  With the high tempo-spatial \emph{Interface Region Imaging Spectrograph} 1330
{\AA} images, we find that many bright structures are rooted in the light
bridge of NOAA 12192, forming a \emph{light wall}. The light wall is brighter
than the surrounding areas, and the wall top is much brighter than the wall
body. The New Vacuum Solar Telescope H$\alpha$ and the \emph{Solar Dynamics
Observatory} 171 {\AA} and 131 {\AA} images are also used to study the light
wall properties. In 1330 {\AA}, 171 {\AA}, and 131 {\AA}, the top of the wall
has a higher emission, while in the H$\alpha$ line, the wall top emission is
very low. The wall body corresponds to bright areas in 1330 {\AA} and dark
areas in the other lines. The top of the light wall moves upward and downward
successively, performing oscillations in height. The deprojected mean height,
amplitude, oscillation velocity, and the dominant period are determined to be
3.6 Mm, 0.9 Mm, 15.4 km s$^{-1}$, and 3.9 min, respectively. We interpret the
oscillations of the light wall as the leakage of \emph{p}-modes from below the
photosphere. The constant brightness enhancement of the wall top implies the
existence of some kind of atmospheric heating, e.g., via the persistent
small-scale reconnection or the magneto-acoustic waves. In another series of
1330 {\AA} images, we find that the wall top in the upward motion phase is
significantly brighter than in the downward phase. This kind of oscillations
may be powered by the energy released due to intermittent impulsive magnetic
reconnection.
