  Two Galactic star forming regions, one in a very early phase of evolution and
another evolved one, associated with the IRAS sources 00338+6312 and 03595+5110
(RAFGL 5111) respectively have been studied in detail. These sources have been
mapped simultaneously in two far infrared bands at 143 & 185 \micron), with
about 1.5 arcmin angular resolution, using the TIFR 100 cm balloon borne
telescope. The HIRES processed IRAS maps at 12, 25, 60 & 100 \micron, have been
used for comparison. Whereas IRAS 00338+6312 is resolved only in the TIFR
bands, RAFGL 5111 is very well resolved in both the TIFR bands, as well as in
at least 3 IRAS bands. The neighbouring fainter source IRAS 04004+5114 has also
been resolved in the TIFR bands. Taking advantage of the identical beams in the
two TIFR bands at 143 & 185 \micron, dust colour temperature, $T(143/185)$, and
optical depth, $\tau_{150}$, maps have been generated for RAFGL 5111. These
maps show interesting structural details. Radiative transfer modelling in
spherical geometry has been carried out for individual sources. The best fit
models are in good agreement with the observed spectral energy distribution
(SED), radio continuum data etc. Another scheme of radiative transfer through
the interstellar dust-gas cloud including the heavier elements has been used to
predict ionic nebular line emission, which are in reasonable agreement with the
measurements for RAFGL 5111. An important conclusion from the present study is
that, for all the three sources (IRAS 00338+6312; 03595+5110; and 04004+5114, a
faint source in the neighbourhood of RAFGL 5111), the best fit to the observed
SED is obtained for a uniform density ($n(r) \sim r^0$) cloud.
