  The planet formation environment around M dwarf stars is different than
around G dwarf stars. The longer hot protostellar phase, activity levels and
lower protoplanetary disk mass of M dwarfs all may leave imprints on the
composition distribution of planets. We use hierarchical Bayesian modeling
conditioned on the sample of transiting planets with radial velocity mass
measurements to explore small planet mass-radius distributions that depend on
host star mass. We find that the current mass-radius dataset is consistent with
no host star mass dependence. These models are then applied to the
\textit{Kepler} planet radius distribution to calculate the mass distribution
of close-orbiting planets and how it varies with host star mass. We find that
the average heavy-element mass per star at short orbits is higher for M dwarfs
compared to FGK dwarfs, in agreement with previous studies. This work will
facilitate comparisons between microlensing planet surveys and \textit{Kepler},
and will provide an analysis framework that can readily be updated as more M
dwarf planets are discovered by ongoing and future surveys such as \textit{K2}
and \textit{TESS}.
