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very-long-baseline interferometry

(interferometry based upon storing timing data at each telescope)

Very-long-baseline interferometry (VLBI) is a type of radio telescope interferometry where the necessary timing is stored at each telescope and later analysis is used to determine the direction from which the signal came, allowing telescopes far apart to be used. It has achieved angular resolution in the 10 microarcsecond range.

While it clearly is useful for observing sufficiently bright radio sources, it offers as a byproduct, measurement of changes in the distance between receivers, down to the millimeter range, thus reveals the effects of plate tectonics.

The arrays often use existing telescopes, and may be short-term projects, e.g., for specific surveys. Some VLBI arrays:

A recent development is electronic very-long-baseline interferometry, which is near-real-time transmission of the data for immediate analysis.


Referenced by:
Australia Telescope Compact Array (ATCA)
Dominion Radio Astrophysical Observatory (DRAO)
Earth-sized VLBI
electronic very-long-baseline interferometry (e-VLBI)
European VLBI Network (EVN)
Green Bank 140 Foot Telescope
Greenland Telescope (GLT)
Gould's Belt Distances Survey (GOBELINS)
International Celestial Reference System (ICRS)
Mark II (MKII)
Max Planck Institute for Radio Astronomy (MPIR)
radio astronomy
spectral correlator