Comparison between environmental estimates for luminous giants (large dots) and LoTSS DR1 RGs (small dots) generated by BCGs in the Local Universe. We compare cluster masses M₅₀₀ from Wen & Han (2015) with relative densities 1 + δ from the BORG SDSS, and colour the dots based on their cluster probability p₁ (relative to the average cluster probability ${\overline{p}}_1$ for luminous giants and LoTSS DR1 RGs). For three randomly chosen giants and three randomly chosen RGs, we visualise uncertainties. Generally, as expected, RG-generating BCGs claimed to be in more massive clusters by Wen & Han (2015) have higher BORG SDSS densities and T-web cluster probabilities. The contours indicate fractions of the density expected through M₅₀₀, and show that our relative densities fall short significantly in the cluster regime – by a factor that ranges from less than two to more than an order of magnitude. Densities of low-mass clusters are less biased than densities of high-mass clusters. We used flexible voxel method densities here.