A solar type I noise storm was observed on 30 July, 1992 with the radio spectrometer Phoenix of ETH Zurich, the Very Large Array (VLA) and the soft X-ray (SXR) telescope on board the Yohkoh satellite. The spectrogram was used to identify the type I noise storm. In the VLA images at 333 MHz a fully left circular polarized (100% LCP) continuum source and several highly polarized (70% to 100% LCP) burst sources have been located. The continuum and the bursts are spatially separated by about 100 '' and apparently lie on different loops as outlined by the SXR. Continuum and bursts are separated in the perpendicular direction to the magnetic field configuration. Between the periods of strong burst activities, burst-like emissions are also superimposed on the continuum source. There is no obvious correlation between the flux density of the continuum and the bursts. The burst sources have no systematic motion, whereas the the continuum source shows a small drift of approximate to 0.2 '' min(-1) along the X-ray loop in the long-time evolution. The VLA maps at higher frequency (1446 MHz) show no source corresponding to the type I event. The soft X-ray emission measure and temperature were calculated. The type I continuum source is located (in projection) in a region with enhanced SXR emission, a loop having a mean density of [n(e)] = (1.5 +/- 0.4) x 10(9) and cm(-3) and a temperature of T = (2.1 +/- 0.1) x 10(6) K. The centroid positions of the left and right circularly polarized components of the burst sources are separated by 15 ''-50 '' and seem to be on different loops. These observations contradict the predictions of existing type I theories.
