Radial dependence of the intrinsic galaxy ellipticity in the particular cases (Keplerian and DM filament fields) considered in this paper, computed through the equipotential approximation (equi, see Appendix B) and through the distribution function formalism (f, see Sect. 3). Note the different radial dependence of the Keplerian (R^-3) and the DM filament (R^-2) cases; the equipotential approximation and the distribution function formalism yield the same radial dependence in the two cases, but different multiplicative factors (see the text for details).