In order to make accurate comparisons between state-of-the-art astrophysical simulations and observations, the simulations have to be post-processed by modern radiative transfer codes like RADMC-3D or POLARIS. In this manner, we obtain so-called synthetic observations.
For this purpose (as well as the purpose of a proper thermodynamical behaviour of the simulations) detailed information about the chemical abundances are required which we guarantee by applying astrochemical networks in our simulations.
Similar to the simulations, our synthetic observations span large physical ranges from galactic to protostellar disk scales. With these synthetic observations we able to not only interpret existing observations but even more make predictions and guide lines for future observations.
The latter allowed our working group to get involved in a number of observational proposals with e.g. ALMA and SOFIA.