  We present an evaluative study of some current methods utilized in the
analysis of infrared (IR) observatinons of star-forming regions. A series of
self-consistent radiative transfer models are constructed, with the outputs
analysed using these methods to infer source properties such as dust
temperature, mass, opacity function, and density distribution. Any
discrepancies between the inferred and model quantities can be attributed to
the analysis methods. The range of validity of most methods is smaller than
expected, due to two effects: (1) limited applicability of the Rayleigh-Jeans
limit except to very long wavelengths, and (2) significant errors in the
isothermal approximation, even when temperature variations are less than 2 K
over 90% of the region. Still, an accurate mean dust temperature can be found
using a modified Wien's law. This temperature can yield dust masses to within
10-25% -- much better than masses inferred from the integrated luminosity.
Using long wavelengths (greater than 1000 - 2000 microns), the opacity index
can be determined from the far-IR spectrum to within 20%. Fitting the spectrum
yields better results. The desnity distribution can be somewhat constrained by
fitting the surface brightness, for well-resolved sources. Better results are
found by fitting the flux spectrum with detailed models.
