  We conducted a very long baseline interferometric observation of 5 nearby
pulsars and did not resolve the scattering disks of any of these sources. Using
our upper limits on the angular diameters of these scattering disks and
published values of the broadening times and proper motion velocities, we
constrain the possible distributions of scattering material. The material
responsible for scattering these sources is neither uniformly distributed nor
concentrated at the surface of the Local Bubble. We argue that these pulsars
themselves influence their environments to produce this scattering material.
