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 - K _ { s } color . Both the optical continuum and broad emission lines are reddened by SMC-like dust of E ( B - V ) \simeq 1.0 mag , while its near-infrared color ( J - K _ { s } = 1.60 ) shows little reddening . The CaII absorption lines are saturated and resolved with an FWHM of 362 km s ^ { -1 } and an equivalent width of W _ { \mathrm { C } aII K } = 4.2 Å ( 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 .