Super-Massive Black Holes and Dark Halos

Abstract

The relations between masses of Super-Massive Black Holes, Mbh, in galactic nuclei, maximal rotational velocities, Vm, and indicative masses, Mi, of galaxies are studied for galaxies with the available rotation curves. Mbh correlates with both Vm and Mi, although much weaker than with the central velocity dispersion S0. Masses Mbh for early-type galaxies (S0-Sab), which usually possess more luminous bulges, are, on average, larger than those for late-type galaxies with similar velocities of rotation. It enables to conclude that masses of black holes are determined mainly by the bulge properties, and - much weaker - by dark haloes of galaxies.

ARep, in press

References in corpus (5)

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Cited by in corpus (9)

• Revisiting the Scaling Relations of Black Hole Masses and Host Galaxy Properties
• On the Correlations between Galaxy Properties and Supermassive Black Hole Mass
• Galaxy bulges and their massive black holes: a review
• Bulge and Halo Kinematics Across the Hubble Sequence
• Stars and Black Holes from the very Early Universe
• A Consistent Set of Empirical Scaling Relations for Spiral Galaxies: The $(v_{\max },M_{\mathrm{DM}})$-$({\sigma }_0,M_{\mathrm{BH}},\varphi )$ Relations
• The Blackhole-Dark Matter Halo Connection
• Supermassive Black Holes and Nuclear Star Clusters: Connection with the Host Galaxy Kinematics and Color
• Dark halo microphysics and massive black hole scaling relations in galaxies