----------------------------
  $\pm\timeform{1.4D}/\timeform{2.1D}$ band     $1.0\pm0.1$        $112\pm6$           1.86     Beagle/Karin families
  $\pm\timeform{10D}$ band                      $1.3\pm0.1$         $95\pm5$           2.16     Veritas family

  : Geometry of the dust bands in the AKARI maps.[]{data-label="tab:geometry"}

It is also evident that the surface brightness of the dust bands varies as a function of ecliptic longitude. @Reach97 refer to the phenomenon that the northern component is bright when the southern component is faint, and [*vice versa*]{}, as “glints”. In the DIRBE maps, the northern and southern glints occur roughly 180$\degree$ apart, while the leading and trailing maps are roughly 180$\degree$ out of phase [@Reach97]. Although the difference between the leading and trailing direction is faint, similar dust-band glints are detected in the AKARI maps, and can be seen in the component maps (figure \[fig:ZEmodel\_lt\]) in particular for the $\pm 10\degree$ band. We also performed sinusoidal fits to the longitudinal brightness variations of the northern and southern components. Based on the brightnesses, latitudes and band widths derived from the sinusoidal fitting procedure outlined above (see Tables \[tab:gaussian\] and \[tab:geometry\], figure \[fig:peak\]), we constructed a model map for the dust-band structure in the far-IR regime. Our model maps for each component in the Earth-leading and trailing directions are shown in figure \[fig:ZEmodel\_lt\].

![Model maps 