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Passive galaxies are ubiquitous in the local universe, and various physicalchannels have been proposed that lead to this passivity. To date, robustpassive galaxy candidates have been detected up to $z \leqslant 5$, but it isstill unknown if they exist at higher redshifts, what their relative abundancesare, and what causes them to stop forming stars. We present predictions fromthe First Light And Reionisation Epoch Simulations (FLARES), a series of zoomsimulations of a range of overdensities using the EAGLE code. Passive galaxiesoccur naturally in the EAGLE model at high redshift, and are in good agreementwith number density estimates from HST and early JWST results at $3 \leqslant z\leqslant 5$. Due to the unique FLARES approach, we extend these predictions tohigher redshifts, finding passive galaxy populations up to $z \sim 8$. Feedbackfrom supermassive black holes is the main driver of passivity, leading toreduced gas fractions and star forming gas reservoirs. We find that passivegalaxies at $z \geqslant 5$ are not identified in the typical UVJ selectionspace due to their still relatively young stellar populations, and present newrest--frame selection regions. We also present NIRCam and MIRI fluxes, and findthat significant numbers of passive galaxies at $z \geqslant 5$ should bedetectable in upcoming wide surveys with JWST. Finally, we present JWST colourdistributions, with new selection regions in the observer--frame foridentifying these early passive populations.

First Light And Reionisation Epoch Simulations (FLARES) VIII. The Emergence of Passive Galaxies at $z \geqslant 5$