Pushing ALMA to the limit: 140 pc resolution observations of a z=6.6 quasar-galaxy merger resolve strikingly different morphologies of dust continuum and [CII] 158 um emission

We present $0.\mathrm{"}026$ $(140\mathrm{p}\mathrm{c})$ resolution ALMA observations of [C II] $158\mu \mathrm{m}$ and dust continuum emission of the $z=6.6$ quasar J0305–3150, resolved over $\sim 300-400$ independent resolution elements. The dust continuum emission is compact with $\sim 80\mathrm{\%}$ recovered within $r<0.\mathrm{"}3$ $(1.6\mathrm{k}\mathrm{p}\mathrm{c})$, whereas the [C II] emission profile is composed of a central Gaussian ($r<0.\mathrm{"}4$, i.e. $<2.2\mathrm{k}\mathrm{p}\mathrm{c}$) and an extended component (detected up to $\sim 10\mathrm{k}\mathrm{p}\mathrm{c}$ at $>3\sigma$). We infer a direct contribution of the quasar to the observed 260\ \rm{GHz} continuum $S_{\nu ,\mathrm{Q}\mathrm{S}\mathrm{O}}\mathrm{/}{S}_{\nu ,\mathrm{Q}\mathrm{S}\mathrm{O}+\mathrm{H}\mathrm{o}\mathrm{s}\mathrm{t}}\lesssim 1\mathrm{\%}$. We report the detection of FIR-detected star-forming clumps with $r<200\mathrm{p}\mathrm{c}$ and properties similar to that of rest-frame UV-optical clumps reported in the literature. The $200\mathrm{p}\mathrm{c}$ resolved [C II]/FIR ratio follows the global relation with the FIR surface brightness established in low- and high-redshift galaxies, even at the quasar location. We find that dust continuum is emitted in regions of $\sim 0.\mathrm{"}02-0.\mathrm{"}04$ consistent with the size of photo-dissociation regions (PDR), whereas $50\mathrm{\%}$ of the [C II] originates from larger physical scales ($\theta \gtrsim 2\mathrm{"}$). The large-scale [C II] emission presents a velocity gradient aligned with a nearby companion with perturbed kinematics, and misaligned with the kinematics of the small-scale emission. The absence of significant [C II] emission by structures with physical scale $\lesssim 1\mathrm{k}\mathrm{p}\mathrm{c}$ implies that [C II] emission is not produced in dense PDR located at the boundary of Giant Molecular Clouds. We argue instead that [C II] is produced in low-density PDRs in the interstellar medium and diffuse HI gas tidally-stripped during the ongoing merger.