  The phases of the Fourier transform of any linear cosmological perturbation
may be random (the Gaussian case) or not (the non-Gaussian case). If a
non-Gaussian inhomogeneity was generated during the inflationary era by some
process of very high energy physics, its evolution may be computed using the
usual linear theory. I focus on the perturbations induced on the microwave
background (CMB) by an underlying non-Gaussian distribution of dark matter
(DM). Giving the specific example of an inflationary bubble, I show how
non-Gaussian structures lying on the last scattering surface (LSS) may give
rise to ordered patterns in the CMB anisotropy field. The next high resolution
observations of the CMB sky may eventually detect these signals.
