Radial variation of the b_X emissivity bias when each clump candidate is included or excluded, compared to the results from the ROSAT sample of 31 galaxy clusters (Eckert et al. 2015). The 24 clump candidates, although being not genuine clumps, cause an increased level of bias above ∼0.8 r₂₀₀ in Abell 1795. When each clump candidate is excluded, the profile flattens at b_X ≥ 1. Note: b_X is subject to projection effects and influenced by the sky background contribution, which exhibit very different levels for the Chandra and ROSAT data sets.