  The occurrence rate of young giant planets from direct imaging surveys is a
fundamental tracer of the efficiency with which planets form and migrate at
wide orbital distances. These measurements have progressively converged to a
value of about 1% for the most massive planets ($\approx$5-13 $M_\mathrm{Jup}$)
averaged over all stellar masses at separations spanning a few tens to a few
hundreds of AU. The subtler statistical properties of this population are
beginning to emerge with ever-increasing sample sizes: there is tentative
evidence that planets on wide orbits are more frequent around stars that
possess debris disks; brown dwarf companions exist at comparable (or perhaps
slightly higher) rates as their counterparts in the planetary-mass regime; and
the substellar companion mass function appears to be smooth and may extend down
to the opacity limit for fragmentation. Within a few years, the conclusion of
second-generation direct imaging surveys will enable more definitive
interpretations with the ultimate goal of identifying the dominant origin of
this population and uncovering its relationship to planets at smaller
separations.
