The Cosmic Microwave Background (CMB) is relic radiation from an early dense and hot phase of the cosmological evolution of the Universe, originating from a cosmic "photosphere" of last scattering at a redshift z~1100. Conditions in the Universe at that time, plus subsequent evolution and geometrical factors, are imprinted on the CMB radiation pattern. For example, the angular power spectrum of the CMB has recently been measured to high accuracy by a variety of observational experiments and places stringent constraints on cosmological parameters. A number of CMB measurements have been made with interferometers such as DASI, the VSA, and the CBI. Because interferometers directly measure the Fourier domain properties of the radiation field, interferometric observations of the CMB are relatively easy to analyze in the context of angular power spectrum determination. Inclusion of polarization in the observations and analysis is also relatively straightforward. In this talk I discuss the basics of CMB interferometry (in comparison with direct imaging) and the extraction of the power spectrum from such measurements, calibration and imaging, and polarization considerations. I also review the most recent scientific results from CMB interferometry (focusing on the CBI project of which I am a co-investigator) and discuss future prospects.
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