Comparison between observed profiles (black) and those produced by our simulation, as described in Sect. 4, using the model parameters with the highest likelihood and a prograde (PG) pulsar spin (red). Green lines show the most likely profiles of an alternative model with a retrograde (RG) pulsar spin. The profiles shown have been tabulated according to orbital phase window, that is, BP1, BP2, IP, and WP, and the MJD range to which they belong. The grey lines show the lower and upper 1σ_sys confidence limits of the observed flux density, multiplied by the most likely error coefficients (q_kj) that were derived from our analysis.