spectrum [@Reach97]. However, in the $\timeform{0.2D}$ resolution AKARI maps at much longer wavelengths, these two bands are apparently almost blended and look to be a single band. Hereafter, we refer to this pair as the $\pm \timeform{1.4D}/\timeform{2.1D}$ band. Five-Gaussian fits (two Gaussians each for the $\pm\timeform{1.4D}/\timeform{2.1D}$ and $\pm \timeform{10D}$ dust-band pairs and one for the circumsolar ring) were performed to latitudinal profiles every 1$\degree$ in longitude, for the leading and trailing maps in figure \[fig:diffmap\]. Although we reduced the Galactic cirrus contribution using the difference maps, a Galactic-emission component remains present in the maps, as seen in figure \[fig:diffmap\]. No $|\beta| < 25\degree$ scans passing within 15$\degree$ of the Galactic plane were used for fitting. We adopted Gaussian profiles because they are convenient fitting functions and they were able to reproduce the profiles adequately (see [@Reach92; @Reach97]). Examples of five-Gaussian fits are shown in figure \[fig:latprofile\].

![Latitudinal profiles taken from the difference map at $\lambda = 125\degree$ and $355\degree$ in the Earth-leading direction (open circles) and a five-Gaussian fit (thick solid line), together with the circumsolar-ring (dashed line) and dust-band components (thin solid line). Dotted line: residual emission.[]{data-label="fig:latprofile"}](latprofiles.eps){width="17cm"}

![Ecliptic latitudes of the dust-band peak brightnesses in the Earth-leading (top) and 