Himiko is one of the most luminous Ly emitters at z = 6.595. It has three star-forming clumps detected in the rest-frame UV, with a total SFR = 20 M yr−1. We report the Atacama Large Millimeter/submillimeter Array (ALMA) detection of the C ii158 m line emission in this Galaxy with a significance of 8 . The total C ii luminosity (LC ii = 1.2 × 108 L ) is fully consistent with the local LC ii-SFR relation. The ALMA high-angular resolution reveals that the C ii emission is made of two distinct components. The brightest C ii clump is extended over 4 kpc and is located on the peak of the Ly nebula, which is spatially offset by 1 kpc relative to the brightest UV clump. The second C ii component is spatially unresolved (size <2 kpc) and coincident with one of the three UV clumps. While the latter component is consistent with the local LC ii-SFR relation, the other components are scattered above and below the local relation. We shortly discuss the possible origin of the C ii components and their relation with the star-forming clumps traced by the UV emission.