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tokens: photometric redshifts, we can constrain cosmology, in particular measure σ 8 at high redshifts. Since the galaxy power spectrum constrains σ 8 × b gal in the linear regime, we need to add at least another measurement. The possibilities include: galaxy overdensity–weak lensing correlations; constrain the bias itself using counts-in-cells distributions (Szapudi Pan 2004 ; Repp Szapudi 2019 ), and then fit σ 8 ; compute higher order statistics, going to three-point correlations instead of using two-point correlations only (e.g. Pan Szapudi 2005 ). In summary, we found that within the context of Planck concordance cosmology, a linear bias model adequately explains the clustering of galaxies at z ≃ 3–6.5. With 10 times more data in the near future and better redshift calibration, the H20 survey will produce high-redshift constraints on cosmological parameters and galaxy formation. APPENDIX A: AN ANALYSIS OF MAGNIFICATION BIAS The galaxy overdensity that is observed in magnitude-limited galaxy samples can be modulated by an effect known as magnification bias. Foreground matter density can enhance (or diminish) observed source counts via weak gravitational lensing, by pushing sources above (or below) the detection limit. Here, we provide an analysis of how magnification bias affects our results. First, we give a short summary of how the modelling described in Section 3 changes due to the inclusion of magnification bias. The formulae are based on the works of Hui, Gaztañaga Loverde ( 2007 ), Loverde et al. ( 2008 ), Ziour Hui ( 2008 ), and Joachimi Bridle ( 2010 ), refer to these for more theoretical details. Instead of measuring the galaxy overdensity directly, the overdensity we observe can be written as where O denotes observed, and μ denotes the magnification contribution. Accordingly, the empirical spherical autocorrelation power spectrum of this observed overdensity becomes , and the theoretical model for it is The g μ and μμ terms can be computed through the analogues of equation ( 6 ), and where we introduced the kernel function for lensing magnification Above, H 0 is the Hubble constant at present time, Ω m denotes the cosmological mass density parameter, c is the speed of light, is the slope of the galaxy number count function at the limiting magnitude m 0 , and finally is the lensing weight function. Again, we adopt the Limber approximation (Limber 1953 ) to speed up the computation, yielding and Examining the components of in equation ( A2 ), it is clear that scales with (see equation 9 ), scales with b gal , and does not depend on the galaxy bias. We evaluated the theoretical expressions via sphericosmo , and performed the linear galaxy bias fit on the dropout samples using our fiducial EAZY-new-sm Π ( z ) distribution. The results are b gal, g = 3.89 ± 0.29, b gal, r = 8.44 ± 0.55, and b gal, i = 11.93 ± 2.00 (statistical error only) for the three dropout galaxy samples. These values are indistinguishable from the original EAZY-new-sm