  We have carried out interferometric observations of cyanopolyynes, HC$_{3}$N,
HC$_{5}$N, and HC$_{7}$N, in the 36 GHz band toward the G28.28$-$0.36 high-mass
star-forming region using the Karl G. Jansky Very Large Array (VLA) Ka-band
receiver. The spatial distributions of HC$_{3}$N and HC$_{5}$N are obtained.
HC$_{5}$N emission is coincident with a 450 $\mu$m dust continuum emission and
this clump with a diameter of $\sim 0.2$ pc is located at the east position
from the 6.7 GHz methanol maser by $\sim 0.15$ pc. HC$_{7}$N is tentatively
detected toward the clump. The HC$_{3}$N : HC$_{5}$N : HC$_{7}$N column density
ratios are estimated at 1.0 : $\sim 0.3$ : $\sim 0.2$ at an HC$_{7}$N peak
position. We discuss possible natures of the 450 $\mu$m continuum clump
associated with the cyanopolyynes. The 450 $\mu$m continuum clump seems to
contain deeply embedded low- or intermediate-mass protostellar cores, and the
most possible formation mechanism of the cyanopolyynes is the warm carbon chain
chemistry (WCCC) mechanism. In addition, HC$_{3}$N and compact HC$_{5}$N
emission is detected at the edge of the 4.5 $\mu$m emission, which possibly
implies that such emission is the shock origin.
