  Axisymmetric density distributions are constructed which are invisible when
viewed from a range of inclination angles $i$. By adding such distributions to
a model galaxy, it can be made either disky or boxy without in any way
affecting its projected image. As the inclination of a galaxy decreases from
edge-on to face on, the range of `invisible' densities, the uncertainty in the
deprojection, and the sensitivity of the deprojection to noise all increase.
The relation between these phenomena is clarified by an analysis of Palmer's
deprojection algorithm.
  These results imply that disk-to-bulge ratios are in principle ill-determined
from photometry unless the disk is strong or the system is seen precisely
edge-on. The uncertain role of third integrals in galaxies makes it unclear to
what degree this indeterminacy can be resolved by kinematic studies.
