  I present four-frequency radio observations of the wide-angle tail radio
galaxy 3C130. By a technique of simulated observations, I assess the systematic
errors in the data due to the varying uv plane coverage in the different
observations used. Using spectral tomography I show that, at least in the
southern plume, the source can be represented by a two-component model
consisting of a flat-spectrum core and steep-spectrum sheath, as recently found
in other FRI sources. In addition, there is a strong difference in the
high-frequency spectra of the northern and southern plumes. I discuss the
implications of these observations for the source's jet dynamics and particle
acceleration, and discuss models of the class of WATs as a whole.
