usos para inteligência militar, incluindo a localização de instalações de radar soviéticas por meio da detecção de seus sinais refletidos na lua.

Ocorreram operações de rádio amador limitadas, usando o salto da lua ou comunicação Terra-Lua-Terra, em que os sinais de rádio direcionados à Lua são refletidos de volta para a Terra. A primeira dessas operações foi de 13 a 14 de junho de 1964, usando a chamada KP4BPZ. Cerca de uma dúzia de contatos bidirecionais foram feitos em 144 e 432 MHz. Em 3 e 24 de julho de 1965, KP4BPZ foi novamente ativado em 432 MHz, fazendo aproximadamente 30 contatos em 432 MHz durante os slots de tempo limitados disponíveis. Para esses testes, um gravador de instrumentação de banda muito larga capturou um grande segmento da largura de banda de recepção, permitindo a verificação posterior de outros indicativos de estação de amador. Não eram contatos bidirecionais. De 16 a 18 de abril de 2010, novamente, o Arecibo Amateur Radio Club KP4AO conduziu uma atividade lunar usando a antena. Em 10 de novembro de 2013, o KP4AO Arecibo Radioamador Clube realizou uma Ativação Comemorativa dos Cinquenta Anos, com duração de sete horas em 14 250 MHz SSB, sem o uso da antena parabólica principal.

Referências

1. ↑ Juan Llanes Santos (20 de março de 2007). "National Register of Historic Places Registration: National Astronomy and Ionosphere Center / Arecibo Observatory" (PDF). National Park Service. Cópia arquivada (PDF) em 30 de maio de 2009 (72 pages, with many historic b&w photos and 18 color photos)

2. ↑ "Milestones:NAIC/Arecibo Radiotelescope, 1963". IEEE Global History Network. IEEE. Cópia arquivada em 6 de março de 2012

3. ↑ "NSF begins planning for decommissioning of Arecibo Observatory's 305-meter telescope due to safety concerns [News Release 20-010]". www.nsf.gov (em inglês). Cópia arquivada em 19 de novembro de 2020

4. ↑ Clery, Daniel (19 de novembro de 2020). "Famed Arecibo telescope, on the brink of collapse, will be dismantled". Science | AAAS (em inglês). Cópia arquivada em 19 de novembro de 2020

5. ↑ Witze, A (novembro de 2020). "Legendary Arecibo telescope will close forever - scientists are reeling.". Nature. 587 (7835): 529-530. doi:10.1038/d41586-020-03270-9

6. ↑ "Giant Arecibo radio telescope collapses in Puerto Rico". The Guardian. Associated Press. 1 de dezembro de 2020

7. ↑ Coto, DÁNICA (1 de dezembro de 2020). "Huge Puerto Rico radio telescope, already damaged, collapses". Associated Press - via Yahoo!

8. ↑ "Environmental Impact Statement for the Arecibo Observatory Arecibo, Puerto Rico (Draft)" (PDF). nsf.gov. NSF. p. 66. At the Arecibo Observatory, a mix of shade-tolerant species have colonized the area beneath the 305-meter radio telescope dish.

9. ↑ a Goldsmith, P. F.; Baker, L. A.; Davis, M. M.; Giovanelli, R. (1995). "Multi-feed Systems for the Arecibo Gregorian". Astronomical Society of the Pacific Conference Series. 75: 90-98. Bibcode:1995ASPC...75...90G b

10. ↑ Eliana Nossa (8 de dezembro de 2017). "Arecibo Call for Ionospheric Modification (HF facility) Proposals - 2018" (PDF). Arecibo Observatory

11. ↑ Jean-Luc Margot; et al. (2018). "A Search for Technosignatures from 14 Planetary Systems in the Kepler Field with the Green Bank Telescope at 1.15-1.73 GHz". Astronomical Journal. 155 (5): 209. Bibcode:2018AJ....155..209M. arXiv:1802.01081 . doi:10.3847/1538-3881/aabb03

12. ↑ Hagen, Jon (2005). "Areciebo 430 MHz Radar Operation and Maintenance Manual" (PDF). NAIC. pp. 6-7

13. ↑ Cohen, Marshall H. (2009). "Genesis of the 1000-foot Arecibo Dish". Journal of Astronomical History and Heritage. 12 (2): 141-1526. Bibcode:2009JAHH...12..141C

14. ↑ "Telescope Description". National Astronomy and Ionosphere Center. Cópia arquivada em 20 de novembro de 2020

15. ↑ Nicholson, Philip D., Richard G. French, Donald B. Campbell, Jean-Luc Margot, Michael C. Nolan, Gregory J. Black, and Heikki J. Salo (2005). "Radar imaging of Saturn's rings". Icarus. 177 (1): 32-62. CiteSeerX 10.1.1.527.7256 . doi:10.1016/j.icarus.2005.03.023

16. ↑ Clery, Daniel (14 de janeiro de 2021). "How the famed Arecibo telescope fell-and how it might rise again". Science

17. ↑ November 2020, Meghan Bartels-Space com Senior Writer 19. "Arecibo radio telescope, an icon of astronomy, is lost". livescience.com (em inglês)

18. ↑ "É o fim: Observatório de Arecibo desaba após meses de deterioração". Canaltech. 1 de dezembro de 2020

19. ↑ Dyce, R. B.; Pettengill, G. H.; Shapiro, I. I. (abril de 1967). "Radar determination of the rotations of Venus and Mercury". Astron. J. 72 (3): 351-359. Bibcode:1967AJ.....72..351D. doi:10.1086/110231

20. ↑ Richard V.E. Lovelace. "Discovery of the Period of the Crab Nebula Pulsar" (PDF). Cornell University. Cópia arquivada (PDF) em 12 de setembro de 2008

21. ↑ Wolszczan, A. (22 de abril de 1994). "Confirmation of Earth-Mass Planets Orbiting the Millisecond Pulsar PSR B1257 + 12". Science. 264 (5158): 538-542. Bibcode:1994Sci...264..538W. PMID 17732735. doi:10.1126/science.264.5158.538

22. ↑ Harmon, J.K; Campbell, D.B; Ostro, S.J; Nolan, M.C (1999). "Radar observations of comets" (PDF). Planetary and Space Science. 47 (12): 1409-1422. Bibcode:1999P&SS...47.1409H. doi:10.1016/S0032-0633(99)00068-9

23. ↑ Staff (15 de janeiro de 2008). "Life's Ingredients Detected in Far Off Galaxy". ScienceDaily. ScienceDaily LLC. Cópia arquivada em 21 de abril de 2008. [Article] Adapted from materials provided by Cornell University.

24. ↑ Route, M.; Wolszczan, A. (10 de março de 2012). "The Arecibo Detection of the Coolest Radio-flaring Brown Dwarf". The Astrophysical Journal. 747 (2): L22. Bibcode:2012ApJ...747L..22R. arXiv:1202.1287 . doi:10.1088/2041-8205/747/2/L22

25. ↑ Larry Klaes (30 de novembro de 2005). "Making Contact". Ithaca Times. Cópia arquivada em 5 de dezembro de 2008

26. ↑ Peter Backus (14 de setembro de 2003). "Project Phoenix: SETI Prepares to Observe at Arecibo". Space.com. Cópia arquivada em 4 de dezembro de 2008

27. ↑ Steve Blank "Secret history of Silicon Valley" talk

Ligações externas

# data[].attributes.attachment_link.title
Radiotelescópio de Arecibo - Wikipédia, a enciclopédia livre

# data[].attributes.attachment_link.description
O Radiotelescópio de Arecibo ou Telescópio de Arecibo ou Observatório de Arecibo era um radiotelescópio refletor esférico de 305 m (1 000 pés) construído em um sumidouro natural no Observatório de Arecibo localizado perto de Arecibo, Porto Rico. Um receptor orientável montado por cabo e vários transmissores de radar para emitir sinais foram montados 150 m (492 pés) acima do prato.

# data[].attributes.location_name
Five hundred meter Aperture Spherical Telescope, Unnamed Road, Pingtang County, Qiannan Buyei and Miao Autonomous Prefecture, Guizhou, China

# data[].attributes.headline
Five hundred meter Aperture Spherical Telescope, Unnamed Road, Pingtang County, Qiannan Buyei and Miao Autonomous Prefecture, Guizhou, China

# data[].attributes.subject
Five hundred meter Aperture Spherical Telescope, Unnamed Road, Pingtang County, Qiannan Buyei and Miao Autonomous Prefecture, Guizhou, China

# data[].attributes.attachment_link.readable_text
Five hundred meter Aperture Spherical Telescope ( FAST; em português: Rádiotelescópio Esférico com 500 metros de Abertura) é um radiotelescópio localizado na depressão Dawodang (大 窝 凼 洼地), uma bacia natural no condado Pingtang, província de Guizhou, sudoeste da China. É constituído por um prato fixo de 500 metros fabricado de acordo com a depressão natural na paisagem. É o maior radiotelescópio do mundo e a segunda maior abertura de um único prato depois do RATAN-600 na Rússia.

A construção do projeto FAST começou em 2011 e alcançou a primeira captação em 25 de setembro de 2016. Esteve 3 anos passando por testes e comissionamento.

A estrutura iniciou em Janeiro de 2020 oficialmente as suas operações após um período de testes de três anos.

O telescópio está a cumprir todos os requisitos necessários para o seu funcionamento. A equipa por trás do FAST prevê que o rádiotelescópio ajude os cientistas de todo o mundo a fazer descobertas importantes ao longo dos próximos dois a três anos.

A sua superfície composta por 4 450 refletores triangulares faz com que tenha a mais elevada sensibilidade de deteção de sinais vindos do espaço, servindo para observar fenómenos relacionados com matéria negra e até procurar vida extraterrestre.

O FAST é uma das prioridades na estratégia espacial da China, sendo que o seu desenvolvimento rondou valores na ordem dos 180 milhões de dólares. No entanto, a sua construção implicou um "custo" em particular. Cerca de 9 100 pessoas que residiam num raio de 5 km da estrutura foram obrigadas a abandonar as suas casas. Em questão estariam os efeitos negativos do campo de ondas sonoras e eletromagnéticas na população em seu redor.

Até 2020, o observatório identificou 114 novos pulsares desde que começou a operar na sua fase de testes, em dezembro de 2016. O telescópio realizou quase 1 000 horas de observações entre 1 de janeiro a 23 de março de 2020. A observação de pulsares é uma tarefa importante para o FAST, uma vez que estes podem ser utilizados para confirmar a existência de radiação gravitacional e buracos negros, bem como outras questões importantes da Física. O radiotelescópio também está focado em explorar moléculas interestelares e sinais de comunicação interestelar.

Referências

# data[].attributes.attachment_link.title
Five hundred meter Aperture Spherical Telescope - Wikipédia, a enciclopédia livre

# data[].attributes.attachment_link.description
Five hundred meter Aperture Spherical Telescope ( FAST; em português: Rádiotelescópio Esférico com 500 metros de Abertura) é um radiotelescópio localizado na depressão Dawodang (大 窝 凼 洼地), uma bacia natural no condado Pingtang, província de Guizhou, sudoeste da China. É constituído por um prato fixo de 500 metros fabricado de acordo com a depressão natural na paisagem.

# data[].attributes.location_name
Centro Operacional de Satélites do Continente, Almargem do Bispo

# data[].attributes.headline
Centro Operacional de Satélites do Continente, Almargem do Bispo

# data[].attributes.subject
Centro Operacional de Satélites do Continente, Almargem do Bispo

# data[].attributes.location_name
Atacama Large Millimeter Array, San Pedro de Atacama, Chile

# data[].attributes.headline
Atacama Large Millimeter Array, San Pedro de Atacama, Chile

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Atacama Large Millimeter Array, San Pedro de Atacama, Chile

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O Atacama Large Millimeter Array (ALMA) é um rádio-observatório constituído por um conjunto de 66 antenas, das quais 54 com 12 metros de diâmetro e as demais com 7 metros de diâmetro.

Sua construção começou em 2003 e as observações científicas tiveram início em 2011. ALMA está localizado a uma altitude de 5 000 metros, na Zona de Chajnantor, a leste da vila de San Pedro de Atacama, no Chile - um dos maiores sítios de observação astronômica do mundo. Foi inaugurado no dia 13 de março de 2013. Orçado em um bilhão de euros, ele faz parte de uma parceria entre países da Europa, da Ásia Oriental e da América do Norte em cooperação com a República do Chile. O Observatório Europeu do Sul é o parceiro europeu no projeto ALMA.

A sensibilidade do conjunto de antenas torna possível a observação de galáxias muito distantes. Espera-se para outubro de 2015 observações com as 66 antenas em pleno funcionamento.

Em 11 de agosto de 2014, os astrônomos liberado estudos, utilizando o Atacama Large Millimeter/submillimeter Array (ALMA), pela primeira vez, que detalhou a distribuição de HCN, HNC, e poeira no interior do cauda de cometas C/2012 F6 (Lemmon) e C/2012 S1(ISON).

Referências

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Atacama Large Millimeter Array - Wikipédia, a enciclopédia livre

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O Atacama Large Millimeter Array (ALMA) é um rádio-observatório constituído por um conjunto de 66 antenas, das quais 54 com 12 metros de diâmetro e as demais com 7 metros de diâmetro. Sua construção começou em 2003 e as observações científicas tiveram início em 2011.

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Image from eventbrite.es

En la década de 1970, Colombia puso en funcionamiento un par de antenas de 32 metros en Chocontá Cundinamarca, que abrieron en una ventana al mundo para recibir sus primeras señales de televisión satelital. Hoy, a través de esta misma ventana, podríamos observar estrellas, agujeros negros, galaxias en nacimiento, los ecos del origen del Universo e incluso las señales de posibles civilizaciones extraterrestres.

Invitado: Germán Chaparro Molano, PhD en Astrofísica Universidad de Groningen, Miembro de la Unión Astronómica Internacional, Profesor Titular Universidad ECCI, Bogotá | 6:30 p.m. | Auditorios Explora | Entrada libre |

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Radiotelescopio de Chocontá - 2018-05-29 May 2018

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Image from eventbrite.es En la década de 1970, Colombia puso en funcionamiento un par de antenas de 32 metros en Chocontá Cundinamarca, que abrieron en una ventana al mundo para recibir sus primeras señales de televisión satelital.

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Arecibo, PR-625, Arecibo, 00612, Porto Rico

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Arecibo, PR-625, Arecibo, 00612, Porto Rico

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Arecibo, PR-625, Arecibo, 00612, Porto Rico

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Observatório Espacial de Pampilhosa da Serra

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Observatório Espacial de Pampilhosa da Serra

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Read more: http://www.cm-pampilhosadaserra.pt/pages/431?news_id=2186

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Novo telescópio ficará ao serviço do Ministério da Defesa Nacional para monitorizar satélites geoestacionários.

O Observatório Espacial da Pampilhosa da Serra, na aldeia de Porto da Balsa, recebeu um novo telescópio que ficará ao serviço do Ministério da Defesa Nacional, anunciou esta terça-feira aquele município do interior do distrito de Coimbra.

Apenas as autoridades designadas pelo Ministério da Defesa Nacional, o Instituto de Telecomunicações e as instituições protocoladas podem operar este novo aparelho, que permitirá monitorizar satélites geoestacionários.

Domingos Barbosa, investigador do Instituto de Telecomunicações de Aveiro, explica em nota de imprensa que observatório possui agora uma "capacidade única em Portugal para rastrear e detectar satélites, assim como para monitorizar os detritos espaciais que podem provocar danos nesses satélites".

O investigador diz ainda que esta é a "estação radioastronómica de referência em Portugal continental e a única estação completa - radioastronómica e observação óptica" - em todo o território nacional, incluindo ilhas.

"Para além da vertente de investigação, estas características fazem com que este seja igualmente um espaço com forte propensão para o astroturismo ", sintetiza a nota de imprensa. Domingos Barbosa refere também que está a ser realizado um trabalho de fundo, em colaboração com a Câmara Municipal de Pampilhosa da Serra, "para haver um regime de visitas e para poderem visitar os equipamentos".

"O Observatório Espacial de Pampilhosa da Serra é uma estrutura que serve as ciências espaciais e a indústria aeroespacial europeia. Para além do novo telescópio, o local já contava com dois radiotelescópios. Um deles está actualmente a receber a instalação de um radar espacial, sendo que o outro é utilizado para acções formativas no âmbito da astrofísica, astronomia e ciências espaciais."

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Observatório Espacial de Pampilhosa da Serra recebe novo telescópio

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Novo telescópio ficará ao serviço do Ministério da Defesa Nacional para monitorizar satélites geoestacionários. O Observatório Espacial da Pampilhosa da Serra, na aldeia de Porto da Balsa, recebeu um novo telescópio que ficará ao serviço do Ministério da Defesa Nacional, anunciou esta terça-feira aquele município do interior do distrito de Coimbra.

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Secondary School Maria Lamas, Rua Escola Secundária, Torres Novas, Portugal

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Secondary School Maria Lamas, Rua Escola Secundária, Torres Novas, Portugal

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Secondary School Maria Lamas, Rua Escola Secundária, Torres Novas, Portugal

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Manila Observatory, Father Masterson Drive, Quezon City, Metro Manila, Philippines

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Manila Observatory, Father Masterson Drive, Quezon City, Metro Manila, Philippines

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Manila Observatory, Father Masterson Drive, Quezon City, Metro Manila, Philippines

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Jordan Leane; Clonkeen College

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Jordan Leane; Clonkeen College

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John Murray; Coláiste Chluain Chaoin (Clonkeen College)

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https://en.wikipedia.org/wiki/S%C3%A3o_Gi%C3%A3o_Radio_Telescope
http://www.parac.eu

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Giant Ukrainian Radio Telescope (GURT)

John Murray; Coláiste Chluain Chaoin (Clonkeen College)

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John Murray; Coláiste Chluain Chaoin (Clonkeen College)

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Thai National Radio Observatory, Mae Pong, Doi Saket District, Chiang Mai, Thailand

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Thai National Radio Observatory, Mae Pong, Doi Saket District, Chiang Mai, Thailand

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Thai National Radio Observatory, Mae Pong, Doi Saket District, Chiang Mai, Thailand

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John Murray; Clonkeen College

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Kilpisjärvi Atmospheric Imaging Receiver Array (KAIRA)

John Murray Clonkeen College

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Signal Hill Road, Opoho, Dunedin, New Zealand

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Signal Hill Road, Opoho, Dunedin, New Zealand

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Signal Hill Road, Opoho, Dunedin, New Zealand

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TART-2-signal

John Murray; Clonkeen College

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Siberian Solar Radio Telescope

upgraded in 2017

John Murray; Clonkeen College

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Molonglo Observatory Synthesis Telescope, Hoskinstown NSW, Australia

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Molonglo Observatory Synthesis Telescope, Hoskinstown NSW, Australia

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Molonglo Observatory Synthesis Telescope, Hoskinstown NSW, Australia

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John Murray; Clonkeen College

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Estacion Del Espacio Lejano BASE CIENTIFICA China, Loncopué, Neuquen, Argentina

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Estacion Del Espacio Lejano BASE CIENTIFICA China, Loncopué, Neuquen, Argentina

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Estacion Del Espacio Lejano BASE CIENTIFICA China, Loncopué, Neuquen, Argentina

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John Murray; Clonkeen College

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Ghana Radio Astronomy Observatory, Kutunse, Ghana, Kutunse, Ghana

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Ghana Radio Astronomy Observatory, Kutunse, Ghana, Kutunse, Ghana

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Ghana Radio Astronomy Observatory, Kutunse, Ghana, Kutunse, Ghana

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John Murray Clonkeen College

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Adam Ring, Clonkeen College

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These photos may be downloaded and used for education and communication purposes.

Please credit "South African Radio Astronomy Observatory (SARAO)".

For high resolution versions of these images, or detailed captions, please email aflowers@ska.ac.za.

Or contact on 021 506 7395

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These photos may be downloaded and used for education and communication purposes. Please credit "South African Radio Astronomy Observatory (SARAO)". For high resolution versions of these images, or detailed captions, please email aflowers@ska.ac.za. Or contact on 021 506 7395

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Nobeyama radio observatory, 462-2 Nobeyama, Minamimaki, Nagano, Japan

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Nobeyama radio observatory, 462-2 Nobeyama, Minamimaki, Nagano, Japan

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Nobeyama radio observatory, 462-2 Nobeyama, Minamimaki, Nagano, Japan

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C Projects

About Nobeyama Radio Observatory

The Nobeyama Radio Observatory (NRO) operates the 45-m Radio Telescope that is one of the largest telescopes for millimeter wave observations in the world. Radio telescopes can reveal the structures of the Universe that we cannot see with our own eyes. For example, a radio map of the interstellar medium in our galaxy enables us to investigate how various stars are formed. Until today, the 45-m telescope has obtained significant results such as detecting signature of an intermediate mass black hole near the center of our galaxy and exploring the formation process of bio-molecules. The 45-m telescope continues to to unveil the invisible Universe.

Radio image of the Milky Way obtained with the new receiver mounted on the 45-m radio telescope

Radio image of the Milky Way obtained with the new receiver mounted on the 45-m radio telescope (the upper left). High angular resolution enables us to image fine structures of molecular clouds. Red, green, and blue represent the radio intensities of the carbon monoxide isotope.

Telescopes

The 45-m radio telescope

The Nobeyama 45-m Radio Telescope boasts one of the world's largest apertures for radio telescopes observing the radio waves known as "millimeter waves." It has led Japanese radio astronomy since its completion in 1982.
The 45-m radio telescope

Nobeyama Radio Polarimeters

This instrument measures the intensity and orientation (polarization) of radio waves emitted from the full solar disk to monitor the state of solar activity.

Nobeyama Radioheliograph

The Nobeyama Radioheliograph is a radio telescope dedicated to solar observations. Using 84 antennas, it realizes a resolution equivalent to a radio telescope with a diameter of 500 meters.

Nobeyama Millimeter Array

The Millimeter Array observed with 6 antennas simultaneously and captured astronomical images with a resolution equivalent to radio telescopes with diameters of up to about 600 meters at maximum. Science operation has finished.

Access

Nobeyama Radio Observatory Official Website

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C Projects The Nobeyama Radio Observatory (NRO) operates the 45-m Radio Telescope that is one of the largest telescopes for millimeter wave observations in the world. Radio telescopes can reveal the structures of the Universe that we cannot see with our own eyes.

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Amundsen-Scott South Pole Station, Antarctica

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Amundsen-Scott South Pole Station, Antarctica

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Amundsen-Scott South Pole Station, Antarctica

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Garvan Molony

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Allen Telescope Array, Hat Creek, CA, USA

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Allen Telescope Array, Hat Creek, CA, USA

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Allen Telescope Array, Hat Creek, CA, USA

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Matthew Duffin, Clonkeen College

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CSIRO - Parkes Observatory, Telescope Road, Parkes NSW, Australia

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CSIRO - Parkes Observatory, Telescope Road, Parkes NSW, Australia

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CSIRO - Parkes Observatory, Telescope Road, Parkes NSW, Australia

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Matthew Duffin, Clonkeen College

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National Astronomical Observatory of Japan, 2 Chome-21-1 Ōsawa, Mitaka, Tokyo, Japan

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National Astronomical Observatory of Japan, 2 Chome-21-1 Ōsawa, Mitaka, Tokyo, Japan

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National Astronomical Observatory of Japan, 2 Chome-21-1 Ōsawa, Mitaka, Tokyo, Japan

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Callum O'Riordan, Clonkeen College

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The Westerbork Synthesis Radio Telescope (WSRT) is a powerful radio telescope that uses a technique called "aperture synthesis" to generate radio images of the sky. The telescope consists of 14 steerable 25m dish antennas and enables astronomers to study a wide range of astrophysics phenomena. The WSRT is an open user facility available for scientists from any country. It is also part of the European VLBI network (EVN) of radio telescopes.

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The Westerbork Synthesis Radio Telescope (WSRT) is a powerful radio telescope that uses a technique called "aperture synthesis" to generate radio images of the sky. The telescope consists of 14 steerable 25m dish antennas and enables astronomers to study a wide range of astrophysics phenomena.

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Callum O'Riordan, Clonkeen College

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Buranın, Türkiye'nin ilk radyo teleskopu olduğunu Astronomi ve Uzay Bilimleri Bölümü Başkanı Prof.Dr. İbrahim KÜÇÜK, "Aslında bu, büyük bir projenin küçük bir parçası. Aslında bir Ulusal Radyo Gözlemevi Kurulum Çalışması var. Bununla ilgili olarak TUBİTAK Ulusal Gözlemevi tarafından bir Kalkınma Bakanlığı çalışması yürütülüyor. Ama devam ettirilmedi.

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Callum O'Riordan, Clonkeen College

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Announcement Scientific Achievements FAST Approved Projects

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Callum O'Riordan, Clonkeen College

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Institute for Radio Astronomy and Space Research - AUT

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The Institute for Radio Astronomy and Space Research (IRASR) offers undergraduate teaching in Astronomy and Masters and PhD research in Radio Astronomy, Astrophysics and Space Geodesy. We have a 12m radio telescope and cutting edge IBM computing technology. We lead New Zealand’s academic effort to j…

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Atacama Large Millimeter Array - ALMA Radio Telescope, San Pedro de Atacama, Chile

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Atacama Large Millimeter Array - ALMA Radio Telescope, San Pedro de Atacama, Chile

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Atacama Large Millimeter Array - ALMA Radio Telescope, San Pedro de Atacama, Chile

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Fionnán Kelly, Clonkeen College

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Giant Metrewave Radio Telescope, Khodad, Maharashtra, India

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Giant Metrewave Radio Telescope, Khodad, Maharashtra, India

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Giant Metrewave Radio Telescope, Khodad, Maharashtra, India

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Fionnán Kelly, Clonkeen College

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NCRA a center of the school of natural sciences of the TIFR has set up a unique facility, the GMRT for radio astronomical research at metre wavelengths. GMRT is a very versatile instrument for investigating a variety of radio astrophysical problems ranging from nearby Solar system to the edge of observable Universe.

Introducing GMRT

NCRA has set up a unique facility for radio astronomical research using the metrewavelengths range of the radio spectrum, known as the Giant Metrewave Radio Telescope (GMRT), it is located at a site about 80 km north of Pune. GMRT consists of ... Continue Reading "

Upgraded GMRT

The UGMRT will increase its sensitivity by up to three times and make it a more powerful and versatile faclility. We describe the main goals of this upgrade, highlight the technical features and challenges, outline the science potential and update.. Continue Reading "

Expanded GMRT

At frequencies ranging from tens of MHz to hundreds of GHz, radio astronomy provides an outstanding and a unique window to study a wide range of astrophysical objects and phenomena. Continue Reading "

SKA India

The Square Kilometre Array (SKA), the next generation radio telescope, has almost completed the design stage for phase-I, after which SKA-I construction will start around 2019. Early science ... Continue Reading "

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Australian SKA Pathfinder Telescope, Murchison WA, Australia

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Australian SKA Pathfinder Telescope, Murchison WA, Australia

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Australian SKA Pathfinder Telescope, Murchison WA, Australia

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Fionnán Kelly, Clonkeen College

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Fionnán Kelly, Clonkeen College

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James Clerk Maxwell Telescope, N. A'ohoku Place University Park, Hilo, HI, USA

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James Clerk Maxwell Telescope, N. A'ohoku Place University Park, Hilo, HI, USA

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James Clerk Maxwell Telescope, N. A'ohoku Place University Park, Hilo, HI, USA

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Eoin Manning Clonkeen College

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Dr. Alex Tetarenko, a Hilo based astronomer who works at the James Clerk Maxwell Telescope (JCMT), has been collaborating with an international team of researchers to analyze new observations of the first black hole ever detected. Their discovery is leading astronomers to question what they know about the Universe's most mysterious objects.

Published today in the journal Science, the research shows that the system known as Cygnus X-1, contains the most massive stellar-mass black hole ever detected without the use of gravitational waves. "Our new observations have shown us that Cygnus X-1 is further away from Earth than previously thought, which in turn tells us this black hole is much larger than previous estimates, weighing in at more than 20 times the mass of our own Sun" says Dr. Tetarenko.

Cygnus X-1 is one of the closest black holes to Earth. It was discovered in 1964 when a pair of Geiger counters were carried on board a sub-orbital rocket launched from New Mexico. This object was famously the focus of a scientific wager between physicists Stephen Hawking and Kip Thorne, with Hawking betting in 1974 that it was not a black hole and eventually conceding the bet in 1990.

In this latest work, astronomers observed a full orbit of the black hole over a six day period using the Very Long Baseline Array - a continent-sized radio telescope made up of 10 dishes spread across the United States - together with a clever technique to measure distances in space. "One of the telescopes in the Very Long Baseline Array is located in Hawaiʻi on the slopes of Maunakea, and this antenna plays a critical role in making it possible to do this kind of science" explains Dr. Tetarenko.

Lead researcher, Professor James-Miller Jones from Curtin University and the International Centre for Radio Astronomy Research (ICRAR) outlines the clever technique used by this team of researchers. "If we can view the same object from different locations, we can calculate its distance away from us by measuring how far the object appears to move relative to the background. If you hold your finger out in front of your eyes and view it with one eye at a time, you'll notice your finger appears to jump from one spot to another. It's exactly the same principle."

"The domino effect of our new observations has led to fascinating new insights about how stars evolve and how black holes form" says co-author Dr. Arash Bahramian, who is also at Curtin University and ICRAR. Tetarenko and Bahramian are longtime colleagues, having both completed their PhDs at the University of Alberta in Canada.

In fact, this study has sparked two more companion papers. Co-author Professor Ilya Mandel from Monash University and the ARC Centre of Excellence in Gravitational Wave Discovery (OzGrav) further explains the wide reaching implications of this work.

"Cygnus X-1 in particular began life as a star approximately 60 times the mass of the Sun and collapsed tens of thousands of years ago. During their lifetime stars lose mass to their surrounding environment through stellar winds that blow away from their surface. But to make a black hole as heavy as Cygnus X-1, we need to dial down the amount of mass that bright stars lose during their lifetimes".

The new measurements of distance and mass also tell us that the black hole in Cygnus X-1 is spinning incredibly quickly (very close to the speed of light), as shown in a second companion paper led by PhD candidate, Xueshan Zhao, at the Chinese Academy of Sciences.

"All of these exciting discoveries were made possible by the collaboration between a diverse group of international astronomers focused on different observational and theoretical aspects of black holes, all coming together for a new extensive and rigorous look at a known but previously elusive black hole." adds Dr. Bahramian.

As the next generation of telescopes comes online, their improved sensitivity reveals the Universe in increasingly more detail, leveraging decades of effort invested by scientists and research teams around the world to better understand the cosmos and the exotic and extreme objects that exist.

"Studying black holes is like shining a light on the Universe's best kept secret-it's a challenging but incredibly exciting area of research" says Professor Miller-Jones. "There is so much left to discover about these enigmatic astrophysical objects" adds Dr. Tetarenko.

Original Publication:
'Cygnus X-1 contains a 21-solar mass black hole - implications for massive star winds', published in Science on February 18th, 2021.

Companion Papers:
'Reestimating the Spin Parameter of the Black Hole in Cygnus X-1', published in The Astrophysical Journal on February 18th, 2021.

'Wind mass-loss rates of stripped stars inferred from Cygnus X-1', published in The Astrophysical Journal on February 18th, 2021.
Contacts:
Dr. Alex Tetarenko, EAO Fellow, East Asian Observatory
a.tetarenko@eaobservatory.org

Dr. Jessica Dempsey, Deputy Director of the East Asian Observatory (EAO) and JCMT
j.dempsey@eaobservatory.org
Local Media Coverage

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Dr. Alex Tetarenko, a Hilo based astronomer who works at the James Clerk Maxwell Telescope (JCMT), has been collaborating with an international team of researchers to analyze new observations of the first black hole ever detected. Their discovery is leading astronomers to question what they know about the Universe's most mysterious objects.

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Effelsberg 100-m Radio Telescope, Bad Münstereifel, Germany

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Effelsberg 100-m Radio Telescope, Bad Münstereifel, Germany

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Effelsberg 100-m Radio Telescope, Bad Münstereifel, Germany

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Eoin Manning Clonkeen College

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Mit 100 Metern Durchmesser gehört das am 12. Mai 1971 eingeweihte Radioteleskop Effelsberg zu den beiden größten vollbeweglichen Radioteleskopen der Erde. Seit der vollen Inbetriebnahme im Jahre 1972 wird kontinuierlich an der Verbesserung seiner Technologie gearbeitet. So wurden z.B. die Oberfläche des Hauptspiegels erneuert, Antriebsmotoren und -getriebe ausgetauscht, bessere und modernere Empfänger und Auswertegeräte („Backends") eingesetzt und natürlich auch die benutzten Rechner immer wieder durch aktuelle Hardware ersetzt. Daher gilt das Teleskop auch heute noch als eines der weltweit modernsten Teleskope.

Das Teleskop wird eingesetzt zur Beobachtung von Radiostrahlung aus dem gesamten Kosmos. Beobachtet werden u.a. Pulsare, kalte Gas- und Staubwolken, Sternentstehungsgebiete, Magnetfelder in der Milchstraße und von weiteren Galaxien, von Schwarzen Löchern ausgehenden Materiestrahlen und Kerne ferner Galaxien.

Effelsberg ist eine wichtige Station für das weltweite Zusammenschalten von Radioteleskopen. Mit dieser Technik gelingen die schärfsten Aufnahmen vom Kosmos überhaupt. Zur Verbesserung dieser Technologie arbeitet das Institut in mehreren Projekten zusammen mit nationalen und internationalen Forschungsinstituten und anderen Organisationen.

Einmalig - Europas leistungsfähigstes Radioteleskop in Bad Münstereifel-Effelsberg

Das Max-Planck-Institut für Radioastronomie (MPIfR) erforscht mit Hilfe des 100-Meter Radioteleskops in Bad Münstereifel - Effelsberg Vorgänge im Weltraum, die die Phantasie nicht weniger beflügeln als Hollywood-Produktionen.

Das Radioteleskop Effelsberg ist eines der leistungsfähigsten Observatorien in Europa. Die große Oberfläche der Antenne mit einer Öffnung von etwa 7.850 Quadratmetern ist wichtig für den sicheren Empfang der außerordentlich schwachen Radiosignale aus weiten Entfernungen. Der große Durchmesser von 100 m ist maßgeblich für das vergleichsweise hohe Winkelauflösungsvermögen. Das Gesamtgewicht der Stahlkonstruktion beträgt 3.200 Tonnen. In knapp fünfzehn Minuten kann der Parabolspiegel des Teleskops um 360 Grad gedreht und in ca. fünf Minuten um nahezu 90 Grad gekippt werden. Dadurch kann der gesamte Himmel über dem Horizont mit dem Teleskop beobachtet werden.

Ein Ziel für Besucher aus aller Welt

Das Radioteleskop zieht seit seiner Fertigstellung im Jahre 1971 viele Besucher aus dem In- und Ausland an.

In einem Pavillon direkt in Sichtweite des Radioteleskops Effelsberg finden regelmäßig Vorträge für Besuchergruppen statt.

Die Radioteleskope des Radio-Observatoriums Effelsberg (100-m-Teleskop & LOFAR-Station Effelsberg) sind hochempfindliche Empfangsanlagen für extrem schwache Radiosignale von astronomischen Quellen aus den Tiefen des Universums. Von Menschen erzeugte Radiostrahlung unterschiedlichster Art kann diese Messungen empfindlich stören.

Daher Handys, Tablets und andere elektronische Geräte in der direkten Umgebung des 100-m-Radioteleskops am besten ganz aus oder aber in den Flugmodus schalten!

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Mit 100 Metern Durchmesser gehört das Radioteleskop Effelsberg zu den größten vollbeweglichen Radioteleskopen der Erde. Seit der Inbetriebnahme im Jahre 1972 wurde kontinuierlich an der Verbesserung seiner Technologie gearbeitet (z.B. eine neue Oberfläche der Antennen-Schüssel, bessere Empfänger für hochqualitative Daten, extrem rauscharme Elektronik) so dass es auch heute noch als eins der weltweit modernsten Teleskope gilt.

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Green Bank Telescope, Observatory Road, Green Bank, WV, USA

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Green Bank Telescope, Observatory Road, Green Bank, WV, USA

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Green Bank Telescope, Observatory Road, Green Bank, WV, USA

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Eoin Manning Clonkeen College

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New 'black widow' millisecond pulsar discovered

Multi-band radio pulse profiles of PSR J1555-2908. Credit: Ray et al., 2022.

An international team of astronomers reports the detection of a new millisecond pulsar (MSP) using the Green Bank Telescope (GBT). The newfound pulsar, designated PSR J1555−2908, turns out to be one of the so-called "black widow" MSPs. The finding is detailed in a paper published February 10 on arXiv.org.

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New 'black widow' millisecond pulsar discovered An international team of astronomers reports the detection of a new millisecond pulsar (MSP) using the Green Bank Telescope (GBT). The newfound pulsar, designated PSR J1555−2908, turns out to be one of the so-called "black widow" MSPs. The finding is detailed in a paper published February 10 on arXiv.org.

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Arecibo Observatory, Puerto Rico 625, Arecibo, Puerto Rico

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Arecibo Observatory, Puerto Rico 625, Arecibo, Puerto Rico

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Arecibo Observatory, Puerto Rico 625, Arecibo, Puerto Rico

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Eoin Manning Clonkeen College

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The Green Bank Observatory (GBO) and Arecibo Observatory (AO) are jointly hosting a hybrid in-person/remote Single Dish Observing School and GBT Training Workshop from September 13-21 in Green Bank, West Virginia. Please feel free to pass this message on to any interested colleagues. + Read More

# data[].attributes.location_name
I-LOFAR, Rosse Row, Townparks, Birr, County Offaly

# data[].attributes.headline
I-LOFAR, Rosse Row, Townparks, Birr, County Offaly

# data[].attributes.subject
I-LOFAR, Rosse Row, Townparks, Birr, County Offaly

# data[].attributes.body
Eoin Manning Clonkeen College

# data[].attributes.attachment_link.description
Exploring the radio universe from Ireland

# data[].attributes.location_name
Clonkeen College, Clonkeen Road, Deansgrange, Blackrock, County Dublin, Ireland

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Clonkeen College, Clonkeen Road, Deansgrange, Blackrock, County Dublin, Ireland

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Clonkeen College, Clonkeen Road, Deansgrange, Blackrock, County Dublin, Ireland

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We are a boys school in south Dublin with approximately 575 students.