debris structures. The three debris components are very similar to the ones of the HR 8799 system – (1) an inner warm emission representing the dust in an asteroid-belt analog, (2) an outer cold emission representing the dust in a Kuiper-belt analog, and (3) an extended disk halo surrounding the aforementioned two components and composed of small grains. Since only the extended disk halo is resolved in the far infrared, the exact boundaries of the different components are very uncertain and not well constrained by the SED model. The presence of an asteroid-belt analog is only constrained by the excess emission detected in the [*Spitzer*]{} IRS spectrum and unresolved MIPS 24 [${\rm \mu m}$ ]{}photometry; therefore, its location is set by the observed dust temperature ($\sim$175 K, i.e., 7–10 au). Given the warm temperature and large distance to the system, this asteroid-belt component is not expected to be detected nor resolved by the ALMA observation.

Since we now have the measured size for the cold disk ($R_{in}$=106 au and $R_{out}$=320 au compared to the old SED 63–189 au value), the 3-component SED model needs revision. Furthermore, a re-reduction of the archive APEX/LABOCA 870 [${\rm \mu m}$ ]{}data on HD 95086 