  The physical conditions of the interstellar medium and stellar components in
the regions of the southern Galactic star forming complexes associated with
IRAS 10049-5657 and IRAS 10031-5632 have been investigated. These regions have
been mapped simultaneously in two far infrared bands lambda_eff ~ 150 & 210
micron, with ~ 1' angular resolution using the TIFR 1-m balloon borne
telescope. Spatial distribution of the temperature of cool dust and optical
depth at 200 micron have been obtained. Using the 2MASS sources, the stellar
populations of the embedded young clusters have been studied. A rich cluster of
OB stars in the IRAS 10049-5657 region has been found with a cluster radius ~ 2
pc. The source in the cluster closest to the IRAS peak, lies above the ZAMS
curve of spectral type O5 in the colour-magnitude diagram. Unlike IRAS
10049-5657, a small cluster comprising of a few deeply embedded sources is seen
at the location of IRAS 10031-5632. Self consistent radiative transfer
modelling aimed at extracting important physical and geometrical details of the
two IRAS sources show that the best fit models are in good agreement with the
observed spectral energy distributions. The geometric details of the associated
cloud and optical depths (at 100 micron) have been estimated. A uniform density
distribution of dust and gas is implied for both the sources. In addition, the
infrared ionic fine-structure line emission from gas has been modelled for both
these regions and compared with data from IRAS-Low Resolution Spectrometer. For
IRAS 10049-5657, the observed and modelled luminosities for most lines agree to
within a factor of four while for IRAS 10031-5632, we find a discrepancy of a
factor of 100.
