  We present a study of the central zone of the star-forming region L1448 at
217--230 GHz ($\sim$ 1.3 mm) using ALMA observations. Our study focuses on the
detection of proto-stellar molecular outflows and the interaction with the
surrounding medium toward sources L1448--C(N) and L1448--C(S). Both sources
exhibit continuum emission, with L1448--C(N) being the brightest one. Based on
its spectral index and the associated bipolar outflow, the continuum emission
is the most likely to be associated with a circumstellar disk. The $^{\rm
12}$CO(J=2$\rightarrow$1) and SiO(J= 5$\rightarrow$4) emissions associated with
L1448--C(N) trace a bipolar outflow and a jet oriented along the
northwest-southeast direction. The $^{\rm 12}$CO(J=2$\rightarrow$1) outflow for
L1448--C(N) has a wide-open angle and a V-shape morphology. The SiO jet is
highly collimated and has an axial extent comparable with the $^{\rm
12}$CO(J=2$\rightarrow$1) emission. There is not SiO(J= 5$\rightarrow$4)
emission towards L1448--C(S), but there is $^{\rm 12}$CO(J=2$\rightarrow$1)
emission. The observations revealed that the red-shifted lobes of the $^{\rm
12}$CO(J=2$\rightarrow$1) outflows of L1448--C(N) and L1448--C(S) are
colliding. As a result of this interaction, the L1448-C(S) lobe seems to be
truncated. The collision of the molecular outflows is also hinted by the SiO(J=
5$\rightarrow$4) emission, where the velocity dispersion increases
significantly in the interaction zone. We also investigated whether it could be
possible that this collision triggers the formation of new stars in the
L1448--C system.
