  Young stars are frequently observed to host circumstellar disks, within which
their attendant planetary systems are formed. Scattered light imaging of these
proto-planetary disks reveals a rich variety of structures including spirals,
gaps and clumps. Self-consistent modelling of both imaging and multi-wavelength
photometry enables the best interpretation of the location and size
distribution of disks' dust. Epsilon Sagittarii is an unusual star system. It
is a binary system with a B9.5III primary that is also believed to host a
debris disk in an unstable configuration. Recent polarimetric measurements of
the system with the High Precision Polarimetric Instrument (HIPPI) revealed an
unexpectedly high fractional linear polarisation, one greater than the
fractional infrared excess of the system. Here we develop a spectral energy
distribution model for the system and use this as a basis for radiative
transfer modelling of its polarisation with the RADMC-3D software package. The
measured polarisation can be reproduced for grain sizes around 2.0 microns.
