  We present new Atacama Large Millimeter/submillimeter Array (ALMA) results
obtained from spatially resolved CO $J$=2-1 line ($0.4''$ resolution) and 870
$\mu$m continuum ($0.2''$ resolution) observations of cluster galaxies in
XMMXCS J2215.9-1738 at $z=1.46$. Our sample comprises 17 galaxies within
$\sim0.5$ Mpc ($0.6R_{200}$) of the cluster center, all of which have
previously been detected in the CO $J$=2-1 line at a lower resolution. The
effective radii of both the CO $J$=2-1 line and 870 $\mu$m dust continuum
emissions are robustly measured for nine galaxies by modeling the visibilities.
We find that the CO $J$=2-1 line emission in all of the nine galaxies is more
extended than the dust continuum emission by a factor of $2.8\pm1.4$. We
investigate the spatially resolved Kennicutt-Schmidt (KS) relation in two
regions within the interstellar medium of the galaxies. The relation for our
sample reveals that the central region ($0<r<R_{e,{\rm 870\mu m}}$) of galaxies
tends to have a shorter gas depletion timescale, i.e., a higher star formation
efficiency, compared to the extended region ($R_{e,{\rm 870\mu m}}<r<R_{e,{\rm
CO}}$). Overall, our result suggests that star formation activities are
concentrated inside the extended gas reservoir, possibly resulting in the
formation of a bulge structure. We find consistency between the ALMA 870 $\mu$m
radii of star-forming members and the Hubble Space Telescope/1.6 $\mu$m radii
of passive members in a mass-size distribution, which suggests a transition
from star-forming to passive members within $\sim0.5$ Gyr. In addition, no
clear differences in the KS relation nor in the sizes are found between
galaxies with and without a close companion.
