Comparison of the two cross-correlation estimators in physical units for the stellar mass selected galaxy samples. Differently colored lines represent different samples, identified here by the logarithm of their minimum stellar mass, in solar masses. The color scheme follows that of Fig. 1. The background subtracted surface brightness profiles in the 0.5–2 keV soft band as a function of proper separation (r_p, kpc) is shown in steps (${\mathit{w}}_{DP83}^{\mathit{stack}}\times S_X^R$, Eq. (3)). The cross-correlation between galaxies and X-ray events is shown with dashed lines (${\mathit{w}}_{LS93}^{\mathrm{X}-\mathrm{corr}}\times S_X^R$, Eq. (2)). The brightness of the emission is correlated with the stellar mass threshold. The shape of the profiles changes with the stellar mass threshold. The individual best-fit models for these surface brightness profile are presented in Figs. 8, 9, and 10.