  Near-infrared Fabry-Perot imaging has revealed H2 emission extended to about
130 pc from the disk of NGC 253. It is closely related to the hot plasma
observed in soft X-rays: filamentary H2 features are found at the edges of the
hot plasma. These are the places of direct interaction between a superwind and
its surrounding molecular gas. We suggest that the filamentary features
actually trace a more or less conical shell-like structure, whose tangential
line of sight to us is intensely observed. The H2 emission shell is most likely
from the molecular gas blown out or swept to the side by the hot plasma
outflow. Dust is associated with this molecular gas structure. The outflow is
tilted with respect to the disk, possibly suggesting the inhomogeneous nature
of the interstellar medium in which the starburst takes place.
