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Debris disks are tenuous, dusty belts surrounding main sequence starsgenerated by collisions between planetesimals. HD 206893 is one of only twostars known to host a directly imaged brown dwarf orbiting interior to itsdebris ring, in this case at a projected separation of 10.4 au. Here we resolvestructure in the debris disk around HD 206893 at an angular resolution of 0.6"(24 au) and wavelength of 1.3 mm with the Atacama LargeMillimeter/submillimeter Array (ALMA). We observe a broad disk extending from aradius of <51 au to 194^{+13}_{-2} au. We model the disk with a continuous,gapped, and double power-law model of the surface density profile, and findstrong evidence for a local minimum in the surface density distribution near aradius of 70 au, consistent with a gap in the disk with an inner radius of63^{+8}_{-16} au and width 31^{+11}_{-7} au. Gapped structure has been observedin four other debris disks -- essentially every other radially resolved debrisdisk observed with sufficient angular resolution and sensitivity with ALMA --and could be suggestive of the presence of an additional planetary-masscompanion.

Resolving Structure in the Debris Disk around HD 206893 with ALMA