Mapping of the properties of PRGs onto the RGB image of the protocluster, as seen in Figure 1. Each galaxy is shown by an unfilled point, where the colour indicates the galaxy property that is studied in each panel. Circular points indicate ‘non-core’ galaxies, while square points indicate core galaxies. Each panel includes a zoom of the most clustered region of the protocluster, for ease of viewing. The following galaxy properties are shown: (top left:) The logarithm of the ratio of the recent (average over the last 10 Myr) to slightly more extended (average over the last 30 Myr) SFRs; (top right:) The logarithm of the neutral hydrogen column densities; (bottom left:) the slope of the UV continuum, β; (bottom right:) The logarithm of the stellar mass. The mapping of these galaxy properties onto the protocluster indicates that the two most clustered regions tend to host the most massive, dusty galaxies that have declining star-formation histories and extreme neutral hydrogen column densities. The more sparsely distributed galaxies tend to be less massive, highly star-forming objects.