  We present a new observation of the compact HII region, G29.96-0.02, that
allows us to compare the velocity structure in the ionised gas and surrounding
molecular gas directly. This allows us to remove most of the remaining
ambiguity about the nature of this source. In particular, the comparison of the
velocity structure present in the 4S-3P HeI lines with that found in the 1-0
S(1) of molecular hydrogern convincingly rules out a bow shock as being
important to the kinematics of this source. Our new observation therefore
agrees with our previous conclusion, drawn from a velocity resolved HI Br gamma
map, that most of the velocity structure in G29.96-0.02 can largely be
explained as a result of a champagne flow model. We also find that the best
simple model must invoke a powerful stellar wind to evacuate the `head' of the
cometary HII region of ionised gas. However, residual differences between model
and data tend to indicate that no single simple model can adequately explain
all the observed features.
