  We present new Submillimeter Array (SMA) observations of CO(2-1) outflows
toward young, embedded protostars in the Perseus molecular cloud as part of the
Mass Assembly of Stellar Systems and their Evolution with the SMA (MASSES)
survey. For 57 Perseus protostars, we characterize the orientation of the
outflow angles and compare them with the orientation of the local filaments as
derived from $Herschel$ observations. We find that the relative angles between
outflows and filaments are inconsistent with purely parallel or purely
perpendicular distributions. Instead, the observed distribution of
outflow-filament angles are more consistent with either randomly aligned angles
or a mix of projected parallel and perpendicular angles. A mix of parallel and
perpendicular angles requires perpendicular alignment to be more common by a
factor of $\sim$3. Our results show that the observed distributions probably
hold regardless of the protostar's multiplicity, age, or the host core's
opacity. These observations indicate that the angular momentum axis of a
protostar may be independent of the large-scale structure. We discuss the
significance of independent protostellar rotation axes in the general picture
of filament-based star formation.
