The importance of a Dome C facility for studies of massive star
formation is highlighted. Using an example of a statistical study of
380 candidate massive protostars based on the GLIMPSE legacy program
data from the Spitzer Space Telescope, the relevance of a Dome C
facility for further science progress is argued. The GLIMPSE point
source photometry was used to a conduct colour-magnitude analysis, and
radiative transfer modelling of the spectral energy distributions of
the massive protostars. The results support an accretion scenario
for the process of massive star formation up to masses of
50 M๏. The available spectral energy distrubutions of the massive
protostellar candidates are largely inadequate in the crucial bands
from 10–500 μm. This wavelength range can be effectively filled
in with a nominal Dome C observing facility which can be highly cost
effective compared to a space facility. Narrow-band emission line
imaging of massive star forming regions in the 10–20 micron bands
using high temperature emission lines can yield invaluable
information on the nature of OB stars in the Milky Way and nearby
galaxies. Such observations are crucial for our understanding of the
influence of OB stars in controlling the galactic turbulence,
feedback effects, influence on other low mass stars in the vicinity,
and controlling the star formation rate.