  We used high-resolution [C II] 158 $\mu$m mapping of two nebulae IC 59 and IC
63 from SOFIA/upGREAT in conjunction with ancillary data on the gas, dust, and
polarization to probe the kinematics, structure, and magnetic properties of
their photo-dissociation regions (PDRs). The nebulae are part of the Sh 2-185 H
II region illuminated by the B0 IVe star $\gamma$ Cas. The velocity structure
of each PDR changes with distance from $\gamma$ Cas, consistent with driving by
the radiation. Based on previous FUV flux measurements of, and the known
distance to $\gamma$ Cas along with the predictions of 3D distances to the
clouds, we estimated the FUV radiation field strength (G0) at the clouds.
Assuming negligible extinction between the star and clouds, we find their 3D
distances from $\gamma$ Cas. For IC 63, our results are consistent with earlier
estimates of distance from Andersson et al. (2013), locating the cloud at 2 pc
from $\gamma$ Cas, at an angle of 58 to the plane of the sky, behind the star.
For IC 59, we derive a distance of 4.5 pc at an angle of 70 in front of the
star. We do not detect any significant correlation between the orientation of
the magnetic field (Soam et al. 2017) and the velocity gradients of [C II] gas,
indicating a moderate magnetic field strength. The kinetic energy in IC 63 is
estimated to be order of ten higher than the magnetic energies. This suggests
that kinetic pressure in this nebula is dominant.
