  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 show that the intrinsic performance of the CLEAN
algorithm is resolution-limited. Then analyzing all 20 DSHARP sources using the
1D, super-resolution code Frankenstein (frank), we accurately fit the 1D
visibilities to a mean factor of 4.3 longer baseline than the Fourier transform
of the CLEAN images and a factor of 3.0 longer baseline than the transform of
the CLEAN component models. 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. Across the survey, high contrast gaps are an
average 14% wider and 44% deeper in the frank profiles relative to CLEAN, and
high contrast rings are an average 26% narrower. Categorizing the frank
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. Finally the rings in the frank profiles are narrower than the
previously inferred deconvolved widths, indicating smaller alpha / St ratios in
the local gas disc.
