What does CIV<i>λ</i>1549 tell us about the physical driver of the Eigenvector quasar sequence?

Sulentic, J. W.; Olmo, A. del; Marziani, Paola; Martínez-Carballo, M. A.; D’Onofrio, M.; Dultzin, D.; Perea, J.; Martínez-Aldama, Mary Loli; Negrete, C. A.; Stirpe, G. M.; Zamfir, S.

doi:10.1051/0004-6361/201630309

Cited by 74 publications

(131 citation statements)

References 125 publications

(189 reference statements)

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“…The profile can be interpreted as an almost symmetric, unshifted "virialized" emitting region + an outflow/wind component that dominates in A3/A4 spectral types (e.g., [78][79][80][81]) and at high luminosity. The largest shifts of CIVλ1549 centroid at 1/2 along the MS are found in Population A [4,6,14]. The Vestergaard and Peterson [29] scaling laws…”

Section: CIVmentioning

confidence: 95%

“…They provide feedback effects to the host galaxy, and are even invoked to account for the M BH -bulge velocity dispersion correlation [15][16][17]. The ratio between radiation and gravitation forces also influences broad-line region dynamics; lower column density material may flow out of the emitting region [14,18,19]. Black hole masses of high redshift quasars provide constraints on primordial black hole collapse (and references therein [20,21]).…”

Section: Importance Of Black Hole Mass Determinationmentioning

confidence: 99%

“…Our analysis is then focused on virial broadening estimators (VBEs; Section 5) from: (a) LILs (IP < 15 eV: Hβ, MgII 2800); (b) HILs (IP > 40 eV: CIVλ1549); (c) intermediate-ionization lines (IILs: SiIII]λ1892, Al IIIλ1860), for which we provide a brief summary of preliminary results. Reported results from our group were published during the last decade [11][12][13][14]. We finally suggest that "photoioionization" computations of M BH (Section 6) may offer a solution to some of the problems associated with the use of an average scaling law.…”

Section: Introduction: Statement Of the Problemmentioning

confidence: 96%

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Quasar Black Hole Mass Estimates from High-Ionization Lines: Breaking a Taboo?

Marziani

Olmo

Martínez-Aldama

et al. 2017

Atoms

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Abstract:Can high ionization lines such as CIVλ1549 provide useful virial broadening estimators for computing the mass of the supermassive black holes that power the quasar phenomenon? The question has been dismissed by several workers as a rhetorical one because blue-shifted, non-virial emission associated with gas outflows is often prominent in CIVλ1549 line profiles. In this contribution, we first summarize the evidence suggesting that the FWHM of low-ionization lines like Hβ and MgIIλ2800 provide reliable virial broadening estimators over a broad range of luminosity. We confirm that the line widths of CIVλ1549 is not immediately offering a virial broadening estimator equivalent to the width of low-ionization lines. However, capitalizing on the results of Coatman et al. (2016) and Sulentic et al. (2017), we suggest a correction to FWHM CIVλ1549 for Eddington ratio and luminosity effects that, however, remains cumbersome to apply in practice. Intermediate ionization lines (IP ∼ 20-30 eV; AlIIIλ1860 and SiIII]λ1892) may provide a better virial broadening estimator for high redshift quasars, but larger samples are needed to assess their reliability. Ultimately, they may be associated with the broad-line region radius estimated from the photoionization method introduced by Negrete et al. (2013) to obtain black hole mass estimates independent from scaling laws.

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Section: CIVmentioning

confidence: 95%

Section: Importance Of Black Hole Mass Determinationmentioning

confidence: 99%

Section: Introduction: Statement Of the Problemmentioning

confidence: 96%

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Quasar Black Hole Mass Estimates from High-Ionization Lines: Breaking a Taboo?

Marziani

Olmo

Martínez-Aldama

et al. 2017

Atoms

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“…Considerable progress along these line have been made by Sulentic et al (2007a) and Sulentic et al (2017) …”

Section: Futurementioning

confidence: 99%

The Physical Driver of the Optical Eigenvector 1 in Quasar Main Sequence

Panda

Wildy

2017

Front. Astron. Space Sci.

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Quasars are complex sources, characterized by broad band spectra from radio through optical to X-ray band, with numerous emission and absorption features. This complexity leads to rich diagnostics. However, Boroson and Green (1992) used Principal Component Analysis (PCA), and with this analysis they were able to show significant correlations between the measured parameters. The leading component, related to Eigenvector 1 (EV1) was dominated by the anticorrelation between the FeII optical emission and [OIII] line and EV1 alone contained 30% of the total variance. It opened a way in defining a quasar main sequence, in close analogy to the stellar main sequence on the Hertzsprung-Russel (HR) diagram (Sulentic et al., 2001). The question still remains which of the basic theoretically motivated parameters of an active nucleus (Eddington ratio, black hole mass, accretion rate, spin, and viewing angle) is the main driver behind the EV1. Here we limit ourselves to the optical waveband, and concentrate on theoretical modeling the FeII to Hβ ratio, and we test the hypothesis that the physical driver of EV1 is the maximum of the accretion disk temperature, reflected in the shape of the spectral energy distribution (SED). We performed computations of the Hβ and optical FeII for a broad range of SED peak position using CLOUDY photoionisation code. We assumed that both Hβ and FeII emission come from the Broad Line Region represented as a constant density cloud in a plane-parallel geometry. We expected that a hotter disk continuum will lead to more efficient production of FeII but our computations show that the FeII to Hβ ratio actually drops with the rise of the disk temperature. Thus either hypothesis is incorrect, or approximations used in our paper for the description of the line emissivity is inadequate.

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“…Alternative hypotheses about QSO absorption lines see them as the signature of a peculiar stage of QSO evolution (e.g., Green et al, 2001). Sometimes a blue asymmetry in the C IV emission line is observed, and this has been associated with outflows (see, e.g., Sulentic et al 2017).…”

Section: Introductionmentioning

confidence: 99%

C IV Broad Absorption Line Variability in QSO Spectra from SDSS Surveys

Cicco

Brandt

Grier

et al. 2017

Front. Astron. Space Sci.

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Broad absorption lines (BALs) in the spectra of quasi-stellar objects (QSOs) are thought to arise from outflowing winds along our line of sight; winds, in turn, are thought to originate from the accretion disk, in the very surroundings of the central supermassive black hole (SMBH), and they likely affect the accretion process onto the SMBH, as well as galaxy evolution. BALs can exhibit variability on timescales typically ranging from months to years. We analyze such variability and, in particular, BAL disappearance, with the aim of investigating QSO physics and structure. We search for disappearing C IV BALs in the spectra of 1,319 QSOs from different programs from the Sloan Digital Sky Survey (SDSS); the analyzed time span covers 0.28-4.9 year (rest frame), and the source redshifts are in the range 1.68-4.27. This is to date the largest sample ever used for such a study. We find 67 sources (5.1 +0.7 −0.6 % of the sample) with 73 disappearing BALs in total (3.9 +0.5 −0.5 % of the total number of C IV BALs detected; some sources have more than one BAL that disappears). We compare the sample of disappearing BALs to the whole sample of BALs, and investigate the correlation in the variability of multiple troughs in the same spectrum. We also derive estimates of the average lifetime of a BAL trough and of the BAL phase along our line of sight.

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What does CIVλ1549 tell us about the physical driver of the Eigenvector quasar sequence?

Cited by 74 publications

References 125 publications

Quasar Black Hole Mass Estimates from High-Ionization Lines: Breaking a Taboo?

Quasar Black Hole Mass Estimates from High-Ionization Lines: Breaking a Taboo?

The Physical Driver of the Optical Eigenvector 1 in Quasar Main Sequence

C IV Broad Absorption Line Variability in QSO Spectra from SDSS Surveys

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