  We have carried out the NH$_3$ $(J,K)=(1,1),(2,2),$ and $(3,3)$ mapping
observations toward the Galactic infrared bubble N49 (G28.83-0.25) using the
Nobeyama 45 m telescope. Three NH$_3$ clumps (A, B, and C) were discovered
along the molecular filament with the radial velocities of $\sim$ 96, 87, and
89 km s$^{-1}$, respectively. The kinetic temperature derived from the NH$_3$
(2,2)/NH$_3$ (1,1) shows $T_{\rm kin} = 27.0 \pm 0.6$ K enhanced at Clump B in
the eastern edge of the bubble, where position coincides with massive young
stellar objects (MYSOs) associated with the 6.7 GHz class II methanol maser
source. This result shows the dense clump is locally heated by stellar feedback
from the embedded MYSOs. The NH$_3$ Clump B also exists at the 88 km s$^{-1}$
and 95 km s$^{-1}$ molecular filament intersection. We therefore suggest that
the NH$_3$ dense gas formation in Clump B can be explained by a
filament-filament interaction scenario. On the other hand, NH$_3$ Clump A and C
at the northern and southern side of the molecular filament might be the sites
of spontaneous star formation because these clumps are located $\sim$5$-$10 pc
away from the edge of the bubble.
