  The DSHARP survey evidenced the ubiquity of substructure in the mm dust
distribution of large, bright protoplanetary discs. Intriguingly, these
datasets have yet higher resolution information that is not recovered in a
CLEAN image. We first identify that the various resolution limitations in the
CLEAN algorithm effectively increase the CLEAN beam width by a mean factor of
1.16 across the survey. Then analyzing all 20 DSHARP sources using the 1D,
super-resolution code Frankenstein (frank), we accurately fit the visibilities
to a mean factor of 4.1 longer baseline than CLEAN (determined by the baseline
out to which the frank and CLEAN visibility fit errors are <20%). This yields a
higher resolution brightness profile for each source, identifying new
substructure interior to 30 au in multiple discs; resolving known gaps to be
deeper, wider, and more structured; and known rings to be narrower and
brighter. Categorizing these brightness profiles into trends, we find that the
relative scarcity of features interior to 30 au in the survey's CLEAN images is
an artifact of resolving power, rather than an intrinsic rarity of inner disc
(or compact disc) substructure.
