  In this contribution, I review the applications and potential limitations of
the spectral energy distribution fitting tool that I have developed, with a
strong emphasis on the limits to which this tool can be used to improve our
understanding of massive star formation. I discuss why our current grid of
models cannot be used to distinguish between the several competing theories of
massive star formation. I also discuss stellar mass determinations, artificial
correlations between parameters in the grid of models, multiplicity, confusion,
dust assumptions, and unique fits. I briefly review the improvements we intend
to carry out for our next grid of models, which will eliminate many of these
limitations. Finally, I show examples of applications of this tool to massive
young stars.
