Abstract
The Nobeyama Radioheliograph started routine observations in late June, 1992, after two years of construction and system integration. In two years of observations, which contain a last part of the maximum phase of the solar cycle 22, it was possible to obtain almost every aspect of solar activity at 17 GHz. They include two X-class flares, tens of M-class flares, hundreds of flares from the very initial phase through the late decay phase, or from pre-flare enhancements through post-flare loops, slowly varying components from active regions, bright points, prominence eruptions, and so on, with a spatial resolution of 10 arcsec and a time resolution of 1 s and 50 ms for specific events.
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