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tokens: (dark matter + baryonic gas, excluding stars). We show the following simulation projects: Technicolor Dawn (Finlator et al. 2018 ), GIMIC (Crain et al. 2009 ), EAGLE (Crain et al. 2015 ; Schaye et al. 2015 ), CROC (Gnedin 2014 ), CoDa (Ocvirk et al. 2016 ), Illustris (Vogelsberger et al. 2014 ), Renaissance (Barrow et al. 2017 ), the Katz et al. ( 2017 ) simulations, SPHINX (Rosdahl et al. 2018 ), and bluetides (Feng et al. 2016 ). We also show FLARES with the total resimulated high-resolution volume, as well as a vertical line showing the representative volume, given by that of the parent box. There is a strong negative correlation for periodic volumes between the volume that can be simulated and the resolution that can be achieved. The resimulation approach, with appropriate weighting, allows us to extend the volume axis significantly. In this paper, we introduce FLARES, zoom resimulations during the EoR using the eagle model. 2 The eagle project (Crain et al. 2009 ; Schaye et al. 2015 ) is a suite of smoothed particle hydrodynamics (SPH) simulations, calibrated to reproduce the stellar mass function and sizes of galaxies in the local Universe. EAGLE has been shown to be in good agreement with a large number of observables not used in the calibration (e.g. Lagos et al. 2015 ; Trayford et al. 2015 , 2017 ; Bahé et al. 2016 ; Crain et al. 2017 ; Furlong et al. 2017 ). This includes predictions at high redshift: Furlong et al. ( 2015 ) found reasonably good agreement with observationally inferred distribution functions of stellar mass and SFR out to z = 7. Unfortunately, there are very few galaxies in the fiducial EAGLE volume during the EoR. This is particularly the case for the most massive objects, which predominantly reside in protocluster environments, the progenitors of today’s collapsed clusters (Chiang et al. 2017 ; Lovell, Thomas Wilkins 2018 ). FLARES allows us to significantly increase the number of galaxies simulated during the EoR with EAGLE. It also allows us to test the already incredibly successful EAGLE model in a new regime of extreme, high- z environments, whilst still resolving hydrodynamic processes at resolution, and provide predictions for a number of key upcoming observatories. In this, the first FLARES paper, we introduce the resimulation method, our suite of zoom simulations, and present our first predictions for the distribution of galaxies by stellar mass and SFR using the composite approach. This is the first in a series of papers studying the galaxy properties in the FLARES sample; in Paper II we forward-model the full spectrophotometric properties, and predict the UV luminosity function and its high redshift evolution (Vijayan et al. 2020 ). In future papers, we plan to study the passive and starbursting galaxy population in FLARES, as well as the evolution of galaxy sizes and environmental bias. We assume a Planck year 1 cosmology (Ω 0 = 0.307, Ω Λ = 0.693, h = 0.6777, Planck Collaboration I 2014 ) and a