  Stellar feedback plays a fundamental role in shaping the evolution of
galaxies. Here we explore the use of ionised gas kinematics in young, bipolar H
II regions as a probe of early feedback in these star-forming environments. We
have undertaken a multiwavelength study of a young, bipolar H II region in the
Galactic disc, G$316.81-0.06$, which lies at the centre of a massive
($\sim10^3$ M$_{\odot}$) infrared-dark cloud filament. It is still accreting
molecular gas as well as driving a $\sim 0.2$ pc ionised gas outflow
perpendicular to the filament. Intriguingly, we observe a large velocity
gradient ($47.81 \pm 3.21$ km s$^{-1}$ pc$^{-1}$) across the ionised gas in a
direction perpendicular to the outflow. This kinematic signature of the ionised
gas shows a reasonable correspondence with the simulations of young H II
regions. Based on a qualitative comparison between our observations and these
simulations, we put forward a possible explanation for the velocity gradients
observed in G$316.81-0.06$. If the velocity gradient perpendicular to the
outflow is caused by rotation of the ionised gas, then we infer that this
rotation is a direct result of the initial net angular momentum in the natal
molecular cloud. If this explanation is correct, this kinematic signature
should be common in other young (bipolar) H II regions. We suggest that further
quantitative analysis of the ionised gas kinematics of young H II regions,
combined with additional simulations, should improve our understanding of
feedback at these early stages.
