  We report the ALMA Cycle 2 observations of the Class I binary protostellar
system L1551 NE in the 0.9-mm continuum, C18O (3-2), 13CO (3-2), SO (7_8-6_7),
and the CS (7-6) emission. At 0.18" (= 25 AU) resolution, ~4-times higher than
that of our Cycle 0 observations, the circumbinary disk as seen in the 0.9-mm
emission is shown to be comprised of a northern and a southern spiral arm, with
the southern arm connecting to the circumstellar disk around Source B. The
western parts of the spiral arms are brighter than the eastern parts,
suggesting the presence of an m=1 spiral mode. In the C18O emission, the infall
gas motions in the inter-arm regions and the outward gas motions in the arms
are identified. These observed features are well reproduced with our numerical
simulations, where gravitational torques from the binary system impart angular
momenta to the spiral-arm regions and extract angular momenta from the
inter-arm regions. Chemical differentiation of the circumbinary disk is seen in
the four molecular species. Our Cycle 2 observations have also resolved the
circumstellar disks around the individual protostars, and the beam-deconvolved
sizes are 0.29" X 0.19" (= 40 X 26 AU) (P.A. = 144 deg) and 0.26" X 0.20" (= 36
X 27 AU) (P.A. = 147 deg) for Sources A and B, respectively. The position and
inclination angles of these circumstellar disks are misaligned with that of the
circumbinary disk. The C18O emission traces the Keplerian rotation of the
misaligned disk around Source A.
