  The center of the nearby galaxy NGC\,253 hosts a population of more than a
dozen super star clusters (SSCs) which are still in the process of forming. The
majority of the star formation of the burst is concentrated in these SSCs, and
the starburst is powering a multiphase outflow from the galaxy. In this work,
we measure the 350~GHz dust continuum emission towards the center of NGC\,253
at 47~milliarcsecond (0.8 pc) resolution using data from the Atacama Large
Millimeter/submillimeter Array (ALMA). We report the detection of 350~GHz
(dust) continuum emission in the outflow for the first time, associated with
the prominent South-West streamer. In this feature, the dust emission has a
width of $\approx$~8~pc, is located at the outer edge of the CO emission, and
corresponds to a molecular gas mass of $\sim~(8-17)\times10^6$~M$_\odot$. In
the starburst nucleus, we measure the resolved radial profiles, sizes, and
molecular gas masses of the SSCs. Compared to previous work at somewhat lower
spatial resolution, the SSCs here break apart into smaller substructures with
radii $0.4-0.7$~pc. In projection, the SSCs, dust, and dense molecular gas
appear to be arranged as a thin, almost linear, structure roughly 155~pc in
length. The morphology and kinematics of this structure can be well explained
as gas following $x_2$ orbits at the center of a barred potential. We constrain
the morpho-kinematic arrangement of the SSCs themselves, finding that an
elliptical, angular momentum-conserving ring is a good description of the both
morphology and kinematics of the SSCs.
