interferometer

Of these, the last is peculiar to the interferometer itself.

They are part of a project to build an astronomical interferometer.

These large telescopes can also work together in groups of two or three as a giant interferometer.

Most interferometers use light or some other form of electromagnetic wave.

Another interferometer often used has a white light source.

The wave character of matter can be exploited to build interferometers.

The telescopes can operate together to form a single astronomical interferometer.

They did this with a device called an interferometer.

The other interferometer arm is bounced off a reference mirror.

No, there are always two ports on an interferometer.

Early radio telescope interferometers used a single baseline for measurement.

The advantage of the Rayleigh interferometer is its simple construction.

From 1980-1985 a 3-element interferometer was constructed, with another four antennas added between 1990-1992.

Up to five interferometers can be set up in each vacuum system.

The basic configuration is the same as a Michelson interferometer.

In 1946 he built the first multi-element astronomical radio interferometer.

One interferometer must use a broadband source that will probe the sample.

Fig. 1 shows the interferometer set up to test a spherical mirror.

By passing through the interferometer, the neutron appears to act as a wave.

Interferometers are for measuring the interference properties of light waves.

It should also be noted that the movable mirror is the same for all interferometers.

It is an optical interferometer with two perpendicular arms 100 m long.

Also for accuracy laser interferometers need to be used.

The x- and y-axes are read out by laser interferometers.

Note that it is not necessary for to be modulated by the sample before the interferometer.