  Source imaging of solar radio bursts can be used to track energetic electrons
and associated magnetic structures. Here we present a combined analysis of data
at different wavelengths for an eruption associated with a moving type-IV
(t-IVm) radio burst. In the inner corona, the sources are correlated with a hot
and twisted eruptive EUV structure, while in the outer corona the sources are
associated with the top front of the bright core of a white light coronal mass
ejection (CME). This reveals the potential of using t-IVm imaging data to
continuously track the CME by lighting up the specific component containing
radio-emitting electrons. It is found that the t-IVm burst presents a clear
spatial dispersion with observing frequencies. The burst manifests broken
power-law like spectra in brightness temperature, which is as high as
$10^7$-$10^9$ K while the polarization level is in-general weak. In addition,
the t-IVm burst starts during the declining phase of the flare with a duration
as long as 2.5 hours. From the differential emission measure analysis of AIA
data, the density of the T-IVm source is likely at the level of 10$^8$
cm$^{-3}$ at the start of the burst, and the temperature may reach up to
several MK. These observations do not favor gyro-synchrotron to be the
radiation mechanism, yet in line with a coherent plasma emission excited by
energetic electrons trapped within the source. Further studies are demanded to
elucidate the emission mechanism and explore the full diagnostic potential of
t-IVm bursts.
