There are two types of telescopes commonly used to explore the universe. Optical telescopes, such as Hubble and James Webb, rely on visible light emitted from the stars, planets and other bodies in space and produce photographic images. The other type, radio telescopes, are designed to detect the radio waves emitted by these same bodies and other sources.
A key advantage of radio waves is that they can pass through gases, clouds and other obstacles in space that might block or obscure visible light, making visible many bodies that otherwise could remain hidden. Radio signals also offer information about invisible aspects of the universe: gravity, magnetism, black holes and dark energy. These data help astronomers and physicists develop a better understanding of how the universe began, how it’s organized, how it behaves and how it’s evolving.
Because radio signals have longer wavelengths than visible light, the radio telescope used to detect them doesn’t have to be as precisely shaped as its optical cousin. But to obtain the same level of detail and resolution as the optical version, radio telescopes must have a much larger collection area. The largest radio telescope in the world, with a main reflector dish diameter of 300m/984 ft, is the Arecibo telescope, in Puerto Rico. However, even a dish of this size cannot match the resolution of an optical
To produce photo-equivalent detail and resolution, a radio telescope’s reflector dish must have an area measured in kilometers, not meters. This can be accomplished in one of two ways. One is to manufacture one large dish that measures about 1 km2/0.39 mi2. Such a large dish, however, would have to be in a fixed position and thus could not be repositioned to receive signals from different regions of space. Ideally, then, radio signal exploration would require a large adjustable dish, able to maintain positional accuracy within ±1 mm/0.04 inch. A more feasible alternative is to manufacture a series of smaller dishes in an array known as an interferometer. Practically, these individual dishes may be located anywhere, as long as each can “see” the same portion of the sky. The goal of an interferometer, then, is a combined dish area of about 1 km2. Signals received by each dish in an interferometer are centrally collected and processed by a correlator, which combines the signals (adjusting for each telescope’s position in the array) to simulate a much larger telescope.
This is the premise of the Square Kilometre Array program (SKA, Manchester, U.K., www.skatelescope.org). A multinational effort, its participants hope, by 2030, to have in place thousands of radio telescopes clustered in remote regions of South Africa and Australia. SKA envisions the manufacture of three types of radio telescope: A conventional circular dish, a low-frequency aperture array and a mid-frequency aperture array. SKA has gathered consortia of manufacturers and software developers to create the telescope systems and the other equipment that the project requires.
One of the first deliverables is a dish type, with a 15m/49.2-ft diameter primary reflector, which is being competitively prototyped by three organizations, one in Canada (called DVA-1), one in China (DVA-C) and one in South Africa (MeerKAT 1). Of these, only the Chinese and Canadian versions employ carbon fiber composites in significant amounts. The Canadian fabrication marks one of the most ambitious applications of carbon fiber composites in a dish structure of any kind.
Building the perfect dish
The Canadian DVA-1 dish is an offset Gregorian type. Its mostly composite 15m primary reflector reflects captured radio signals up to a 4m/13.1-ft diameter secondary reflector dish, positioned on support legs over the main dish. From the secondary reflector, radio signals are received by hardware on a feed support platform located between the secondary and primary reflectors (see opening image). Of the other critical structures, some are fabricated from metals and some are fabricated from composites. The main dish’s support truss, as well as the pedestal on which it rests, for example, are metallic. However, the feedlegs that support the secondary reflector and feed support platform are manufactured with carbon fiber composites.
DVA-1 was built by the National Research Council Canada (NRC-Canada, Ottawa, Ontario, Canada). Most production work was done at NRC’s facility in Penticton, British Columbia. Gordon Lacy, an NRC-Canada mechanical engineer and DVA-1’s lead engineer, has been working on dish design and development since 2006, adjusting to shifting political and financial winds as a variety of governments and government agencies around the world entered and exited the SKA project. He admits that the decision to use carbon fiber might be questioned because of the material’s cost, but when NRC-Canada looked at the mechanical requirements, he says carbon fiber was the logical choice.
“The dish requires very high precision of the reflective surfaces under wind, gravity and temperature changes,” he notes. “For the best radio-frequency performance, we need the reflectors to retain their design shape under all conditions. We also need the reflector to have a high reflectivity to radio waves. For this we have developed an embedded metallic layer. Carbon fiber has a very high stiffness-to-weight ratio, which enables us to more easily meet the gravitational distortion requirements. Carbon fiber composites also have very low coefficients of thermal expansion [CTE], which helps us to meet our thermal stability requirements.”
To meet all of DVA-1’s tolerance requirements, NRC partnered with composites manufacturers that were accustomed to working to that level of precision. Among the first was Janicki Industries (Sedro-Woolley, Wash.), which supplied the massive mold for the main reflector. The tool is possibly the most critical component, says Lacy, because its accuracy dictates the dimensional tolerance of the finished product. “The tool had to keep the shape of the mold, or we had to be able to predict very accurately what the shape change was going to be,” he recalls. “We opted just for keeping the shape under control, so it’s very close to the mold shape.”
Janicki manufactured a five-piece, prototype-type mold of fiberglass, topped by a putty layer, on a steel substructure. Lacy says NRC-Canada used a FARO (Lake Mary, Fla.) laser tracker to accurately fix mold position as the sections were assembled. “It’s a somewhat flexible mold,” he explains, “so we were then able to push up and pull down on the surface from underneath a little bit to adjust it.”
The fully assembled mold offers a surface error of less than 0.5 mm/0.02 inch, reports Lacy. As a testament to the accuracy of the finished, molded main reflector, he adds, a laser scan of it was compared to the CAD model, revealing a surface error — 0.9 mm/0.04 inch — that barely exceeded that of the mold. “You can’t get less than the mold’s error, of course,” Lacy quips. “It means that there is almost no shrinkage in the part.”
The main reflector measures 5.3 mm/0.21 inch thick and comprises — from signal-facing side to back side — a 0.08-mm/0.003-inch layer of aluminum for signal reflectivity, a ply of woven glass fiber to protect against galvanic corrosion, and several plies of A&P Technology’s (Cincinnati, Ohio) QISO triaxial braided carbon fiber — in this case, Toray’s (Tokyo, Japan) T700 material. The entire layup is bagged and the resin, HETRON 922 vinyl ester from Ashland Performance Materials (Columbus, Ohio), is infused in one shot, in about an hour. Lacy reports that infusion provides the greatest process control most affordably. “It’s such a large part that infusion gave us the best trade-off in terms of performance and cost.” Infusion modeling was done by Lacy with Polyworx (Nijverdal, The Netherlands) software.
The main reflector, when installed, must be anchored to the primary support structure, a latticework of metallic tubes that joins the reflector to the mechanized pedestal on which it rests. Each dish must connect to 14 tubes at eight connection points (some connection points receive two tubes). Each connection must be adjustable as the dish is erected, and then tightened and secured when it is properly positioned. Connection points are built into what’s called the dish rim, also a composite. The rim is molded separately and bonded to a vertical flange at the edge of the dish.
Lacy in cooperation with NRC-Canada partner Profile Composites’ (Kingston, Wash.) CEO Geoff Wood, worked on a dish rim connector (DRC). It features a unique ball-and-joint design that cleverly and securely anchors the dish to the support structure. There are several types and sizes of DRC, depending on the DRC’s location and whether or not it’s accommodating one or two support structure tubes.
A 10.2-inch/259-mm long threaded stainless steel bolt, with a 4-inch/102-mm ball on one end, is enclosed in the DRC, which has two primary parts, the DRC inner and the DRC outer. The DRC inner is a compression-molded carbon fiber base that contains half of the ball socket(s) for one or two bolts. The DRC outer is similar and contains each socket’s other half. The bolt’s ball, coated with mold release to keep it “free” in the socket, is placed in the DRC inner and then covered with the DRC outer, thus completing the ball-and-socket joint. These two halves are then bonded together with a methacrylate adhesive (see Step 9). The assembled DRC is then bonded into its own pocket in the dish rim, also with methacrylate adhesive.
When complete, the dish is equipped with eight DRCs, each with either one or two threaded bolts protruding and ready to be attached to support tubes during dish erection. Lacy says that after a dish is installed and oriented on the support structure per specification, CHOCKFAST ORANGE, a poured-in-place epoxy chocking compound from ITW Polymers Coatings (Montgomeryville, Pa.), will be injected into each ball joint to provide rigidity and increase strength. “The fit [of the ball joint] is really quite good,” Lacy explains. “But since we want the best possible positional accuracy, any movement in any joint is detrimental to this alignment.”
A little wind
NRC-Canada completed the primary dish for DVA-1 in fall 2013. The next step was to transport the assembled dish, weighing 2.8 metric tonnes (about 6,170 lb), via helicopter to its pedestal, which had been constructed in a secluded “radio-quiet” area about 5 km/3 miles from Penticton. However, as it approached its destination, tethered beneath the helicopter in a horizontal position, a sudden and relatively violent gust of wind flipped it into vertical position. When the gust abated, the dish fell back into its original horizontal position. Although it was still tethered to the helicopter, the dish had buckled, leaving it badly misshapen and deformed (see end note).
Initial reaction to the dish damage at NRC-Canada was pessimistic. “Most people thought it was a write-off,” says Lacy. But as the organization studied its options, repair seemed more and more viable. The first step was to “pop” the dish back into shape with the help of a local industrial-services company that deploys inflatable bags to help move cars and trucks involved in accidents. The bags were inserted under the dish and inflated to “push” the deformed sections back into their original shape.
It worked, says Lacy, and the dish remained remarkably close to the tolerances measured before it was damaged. There remained, however, 21 cracks in the composite structure. These were scarfed, patched, bagged and re-infused at the assembly site under an improvised polymer dome erected over the dish to keep out the cold weather. In the end, he says, NRC-Canada was able to completely restore the dish to specification. “It was a blessing in disguise,” Lacy says of the wind damage. “The process really demonstrated that it could be repaired.”
The refurbished dish was ready again to join the support structure, and the two together weigh 8.7 metric tonnes (nearly 19,200 lb). They were lifted onto and attached successfully to the pedestal. At press time, the telescope was awaiting installation of the secondary collector (a smaller version of the primary collector, also made at NRC-Canada), as well as the feed support platform that holds the signal-receiving equipment. The secondary collector and the platform are supported by a latticework of carbon fiber tubes designed and manufactured by Profile Composites. Profile’s Wood says these tubes also are made from A&P Technology’s unidirectional woven fiber in a tubular preform shape, with elastomeric fibers woven in to give the preforms flexibility for easy fit over mandrels. Infused with epoxy, the tubes are made in three diameters, 75 mm to 100 mm to 151 mm (2.9 to 3.9 to 5.9 inches), in a variety of lengths, with wall thicknesses that range from 4 mm to 6 mm (0.26 inch to 0.24 inch).
After the entire dish is assembled and functional, NRC-Canada will start receiving radio signals as part of the overall testing and evaluation program for SKA. Under the current SKA schedule, a preliminary design review will be conducted in fall 2014, followed by critical design review in spring 2015. If NRC-Canada’s design is selected, a second prototype will be produced in 2016. Phase 1 will follow, which calls for the manufacture of 150 receivers for installation in South Africa and another 50 to 60 receivers for installation in Western Australia. Phase 2 of SKA calls for a substantial ramp-up in production, culminating in the manufacture and installation of a total of 2,500 radio telescopes across the two countries.
Lacy admits that Phase 2 “will require a great deal of international investment,” which is still being arranged and coordinated. However, the fact that SKA has survived and persisted long enough to produce the radio telescope prototypes that are currently under evaluation shows that the project has developed some momentum. The world might yet see the installation of a very large array of very large carbon fiber radio telescopes.
Editor's Note: View the video of dish transport, damage and repair efforts here.
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