Searching for the physical drivers of eigenvector 1: influence of black hole mass and Eddington ratio

Marziani, Paola; Zamanov, R.; Sulentic, J. W.; Calvani, M.

doi:10.1046/j.1365-2966.2003.07033.x

Cited by 133 publications

(277 citation statements)

References 51 publications

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“…Many studies show a tight correlation of source properties with a single parameter (Boroson & Green eigenvector 1, Boroson & Green 1992; see also Marziani et al 2003, and the references therein) most probably representing the Eddington ratio.…”

Section: Discussionmentioning

confidence: 99%

Constraints for the accretion disk evaporation rate in AGN from the existence of the Broad Line Region

Różáńska¹,

Kuraszkiewicz

2004

A&A

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Abstract.We analyze the consequences of the hypothesis that the formation of the Broad Line Region is intrinsically connected to the existence of the cold accretion disk. We assume that the Broad Line Region radius is reliably estimated by the formula of Kaspi et al. (2000, ApJ, 533, 631). We consider three models of the disappearance of the inner disk that limit the existence of the Broad Line Region: (i) the classical ADAF approach, i.e. the inner hot flow develops whenever it can exist; (ii) the disk evaporation model of Meyer & Meyer-Hofmeister (2002, A&A, 392, L5); (iii) the generalized disk evaporation model of Różańska & Czerny (2000b, A&A, 360, 1170. For each of the models, we determine the minimum value of the Eddington ratio and the maximum value of the broad line widths as functions of the viscosity parameter α and the magnetic field parameter β. We compare the predicted parameter space with observations of several AGN. Weak dependence of the maximum value of the FWHM and minimum value of the Eddington ratio on the black hole mass in our sample is noticeable. It seems to favor the description of the cold disk/hot inner flow transition as in the classical ADAF approach rather than with the model of disk evaporation due to conduction between the disk and accreting corona.

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Section: Discussionmentioning

confidence: 99%

Constraints for the accretion disk evaporation rate in AGN from the existence of the Broad Line Region

Różáńska¹,

Kuraszkiewicz

2004

A&A

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“…Bin A3 and A4 sources show a systematic [Oiii]λλ4959,5007 blueshift with respect to low ionization narrow lines. The shift amplitude in these "blue outliers" is also believed to be related to the E1 sequence Marziani et al 2003b;Komossa et al 2008;Hu et al 2008). …”

Section: Generation and Analysis Of Composite Spectramentioning

confidence: 99%

“…A few dozen sources were moved into adjacent bins but none of this fine tuning is likely to have had much effect on resultant median composites. Two bins (A2 and B1) are most densely populated while our binning contains enough sources to permit generation of composites for eight bins that span the FWHM Hβ and R FeII ranges occupied by the majority of low redshift type 1 sources (with an inferred 2 dex range in Edditington ratio, 0.01 < ∼ log L/L Edd < ∼ 1 that is the one of luminous type-1 AGN; Woo & Urry 2002;Marziani et al 2003b;Kollmeier et al 2006;Davis & Laor 2011). Table 1 gives the number of sources (N tot ) in each bin.…”

Section: Sample Selectionmentioning

confidence: 99%

“…Interpreting of quasar spectra in the context of a 4D parameter space stemming from eigenvector studies reveals a wide diversity of line profile properties (Sulentic et al 2000a(Sulentic et al , 2007Marziani et al 2003bMarziani et al , 2010 that are most likely driven by L/L Edd , with M BH and source orientation also playing important roles (Boroson & Green 1992;Marziani et al 2001;Yip et al 2004). The 4DE1 (4D eigenvector 1) formalism owes its Now at Instituto de Astronomía, UNAM, Ensenada Campus, Baja California, México. inception to a principal component analysis study of systematic trends in quasar spectra (Boroson & Green 1992) from the the Palomar-Green (PG) survey.…”

Section: Introductionmentioning

confidence: 99%

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Is MgIIλ2800 a reliable virial broadening estimator for quasars?

Marziani

Sulentic

Plauchu-Frayn

et al. 2013

A&A

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142

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Context. Broad Mgiiλ2800 and Hβ lines have emerged as the most reliable virial estimators of the black hole mass in quasars. Which is more reliable? Part of the challenge centers on comparing Mgiiλ2800 and Hβ line profiles in order to improve the ±1 dex M BH uncertainties inherent in single-epoch FWHM measures from noisy spectra. Aims. We compare Mgiiλ2800 and Hβ profile measures in the same sources and especially FWHM measures that provide the virial broadening estimator. Methods. We identify 680 bright Sloan Digital Sky Survey Data Release 7 quasars with spectra showing both Mgiiλ2800 and Hβ lines at redshift 0.4 ≤ z ≤ 0.75. The S/N of these spectra are high enough to allow binning in the "four-dimensional (4D) eigenvector 1" optical plane and construction of high S/N composite spectra. Results. We confirm that Mgiiλ2800 shows a profile that is ≈20% narrower as suggested in some previous studies. FWHM measures for Population B sources (i.e., with FWHM of Hβ larger than 4000 km s −1 ) are uncertain because they show complex profiles with at least two broad-line components involving a nearly unshifted broad and redshifted very-broad component. Only the broad component is likely to be a valid virial estimator. If Hβ and Mgiiλ2800 are not corrected for the very broad component then black hole mass M BH values for Population B sources will be systematically overestimated by up to Δ logM BH ≈ 0.3−0.4 dex. We suggest a simple correction that can be applied to the majority of sources. Mgiiλ2800 is the safer virial estimator for Population B sources because the centroid shifts with respect to rest frame are lower than for Hβ. In the broad and very broad component profile interpretation, this is a consequence of the lower very broad to broad component intensity ratio for Mgiiλ2800. Eigenvector-based studies show that effective discrimination of black hole mass and Eddington ratio at fixed redshift is not achieved via luminosity binning but rather by binning in a "4D eigenvector 1" context that reflects different broad line region geometry/kinematics probably driven by the Eddington ratio.

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“…The absolute luminosity at 5100 Å is estimated with the following expression (e.g., Marziani et al 2003a):…”

Section: Optical Nuclear Luminosities Of Compact Agnmentioning

confidence: 99%

Radio-optical scrutiny of compact AGN: correlations between properties of pc-scale jets and optical nuclear emission

Arshakian¹,

Torrealba

Chavushyan

et al. 2010

A&A

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Aims. We study the correlations between the VLBA (Very Long Baseline Array) radio emission at 15 GHz, extended emission at 151 MHz, and optical nuclear emission at 5100 Å for a complete sample of 135 compact jets. Methods. We use the partial Kendall's tau correlation analysis to check the link between radio properties of parsec-scale jets and optical nuclear luminosities of host active galactic nuclei (AGN). Results. We find a significant positive correlation for 99 quasars between optical nuclear luminosities and total radio (VLBA) luminosities of unresolved cores at 15 GHz originated at milliarcseconds scales. For 18 BL Lacs, the optical continuum emission correlates with the radio emission of the jet at 15 GHz. We suggest that the radio and optical emission are beamed and originate in the innermost part of the sub-parsec-scale jet in quasars. Analysis of the relation between the apparent speed of the jet and the optical nuclear luminosity at 5100 Å supports the relativistic beaming model for the optical emission generated in the jet, and allows the peak values of the intrinsic optical luminosity of the jet and its Lorentz factor to be estimated for the populations of quasars (2 × 10 20 W Hz −1 and γ = 52), BL Lacs (9 × 10 21 W Hz −1 and γ = 20), and radio galaxies (1.5 × 10 21 W Hz −1 and γ = 9). The radio-loudness of quasars (the ratio of 15 GHz flux density and optical nuclear flux at 5100 Å) is found to increase at high redshifts, which is interpreted as progressively higher Doppler factors in radio regime compared to those in optical. A strong positive correlation is found between the intrinsic kinetic power of the jet (measured from the flux density at 151 MHz) and the apparent luminosities of the total and the unresolved core emission of the jet at 15 GHz. This correlation is interpreted in terms of an intrinsically more luminous parsec-scale jet producing more luminous extended structure, which is detectable at low radio frequencies, 151 MHz. A possibility that the low frequency radio emission is relativistically beamed in superluminal sources and therefore correlates with radio luminosity of the jet at 15 GHz cannot be ruled out. Monitoring of superluminal AGN in a wide range of frequencies is required to check the contribution of each effect.

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Searching for the physical drivers of eigenvector 1: influence of black hole mass and Eddington ratio

Cited by 133 publications

References 51 publications

Constraints for the accretion disk evaporation rate in AGN from the existence of the Broad Line Region

Constraints for the accretion disk evaporation rate in AGN from the existence of the Broad Line Region

Is MgIIλ2800 a reliable virial broadening estimator for quasars?

Radio-optical scrutiny of compact AGN: correlations between properties of pc-scale jets and optical nuclear emission

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