The frequency of dust lanes in edge-on spiral galaxies identified by
  Galaxy Zoo in KiDS imaging of GAMA targets
  Dust lanes bisect the plane of a typical edge-on spiral galaxy as a dark
optical absorption feature. Their appearance is linked to the gravitational
stability of spiral disks; the fraction of edge-on galaxies that displays a
dust lane is a direct indicator of the typical vertical balance between gravity
and turbulence; a balance struck between the energy input from star-formation
and the gravitational pull into the plane of the disk.
  Based on morphological classifications by the Galaxy~Zoo project on the
Kilo-Degree Survey (KiDS) imaging data in the Galaxy and Mass Assembly (GAMA)
fields, we explore the relation of dust lanes to the galaxy characteristics,
most of which were determined using the {\sc magphys} spectral energy
distribution fitting tool: stellar mass, total and specific star-formation
rates, and several parameters describing the cold dust component.
  We find that the fraction of dust lanes does depend on the stellar mass of
the galaxy; they start to appear at $M^* \sim 10^9 M_\odot$. A dust lane also
implies strongly a dust mass of at least $10^5 M_\odot$, but otherwise does not
correlate with cold dust mass parameters of the {\sc magphys} spectral energy
distribution analysis, nor is there a link with star-formation rate, specific
or total. Dust lane identification does not depend on disk ellipticity (disk
thickness) or Sersic profile but correlates with bulge morphology; a round
bulge favors dust lane votes.
  The central component along the line of sight that produces the dust lane is
not associated with either one of the components fit by {\sc magphys}, the cold
diffuse component or the localized, heated component in HII regions, but a mix
of these two.
