ERIS is open to all who wish to gain a better insight to
radio interferometry techniques and methods.
Not exact matches
Not long ago I came across a piece in the Scientific American archives from the earliest days of very - long baseline
radio interferometry, the
technique employed by the Event Horizon Telescope.
This
technique, first introduced by British radioastronomer Roger Clifton Jennison in 1958, has been extensively applied in astronomical
interferometry since the mid 1970s, yielding high resolution images of astronomical sources at
radio, infrared and optical wavelengths.
However, by combining high - frequency
radio telescopes around the world, in a
technique called very long baseline
interferometry, or VLBI, even such a tiny feature is in principle detectable.
Very long baseline
interferometry (VLBI) is a
technique used by
radio astronomers to electronically link widely separated
radio telescopes together so they work as if they were a single instrument with extraordinarily sharp «vision,» or resolving power.
The
technique of combining
radio waves, known as very long baseline
interferometry, is common enough in
radio astronomy.
With the
technique of very long baseline
interferometry, astronomers can hook up
radio telescopes, distant from one another in different countries and on continents, to mimic a single «virtual» telescope with an aperture as wide as Earth.
Very long baseline
interferometry is a
technique used by
radio astronomers to electronically link widely separated
radio telescopes together so they work as if they were a single instrument with extraordinarily sharp «vision,» or resolving power.
Although super small, this angular size can actually be resolved by astronomical observations using an interferometric
technique at
radio wavelengths, called Very Long Baseline
Interferometry or VLBI (see here for details).