  Galactic winds probe how feedback regulates the mass and metallicity of
galaxies. Galactic winds have cold gas, which is mainly observable with
absorption and emission lines. Theoretically studying how absorption lines are
produced requires numerical simulations and realistic starburst UV backgrounds.
We use outputs from a suite of 3D PLUTO simulations of wind-cloud interactions
to first estimate column densities and temperatures. Then, to create synthetic
spectra, we developed a python interface to link our PLUTO simulations to
TRIDENT via the YT-package infrastructure. First we produce UV backgrounds
accounting for the star formation rate of starbursts. For this purpose, we use
fluxes generated by STARBURST99, which are then processed through CLOUDY to
create customised ion tables. Such tables are subsequently read into TRIDENT to
generate absorption spectra. We explain how the various packages and tools
communicate with each other to create ion spectra consistent with spectral
energy distributions of starburst systems.
