  We examine the observational appearance of partial gaps being opened by
planets in protoplanetary disks, considering the effects of the inclination
relative to the line of sight. The gap's trough is darkened by both shadowing
and cooling, relative to the uninterrupted disk. The gap's outer wall is
brightened by direct illumination and also by heating, which puffs it up so
that it intercepts more starlight. In this paper, we examine the effects of
inclination on resolved images of disks with and without gaps at a wide range
of wavelengths. The scattering surface's offset from the disk midplane creates
a brightness asymmetry along the axis of inclination, making the disk's near
side appear brighter than the far side in scattered light. Finite disk
thickness also causes the projected distances of equidistant points on the disk
surface to be smaller on the near side of the disk as compared to the far side.
Consequently, the gap shoulder on the near side of the disk should appear
brighter and closer to the star than on the far side. However, if the angular
resolution of the observation is coarser than the width of the brightened gap
shoulder, then the gap shoulder on the far side may appear brighter because of
its larger apparent size. We present a formula to recover the scale height and
inclination angle of an imaged disk using simple geometric arguments and
measuring disk asymmetries. Resolved images of circumstellar disks have
revealed clearings and gaps, such as the transitional disk in LkCa 15. Models
created using our synthetic imaging attempting to match the morphology of
observed scattered light images of LkCa 15 indicate that the H-band flux
deficit in the inner $\sim0.5\arcsec$ of the disk can be explained with a
planet of mass greater than 0.5 Jupiter mass.
