The M(BH)-Sigma Relation for Supermassive Black Holes

Abstract

We investigate the differences in the M(BH)-sigma relation derived recently by Ferrarese & Merritt (2000) and Gebhardt et al. (2000). The shallower slope found by the latter authors (3.75 vs. 4.8) is due partly to the use of a regression algorithm that ignores measurement errors, and partly to the value of the velocity dispersion adopted for a single galaxy, the Milky Way. A steeper relation is shown to provide a better fit to black hole masses derived from reverberation mapping studies. Combining the stellar dynamical, gas dynamical, and reverberation mapping mass estimates, we derive a best-fit relation M(BH) = 1.30 (+/- 0.36) X 10^8 (sigma_c/200)^{4.72(+/- 0.36)}, where M(BH) is in solar masses, and sigma in km/s.

The Astrophysical Journal, in press

References in corpus (4)

• A Fundamental Relation Between Supermassive Black Holes and Their Host Galaxies
• A Relationship Between Nuclear Black Hole Mass and Galaxy Velocity Dispersion
• Black Hole Mass Estimates from Reverberation Mapping and from Spatially Resolved Kinematics
• Stellar Dynamics in the Galactic centre: Proper Motions and Anisotropy

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• Radio continuum observations of the candidate supermassive black hole in the dwarf elliptical VCC128
• Investigating the residuals in the $M_{\bullet }-M_{\ast }$ relation using the SIMBA cosmological simulation
• HI 21 cm Extended Structures to the North-East, and South-West of NGC 5595: VLA Observations of the Disk Galaxy Pair NGC 5595 and NGC 5597
• The $M_{\bullet }-\sigma$ relation in spherical systems
• The Future of Direct Supermassive Black Hole Mass Estimates
• Optical and near-infrared observations of hard serendipitous Chandra sources
• Black Hole-Galaxy Correlations in Cluster Zoomed-in Simulations: GIZMO-SIMBA and TNG-Cluster