Clustering measurements from our defined GAMA galaxy samples (open circles) overlaid with corresponding measurements from individual, ∼180 deg² MICE subvolumes (dotted lines). Filled triangles show the means of the MICE clustering signals. We see significant differences between MICE and GAMA, particularly at low redshift and large scales, and so choose not to estimate covariances directly from MICE – see Appendix A.2 for details.