the observed data, especially in relation to the asteroidal dust bands and the MMRs. Under these circumstances, we only subtracted the smooth component of the ZE, based on the Gorjian model [@Gorjian00], from the publicly released AKARI far-IR maps (for more details, see [@Doi15]). We have not yet subtracted the asteroidal dust-band and the MMR components from the data. Consequently, contributions from these components remain present in the images, and this is recognisable in the shorter-wavelength bands (N60 and WIDE-S). Next, we investigate the residual ZE contribution to the AKARI far-IR all-sky maps and construct a ZE template map, including the asteroidal dust bands and the MMRs.

Leading/trailing maps and data reduction
----------------------------------------

The AKARI orbit and observation strategy are described in detail by @Murakami07 and @Doi15. AKARI orbited the Earth in a Sun-synchronous polar orbit with a period of about 100 min. During each orbit, the satellite scanned the sky in the Earth-leading and trailing directions. The AKARI orbit processed $\sim 1\degree$ per day, and the AKARI scans were obtained at an approximately constant solar elongation of $90 \pm 1\degree$. A given longitude, observed in the Earth-leading direction, was re-observed in the Earth-trailing direction from a different position 6 