Kepler has observed stars from spectral type M to F, covering about a factor of three in stellar mass. I have written a code to calculate the true occurrence of planets taking into account various observational biases, in particular the stellar properties.
We find that lower mass stars harbor planets more frequently: low-mass M stars have double the amount of Earth to Neptune-sized planets as G stars, a feature currently not predicted by planet formation models. We also find that the population of planets around low-mass stars extends closer in to their host stars. This trend matches the inner boundary of the gas in protoplanetary disks, suggesting planets migrate to their current locations and get trapped, rather than form in-situ.
link: Mulders et al. 2015 (arXiv)