  It has long been known how to analytically relate the clustering properties
of the collapsed structures (halos) to those of the underlying dark matter
distribution for Gaussian initial conditions. Here we apply the same approach
to physically motivated non-Gaussian models. The techniques we use were
developed in the 1980s to deal with the clustering of peaks of non-Gaussian
density fields. The description of the clustering of halos for non-Gaussian
initial conditions has recently received renewed interest, motivated by the
forthcoming large galaxy and cluster surveys. For inflationary-motivated
non-Gaussianites, we find an analytic expression for the halo bias as a
function of scale, mass and redshift, employing only the approximations of
high-peaks and large separations.
