The original AKARI maps have a pixel scale of 15$\arcsec$ and a spatial resolution (i.e., the full width at half maximum of the point-spread function) of 1–1.5$\arcmin$ [@Takita15]. The asteroidal dust bands and the MMR components exhibit much more extensive spatial structures, covering a few and a few tens of degrees along the latitudinal direction, respectively. To reduce the noise and contributions from both much smaller-scale structures and point sources, we reconstructed the maps with a resolution of . We use these maps, in the Earth-leading and trailing directions, to extract the structure of the ZE distribution in the following analysis. The processed sky-brightness maps in the four FIS bands are shown in figure \[fig:ltmaps\] for both the leading and trailing directions. Other IR-satellite survey missions (e.g., IRAS, COBE/DIRBE or WISE) lack certain regions in longitude ($\sim 15$%) in their leading/trailing maps, because their cryogenic mission lifetimes were shorter than 1 year. The AKARI survey data cover all ecliptic longitudes ($\lambda = 0\degree$–360$\degree$), except for the small regions affected by the Moon, both in the leading and trailing maps within the satellite’s 16-month cryogenic mission period. By using the AKARI leading/trailing maps, we can investigate the continuous dust-band structures along 