We present and compare results from two different tomographic reconstruction techniques: a backprojection technique de Pater et al., 1997b> and a three-dimensional (3-D) Fourier technique Sault et al., 1997>. We applied both techniques to very large array (VLA) data of Jupiter's synchrotron radiation and to models which simulate 2-D images of Jupiter's radio emission de Pater et al., 1997a>. The 3-D images thus constructed represent the apparent radio emissivity. Results from the two techniques are quite compatible. A comparison between the tomographic reconstructions of the data and model yields information on models of the electron flux, j(L,αe,E), and the magnetic field configuration. At first glance, results from the data and model agree quite well. Longitudinal differences between the data and model suggest the need for modifications to the magnetic field model, while differences in the radial profile are caused by imperfections in the radial profile of the electron flux. We suggest that the magnetic equatorial surface should be less warped than in the O6 model. We further find that the change in the modeled pitch angle distribution at Amalthea's orbit de Pater et al., 1997a> should be modified by, for example, the inclusion of diffusion both in pitch angle and L, while there also appear to be more emitters at high latitudes outside of Amalthea's orbit than assumed in the model. ¿ 1998 American Geophysical Union