Molecule Formation in AGN-driven outflows: towards a consistent galaxy model
The origin of the fast molecular outflows observed in active galactic nuclei (AGNs) is not fully understood. One feasible scenario is that cold molecular clouds are swept up by the AGN fueled winds. Another plausible scenario is that the detected molecules are formed “in situ” as a consequence of efficient cooling behind the shocked gas. It is unclear whether or not these scenarios are mutually exclusive and how the interplay between AGN and stellar feedback can affect the molecule formation. To investigate the formation scenario in more detail, we perform 3D hydrodynamical simulations of an isotropic AGN wind which results in a fast outflow using the magneto-hydrodynamics code GIZMO, coupled with chemistry, through the code KROME. A key factor in the process is the radiative feedback (from the AGN, but also from the stars), which is typically modelled by averaging the reaction rates using a fixed spectral shape. In particular, as the light travels through gas, the shape of the spectrum of radiation is changing, due to different opacities at different wavelengths. I will show the impact of a more consistent modelling based on spectrum-binning on the results with respect to the common approach, and how this scheme will finally help shedding light on the origin of molecular outflows.
Room U2-2016