  IRAS 21413+5442 and IRAS 21407+5441 are two massive star forming regions of
high luminosity, likely associated with each other. Near-infrared photometry on
these two IRAS sources was performed at UKIRT using the UFTI under excellent
seeing conditions yielding an angular resolution of $\sim$ 0.5 arcsec. Our
results reveal details of stellar content to a completeness limit (90%) of J =
18.5, H = 18.0, and K = 17.5 mag in the two regions. In IRAS 21413+5442, we
identify a late O type star, having large (H-K) color, to be near the centre of
the CO jets observed by earlier authors. The UKIRT images reveal in IRAS
21407+5441, a faint but clear compact HII region around a central high -
intermediate mass star cluster. We have detected a number of sources with large
(H-K) color which are not detected in J band. We also present the GMRT radio
continuum map at 1.28 GHz covering the entire region surrounding the two star
forming clouds. The radio continuum fluxes are used to estimate the properties
of HII regions which seem to support our near-IR photometric results. Based on
our radio continuum map and the archival MSX 8.2 $\mu$m image, we show that the
two IRAS sources likely belong to the same parent molecular cloud and
conjecture that a high mass star of large IR colors, present in between the two
sources, might have triggered star formation in this region. However one can
not rule out the alternative possibility that Star A could be a nearby
foreground star.
