  IW And stars are a recently recognized group of dwarf novae which are
characterized by a repeated sequence of brightening from a standstill-like
phase with damping oscillations followed by a deep dip. Kimura et al. (2019)
recently proposed a model based on thermal-viscous disk instability in a tilted
disk to reproduce the IW And-type characteristics. IM Eri experienced the IW
And-type phase in 2018 and we recorded three cycles of the (damping)
oscillation phase terminated by brightening. We identified two periods during
the IW And-type state: 4-5 d small-amplitude (often damping) oscillations and a
34-43 d long cycle. This behavior is typical for an IW And-type star. The
object gradually brightened within the long cycle before the next brightening
which terminated the (damping) oscillation phase. This observation agrees with
the increasing disk mass during the long cycle predicted by a model of
thermal-viscous disk instability in a tilted disk (Kimura et al. 2019). We,
however, did not succeed in detecting negative superhumps, which are considered
to be the signature of a tilted disk.
