Imaging the Cosmic Microwave Background involves making an all-sky image of a very small signal - only a few millionths of a degree Kelvin - in the presence of foregrounds and instrumental baselines that are ten million times larger. Issues involved with reconstructing the full 4 pi steradians of the celestial sphere from differential measurements in the presence of 1/f noise and systematic errors will be discussed, and the methods used by NASA's Wikinson Microwave Anisotropy Probe and the results from WMAP will be presented.
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