tokens: runs with observational data. The Ly α LFs are obtained by convolving the L Ly α – M h relation measured in the simulations with the theoretical haloe mass function (MF) from Sheth Tormen ( 2002 ). The shaded region indicates the 1σ uncertainty due to the average scatter in the L Ly α – M h relation. The data points show recent estimates of the Ly α LF at = 6.6 from Ouchi et al. ( 2010 ), Matthee et al. ( 2015 ), and Konno et al. ( 2018 ). The Ly α LFs in the CW and VW models reproduce well the shape of the best Schechter fit, both the faint-end slope and the exponential cutoff at the bright-end, while the LF in the NW model appears to be steeper than the Schechter fit. This means that our radiative transfer calculations were able to properly capture the correct scaling between L Ly α and M h in the CW and VW models. However, the LFs in the VW and NW models deviate from the observed one over the entire luminosity range of the data. We speculate that this may be because we do not account for dust in our radiative transfer calculations. While we argue in Appendix A that dust is probably not important for the Ly α line transfer through the IGM in our simulations, it is likely to be an important factor in reducing the escape fraction, , of Lyα photons out of galaxies, especially massive ones. This is also supported by the fact that galaxies in the CW model are the most efficient at ejecting metals from their ISM into their surrounding IGM (as discussed in S16 ), which means that these galaxies should be the least affected by our omission of the dust. This simple explanation is consistent with the fact that the LF in the CW model has the closest match with the observed LF. A quick way to assess the effect of dust on ISM scales in our radiative transfer calculations is by estimating the value of the Ly α escape fraction, , required to match the Lyα LFs of our models with the observed one. For simplicity, here we assume that is independent of haloe mass. Comparing the Ly α LFs obtained in our models with the observed LF shown in Fig. 8 , we find that , and 0.39 for the CW, VW, and NW models, respectively. These values are broadly consistent with the ones measured in detailed Ly α radiative transfer calculations on sub-ISM scales with dust (see e.g. the recent study by Smith et al. 2019 ). 4.2 Comparison with an observed galaxy overdensity at <inline-formula><tex-math id="TM0145" notation="LaTeX"></tex-math></inline-formula> = 7 Recent deep spectroscopic follow-up observations of colour-selected galaxies in the Bremer Deep Field (BDF) have revealed LAEs associated with a galaxy overdensity at ∼ 7 (Castellano et al. 2016 , 2018 , hereafter C18 ). These observations are ideal to compare the results of our CR simulations with real data. The galaxy sample presented in C18 corresponds to 16 colour-selected galaxy candidates previously observed with HST and believed to be associated with a galaxy overdensity at ∼ 7. Out of these 16 objects, only 3 of
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