We present a statistical analysis of the Kepler M dwarf planet hosts , with a particular focus on the fractional number of systems hosting multiple transiting planets .
We manufacture synthetic planetary systems within a range of planet multiplicity and mutual inclination for comparison to the Kepler yield .
We recover the observed number of systems containing between 2 and 5 transiting planets if every M dwarf hosts 6.1 \pm 1.9 planets with typical mutual inclinations of 2.0 ^ { +4.0 } _ { -2.0 } degrees .
This range includes the Solar System in its coplanarity and multiplicity .
However , similar to studies of Kepler exoplanetary systems around more massive stars , we report that the number of singly–transiting planets found by Kepler is too high to be consistent with a single population of multi–planet systems : a finding that can not be attributed to selection biases .
To account for the excess singleton planetary systems we adopt a mixture model and find that 55 ^ { +23 } _ { -12 } % of planetary systems are either single or contain multiple planets with large mutual inclinations .
Thus , we find that the so-called “ Kepler dichotomy ” holds for planets orbiting M dwarfs as well as Sun–like stars .
Additionally , we compare stellar properties of the hosts to single and multiple transiting planets .
For the brightest subset of stars in our sample we find intriguing , yet marginally significant evidence that stars hosting multiply–transiting systems are rotating more quickly , are closer to the midplane of the Milky Way , and are comparatively metal poor .
This preliminary finding warrants further investigation .