continuum that is resolved out by comparing the observed rest-frame 160-$\mu$m continuum fluxes with SED modeling predictions, assuming constant $T_\mathrm{dust}$ and optical depth across the source. Namely, we use [MagPhys]{} to perform SED modeling using all the photometry points apart from the rest-frame 160-$\mu$m continuum. The predicted 160-$\mu$m flux-densities are 11.8 and 7.6 mJy for ALESS 49.1 and 57.1, respectively; the observed flux densities match the predicted ones within $<$10%. Therefore, we conclude that our observations recover the bulk of the 160-$\mu$m emission, in line with the compact continuum sizes inferred in Section \[subsec:uv-plane\].

Discussion {#sec:discussion}
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Comparison with CO(3–2) emission
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Based on the $uv$-plane analysis in Section \[subsec:uv-plane\] which was tested on mock ALMA data in Section \[subsec:mock\_data\], we found the \[\]/160-$\mu$m continuum surface brightness distribution to be dominated by a compact component, embedded within a low-surface-brightness, extended emission. We now compare these morphologies to the CO(3–2) surface brightness profiles, and other low- and high-redshift observations and simulations.

### 160-$\mu$m continuum size

Comparing the 160-$\mu$m continuum emission sizes with the CO(3–2) sizes (Table \[tab:source\_properties\]), the 160-$\mu$m continuum is 1.9$\pm$0.3 (ALESS 49.1) and 3.1$\pm$0.7 (ALESS 57.1) more compact than the CO(3–2) emission.

Compact dust continuum emission embedded in a 