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: rho(BH)(Sb-Im) < 6 x 10(4) 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: M-BH less than or equal to 10(6)-10(7) M., indicating that only low-luminosity activity could possibly have occurred in these objects.
|Titolo:||The masses of black holes in the nuclei of spirals|
|Autori:||Salucci P; Ratnam C; Monaco P; Danese L|
|Data di pubblicazione:||2000|
|Digital Object Identifier (DOI):||10.1046/j.1365-8711.2000.03622.x|
|Appare nelle tipologie:||1.1 Journal article|