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• W1990201068 abstract "We use the innermost kinematics of spirals to investigate whether these galaxies could host the massive black hole remnants that once powered the quasi-stellar object (QSO) phenomenon. Hundreds of rotation curves of early- and late-type spirals are used to place upper limits on the central black hole (BH) masses. We find that (i) in late-type spirals, the central massive dark objects (MDOs) are about 10–100 times smaller than the MDOs detected in ellipticals, and (ii) in early-type spirals, the central bodies are likely to be in the same mass range as the elliptical MDOs. As a consequence, the contribution to the QSO/active galactic nuclei (AGN) phenomenon by the BH remnants eventually hosted in spirals is negligible: ρ BH(Sb—Im)<6×104 M⊙ Mpc−3. We find several hints that the MDO mass versus bulge mass relationship is significantly steeper in spirals than in ellipticals, although the very issue of the existence of such a relation for late Hubble type objects remains open. The upper limits on the masses of the BHs resident in late-type spirals are stringent: MBH ⩽ 106−107 M⊙, indicating that only low-luminosity activity could possibly have occurred in these objects." @default.
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• W1990201068 date "2000-09-01" @default.
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• W1990201068 title "The masses of black holes in the nuclei of spirals" @default.
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• W1990201068 doi "https://doi.org/10.1046/j.1365-8711.2000.03622.x" @default.
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