2001/01/23 by Ari Laor · 2 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Galaxies: Formation, Evolution, Phenomena #astro-ph
paper · pdf · doi:10.1086/320989
Accepted for publication in ApJ, 9 pages inc. 2 figures
arxiv created 2001/01/23 · openalex publication_date 2001/06/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/01
Analysis of (Palomar-Green) PG quasar observations suggests a nonlinear relation between the black hole mass, M BH , and the bulge mass, M bulge , although a linear relation, as proposed for nearby galaxies, cannot be ruled out. New M BH values for nearby galaxies from K. Gebhardt et al., and L bulge measurements for Seyfert 1 galaxies from S. N. Virani et al., are used here to obtain a more accurate value for the slope of the M BH - M bulge relation. The combined sample of 40 active and nonactive galaxies suggests a significantly nonlinear relation, M BH ∝ M . Further support for a nonlinear relation is provided by the slope of the M BH -stellar velocity dispersion relation found recently, and by the low M BH found in late-type spiral galaxies. The mean M BH / M bulge ratio is therefore not a universal constant, but rather drops from ~0.5% in bright ( M V ~ -22) ellipticals to ~0.05% in low-luminosity ( M V ~ -18) bulges. Hubble Space Telescope determinations of M BH in late-type spirals, and of the bulge magnitude in narrow-line Seyfert 1 galaxies (both predicted to have low M BH ), can further test the validity of the nonlinear M BH - M bulge relation.