weak trend that the inner edge of the cold planetesimal zone appears to depend on the luminosity/temperature of the star, indicating a signpost for planetary migration and/or shepherding. However, disk extents estimated from SEDs are degenerate. Any inferred radii depend strongly on the assumed composition and the particle size distribution. Due to this degeneracy, it is very difficult to translate SED measurements into physical sizes directly. Even when there are resolved images available (mostly in the far-infrared), the exact location of the parent bodies is still uncertain due to the effect of non-gravitational forces (radiation and drag) on small grains. The true parent-body distribution in debris disks can be provided by resolved submillimeter/millimeter images which probe large (mm-size) grains that stay close to their parent bodies. Disk morphologies suggestive of influences from unseen planets, such as resonance clumps [@wyatt03] and/or apo-center glow [@pan16], are also best observed at submillimeter/millimeter wavelengths (e.g., @ertel12 [@lohne17]). Existing ALMA data on debris disks show a large variety of Kuiper-belt analogs: some systems have very narrow rings of parent bodies (e.g., Fomalhaut, @boley12 [@macgregor17], and $\epsilon$ Eri, @booth17), and some have either multiple rings (HD 107146, @ricci15a) or broad disks (HR 8799, @booth16; $\tau$ Ceti, 