smooth distribution, resulting in the dominant diffuse emission. However, observations with the Infrared Astronomical Satellite (IRAS) revealed that small-scale structures (on scales of a few to a few tens of degrees) are present in the ZE distribution, such as those tracing the asteroidal dust bands and a circumsolar resonance ring [@Low84; @Dermott84].

The zodiacal dust bands were first discovered with IRAS in its 12 $\mu$m to 100 $\mu$m data [@Low84; @Neugebauer84]. They have subsequently been confirmed by the Diffuse Infrared Background Experiment (DIRBE) onboard the Cosmic Background Explorer (COBE), as well as by ground-based observations [@Spiesman95; @Reach97; @Ishiguro99a; @Ishiguro99b]. They provide a link between the asteroidal source of the IPD and the present distribution of the zodiacal cloud. There are three major band pairs among the dust bands that form small-scale latitudinal features in the ZE. They are thought to be produced by thermal emission from three pairs of circumsolar dust rings near inclinations with respect to the invariant plane of the planets, $i_{\rm p} = \pm \timeform{1.4D}$, $\pm \timeform{2.1D}$, and $\pm \timeform{9.3D}$ [@Sykes88; @Sykes90; @Grogan01]. The two central bands (at $\pm \timeform{1.4D}$ and $\pm \timeform{2.1D}$) are blended in low-resolution data (see e.g., [@Reach97]), and high-resolution maps are required to 