Black Hole Mass and Eddington Ratio as Drivers for the Observable Properties of Radio-loud and Radio-quiet QSOs

By Todd Boroson. 2001

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Recent studies of black holes in the nuclei of both active and normal galaxies have yielded relationships that permit a physical interpretation of the principal components of the spectra of QSOs. It is shown that principal component (or eigenvector) 1 (PC1) is driven predominantly by L/LEdd, and principal component 2 (PC2) is driven by accretion rate. This results in a PC2 versus PC1 diagram in which lines of constant black hole mass are diagonal. Using a sample consisting of the low-redshift PG objects supplemented by 75 radio-loud QSOs, it is shown that such a diagram effectively distinguishes radio-loud from radio-quiet objects and demonstrates that both narrow-line Seyfert 1 galaxies and broad absorption line QSOs lie at the high L/LEdd extreme, although these two types of objects are well separated in the PC2 direction. A simple picture that ties together physical parameters (black hole mass and Eddington ratio) and classification of active galactic nuclei is presented. Based on the location of core-dominated and lobe-dominated radio-loud QSOs, orientation can be modeled as a third parameter in this scheme, implying an enhancement in the radio flux of core-dominated objects.

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Properties of flat-spectrum radio-loud Narrow-Line Seyfert 1 Galaxies (2014, background): “Narrow-line Seyfert 1 galaxies (NLS1s) are a well-known class of active galactic nuclei (AGN), but they are usually considered to be radio-quiet (e.g., Ulvestad et al. 1995, Moran 2000, Boroson 2002).”
THE SIMULTANEOUS OPTICAL-TO-X-RAY SPECTRAL ENERGY DISTRIBUTION OF SOFT X-RAY SELECTED ACTIVE GALACTIC NUCLEI OBSERVED BY SWIFT (2010, background): “…Norman, OK 73019; email: leighly@nhn.ou.edu 4Department of Astronomy, University of Leicester, Leicester, U.K. riety of observed AGN properties such as spectral slopes and some emission-line properties (e.g. Boroson & Green 1992; Sulentic et al. 2000; Boroson 2002; Grupe 2004; Shemmer et al. 2008).”
C IV λ1549 as an Eigenvector 1 Parameter for Active Galactic Nuclei (2007, background): “Exploration of possible physical drivers of source occupation /correlation in 4DE1 (Marziani et al. 2001, 2003b; Boroson 2002) suggest that it is primarily driven by the luminosity to black hole mass (MBH) ratio which is proportional to the Eddington ratio (Lbol /LEdd) with Population A sources…”
On the Nature of Seyfert Galaxies with High [O III] λ5007 Blueshifts (2008, background): “NLS1 galaxies are a subclass of AGN with extreme emission-line and continuum prop- erties which appear to be in part driven by their high Eddington ratios, low black hole masses, and other parameters (e.g., Osterbrock & Pogge 1985, Boroson 2002, Grupe 2004; see Komossa 2008 for a review).”
An Optical Spectroscopic Atlas of Low-Redshift Active Galactic Nuclei (2003, background): “This information is gaining new astrophysical significance following development of the eigenvector 1 parameter space (Sulentic et al. 2000a, 2000c; Boroson 2002).”
A Systematic Analysis of Fe II Emission in Quasars: Evidence for Inflow to the Central Black Hole (2008, background): “…is often suggested to be the main physical driver of the spectral diversity in quasars (Sulentic et al. 2000a, 2000b; Marziani et al. 2001, 2003a; Boroson 2002), and MBH is argued to be an important determinant of radioloudness (Laor 2000; Boroson 2002; McLure & Jarvis 2004, but see Ho 2002).”
A New Sample of Low-Mass Black Holes in Active Galaxies (2007, background): “Finally, there is an apparent connection between [OIII ]/Hβ and Eddington ratio (e.g., Boroson 2002).”
FERMI/LARGE AREA TELESCOPE DISCOVERY OF GAMMA-RAY EMISSION FROM A RELATIVISTIC JET IN THE NARROW-LINE QUASAR PMN J0948+0022 (2009, background): “These properties point to very high (near Eddington) accretion rates and relatively low masses (106 − 108M⊙) (Boroson 2002; see, however, Decarli et al. 2008, Marconi et al. 2008).”
The Sloan Digital Sky Survey View of the Palomar-Green Bright Quasar Survey (2005, background): “While it has been difficult to identify the underlying physical drivers behind these eigenvectors, one suggestion is that they might be accretion rate and black hole mass (Boroson 2002).”
Supermassive Black Holes in Galactic Nuclei: Past, Present and Future Research (2004, background): “, several studies have employed the optical relations (e.g. Bian & Zhao 2003; Shields et al. 2003; Netzer 2003; Woo & Urry 2002a&b; Oshlack et al. 2002; Wandel 2002; Boroson 2002; McLure & Dunlop 2001).”
The Karl G. Jansky Very Large Array Sky Survey (VLASS). Science Case and Survey Design (2019, background): “Further insight can be gained from radio demographics as a function of quasar emission line ratios and widths (e.g., Boroson 2002).”
Discovery of extreme [O III] λ5007 Å outflows in high-redshift red quasars (2015, background): “…1 of the quasar population – type 1 active galactic nuclei with strong Fe II, low [O III]/Hβ and relatively strong [O III] blueshifts which are exemplified in the low-redshift universe by the so-called narrow-line Seyfert 1 galaxies (Boroson & Green 1992; Boroson 2002; Zamanov et al. 2002).”
Narrow-line region gas kinematics of 24 264 optically selected AGN: the radio connection (2013, background): “4 There is a known correlation between the equivalent widths of the Fe II complex and λEdd, see Boroson & Green (1992) and Boroson (2002). at D urham U niversity L ibrary on June 19, 2014 http://m nras.oxfordjournals.org/ D ow nloaded from The results of this experiment are shown in Fig.”
Continuum and Emission-Line Properties of Broad Absorption Line Quasars (2003, background): “The differences between BALQSOs and non-BALQSOs (and among BALQSOs themselves) could then be due to luminosity (Corbin 1990), accretion rate (Boroson 2002), inclination (Weymann et al. 1991), some other intrinsic property, or a combination thereof.”
UNIFICATION OF LUMINOUS TYPE 1 QUASARS THROUGH C iv EMISSION (2010, methodology): “This discussion follows from a long history, extending from Boroson & Green (1992) and Boroson (2002) to Sulentic et al. (2007) and beyond.”
Broad-line Balmer decrements in blue active galactic nuclei (2007, background): “Hence for the two populations the central engines or physical processes related to accretion/jet may be different (e.g., Blandford et al. 1990, Boroson 2002, Falcke et al. 1996).”
Radio-loud Narrow-Line Type 1 Quasars (2006, background): “…(e.g., Boroson & Green 1992, Pounds et al. 1995, Wang et al. 1996, Boller et al. 1996, Laor et al. 1997, Czerny et al. 1997, Marziani et al. 2001, Boroson 2002, Simkin & Roychowdhury 2003, Xu et al. 2003, Kawaguchi 2003, Wang & Netzer 2003, Grupe 2004, Grupe & Mathur 2004, Botte et al. 2004,…”