The feedback of atomic jets from embedded protostars in NGC 1333
  Star-formation feedback onto the parent cloud is conventionally examined
through the study of molecular outflows. Little is however known on the effect
that atomic ejecta, tracing fast shocks, can have on the global cloud
properties. In this study we employ Herschel/PACS [OI] and [CII] spectral line
maps of the NGC 1333 star-forming region to assess the relative influence of
atomic jets onto the star-formation process. Atomic line maps are compared
against molecular outflow tracers and atomic ejecta are associated to
individual driving sources. We study the detailed morphology and velocity
distribution of [OI] line using channel and line-centroid maps and derive the
momentum, energy, and mass flux for all the bipolar jets traced by [OI] line
emission. We find that the line-centroid maps can trace velocity structures
down to 5 km s$^{-1}$ which is a factor of $\sim$20 beyond the nominal velocity
resolution reached by Herschel/PACS. These maps reveal an unprecedented degree
of details that assist significantly in the association and characterization of
jets and outflows. Comparisons of the dynamical and kinematical properties
shows that [OI] momentum accounts for only $\sim$1% of the momentum carried by
the large scale CO outflows but the energy released through the jets
corresponds to 50 - 100% of the energy released in outflows. The estimated
ratios of the jet to the outflow momenta and energies are consistent with the
results of two-component, nested jet/outflow simulations, where jets are
associated to episodic accretion events. Under this scenario, the energy from
atomic jets to the cloud is as important as the energy output from outflows in
maintaining turbulence and dissipating the cloud gas.
