  We determine projected rotation velocities v sini in DAZ white dwarfs, for
the first time using the rotational broadening of the CaII K line. The results
confirm previous findings that white dwarfs are very slow rotators, and set
even more stringent upper limits of typically less than 10 km/s. The few
exceptions include 3 stars known or suspected to be variable ZZ Ceti stars,
where the line broadening is very likely not due to rotation. The results
demonstrate that the angular momentum of the core cannot be preserved
completely between main sequence and final stage.
