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tokens: shown separately (solid lines) as well as the dark matter at z = 8, 9, and10. The bottom panels show the associated scale-dependent bias, b g (defined as the square root of the ratio of the galaxy over dark matter correlation). The errors bars are delete-1 jack-knife errors with each jack-knife subsample corresponding to a subvolume obtained by removing one of the octants from the full volume of BLUETIDES . The one-halo term dominates at scales r 0.12 Mpc h −1 above which the two-halo term takes over. As expected, the brighter SAMPLE-H16 galaxies are more strongly clustered; furthermore, also note that clustering is steeper for the more luminous SAMPLE-H16 galaxies; therefore, as we go to smaller scales the clustering becomes more and more sensitive to the flux limit, with the one-halo clustering showing a significantly steeper dependence on the limiting magnitude as compared to two-halo clustering. These features have been found in observational studies of clustering dependence on luminosity (Kashikawa et al. 2006 ; Savoy et al. 2011 ; Harikane et al. 2016 ). Figure 5. Spatial clustering of galaxies predicted by BLUETIDES at redshifts 8, 9, and 10 from left to right for galaxy samples of different limiting magnitudes m UV corresponding to Bouwens et al. ( 2015 ) B15 and Harikane et al. ( 2016 ) H16 in red and blue lines, respectively. Top panels: Solid lines represent the one-halo and two-halo contributions of the two-point galaxy correlation function. The coloured dashed lines are the total correlation functions. Thin black dashed lines are the dark matter correlation functions. Bottom panels: Scale-dependent bias at redshifts 8, 9, and 10. The dashed lines are the large-scale linear biases. A significant scale dependence in the galaxy bias is seen at scales 0.5 Mpc h −1 ≲ r ≲ 10 Mpc h −1 (well within the two-halo regime) indicating the presence of non-linear effects at scales larger than the length scales associated with individual host haloes. Evidence of scale dependence in the halo bias has been previously reported using N -body simulations (Reed et al. 2009 ; Jose et al. 2016 ). Jose et al. ( 2016 ) (hereafter J16 ) uses simulations with volumes comparable or larger than BLUETIDES to study non-linear bias at redshifts z ∼ 2–5. J16 reports some universal properties of (redshift independent) in the scale-dependent bias and provides a fitting function. In our upcoming paper (Bhowmick et. al. in preparation), we investigate whether their results agree with the predictions of BLUETIDES by making a precise comparison for a wide range of halo mass bins. We find that our predictions are in fairly good agreement (only slightly lower by an amount ≲ 0.3 dex in general) with J16 , extending the validity of J16 results to regimes well beyond z ∼ 2–5; we have discussed this in more detail in Bhowmick et. al. (in preparation). The foregoing emphasize the importance of measuring clustering directly with simulations as (we shall see next) the