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Aperture synthesis is the process of combining the data from a collection of radio telescopes to simulate a much larger aperture, resulting in images with higher spatial resolution.

Synthesis imaging is creating images from interferometry data by sampling the spatial frequency domain and then applying an inverse Fourier transform. It allows the creation of high-resolution images from a series of observations at different baselines.

In radio astronomy, the Fourier transform is used to convert the time-domain signals collected by interferometers into the frequency domain. This allows astronomers to reconstruct the spatial distribution of the radio emission, creating an image of the sky.

VLBI is a type of interferometry that uses widely separated radio telescopes from different geographic locations, synthesizing a telescope with a size equivalent to the maximum distance between the antennas, allowing for extremely high-resolution imaging of cosmic radio sources.

The visibility function in interferometry describes the amplitude and phase of the radio signal as a function of the baseline. It is a fundamental quantity from which the sky brightness distribution can be reconstructed.

Super-synthesis refers to the process in aperture synthesis where the rotation of the Earth is used to sample additional points in the spatial frequency plane, providing a more complete coverage and thus better image fidelity.

Angular resolution is the smallest angle between two objects that can be distinctly separated by a telescope. In interferometry, higher angular resolutions can be achieved with longer baselines.

A dirty beam is the point spread function of an interferometer before deconvolution. It represents the response of the interferometer to a point source and usually includes sidelobes and other artifacts that need to be removed to create a 'clean' image.

In interferometry, a baseline is the distance between two radio telescopes or antenna elements. The length and orientation of the baseline determine the resolution and the scale of the features that can be imaged.

A fringe pattern in interferometry refers to the pattern of constructive and destructive interference observed as radio waves combine. Analysis of fringe patterns provides information about the angular position and structure of the radio source.

Delay tracking compensates for the time difference between the arrival of a wavefront at different antennas in an interferometer. Accurate delay tracking is essential for keeping the antennas phased properly and ensuring coherent signal combination.

Interferometry is a technique in radio astronomy that combines the signals received by multiple antennas to effectively create a larger telescope. This allows astronomers to achieve a higher resolution and better image detail that would not be possible with individual telescopes.

In a radio telescope, the primary beam is the field of view of the antenna or the sensitivity pattern of a single dish. It defines the area of the sky that is imaged at any one time and impacts the sensitivity to sources off the center.

Phase calibration in interferometry involves correcting for the variations in the phase of the signals received at different antennas to accurately reconstruct an image. It helps to correct for atmospheric disturbances and system errors.