  Young giant planets, which are embedded in a circumstellar disk, will
significantly perturb the disk density distribution. This effect can
potentially be used as an indirect tracer for planets. We investigate the
feasibility of observing planet-induced gaps in circumstellar disks in
scattered light. We perform 3D hydrodynamical disk simulations combined with
subsequent radiative transfer calculations in scattered light for different
star, disk, and planet configurations. The results are compared to those of a
corresponding study for the (sub)mm thermal re-emission. The feasibility of
detecting planet-induced gaps in scattered light is mainly influenced by the
optical depth of the disk and therefore by the disk size and mass.
Planet-induced gaps are in general only detectable if the photosphere of the
disks is sufficiently disturbed. Within the limitations given by the parameter
space here considered, we find that gap detection is possible in the case of
disks with masses below $\sim 10^{-4\dots-3} \, \rm M_\odot$. Compared to the
disk mass that marks the lower Atacama Large (Sub)Millimeter Array (ALMA)
detection limit for the thermal radiation re-emitted by the disk, it is
possible to detect the same gap both in re-emission and scattered light only in
a narrow range of disk masses around $\sim 10^{-4} \, \rm M_\odot$,
corresponding to $16\%$ of cases considered in our study.
