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We present a novel set of stellar feedback models, implemented in themoving-mesh code Arepo, designed for galaxy formation simulations withnear-parsec (or better) resolution. These include explicit sampling of starsfrom the IMF, allowing feedback to be linked to individual massive stars, animproved method for the modelling of H II regions, photoelectric heating from aspatially varying FUV field and supernova feedback. We perform a suite of 32simulations of isolated $M_\mathrm{vir} = 10^{10}\,\mathrm{M_\odot}$ galaxieswith a baryonic mass resolution of $20\,\mathrm{M_\odot}$ in order to study thenon-linear coupling of the different feedback channels. We find thatphotoionization and supernova feedback are both independently capable ofregulating star formation to the same level, while photoelectric heating isinefficient. Photoionization produces a considerably smoother star formationhistory than supernovae. When all feedback channels are combined, theadditional suppression of star formation rates is minor. However, outflow ratesare substantially reduced relative to the supernova only simulations. We showthat this is directly caused by a suppression of supernova clustering by thephotoionization feedback, disrupting star forming clouds prior to the firstsupernovae. We demonstrate that our results are robust to variations of ourstar formation prescription, feedback models and the gas fraction of the disk.Our results also imply that the burstiness of star formation and the massloading of outflows may be overestimated if the adopted star particle mass isconsiderably larger than the mass of individual stars because this imposes aminimum cluster size.

Efficient early stellar feedback can suppress galactic outflows by reducing supernova clustering