A foundational idea in the theory of in situ planet formation is the "minimum
mass extrasolar nebula" (MMEN), a surface density profile (Ξ£) of disk
solids that is necessary to form the planets in their present locations. While
most previous studies have fit a single power-law to all exoplanets in an
observed ensemble, it is unclear whether most exoplanetary systems form from a
universal disk template. We use an advanced statistical model for the
underlying architectures of multi-planet systems to reconstruct the MMEN. The
simulated physical and Kepler-observed catalogs allows us to directly assess
the role of detection biases, and in particular the effect of non-transiting or
otherwise undetected planets, in altering the inferred MMEN. We find that
fitting a power-law of the form Ξ£=Ξ£0ββ(a/a0β)Ξ² to each
multi-planet system results in a broad distribution of disk profiles;
Ξ£0ββ=336β291+727β g/cm2 and Ξ²=β1.98β1.52+1.55β
encompass the 16th-84th percentiles of the marginal distributions in an
underlying population, where Ξ£0ββ is the normalization at a0β=0.3
AU. Around half of inner planet-forming disks have minimum solid masses of
β³40Mββ within 1 AU. While transit observations do not tend to
bias the median Ξ², they can lead to both significantly over- and
under-estimated Ξ£0ββ and thus broaden the inferred distribution of disk
masses. Nevertheless, detection biases cannot account for the full variance in
the observed disk profiles; there is no universal MMEN if all planets formed in
situ. The great diversity of solid disk profiles suggests that a substantial
fraction (β³23%) of planetary systems experienced a history of
migration.Comment: Accepted to AJ. 14 pages, 6 figures, 1 table. Accompanying code is
available via SysSimPyMMEN, a pip-installable Python package (see
https://syssimpymmen.readthedocs.io/en/latest/