  Second order perturbation theory predicts a specific dependence of the
bispectrum, or three-point correlation function in the Fourier transform
domain, on the shape of the configuration of its three wave vector arguments,
which can be taken as a signature of structure formed by gravitational
instability. Comparing this known dependence on configuration shape with the
weak shape dependence of the galaxy bispectrum has been suggested as an
indication of bias in the galaxy distribution. However, to interpret results
obtained from projected catalogs, we must first understand the effects of
projection on this shape dependence. We present expressions for the projected
power spectrum and bispectrum in both Cartesian and spherical geometries, and
we examine the effects of projection on the predicted bispectrum with
particular attention to the dependence on configuration shape. Except for an
overall numerical factor, for Cartesian projection with characteristic depth $
\Dstar $ there is little effect on the shape dependence of the bispectrum for
wavelengths small compared to $ \Dstar $ or projected wavenumbers $ q \Dstar
\gg 1 $. For angular projection, a scaling law is found for spherical harmonic
index $ \ell \gg 1 $, but there is always a mixing of scales over the range of
the selection function. For large $ \ell $ it is sufficient to examine a small
portion of the sky.
