  We report a tentative correlation between the outflow characteristics derived
from OH absorption at $119\,\mu\text{m}$ and [CII] emission at
$158\,\mu\text{m}$ in a sample of 22 local and bright ultraluminous infrared
galaxies (ULIRGs). For this sample we investigate whether [CII] broad wings are
a good tracer of molecular outflows, and how the two tracers are connected.
Fourteen objects in our sample have a broad wing component as traced by [CII],
and all of these also show OH119 absorption indicative of an outflow (in 1 case
an inflow). The other eight cases, where no broad [CII] component was found,
are predominantly objects with no OH outflow or a low-velocity ($\leq
100\,\text{km s}^{-1}$) OH outflow. The full width at half maximum (FWHM) of
the broad [CII] component shows a trend with the OH119 blue-shifted velocity,
although with significant scatter. Moreover, and despite large uncertainties,
the outflow masses derived from OH and broad [CII] show a 1:1 relation. The
main conclusion is therefore that broad [CII] wings can be used to trace
molecular outflows. This may be particularly relevant at high redshift, where
the usual tracers of molecular gas (like low-J CO lines) become hard to
observe. Additionally, observations of blue-shifted Na I D $\lambda\lambda
5890,5896$ absorption are available for ten of our sources. Outflow velocities
of Na I D show a trend with OH velocity and broad [CII] FWHM. These
observations suggest that the atomic and molecular gas phases of the outflow
are connected.
