Gas mass fraction profile derived from the combined Planck and XMM-Newton pressure profile, assuming for the temperature profile: (H1) the average best fit model across the sample from X-ray spectroscopy (red line and striped area); or (H2) the same but extrapolating beyond R₅₀₀ to a constant value equal to the average temperature measured in the last radial bin across the sample (blue line and striped area). The green dashed curve marks the expected gas fraction profile assuming the A10 pressure profile and kT(r) as in hypothesis (1). The star gives f_gas(r = R₅₀₀) for REXCESS clusters with M₅₀₀ > 5 × 10¹⁴   M_⊙ (Pratt et al. 2009). In maroon we reproduce the gas mass fraction profile derived from Suzaku measurements for the Perseus cluster (Simionescu et al. 2011). The solid and dashed black lines mark the cosmic baryon fraction expected from CMB measurements (Komatsu et al. 2011) and the expected gas fraction, assuming that 12% of baryons are in stars, respectively. The shaded blue and red areas translate the dispersion in the pressure profile across the ESZ–XMM sample as shown on Fig. 4 in our original paper, assuming hypothesis (H1) for kT(r). See Sect. 7.3 in Planck Collaboration (2013)