ALMA detection of extended [CII] emission in Himiko at z=6.6
  Himiko is one of the most luminous Ly{\alpha} emitters at z = 6.595. It has
three star forming clumps detected in the rest-frame UV, with a total SFR = 20
M$_\odot$/yr. We report the ALMA detection of the [CII]158$\mu$m line emission
in this galaxy with a significance of 9$\sigma$. The total [CII] luminosity
(L[CII]= (1.2$\pm$0.2)$\times$10$^{8}$ L$_{\odot}$) is fully consistent with
the local L[CII]-SFR relation. The ALMA high-angular resolution reveals that
the [CII] emission is made of two distinct components. The brightest [CII]
clump is extended over 4 kpc and is located on the peak of the Ly{\alpha}
nebula, which is spatially offset by 1 kpc relative to the brightest UV clump.
The second [CII] component is spatially unresolved (size $<$2 kpc) and
coincident with one of the three UV clumps. While the latter component is
consitent with the local L[CII]-SFR relation, the other components are
scattered above and below the local relation. We shortly discuss the possible
origin of the [CII] components and their relation with the star forming clumps
traced by the UV emission.
