all ecliptic longitudes.

![image](lt_4bands.eps){width="17cm"}

Asteroidal dust bands appear as pairs of equally spaced parallel bands that are oriented along the ecliptic longitude direction in a sinusoidal fashion above and below the ecliptic plane. The continuous, smooth distribution of the dust bands and the MMR component along the ecliptic plane can be seen in the N60 and WIDE-S maps (see figure \[fig:ltmaps\]). In the “snap-shot image” of the DIRBE weekly sky map covering the wide solar elongation angle of 60$\degree$–120$\degree$, the MMR component in the Earth’s orbit shows an elliptical structure. The full-width at half-maximum brightness of the trailing blob is 30$\degree$ in latitude and 15$\degree$ in longitude [@Reach95]. AKARI always scans the central part of the MMR component at the solar elongation of $\sim 90\degree$. As a consequence, the superposition of the MMR component in the AKARI all-sky map appear as a horizontal faint band structure of $\sim 30\degree$ width in latitude oriented along the ecliptic longitude direction. Note that the ZE smooth cloud component has been subtracted from the AKARI images. To reduce the effects of non-Solar System contributions to the sky brightness and to extract the dust-band distribution, we constructed difference maps using the WIDE-S and WIDE-L bands. 