Comparison of our predicted M_BH − M_*, b relation with the data for all galaxies at z ≤ 0.1. The color code corresponds to the logarithm of the fraction of galaxies with different M_BH in a given log M_*, b bin. Panel A: Predicted relation between the BH mass M_BH and the bulge stellar mass M_*, b. The data points are from Kormendy & Ho (2013; black squares and triangles for elliptical galaxies and bulges, respectively), Savorgnan & Graham (2016; red dots), and Ho & Kim (2014; orange filled squares). Panel B: Same as panel A, but including the selection bias discussed in Sect. 3, i.e., considering only model galaxies satisfying the condition in Eq. (12) with θ_crit = 0.1. Panel C: Same as panel A, but considering only model galaxies hosting AGN with bolometric luminosity L_AGN ≥ 10⁴⁴ erg s⁻¹. Bottom right panel: Rms value of the scatter of the distributions shown in panel A (brown histogram), panel B (blue histogram), and panel C (orange histogram) for different bins of M_*, b. The horizontal strip corresponds to the range of measured intrinsic scatter by different authors. The lower value ϵ = 0.28 was obtained by Kormendy & Ho (2013) and the upper value ϵ = 0.4 was obtained by Savorgnan et al. (2016).