  The radio galaxy NGC 1052 casts absorption features of sulfur-bearing
molecules, H$_2$S, SO, SO$_2$, and CS toward the radio continuum emission from
the core and jets. Using ALMA, we have measured the equivalent widths of SO
absorption features in multiple transitions and determined the temperatures of
$344 \pm 43$ K and $26 \pm 4$ K in sub-millimeter and millimeter wavelengths,
respectively. Since sub-mm and mm continuum represents the core and jets, the
high and low temperatures of the absorbers imply warm environment in the
molecular torus and cooler downstream flows. The high temperature in the torus
is consistent with the presence of 22-GHz H$_2$O maser emission, vibrationally
excited HCN and HCO$^+$ absorption lines, and sulfur-bearing molecules in gas
phase released from dust. The origin of the sulfur-bearing gas is ascribed to
evaporation of icy dust component through jet-torus interaction. Shock heating
is the sole plausible mechanism to maintain such high temperature of gas and
dust in the torus. Implication of jet-torus interaction also supports
collimation of the sub-relativistic jets by gas pressure of the torus.
