1999MNRAS.305..701L

We present a new observation of the compact H II region, G 29.96-0.02, that allows us to compare the velocity structure in the ionized 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 4^1,3S-3^1,3P He I lines with that found in the 1-0 S(1) H₂ line 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 H I Brγ map, that most of the velocity structure in G 29.96-0.02 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 H II region of ionized gas. However, residual differences between model and data tend to indicate that no single simple model can adequately explain all the observed features.