  We present a multi-wavelength (from far ultraviolet to HI emission) study of
star formation feedback on the kinematics of the interstellar medium in the
Sculptor Galaxy, NGC253. Its three well-known features (a disrupted stellar
disc, a previously reported delining rotation curve, and anomalous HI gas) are
studied in a common context of disc asymmetries. About 170 h of on-source ATCA
observations are collected and reduced into two versions of \HI\ data cubes of
different angular resolution (30'' / 2') and HI column density sensitivity (7.4
$\times$ $10^{19}$cm$^{-2}$ / 4$\times$ $10^{18}$cm$^{-2}$). We separate the
anomalous gas from the disc using a custom-made line profile fitting toolkit
called FMG. Two star formation tracers (H$\alpha$, FUV emission) are carefully
processed and studied. We find that at $R > 7.5~\mathrm{kpc}$ the star
formation activity is strongly lopsided (SFR$_{NE}$ >SFR$_{SW}$), and
investigate several other properties (H$\alpha$/FUV, dust temperature, stellar
age, and disc stability parameters). We also find that the declining nature of
the rotation curve perceived by previous studies is not intrinsic but a
combined effect of kinematical asymmetries at $R = 7.5$--$16~\mathrm{kpc}$.
This is likely the consequence of star formation triggered outflow. The mass
distribution and the timescale of the anomalous gas also imply that it
originates from gas outflow, which is perhaps caused by galaxy-galaxy
interaction considering the crowded environment of NGC253.
