Parkes Observatory is aradio astronomy observatory, located 20 kilometres (12 mi) north of the town ofParkes, New South Wales, Australia. It hostsMurriyang, the 64 m CSIRO Parkes Radio Telescope also known as "The Dish",[1] along with two smallerradio telescopes. The 64 m dish was one of several radio antennae used to receive live television images of theApollo 11 Moon landing. Its scientific contributions over the decades led theABC to describe it as "the most successful scientific instrument ever built in Australia" after 40 years of operation.[1]
TheParkes Radio Telescope, completed in 1961, was the brainchild ofE. G. "Taffy" Bowen, chief of theCSIRO's Radiophysics Laboratory. During theSecond World War, he had worked on radar development in the United States and had made connections in its scientific community. Calling on thisold boy network, he persuaded two philanthropic organisations, theCarnegie Corporation and theRockefeller Foundation, to fund half the cost of the telescope. It was this recognition and key financial support from the United States that persuaded Australian prime minister,Robert Menzies, to agree to fund the rest of the project.[3]
The Parkes site was chosen in 1956, as it was accessible, but far enough from Sydney to have clear skies. Additionally the mayor Ces Moon and landowner Australia James Helm were both enthusiastic about the project.[4]
The 64-metre (210 ft) diameter dish with the 18-metre (59 ft) dish in the foreground (mounted on rails and used in interferometry)
The primary observing instrument is the 64-metre (210 ft) movable dish telescope, second largest in the Southern Hemisphere, and one of the first large movable dishes in the world (DSS-43 atTidbinbilla was extended from 64-metre (210 ft) to 70-metre (230 ft) in 1987, surpassing Parkes).[7]
The inner part of the dish is solidaluminium and the outer area a fine aluminium mesh,[8] creating its distinctive two-tone appearance.
In the early 1970s the outer mesh panels were replaced by perforated aluminium panels. The inner smooth plated surface was upgraded in 1975 which provided focusing capability for centimetre- and millimetre-lengthmicrowaves.[9]
The inner aluminium plating was expanded out to a 55 metres (180 ft) diameter in 2003, improving signals by 1dB.[10]
The telescope has analtazimuth mount. It is guided by a small mock-telescope placed within the structure at the same rotational axes as the dish, but with anequatorial mount. The two are dynamically locked when tracking an astronomical object by alaser guiding system. This primary-secondary approach was designed byBarnes Wallis.
The focus cabin is located at the focus of the parabolic dish, supported by three struts 27 metres (89 ft) above the dish. The cabin contains multipleradio andmicrowave detectors, which can be switched into the focus beam for different science observations.
1,050-centimetre (34.4 ft) receiver(Replaced now by UWL)
The Multibeam Receiver – a 13-horned receiver cooled at −200 °C (−328.0 °F; 73.1 K) for the 21-centimetre (8.3 in) Hydrogen line.[12][13]
H-OH receiver(Replaced now by UWL)
GALILEO receiver(Replaced now by UWL)
AT multiband receivers, covering 2.2-2.5,4.5-5.1 and 8.1-8.7 GHz
METH6, covering 5.9-6.8 GHz
MARS (X band receiver), covering 8.1-8.5 GHz
KU-BAND, covering 12–15 GHz
13MM (K band receiver), covering 16–26 GHz
Ultra Wideband Low (UWL) receiver – installed in 2018 it can simultaneously receive signals from 700 MHz to 4 GHz.[14] It is cooled to −255 °C (−427.0 °F; 18.1 K) to minimise noise and will enable astronomers to work on more than one project at once.[6][15]
The 18-metre (59 ft) "Kennedy Dish" antenna was transferred from theFleurs Observatory (where it was part of theMills Cross Telescope) in 1963. Mounted on rails and powered by a tractor engine to allow the distance between the antenna and the main dish to be easily varied, it was used as aninterferometer with the main dish. Phase instability due to an exposed cable meant that its pointing ability was diminished, but it was able to be used for identifying size and brightness distributions. In 1968 it successfully proved thatRadio galaxy lobes were not expanding, and in the same era contributed toHydrogen line andOH investigations. As a stand-alone antenna it was used in studying theMagellanic Stream.[16]
It was used as an uplink antenna in the Apollo program, as the larger Parkes telescope is receive-only.[17] It is preserved by the Australia Telescope National Facility.[18]
The Parkes observatory is positioned to be isolated from radio frequency interference. The site also sees dark skies in optical light, as seen here in June 2017 with the Milky Way Galaxy overhead.
A 1962 series oflunar occultations of the radio source3C 273 observed by the Parkes Telescope were used to locate its exact position, allowing astronomers to find and study its visual component. Soon to be called "quasi-stellar radio sources" (quasar), Parkes observation was the first time this type of object to be associated with an optical counterpart.[19]
1964 to 1966, all-sky survey at 408 MHz of the southern sky is conducted and published (first version of theParkes Catalogue of Radio Sources) finding over 2000 radio sources including many new quasars.[20]
Second all-sky survey at 2,700 MHz begins in 1968 (completed in 1980).[20]
Fast radio bursts were discovered in 2007 whenDuncan Lorimer ofWest Virginia University assigned his student David Narkevic to look through archival data recorded in 2001 by the Parkes radio dish.[23]Analysis of the survey data found a 30-janskydispersed burst which occurred on 24 July 2001,[24] less than 5 milliseconds in duration, located 3° from theSmall Magellanic Cloud.[25] At the time it was theorised FRBs might be signals from another galaxy, emissions from neutron stars or black holes.[26] More recent results confirm thatmagnetars, a kind of highly magnetised neutron star, may be one source of fast radio bursts.[27]
In 1998 Parkes telescope began detecting fast radio bursts and similar looking signals namedperytons. Perytons were thought to be of terrestrial origin, such as interference from lightning strikes.[28][29][30][31] In 2015 it was determined that perytons were caused by staff members opening the door of the facility's microwave oven during its cycle.[32][33][34] When the microwave oven door was opened, 1.4 GHz microwaves from themagnetron shutdown phase were able to escape.[35] Subsequent tests revealed that a peryton can be generated at 1.4 GHz when a microwave oven door is opened prematurely and the telescope is at an appropriate relative angle.[36]
The telescope has been contracted to be used in a search for radio signals from extraterrestrial technologies for the heavily funded projectBreakthrough Listen.[37][38] The principal role of the Parkes Telescope in the program will be to conduct a survey of the Milky Way galactic plane over 1.2 to 1.5 GHz and a targeted search of approximately 1000 nearby stars over the frequency range 0.7 to 4 GHz.
The 64-metre (210 ft) radio telescope at Parkes Observatory as seen in 1969, when it received signals from theApollo 11 Moon landing
During theApollo missions to theMoon, the Parkes Observatory was used to relay communication and telemetry signals toNASA, providing coverage for when the Moon was on the Australian side of the Earth.[39]
The telescope also played a role in relaying data from the NASAGalileo mission to Jupiter that required radio-telescope support due to the use of its backup telemetry subsystem as the principal means to relay science data.
The observatory has remained involved in tracking numerous space missions up to the present day, including:
Voyager missions (but no longer due to distance of the probes, only the 70-metre (230 ft) dish at theCDSCC can still communicate with the two Voyager probes,Voyager 1 andVoyager 2.)[40]
To assist in a busy spaceflight period at the end of 2003 to early 2004, theCanberra Deep Space Communication Complex (CDSCC) incorporated the Parkes dish. NASA upgraded the antenna through the CDSCC with new receivers and equipment capable of handling transmissions from robotic spacecraft. When its research time allows, Parkes can act as a spare 'ear' for CDSCC during times of high activity. While being used thus it is designated as DSS (Deep Space Station)-49.[42]
The CSIRO has made several documentaries on this observatory, with some of these documentaries being posted to YouTube.[43]
WhenBuzz Aldrin switched on the TV camera on theLunar Module, three tracking antennas received the signals simultaneously. They were the 64-metre (210 ft)Goldstone antenna in California, the 26-metre (85 ft) antenna atHoneysuckle Creek near Canberra in Australia, and the 64-metre (210 ft) dish at Parkes.
Since they started the spacewalk early, the Moon was only just above the horizon and below the visibility of the main Parkes receiver. Although they were able to pick up a quality signal from the off axis receiver, the international broadcast alternated between signals from Goldstone and Honeysuckle Creek, the latter of which ultimately broadcastNeil Armstrong's first steps on the Moon worldwide.[44][39]
Celebrations on 19 July 2009 to mark the 40th anniversary of the Moon landing, and Parkes' role in it. "The Dish" behind is at full extension to the ground.
A little under nine minutes into the broadcast, the Moon rose far enough to be picked by the main antenna and the international broadcast switched to the Parkes signal. The quality of the TV pictures from Parkes was so superior that NASA stayed with Parkes as the source of the TV for the remainder of the 2.5-hour broadcast.[45][39]: 287–288
In the lead up to the landing wind gusts greater than 100 km/h (62 mph) were hitting the Parkes telescope, and the telescope operated outside safety limits throughout the moonwalk.[39]: 300–301
In 2012 the observatory received special signals from the Mars roverOpportunity (MER-B), to simulate theCuriosity rover UHF radio.[46] This helped prepare for the then upcomingCuriosity (MSL) landing in early August—it successfully touched down on 6 August 2012.[46]
The Parkes Observatory Visitors Centre allows visitors to view the dish as it moves. There are exhibits about the history of the telescope, astronomy, and space science, and a 3-D movie theatre.
In 1995 the radio telescope was declared aNational Engineering Landmark byEngineers Australia.[47] The nomination cited its status as the largest southern hemisphere radio telescope, elegant structure, with features mimicked by laterDeep Space Network telescopes, scientific discoveries and social importance through "enhancing [Australia's] image as a technologically advanced nation".[48]
On Monday, 31 October 2011, Google Australia replaced its logo with aGoogle Doodle in honour of Parkes Observatory's 50th anniversary.[49]
In 1964 the telescope featured in the opening credit sequence ofThe Stranger, Australia's first locally produced sci-fi TV series. Some scenes were also shot on location at the telescope and inside the observatory.[51]
The observatory and telescope were featured in the 2000 filmThe Dish, a fictionalised account of the observatory's involvement with theApollo 11 Moon landing.[52]
In November 2020, inNAIDOC Week, the Observatory's three telescopes were givenWiradjuri names. The main telescope ("The Dish") isMurriyang, after the home in the stars of Biyaami, the creator spirit. The smaller 12m dish built in 2008 isGiyalung Miil, meaning "Smart Eye". The third, decommissioned antenna isGiyalung Guluman, meaning "Smart Dish".[53]
^Goss, W.M.; Hooker, C.; Ekers, R.D. (2023)."Reflections on GRT Science, post 1961.".Joe Pawsey and the Founding of Australian Radio Astronomy. Historical & Cultural Astronomy. Springer, Cham. pp. 493–517.doi:10.1007/978-3-031-07916-0_32.ISBN978-3-031-07915-3. Retrieved19 March 2023.The Parkes Telescope also proved timely for the US space programme. Bowen received a NASA grant for Minnett to participate in studies at the Jet Propulsion Laboratory … for the design of a 210 ft instrument [in the end three of these were constructed] for communicating with very distant space probes. Many of the Parkes features, including the drive and control concepts, were adopted.
^Staveley-Smith, Lister (27 May 1997)."Multibeam Receiver Description". Australia Telescope National Facility.Archived from the original on 19 March 2019. Retrieved17 July 2019.
Related media on Commons
