Radial variation of metallicity profiles averaged along isophotes for all ATLAS^3D slow rotators and normalised by the half-light radii. Blue circles show metallicity profiles of slow rotators with core-less surface brightness profiles, and red squares show profiles of slow rotators with cores. Green circles belong to NGC 1222, which was not classified because of the dust. As seen in Fig. 7, core galaxies are more massive slow rotators, and the offset between the metallicity profiles of core and core-less galaxies is explained as the mass trend. Core galaxies are also larger than core-less galaxies, which explains the offsets along the horizontal axis between the two types of galaxies. The profiles differ also in their slopes, however.