  Some hydrogen-poor (Type Ibc) supernovae (SNe) are known to have massive
circumstellar matter (CSM) that are well detached from the star. Using the
open-source code CHIPS, we construct a grid of models of SN Ibc interacting
with detached CSM. We find that interaction with detached CSM can produce a
slowly rising phase in the light curve seen in some interacting SN Ibc, which
is difficult to reproduce by interaction with CSM of a density profile
motivated from wind or eruptions that are continuous down to the star. We also
show that SNe having double peaks in their light curves with timescales of
months (e.g., SN 2022xxf) can be explained by radioactive decay of
$^{56}$Ni/$^{56}$Co, followed by interaction with detached CSM.
