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each detector must be sent to the central correlator facility, rather than the amplitude and phase of the signal. The intensity interferometer measures interferometric visibilities like all other astronomical interferometers. These measurements can be used to calculate the diameter and limb darkening coefficients of stars, but with intensity interferometers
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tubes (PMTs), separated by some distance, called the baseline. Both detectors are pointed at the same astronomical source, and intensity measurements are then transmitted to a central correlator facility. A major advantage of intensity interferometers is that only the measured intensity observed by
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or some other method, the physical diameter of the star can then be inferred. An example of an optical intensity interferometer is the
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is to determine the apparent angular diameter of a radio source or star. If the distance to the object can then be determined by
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images cannot be produced as the visibility phase information is not preserved by an intensity interferometer.
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might be said to be intensity interferometers, although the term is usually reserved for
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An intensity interferometer is built from two light detectors, typically either
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