  We present two high-resolution Chandra X-ray observations of supernova (SN)
1994I which show, for the first time, that the interaction of the blast wave
from a Type Ic SN with its surrounding circumstellar material (CSM) can give
rise to soft X-ray emission. Given a 0.3-2 keV band X-ray luminosity of L_x ~ 1
x 10^{37} ergs/s between six and seven years after the outburst of SN 1994I,
and assuming the X-ray emission arises from the shock-heated CSM, we derive a
pre-SN mass-loss rate of \dot{M} ~ 1 x 10^{-5} M_sun/yr (v_w/10 km/s).
Combining the results with earlier ROSAT observations, we construct the X-ray
lightcurve of SN 1994I. A best-fit X-ray rate of decline of L_x \propto t^{-s}
with index s~1 and a CSM density profile of rho_csm \propto r^{-1.9\pm0.1} are
inferred, consistent with what is expected for a constant mass-loss rate and
constant wind velocity profile for the SN progenitor (rho_csm \propto r^{-2}).
