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We present 0".035 resolution (~200 pc) imaging of the 158 um [CII] line andthe underlying dust continuum of the z=6.9 quasar J234833.34-305410.0. The 18 hALMA observations reveal extremely compact emission (diameter ~1 kpc) that isconsistent with a simple, almost face-on, rotation-supported disk with asignificant velocity dispersion of ~160 km/s. The gas mass in just the central200 pc is ~4x10^9 M_sun, about a factor two higher than that of the centralsupermassive black hole. Consequently we do not resolve the black hole's sphereof influence, and find no kinematic signature of the central supermassive blackhole. Kinematic modeling of the [CII] line shows that the dynamical mass atlarge radii is consistent with the gas mass, leaving little room for asignificant mass contribution by stars and/or dark matter. The Toomre-Qparameter is less than unity throughout the disk, and thus is conducive to starformation, consistent with the high infrared luminosity of the system. The dustin the central region is optically thick, at a temperature >132 K. Usingstandard scaling relations of dust heating by star formation, this implies anunprecedented high star formation rate density of >10^4 M_sun / yr / kpc^2.Such a high number can still be explained with the Eddington limit for starformation under certain assumptions, but could also imply that the centralsupermassive black hole contributes to the heating of the dust in the central110 pc.

ALMA 200 pc imaging of a z~7 quasar reveals a compact, disk-like host galaxy