Predictions for the relative centroid positions of the H30α emissions derived for two different kinematical models superimposed (as blue and red thin lines) on the observed data for MWC 349. The thick black line shows the results for the case when photoevaporation occurs at a radius larger than the gravitational radius. The dotted black line shows the case when the ionized outflow does not follow the disk rotation. The radial velocities are the same as in Fig. 4.