  We report the detection of strong CaII/MgII absorption lines at the quasar
redshift in the narrow line quasar SDSS J2339-0912 (z=0.6604). The quasar
exhibits strong FeII, small Balmer emission line width and a very red B-Ks
color. Both the optical continuum and broad emission lines are reddened by
SMC-like dust of E(B-V)~1.0 mag, while its near-infrared color (J-Ks=1.60)
shows little reddening. The CaII absorption lines are saturated and resolved
with an FWHM of 362 km/s and an equivalent width of W_{CaII K}=4.2\AA (in the
source rest frame). MgII absorption lines are also saturated and have a similar
line width. The line profile and the fact that there is no evidence for
starlight from the host galaxy suggest that these absorption lines are not of a
stellar origin. The ratio of column density of CaII to that of dust is
consistent with that of the ISM in our Galaxy. We suggest that both the heavy
reddening and the large absorption line width are due to the highly disturbed
ISM on the line of sight toward the quasar, and that the disturbance is caused
by a galaxy collision or even merger in the quasar host galaxy.
