($I_\mathrm{WIDE-S}-0.30 \times I_\mathrm{WIDE-L}$) maps (see figure \[fig:diffmap\]; hereafter the “difference maps”), we can see prominent sinusoidal dust bands near the ecliptic plane and at $\beta \sim \pm 10\degree$. These images are used to determine the locations and brightnesses of the dust bands.

![Difference maps based on comparison of the WIDE-S and WIDE-L bands, $I_\mathrm{WIDE-S}-0.30 \times I_\mathrm{WIDE-L}$, in the leading (top) and trailing (bottom) directions. The maps are rendered in Cartesian projection in the ecliptic coordinate system, as in figure \[fig:ltmaps\]. There can be seen residual Galactic emission near the Galactic plane (black region), which is attributed to the emission from the Galactic dust that has the temperature different from $T = 18.5$ K.[]{data-label="fig:diffmap"}](lt_diffmaps.eps){width="10cm"}

Results: Zodiacal dust-band structure in the AKARI far-IR maps
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Geometry of asteroidal dust bands and MMRs
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To measure the latitudes of the dust bands and the structure of the circumsolar ring, we fitted the latitudinal profiles at $|\beta| < 25\degree$ with Gaussian functions. Bands at $\pm \timeform{1.4D}$ and $\pm \timeform{2.1D}$ were identified separately in the finer-scale analysis of the $\timeform{0.05D}$ resolution map using the 25 $\micron$ IRAS Infrared Sky Survey Atlas data, which were observed at a wavelength near the peak wavelength of the ZE 