tokens: that halos with M 10 9 M ⊙ were suppressed if located inside an ionized patch of the IGM (Iliev et al. 2007 , 2012 , 2014 ; Ahn et al. 2012 ; Dixon et al. 2016 ). Our ability to distinguish the progress and impact of reionization locally here has enabled us, not only to demonstrate the causal connection between reionization and low-mass halo suppression, but also to show that the time at which local reionization takes place is correlated with local matter overdensity and with the corresponding local variations of the halo mass function. In addition, we found that, with the exception of suppressed low-mass halos, the SFRs and gas-to-dark matter ratios of halos of any given mass are higher in regions that reionized earlier. For the low-mass halos, after their local reionization, when suppression takes place, curves of SFR and per halo vs thereafter decline by following a universal curve which is independent of re . We also found that relatively rare, highly overdense and, consequently, highly developed regions, which were the first to reionize, produced the vast majority of stars during the EOR, while not consuming more ionizing radiation than regions that reionized later. These early-reionizing regions must have exported a surplus of ionizing radiation, therefore, which helped to reionize and/or maintain the reionization of the late-reionizing regions. Future observations of high-redshift galaxies which look for the inhomogeneous distribution of suppressed and gas-poor low-mass dwarf galaxies and partially-suppressed dwarf galaxies of intermediate mass predicted here will be an excellent probe of the EOR. Since the CoDa I simulation used a constrained realization of the initial conditions that represents the Local Universe, we can also apply the results found here to predict relic signatures of suppression in the present-day galaxies of the Local Universe. For example, the neighbourhoods of MW and M31 were found in CoDa I to have reionized at roughly the same redshift, a bit earlier than the global average reionization redshift, a result which was also found by CoDa I-AMR as described in Aubert et al. ( 2018 ). CoDa I-AMR used an improved calibration of subgrid star formation efficiency so as to finish global reionization by = 6.1, making it easier to relate simulation redshifts directly to observations. In Aubert et al. ( 2018 ), the reionization redshift field was based on the redshifts when each cell first reached X ion = 0.5 (rather than X ion = 0.9 as used here). As structure formation changes the comoving positions of mass over time, the time when a mass element first reaches a location that is 50 per cent ionized is defined as its reionization redshift, . The average reionization redshift of the mass elements that constitute MW and M31 at = 0 were found to be for both, while . The spread of reionization times within each galaxy was as large as ∼400 Myrs (max – min), with a 2σ spread of ∼100 − 150 Myrs. Our results here suggest that the
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