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The classification "early-type" galaxy includes both elliptically- andlenticular-shaped galaxies. Theoretically, the spheroid-to-disc flux ratio ofan early-type galaxy can assume any positive value, but in practice studiesoften consider only spheroid/disc decompositions in which the disc neatlydominates over the spheroid at large galaxy radii, creating an inner "bulge" asobserved in most spiral galaxies. Here we show that decompositions in which thedisc remains embedded within the spheroid, labelled by some as "unphysical",correctly reproduce both the photometric and kinematic properties of early-typegalaxies with intermediate-scale discs. Intermediate-scale discs have oftenbeen confused with large-scale discs and incorrectly modelled as such; whenthis happens, the spheroid luminosity is considerably underestimated. This hasrecently led to some surprising conclusions, such as the claim that a number ofgalaxies with intermediate-scale discs (Mrk 1216, NGC 1277, NGC 1271, and NGC1332) host a central black hole whose mass is abnormally large compared toexpectations from the (underestimated) spheroid luminosity. We show that whenthese galaxies are correctly modelled, they no longer appear as extremeoutliers in the (black hole mass)-(spheroid mass) diagram. This not onlynullifies the need for invoking different evolutionary scenarios for thesegalaxies but it strengthens the significance of the observed (black holemass)-(spheroid mass) correlation and confirms its importance as a fundamentalingredient for theoretical and semi-analytic models used to describe thecoevolution of spheroids and their central supermassive black holes.

Explaining the reportedly over-massive black holes in early-type galaxies with intermediate-scale discs