  We present the results from NH$_{3}$ mapping observations towards 34 regions
identified by the Red MSX Source (RMS) survey. We have used the Australia
Telescope Compact Array to map ammonia (1,1) and (2,2) inversion emission
spectra at a resolution of 10'' with velocity channel resolution of
0.4$\,$km$\,$s$^{-1}$ towards the positions of embedded massive star formation.
Complementary data have been used from the ATLASGAL and GLIMPSE Legacy Surveys
in order to improve the understanding of the regions and to estimate physical
parameters for the environments. The fields have typical masses of
~1000$\,$M$\odot$, radii of ~0.15$\,$pc and distances of ~3.5$\,$kpc.
Luminosities range between ~10$^{3}$ to ~10$^{6}$$\,$L$\odot$ and kinetic
temperatures between 10 and 40$\,$K. We classify each field into one of two
subsets in order to construct an evolutionary system for massive star formation
in these regions based on the morphology and relative positions of the NH$_{3}$
emission, RMS sources and ATLASGAL thermal dust emission. Differences in
morphology between NH$_{3}$ emission and ATLASGAL clumps are shown to
correspond to evolutionary stages of ongoing massive star formation in these
regions. The study has been further refined by including the positions of known
methanol and water masers in the regions to gain insight into possible
protostellar regions and triggered star formation.
