Previous studies of planet occurrence rates largely relied on photometric stellar characterizations .
In this paper , we present planet occurrence rates for mid-type M dwarfs using spectroscopy , parallaxes , and photometry to determine stellar characteristics .
Our spectroscopic observations have allowed us to constrain spectral type , temperatures , and in some cases metallicities for 337 out of 561 probable mid-type M dwarfs in the primary Kepler field .
We use a random forest classifier to assign a spectral type to the remaining 224 stars .
Combining our data with Gaia parallaxes , we compute precise ( \sim 3 % ) stellar radii and masses , which we use to update planet parameters and planet occurrence rates for Kepler mid-type M dwarfs .
Within the Kepler field , there are seven M3 V to M5 V stars which host 13 confirmed planets between 0.5 and 2.5 Earth radii and at orbital periods between 0.5 and 10 days .
For this population , we compute a planet occurrence rate of 1.19 ^ { +0.70 } _ { -0.49 } planets per star .
For M3 V , M4 V , and M5 V , we compute planet occurrence rates of 0.86 ^ { +1.32 } _ { -0.68 } , 1.36 ^ { +2.30 } _ { -1.02 } , and 3.07 ^ { +5.49 } _ { -2.49 } planets per star , respectively .