Searching for the Physical Drivers of the Eigenvector 1 Correlation Space

Marziani, Paola; Sulentic, J. W.; Zwitter, T.; Dultzin‐Hacyan, D.; Calvani, M.

doi:10.1086/322286

Cited by 178 publications

(291 citation statements)

References 32 publications

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“…Our work in the 4DE1 context suggests that L/L Edd is the principal driver (Marziani et al 2001). A comparison of this kind requires that populations A and B are separated because quasar spectra are not the same and spectral differences at any fixed redshift are maximized using the population A and B distinction, which is driven by L/L Edd .…”

Section: Comparing Population a And B Uv Spectra At High And Low Redsmentioning

confidence: 91%

“…There is a growing consensus that the leading parameter that governs quasar diversity involves the Eddington ratio (e.g., Marziani et al 2001;Baskin & Laor 2004;Dong et al 2009;Brightman et al 2013). Other factors most likely play important roles and have been discussed in recent reviews (e.g., Marziani et al 2006;Marziani & Sulentic 2014a).…”

Section: Introductionmentioning

confidence: 99%

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GTC spectra ofz≈ 2.3 quasars: comparison with local luminosity analogs

Sulentic¹,

Marziani²,

Olmo³

et al. 2014

A&A

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Context. The advent of 8−10 m class telescopes for the first time makes it possible to compare in detail quasars with similar luminosity and very different redshifts. Aims. We conducted a search for z-dependent gradients in line-emission diagnostics and derived physical properties by comparing, in a narrow bolometric luminosity range (log L ∼ 46.1± 0.4 [erg s −1 ]), some of the most luminous local z < 0.6 quasars with some of the lowest luminosity sources yet found at redshift z = 2.1−2.5. Methods. Moderate signal-to-noise ratio spectra for 22 high-redshift sources were obtained with the 10.4 m Gran Telescopio Canarias (GTC), for which the HST (largely the Faint Object Spectrograph) archive provides a low-redshift control sample. We compared the spectra in the context of the 4D Eigenvector 1 formalism, meaning that we divided both source samples into highly accreting population A and population B sources accreting at a lower rate. Results. Civλ1549, the strongest and most reliable diagnostic line, shows very similar properties at both redshifts, which confirms the Civλ1549 profile differences at high redshift between populations A and B, which are well established in local quasars. The Civλ1549 blueshift that appears quasi-ubiquitous in higher L sources is found in only half (population A) of the quasars observed in the two samples. A Civλ1549 evolutionary Baldwin effect is certainly disfavored. We find evidence for lower metallicity in the GTC sample that may point toward a gradient with z. No evidence for a gradient in M BH or L/L Edd is found. Conclusions. Spectroscopic differences established at low z are also present in much higher redshift quasars. Our results on the Civλ1549 blueshift suggest that it depends both on source luminosity and L/L Edd . Given that our samples involve sources with very similar luminosity, the evidence for a systematic metallicity decrease, if real, points toward an evolutionary effect. Our samples are not large enough to effectively constrain possible changes of M BH or L/L Edd with redshift. The two samples appear representative of a slowly evolving quasar population that is most likely present at all redshifts.

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Section: Comparing Population a And B Uv Spectra At High And Low Redsmentioning

confidence: 91%

Section: Introductionmentioning

confidence: 99%

GTC spectra ofz≈ 2.3 quasars: comparison with local luminosity analogs

Sulentic¹,

Marziani²,

Olmo³

et al. 2014

A&A

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“…The B2 composite is mainly due to spectra of sources whose location in the 4DE1 optical plane is close to the boundary of A2 and B1. In other words, it could be that B2 sources are a physically diverse mixture (Marziani et al 2001). More than anything else, B2 provides a hints of the confusing results that one would obtain by mixing B1 and A2 spectra.…”

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%

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 E1 plane: the data point distribution for low-z quasars in the plane FWHM(Hβ) vs. R Feii is essentially a sequence of Eddington ratio, with orientation acting as the major source of scatter for a narrow black hole mass range (Marziani et al 2001). Classical BAL QSOs tend to occupy the region of higher inclination (∼45 • ).…”

Section: Resultsmentioning

confidence: 99%

BAL QSOs in the eigenvector 1 context: toward a self-consistent model of the line absorbing/emitting regions

Dultzin‐Hacyan¹,

Marziani²,

Sulentic³

et al. 2005

Proc. IAU

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Abstract. We attempt to define the structural properties of Broad Absorption Line (BAL) QSOs and their relationship with the general quasar population using the Eigenvector 1 correlations. We identify 8 low-redshift quasars (z < 0.5, 6 with a BALnicity index > 0 km s −1 ) where it was possible to combine optical and UV spectroscopic observations. The special utility of low-z quasars involves our ability to discuss Civλ1549 BAL QSOs in the context of the Eigenvector 1 optical parameter space and to have a reliable measure of the quasar rest frame. We find that the majority of the BAL sources are population A sources as defined in Sulentic et al. (2000). At least 2 sources that are hosted by ultra-luminous IR galaxies show intriguing effects in their nuclear spectra. A possible correlation between the terminal velocity and luminosity L also suggests that the luminosity to black hole mass ratio (L/M ) is a governing factor with the largest terminal velocity BALs showing the highest L/M values. The Civλ1549 emission line profiles of classical BALs show the ubiquitous E1 population A blue-shift that supports a disk+wind scenario with an opening angle of < 45 • . Observation of "secondary" BAL features roughly in correspondence with the mean radial velocity of the Civλ1549 emission motivates us to model the BAL systems with an additional component that may share the BLR outflow and may be co-axial with the accretion disk, perhaps associated to a significant black hole spin.

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Searching for the Physical Drivers of the Eigenvector 1 Correlation Space

Cited by 178 publications

References 32 publications

GTC spectra ofz≈ 2.3 quasars: comparison with local luminosity analogs

GTC spectra ofz≈ 2.3 quasars: comparison with local luminosity analogs

Is MgIIλ2800 a reliable virial broadening estimator for quasars?

BAL QSOs in the eigenvector 1 context: toward a self-consistent model of the line absorbing/emitting regions

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