  In a multi-wavelength study of thermal emission and scattered light images we
analyse the dust properties and structure of the debris disc around the A1-type
main sequence star 49~Cet. As a basis for this study, we present new scattered
light images of the debris disc known to possess both a high amount of dust and
gas. The outer region of the disc is revealed in former coronagraphic H-band
and our new Y-band images from the Very Large Telescope SPHERE instrument. We
use the knowledge of the disc's radial extent inferred from ALMA observations
and the grain size distribution found by SED fitting to generate semi-dynamical
dust models of the disc. We compare the models to scattered light and thermal
emission data and find that a disc with a maximum of the surface density at
110~au and shallow edges can describe both thermal emission and scattered light
observations. This suggests that grains close to the blow-out limit and large
grains stem from the same planetesimal population and are mainly influenced by
radiation pressure. The influence of inwards transport processes could not be
analysed in this study.
