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Interferometry is used in radio astronomy, with timing offsets of D sin θ. In physics, one of the most important experiments of the late 19th century was the famous "failed experiment" of Michelson and Morley which provided evidence for special relativity.
Aperture synthesis is possible only if both the amplitude and the phase of the incoming signal are measured by each telescope. For radio frequencies, this is possible by electronics, while for optical frequencies, the electromagnetic field cannot be measured directly and correlated in software, but must be propagated by sensitive optics and interfered optically.
The Donald C. Backer Precision Array for Probing the Epoch of Reionization (PAPER) is a radio interferometer funded by the National Science Foundation [1] to detect 21 cm hydrogen (HI) fluctuations occurring when the first galaxies ionized intergalactic gas at around 500 million years after the Big Bang.
BOFFIN : A Personal Story of the Early Days of Radar, Radio Astronomy and Quantum Optics. Adam Hilger. ISBN 978-0-7503-0130-5. Mark P. Silverman (1995). More Than One Mystery: Explorations in Quantum Interference. Springer. ISBN 978-0-387-94376-3. R Hanbury Brown (1974). The intensity interferometer; its application to astronomy. Wiley.
The Submillimeter Array (SMA) consists of eight 6-meter (20 ft) diameter radio telescopes arranged as an interferometer for submillimeter wavelength observations. It is the first purpose-built submillimeter interferometer, constructed after successful interferometry experiments using the pre-existing 15-meter (49 ft) James Clerk Maxwell Telescope and 10.4-meter (34.1 ft) Caltech Submillimeter ...
HERA is a radio interferometer, cross-correlating the signals from pairs of individual antennas. Radio interferometers intended for imaging are usually designed to minimize the number of identical baselines, in order to measure emission at the largest possible number of spatial frequencies for image reconstruction. [ 5 ]
Three radio telescope receivers. A minimum of three antennas are required for closure phase measurements. In the simplest case, with three antennas in a line separated by the distances a 1 and a 2 shown in diagram at the right. The radio signals received are recorded onto magnetic tapes and sent to a laboratory such as the Very Long Baseline Array.
The Atacama Large Millimeter Array (ALMA), many antennas linked together in a radio interferometer An optical image of the galaxy M87 , a radio image of same galaxy using interferometry (Very Large Array, VLA), and an image of the center section (VLBA) using a Very Long Baseline Array (Global VLBI) consisting of antennas in the US, Germany ...