The evolution of young HII regions
  High-mass stars form in much richer environments than those associated with
isolated low-mass stars, and once they reach a certain mass, produce ionised
(HII) regions. The formation of these pockets of ionised gas are unique to the
formation of high-mass stars (M $>8$ M$_\odot$), and present an excellent
opportunity to study the final stages of accretion, which could include
accretion through the HII region itself. This study of the dynamics of the gas
on both sides of these ionisation boundaries in very young HII regions aims to
quantify the relationship between the HII regions and their immediate
environments.We present high-resolution ($\sim$ 0.5$"$) ALMA observations of
nine HII regions selected from the Red MSX Source (RMS) survey with compact
radio emission and bolometric luminosities greater than 10$^4$ L$_\odot$. We
focus on the initial presentation of the data, including initial results from
the radio recombination line H29$\alpha$, some complementary molecules, and the
256 GHz continuum emission. Of the six (out of nine) regions with H29$\alpha$
detections, two appear to have cometary morphologies with velocity gradients
across them, and two appear more spherical with velocity gradients suggestive
of infalling ionised gas. The remaining two were either observed at low
resolution or had signals that were too weak to draw robust conclusions. We
also present a description of the interactions between the ionised and
molecular gas (as traced by CS (J=5-4)), often (but not always) finding theHII
region had cleared its immediate vicinity of molecules. Of our sample of nine,
the observations of the two clusters expected to have the youngest HII regions
(from previous radio observations) are suggestive of having infalling motions
in the H29$\alpha$ emission, which could be indicative of late stage accretion
onto the stars despite the presence of an HII region.
