MBH-σ Relation for a Complete Sample of Soft X-Ray-selected Active Galactic Nuclei

By D. Grupe, S. Mathur. 2003

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We present the black hole mass-bulge velocity dispersion relation for a complete sample of 75 soft X-ray-selected active galactic nuclei (AGNs): 43 broad-line Seyfert 1 galaxies (BLS1s) and 32 narrow-line Seyfert 1 galaxies (NLS1s). We use luminosity and FWHM(Hβ) as surrogates for black hole mass and FWHM([O III]) as a surrogate for the bulge velocity dispersion. We find that NLS1s lie below the MBH-σ relation of BLS1s, confirming the Mathur et al. result. The statistical result is robust and not due to any systematic measurement error. This has important consequences toward our understanding of black hole formation and growth: black holes grow by accretion in well-formed bulges, possibly after a major merger. As they grow, they get closer to the MBH-σ relation for normal galaxies. The accretion is highest in the beginning and dwindles as the time goes by. Our result does not support theories of MBH-σ relation in which the black hole mass is a constant fraction of the bulge mass/velocity dispersion at all times or those in which bulge growth is controlled by AGN feedback.

Subfields: Astronomy and Astrophysics, Global and Planetary Change

View Paper: https://www.semanticscholar.org/paper/5a11310cccd2e308a872f262eee98b64087166c5

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Citations in the corpus

Radio-loud Narrow-Line Type 1 Quasars (2006, methodology): “It has been suggested that NLS1 galaxies are less evolved than Seyferts in that their black holes are still in the process of growing by rapid accretion (e.g., Mathur 2001, Grupe & Mathur 2004, Botte et al. 2004, Mathur & Grupe 2005).”
The Effect of Radiation Pressure on Virial Black Hole Mass Estimates and the Case of Narrow-Line Seyfert 1 Galaxies (2008, background): “It has also been noted that the distance of NLS1 galaxies from theMBHLsph/σe relations is larger for objects with larger Eddington ratios (Grupe & Mathur 2004) suggesting that smaller BHs are growing faster.”
On the Nature of Seyfert Galaxies with High [O III] λ5007 Blueshifts (2008, background): “…on the MBH − σ plane, which was the focus of a number of subsequent studies (Wang & Lu 2001, Wandel 2002, Botte et al. 2004, 2005, Bian et al. 2004, Grupe & Mathur 2004, Barth et al. 2005, Greene & Ho 2005, Mathur & Grupe 2005a,b, Zhou et al. 2006, Ryan et al. 2007, Watson et al. 2007, Komossa…”
PRECISE BLACK HOLE MASSES FROM MEGAMASER DISKS: BLACK HOLE–BULGE RELATIONS AT LOW MASS (2010, methodology): “…AGN contamination, we remove the nuclear luminosity as measured by Ho &Peng (2001) and convert to a V−band magnitude usingB−V = 0.8±0.2 mag (Fukugita et al. 1995) masses, and thus may be growing towards the inactiveMBH −σ∗ relation (e.g., Grupe & Mathur 2004; Ho et al. 2008; Kim et al. 2008).”
Supermassive Black Holes in Active Galactic Nuclei. II. Calibration of the Black Hole Mass-Velocity Dispersion Relationship for Active Galactic Nuclei (2004, background): “Statistically identical distributions in FWHM([O III]) were found for the broad-line and narrow-line Seyfert 1s in an X-ray selected sample of AGNs, which placed the narrow-line Seyfert 1s preferentially below the MBH–σ∗ relation (Grupe & Mathur 2004).”
The Relationship between Luminosity and Broad-Line Region Size in Active Galactic Nuclei (2005, methodology): “…scaling relation is universal to AGNs of all luminosities and redshifts, several recent studies have used the relation to estimate the central masses in large AGN samples using a single-epoch measurement of the luminosity and the linewidth (e.g.,Wang&Lu 2001;Woo&Urry 2002; Grupe & Mathur 2004).”
Cosmic Evolution of Mass Accretion Rate and Metallicity in Active Galactic Nuclei (2006, background): “For example, FWHM([O III ] λ5007) has been suggested as a proxy forσ∗ in type-I AGNs (e.g. Nelson 2000; Shields et al. 2003; Grupe & Mathur 2004; Boroson 2003; Boroson 2005).”
Black Holes in Pseudobulges and Spheroidals: A Change in the Black Hole-Bulge Scaling Relations at Low Mass (2008, background): “…galactic nuclei (AGNs) have anomalously low BHmasses compared to their surrounding galaxies, based on both the line widths of the narrow emission lines (e.g., Bian & Zhao 2004; Grupe & Mathur 2004) and the circular velocity of the host inferred from the integrated H i line width (Ho et al. 2008).”