  We have analyzed the ALMA archival data of the SO ($J_N=6_5-5_4$ and
$J_N=7_6-6_5$), CO ($J=2-1$), and CCH ($N=3-2, J=7/2-5/2, F=4-3$) lines from
the class 0 protobinary system, NGC1333 IRAS 4A. The images of SO ($J_N =
6_5-5_4$) and CO ($J=2-1$) successfully separate two northern outflow lobes
connected to each protostar, IRAS 4A1 and IRAS 4A2. The outflow from IRAS 4A2
shows an S-shaped morphology, consisting of a flattened envelope around IRAS
4A2 with two outflow lobes connected to both edges of the envelope. The
flattened envelope surrounding IRAS 4A2 has an opposite velocity gradient to
that of the circumbinary envelope. The observed features are reproduced by the
magnetohydrodynamic simulation of the collapsing core whose magnetic field
direction is misaligned to the rotational axis. Our simulation shows that the
intensity of the outflow lobes is enhanced on one side, resulting in the
formation of S-shaped morphology. The S-shaped outflow can also be explained by
the precessing outflow launched from an unresolved binary with a separation
larger than 12 au (0.04arcsec). Additionally, we discovered a previously
unknown extremely high velocity component at $\sim$45-90 km/s near IRAS 4A2
with CO. CCH ($J_{N,F}=7/2_{3,4}-5/2_{2,3}$) emission shows two pairs of blobs
attaching to the bottom of shell like feature, and the morphology is
significantly different from those of SO and CO lines. Toward IRAS 4A2, the
S-shaped outflow shown in SO is overlapped with the edges of CCH shells, while
CCH shells have the velocity gradients opposite to the flattened structure
around IRAS 4A2.
