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Feedback from accreting supermassive black holes, active galactic nuclei(AGN), is now a cornerstone of galaxy formation models. In this work, wepresent radiation-hydrodynamic simulations of radiative AGN feedback using thenovel Arepo-RT. A central black hole emits radiation at a constant luminosityand drives an outflow via radiation pressure on dust grains. Utilising anisolated NFW halo we validate our setup in the single and multi-scatteringregimes, with the simulated shock front propagation in excellent agreement withthe expected analytic result. For a spherically symmetric NFW halo, anexamination of the simulated outflow properties generated by radiative feedbackdemonstrates that they are lower than typically observed at a fixed AGNluminosity, regardless of the collimation of the radiation. We then explore theimpact of a central disc galaxy and the assumed dust model on the outflowproperties. The contraction of the halo during the galaxy's formation andmodelling the production of dust grains results in a factor $100$ increase inthe halo's optical depth. Radiation is then able to couple momentum moreefficiently to the gas, driving a stronger shock and producing a mass-loaded$\sim10^{3}\,\mathrm{M}_{\odot}\,\mathrm{yr}^{-1}$ outflow with a velocity of$\sim2000\,\mathrm{km}\,\mathrm{s}^{-1}$, in agreement with observations.However, the inclusion of dust destruction mechanisms, like thermal sputtering,leads to the rapid destruction of dust grains within the outflow, reducing itsproperties below typically observed values. We conclude that radiative AGNfeedback can drive outflows, but a thorough numerical and physical treatment isrequired to assess its true impact.

Radiative AGN feedback on a moving mesh: the impact of the galactic disc and dust physics on outflow properties