radio telescope

Radio telescopes, like this one (the world's largest) at Arecibo, Puerto Rico, allow astronomers to analyse a broad range of low-frequency electromagnetic waves – visible light is only a small part of the electromagnetic spectrum. Pulsars and quasars were first discovered by radio telescopes.

A radio telescope dish at Soccorro, New Mexico, USA. This particular site contains the VLA or Very Large Array, in which 27 dishes are so arranged and linked that they simulate the capabilities of a single dish 27 km/17 mi in diameter. Each dish in the VLA is 25 m/82 ft in diameter.

The 70-m/230-ft antenna of the Canberra deep-space communications complex. The Australian facility is one of three sites that make up NASA's deep-space network, the others are in Goldstone, California, and Robledo near Madrid, Spain.

Instrument for detecting radio waves from the universe in radio astronomy. Radio telescopes usually consist of a metal bowl that collects and focuses radio waves the way a concave mirror collects and focuses light waves. Radio telescopes are much larger than optical telescopes, because the wavelengths they are detecting are much longer than the wavelength of light. The largest single dish is at Arecibo Observatory, Puerto Rico.

A large dish such as that at Jodrell Bank, Cheshire, England, can see the radio sky less clearly than a small optical telescope sees the visible sky. Interferometry is a technique in which the output from two dishes is combined to give better resolution of detail than with a single dish. Very long baseline interferometry (VBLI) uses radio telescopes spread across the world to resolve minute details of radio sources. The deep-space network (DSN) works in this way to track artificial satellites.

In aperture synthesis, several dishes are linked together to simulate the performance of a very large single dish. This technique was pioneered by English radio astronomer Martin Ryle at the Mullard Radio Astronomy Observatory, Cambridge, England, site of a radio telescope consisting of eight dishes in a 5-km/3-mi line. The Very Large Array in New Mexico consists of 27 dishes arranged in a Y-shape, which simulates the performance of a single dish 27 km/17 mi in diameter. Other radio telescopes are shaped like long troughs, and some consist of simple rod-shaped aerials.

The building of two new large-array telescopes was approved by different international teams in August 2000. The Atacama Large Millimeter Array (ALMA), scheduled for completion by 2010 and situated in the Atacama Desert, Chile, will consist of 64 antennae, each measuring 12 m/39 ft. The Square Kilometre Array (SKA) is scheduled to begin construction in 2010 and its design and location are still to be decided. It will be a centimetre-wave radio array with a total collecting area, possibly scattered over many instruments, of one square kilometre (a million square metres).