  We measure the binarity of detached M-dwarfs in the Kepler field with orbital
periods in the range of 1-90 days. Kepler's photometric precision and nearly
continuous monitoring of stellar targets over time baselines ranging from 3
months to 4 years make its detection efficiency for eclipsing binaries nearly
complete over this period range and for all radius ratios. Our investigation
employs a statistical framework akin to that used for inferring planetary
occurrence rates from planetary transits. The obvious simplification is that
eclipsing binaries have a vastly improved detection efficiency that is limited
chiefly by their geometric probabilities to eclipse. For the M-dwarf sample
observed by the Kepler Mission, the fractional incidence of eclipsing binaries
implies that there are $0.11 ^{+0.02} _{-0.04}$ close stellar companions per
apparently single M-dwarf. Our measured binarity is higher than previous
inferences of the occurrence rate of close binaries via radial velocity
techniques, at roughly the 2$\sigma$ level. This study represents the first use
of eclipsing binary detections from a high quality transiting planet mission to
infer binary statistics. Application of this statistical framework to the
eclipsing binaries discovered by future transit surveys will establish better
constraints on short-period M$+$M binary rate, as well as binarity measurements
for stars of other spectral types.
