2005/03/03 by E. W. Bonning, G. A. Shields, S. Salviander +1 · 3 citations
Physics and Astronomy · #Active galactic nucleus #Astronomy #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Astrophysics #Black hole (networking) #Bulge #Galaxies: Formation, Evolution, Phenomena #Galaxy #Luminosity #Physics #QSOS #Quasar #Redshift #Star formation #Stellar mass #astro-ph
paper · pdf · doi:10.1086/429882
published as Astrophys.J. 626 (2005) 89-94 · ApJ, in press. 20 pages, 5 figures
arxiv created 2005/03/03 · openalex publication_date 2005/06/02 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Galaxy bulge luminosity L , black hole mass M BH , and stellar velocity dispersion σ * increase together in a way suggesting a close evolutionary relationship. Measurements of the M BH -σ * relationship as a function of cosmic time may shed light on the origin of this relationship. Direct measurements of σ * at high redshift are difficult, and the width of the narrow emission lines of active galactic nuclei (AGN) has been proposed as a surrogate for σ * . We investigate the utility of using σ for σ * by examining host galaxy magnitudes and [O III] line widths for low-redshift QSOs. For radio-quiet QSOs, σ is consistent in the mean with the value of σ * predicted by the Faber-Jackson relation. For our limited range of L host , scatter obscures the expected increase of σ with L host . However, for a sample of AGN covering a wide range of measured or inferred σ * , there is a clear increase of σ with σ * . Radio-loud QSOs on average have σ smaller by 0.1 dex than radio-quiet QSOs of similar L host , at least for luminosities typical of PG QSOs. Star formation rates in our low-redshift QSOs are smaller than required in order to maintain the typical observed ratio of bulge mass to black hole mass.