Same model as in Fig. 5, but now showing the scaled total flux F_I (the scaling places the max value at one) and polarized flux |F_Q| (i.e., its absolute value, with a scaling such that it peaks at a value of 0.5) for an inclination of 50, 90, and 130 deg to the symmetry axis. The polarized flux corresponds closely to the total flux with an offset in magnitude (by a factor 1∕P, hence about 10² to 10³ smaller – see Fig. 5 for the exact offset) and a redshift whose magnitude increases with inclination. The clean, distinct redshift seen in the scattered flux, corresponding to V_blob (1 − cosα_los), is a fundamental prediction of this work for a high-velocity scatterer (see also Appendix A). To aid in the direct comparison between features seen in the polarized (i.e., scattered) flux compared with the total flux, in several future figures we artificially apply the appropriate blueshift to the predicted polarized flux spectra, such that it overlaps with the total flux spectrum.