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Using results from structural analysis of a sample of nearly 1000 local galaxies from the Sloan Digital Sky Survey, we estimate how the mass in central black holes is distributed amongst elliptical galaxies, classical bulges and pseudo‐bulges, and investigate the relation between their stellar masses and central stellar velocity dispersion σ. Assuming a single relation between elliptical galaxy/bulge mass,  M  Bulge , and central black hole mass,  M  BH , we find that  55 +8  −4   per cent of the mass in black holes in the local universe is in the centres of elliptical galaxies,  41 +4  −2   per cent in classical bulges and  4 +0.9  −0.4   per cent in pseudo‐bulges. We find that ellipticals, classical bulges and pseudo‐bulges follow different relations between their stellar masses and σ, and the most significant offset occurs for pseudo‐bulges in barred galaxies. This structural dissimilarity leads to discrepant black hole masses if single   M  BH – M  Bulge   and   M  BH –σ  relations are used. Adopting relations from the literature, we find that the   M  BH –σ  relation yields an estimate of the total mass density in black holes that is roughly 55 per cent larger than if the   M  BH – M  Bulge   relation is used.

The growth of supermassive black holes in pseudo‐bulges, classical bulges and elliptical galaxies