  We investigate a possible correlation between the solid surface density
$\Sigma$ of the minimum-mass extrasolar nebulae (MMEN) and the host star mass
$M_\star$ and metallicity [Fe/H]. Leveraging on the precise host star
properties from the California-{\it Kepler}-Survey (CKS), we found that
$\Sigma=$ 50^{+33}_{-20} \rm{~g~cm}^{-2} $(a/1AU)^{-1.75\pm0.07}$
$(M_\star/M_\odot)^{1.04\pm0.22}$ $10^{0.22\pm0.05{\rm [Fe/H]}}$ for {\it
Kepler}-like systems (1-4$R_\oplus$; $a<$1AU). The strong $M_\star$ dependence
is reminiscent of previous dust continuum results that the solid disk mass
scales with $M_\star$. The weaker [Fe/H] dependence shows that sub-Neptune
planets, unlike giant planets, form readily in lower-metallicity environment.
The innermost region ($a<$ 0.1AU) of a MMEN maintains a smooth profile despite
a steep decline of planet occurrence rate: a result that favors the truncation
of disks by co-rotating magnetospheres with a range of rotation periods, rather
than the sublimation of dusts. The $\Sigma$ of {\it Kepler} multi-transiting
systems shows a much stronger correlation with $M_\star$ and [Fe/H] than
singles. This suggests that the dynamically hot evolution that produced single
systems also partially removed the memory of formation in disks.
Radial-velocity planets yielded a MMEN very similar to CKS planets;
transit-timing-variation planets' postulated convergent migration history is
supported by their poorly constrained MMEN. We found that lower-mass stars have
a higher efficiency of forming/retaining planets: for sun-like stars about 20\%
of the solid mass within $\sim$1AU are converted/preserved as sub-Neptunes,
compared to 70\% for late-K-early-M stars. This may be due to the lower binary
fraction, lower giant-planet occurrence or the longer disk lifetime of
lower-mass stars.
