Full polarisation is back! You can now simulate visibilities using QUV information in the skymodel, and they can be independent to Stokes I. In fact, you can set Stokes I to zero in the sky model, and still enter QUV information. Stokes V can either be a power-law, curved power-law, be a polarisation fraction of Stokes I, or be a list of flux densities. Linear polarisation (Q and U) can either be a power-law, curved power-law, be a polarisation fraction of Stokes I, or be a list of flux densities. The first three are always used in conjunction with a rotation measure. List-type fluxes can be given separately for Q and U, which makes Q and U independent of each other. Alternatively, a single list of linear polarisation fluxes can be given, which is used in conjunction with a rotation measure to determine Q and U. Also worked out a way to dynamically create the ctypes classes used to mirror the structs used in the C code, as they needed either float or double precision. Removes the need for having two different sets of near identical code.