identify and distinguish the band pairs. It has been proposed that recent disruption events among multi-kilometer bodies in the main asteroid belt, which would have occurred within the last several million years, may be major supply sources of dust particles, and they would produce edge-brightened toroidal dust distributions (referred to as the “catastrophic” or “non-equilibrium” model; [@Sykes86; @Sykes88]). Recent detailed studies [@Nesvorny02; @Nesvorny03; @Nesvorny06a; @Nesvorny08] have provided evidence supporting the disruption model as the possible origin of the asteroidal dust bands. @Nesvorny03 proposed that the dust band characterized by an inclination of $\pm \timeform{9.3D}$ may have originated from the Veritas asteroid family, at a distance of 3.17 a.u. from the Sun, which formed through collisional disruption $8.3 \pm 0.5$ Myr ago, while the $\pm \timeform{2.1D}$ band may have originated from the Karin family, which formed $5.75 \pm 0.05$ Myr ago and is located inside the Koronis asteroid family at a solar distance of 2.87 a.u. [@Nesvorny02; @Nesvorny03; @Nesvorny06b]. @Nesvorny08 also proposed a recent breakup of the new candidate Beagle asteroid family as the source of the $\pm \timeform{1.4D}$ band. Dust from the asteroids and comets, which continues to spiral in towards the inner Solar System, is subject to gravitational perturbations 