  Complex Organic Molecules (COMs) have been found toward low-mass protostars
but the origins of the COM emission are still unclear. It can be associated
with, for example, hot corinos, outflows, and/or accretion shock/disk
atmosphere. We have conducted NOEMA observations toward SVS13A from the
PROtostars & DIsks: Global Evolution (PRODIGE) program. Our previous \ce{DCN}
observations reveal a possible infalling streamer, which may affect the
chemistry of the central protobinary by inducing accretion outbursts and/or
shocked gas. Here, we further analyze six O-bearing COMs: CH3OH, aGg'-(CH2OH)2,
C2H5OH, CH2(OH)CHO, CH3CHO, and CH3OCHO. Although the COM emission is not
spatially resolved, we constrain the source sizes to $\lesssim0.3-0.4$ arcsec
(90$-$120 au) by conducting uv-domain Gaussian fitting. Interestingly, the
high-spectral resolution data reveal complex line profiles with multiple peaks
showing differences between these six O-bearing COMs. The LTE fitting unveils
differences in excitation temperatures and emitting areas among these COMs. We
further conduct multiple-velocity-component LTE fitting to decompose the line
emission into different kinematic components. Up to 6 velocity components are
found from the LTE modeling. The temperature, column density, and source size
of these components from each COM are obtained. We find a variety in excitation
temperatures ($100-500$ K) and source sizes (D$\sim10-70$ au) from these
kinematic components from different COMs. The emission of each COM can trace
several components and different COMs most likely trace different regions.
Given this complex structure, we suggest that the central region is
inhomogeneous and unlikely to be heated by only protostellar radiation. We
conclude that accretion shocks induced by the large-scale infalling streamer
likely exist and contribute to the complexity of the COM emission.
