  Stellar coronal mass ejections (CMEs) have recently attracted much attention
for their impacts on stellar evolution and surrounding exoplanets. RS CVn-type
stars could produce large flares, and therefore may have frequent CMEs. Here we
report the capture of a possible CME or chromospheric condensation on the RS
CVn-type star II Pegasi (II Peg) using high-resolution spectroscopic
observation. Two flares were detected during the observation, and the low
limits of the flare energies are of the order of $10^{33}$ erg and $10^{34}$
erg, respectively. Using mean spectrum subtraction, the H$_{\alpha}$ residual
shows red asymmetry during the flares, and the redshifted broad emission
components are probably caused by chromospheric condensation or coronal rain.
Moreover, a far redshifted extra emission component with a high bulk velocity
of 429 km s$^{-1}$ was observed during the second flare and is probably due to
a prominence eruption. The velocity greatly exceeds the star's escape velocity,
which means that this eruption can develop into a CME. The CME mass is
estimated to be 0.83-1.48 $\times 10^{20}$ g, which is slightly larger than the
value expected from solar flare-CME extrapolation. The kinetic energy of CME,
derived to be 0.76-1.15 $\times 10^{35}$ erg, is less than the kinetic energy
extrapolated from solar events. Additionally, we could not completely rule out
the possibility of chromospheric condensation resulting in the far redshifted
extra emission. Finally, there is a blueshifted broad component in the
subtracted H$_{\alpha}$ profile derived using synthesized spectral subtraction
when no flare happened, and its behavior is associated with the H$_{\alpha}$
activity features.
