  We present observations of SO and $\rm SO_2$ lines toward the shocked regions
along the L1157 chemically rich outflow, taken in the context of the Seeds Of
Life In Space IRAM-NOrthern Extended Millimeter Array Large Program, and
supported by data from Submillimeter Array and IRAM-30 m telescope at 1.1--3.6
mm wavelengths. We simultaneously analyze, for the first time, all of the
brightest shocks in the blueshifted lobe, namely, B0, B1, and B2. We found the
following. (1) SO and $\rm SO_2$ may trace different gas, given that the
large(-scale) velocity gradient analysis indicates for $\rm SO_2$ a volume
density ($\rm 10^5\text{--}10^6\,cm^{-3}$) denser than that of the gas emitting
in SO by a factor up to an order of magnitude. (2) Investigating the 0.1 pc
scale field of view, we note a tentative gradient along the path of the
precessing jet. More specifically, $\rm \chi({SO/SO_2})$ decreases from the
B0-B1 shocks to the older B2. (3) At a linear resolution of 500--1400 au, a
tentative spatial displacement between the two emitting molecules is detected,
with the SO peak closer (with respect to $\rm SO_2$) to the position where the
recent jet is impinging on the B1 cavity wall. Our astrochemical modeling shows
that the SO and $\rm SO_2$ abundances evolve on timescales less than about 1000
years. Furthermore, the modeling requires high abundances ($2\times10^{-6}$) of
both $\rm H_2S/H$ and S/H injected in the gas phase due to the shock
occurrence, so pre-frozen OCS only is not enough to reproduce our new
observations.
