Detailed analysis of the University of Iowa Pioneer 10 data using several design features of the instrument to accomplish particle species identification shows that the observed counting rates within the magnetosphere of Jupiter were caused primarily by electrons, Ee>0.06 MeV. This identification holds for the magnetodisc region (r≲20 RJ (Jovian radii)) as well as for the central magnetosphere (r (≲20 RJ), as reported previously by Van Allen et al. (1974b). Absolute omnidirectional intensities of electrons in the magnetodisc are presented for five integral energy ranges: Ee>0.06, >0.55, >5, >21, and >31 MeV. A model electron differential energy spectrum of the form dJ/dE=KE-1.5[1+(E/H)>-n is found to fit the observed intensities throughout most of the encounter trajectory, where J is the omnidirectional electron intensity; E is the kinetic energy; and K, H, and n are fitting parameters dependent on radial distance from the planet and magnetic latitude. It is suggested that the observed spectral shape may be interpreted as resulting from losses of high-energy electrons by pitch angle scattering. Observed equatorial energy spectra are used to compute phase space densities (distribution functions) at several selected values of the first adiabatic invariant &mgr;. Radial profiles of the phase space densities have maxima at ~50 RJ inbound and at ~90 RJ outbound and diminish strongly for lesser radii. The profiles seem broadly consistent with inward radial transport form the maxima. Strong losses seem to be required to explain the large decreases in the densities observed. Resonant electron whistler mode pitch angle scattering is a candidate mechanism for such losses.