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We present a comparison of the interstellar medium traced by [CII] (ALMA),and ionised halo gas traced by Lya (MUSE), in and around QSO host galaxies atz~6. To date, 18 QSOs at this redshift have been studied with both MUSE andhigh-resolution ALMA imaging; of these, 8 objects display a Lya halo. Usingdatacubes matched in velocity resolution, we compare and contrast the spatialand kinematic information of the Lya halos and the host galaxies' [CII] (anddust-continuum) emission. We find that the Lya halos extend typically 3-30times beyond the interstellar medium of the host galaxies. The majority of theLya halos do not show ordered motion in their velocity fields, whereas most ofthe [CII] velocity fields do. In those cases where a velocity gradient can bemeasured in Lya, the kinematics do not align with those derived from the [CII]emission. This implies that the Lya emission is not tracing the outskirts of alarge rotating disk that is a simple extension of the central galaxy seen in[CII] emission. It rather suggests that the kinematics of the halo gas aredecoupled from those of the central galaxy. Given the scattering nature of Lya,these results need to be confirmed with JWST IFU observations that canconstrain the halo kinematics further using the non-resonant Ha line.

The Decoupled Kinematics of high-z QSO Host Galaxies and their Lya halos