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An astronomical interferometer or telescope array is a set of separate telescopes, mirror segments, or radio telescope antennas that work together as a single telescope to provide higher resolution images of astronomical objects such as stars, nebulas and galaxies by means of interferometry.
In optical astronomy, interferometry is used to combine signals from two or more telescopes to obtain measurements with higher resolution than could be obtained with either telescopes individually. This technique is the basis for astronomical interferometer arrays, which can make measurements of very small astronomical objects if the telescopes ...
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.
Very-long-baseline interferometry (VLBI) is a type of astronomical interferometry used in radio astronomy. In VLBI a signal from an astronomical radio source, such as a quasar, is collected at multiple radio telescopes on Earth or in space. The distance between the radio telescopes is then calculated using the time difference between the ...
The concept of aperture synthesis was first formulated in 1946 by Australian radio astronomers Ruby Payne-Scott and Joseph Pawsey.Working from Dover Heights in Sydney, Payne-Scott carried out the earliest interferometer observations in radio astronomy on 26 January 1946 using an Australian Army radar as a radio telescope.
Holographic interferometer; Jamin interferometer; Laser Doppler vibrometer; Linnik interferometer (microscopy) LUPI variant of Michelson; Lummer–Gehrcke interferometer; Mach–Zehnder interferometer; Martin–Puplett interferometer; Michelson interferometer; Mirau interferometer (also known as a Mirau objective) (microscopy) Moiré ...
Aperture Masking Interferometry is available on the James Webb Space Telescope, which is the first execution of this technique (or any form of interferometry) in space. This is enabled by a non-redundant mask with seven holes (sub-apertures), which is embedded as a mode of the NIRISS instrument.
These ten radio antennas work together as an array that forms the longest system in the world that uses very long baseline interferometry. The longest baseline available in this interferometer is about 8,611 kilometers (5,351 mi). [2] The construction of the VLBA began in February 1986 and it was completed in May 1993.