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We present SPICE, a new suite of RHD cosmological simulations targeting theepoch of reionisation. The goal of these simulations is to systematically probea variety of stellar feedback models, including "bursty" and "smooth" forms ofsupernova energy injection, as well as poorly-explored scenarios such ashypernova explosions and radiation pressure. Subtle differences in thebehaviour of supernova feedback drive profound differences in reionisationhistories, with burstier forms of feedback causing earlier reionisation. Wealso find that some global galaxy properties, such as the dust-attenuatedluminosity functions and star formation main sequence, remain degeneratebetween models. Stellar feedback and its strength determine the morphologicalmix of galaxies emerging by z = 5 and that the reionisation history isinextricably connected to intrinsic properties such as galaxy kinematics andmorphology. While star-forming, massive disks are prevalent if supernovafeedback is "smooth", "bursty" feedback preferentially generatesdispersion-dominated systems. Different modes of feedback produce differentstrengths of outflows, altering the ISM/CGM in different ways, and in turnstrongly affecting the escape of LyC photons. We establish a correlationbetween galaxy morphology and LyC escape fraction, revealing thatdispersion-dominated systems have escape fractions 10-50 times higher thantheir rotation-dominated counterparts at all redshifts. Dispersion-dominatedsystems should thus preferentially generate large HII regions as compared totheir rotation-dominated counterparts. Since dispersion-dominated systems aremore prevalent if stellar feedback is more explosive, reionisation occursearlier in our simulation with burstier feedback. Statistical samples ofpost-reionisation galaxy morphologies probed with JWST, ALMA and MUSE canconstrain stellar feedback and models of cosmic reionisation.

SPICE: the connection between cosmic reionisation and stellar feedback in the first galaxies