Extending the Calibration of C iv-based Single-epoch Black Hole Mass Estimators for Active Galactic Nuclei*

Park, Daeseong; Barth, Aaron J.; Woo, Jong-Hak; Malkan, M. A.; Treu, Tommaso; Bennert, Vardha N.; Assef, Roberto J.; Pancoast, Anna

doi:10.3847/1538-4357/aa6a53

Cited by 47 publications

(74 citation statements)

References 98 publications

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“…In contrast, HILs are commonly blueshifted with respect to the systematic redshift and show significant asymmetry. Shape corrections are required to recover black hole masses consistent with those found with LILs (Collin et al 2006;Shen & Liu 2012;Denney 2012;Park et al 2013;Runnoe et al 2013;Yong et al 2016;Coatman et al 2017;Park et al 2017). This may suggest another velocity component is playing a significant role in the motion of the HIL emitting gas.…”

Section: Proposed Blr Disk-wind Modelmentioning

confidence: 90%

Using the Properties of Broad Absorption Line Quasars to Illuminate Quasar Structure

Yong

King

Webster

et al. 2018

Monthly Notices of the Royal Astronomical Society

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A key to understanding quasar unification paradigms is the emission properties of broad absorption line quasars (BALQs). The fact that only a small fraction of quasar spectra exhibit deep absorption troughs blueward of the broad permitted emission lines provides a crucial clue to the structure of quasar emitting regions. To learn whether it is possible to discriminate between the BALQ and non-BALQ populations given the observed spectral properties of a quasar, we employ two approaches: one based on statistical methods and the other supervised machine learning classification, applied to quasar samples from the Sloan Digital Sky Survey. The features explored include continuum and emission line properties, in particular the absolute magnitude, redshift, spectral index, line width, asymmetry, strength, and relative velocity offsets of high-ionisation C iv λ1549 and low-ionisation Mg ii λ2798 lines.We consider a complete population of quasars, and assume that the statistical distributions of properties represent all angles where the quasar is viewed without obscuration. The distributions of the BALQ and non-BALQ sample properties show few significant differences. None of the observed continuum and emission line features are capable of differentiating between the two samples. Most published narrow disk-wind models are inconsistent with these observations, and an alternative disk-wind model is proposed. The key feature of the proposed model is a disk-wind filling a wide opening angle with multiple radial streams of dense clumps.

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Section: Proposed Blr Disk-wind Modelmentioning

confidence: 90%

Using the Properties of Broad Absorption Line Quasars to Illuminate Quasar Structure

Yong

King

Webster

et al. 2018

Monthly Notices of the Royal Astronomical Society

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“…On correcting the C IV-based BH mass estimates, previous studies have presented other methods based on the parameters relatively independent of the redshift estimates, such as reducing the dependence of the BH masses on the emissionline width (Shen & Liu 2012;Park et al 2013Park et al , 2017, the continuum-subtracted peak flux ratio of the ultraviolet emission-line blend of Si IV+O IV relative to C IV (Runnoe et al 2013), and the C IV shape (Denney 2012).…”

Section: Comparison With Previous Workmentioning

confidence: 99%

“…At redshift larger than 2, both the Hβ line and the Mg II line have moved out of the optical observing window. Such SE estimates have been extrapolated to the C IV λ1549 emission line in the rest-frame ultraviolet wavelength (McLure & Jarvis 2002;Vestergaard 2002;Vestergaard & Peterson 2006;Vestergaard & Osmer 2009;Denney 2012;Park et al 2013Park et al , 2017Coatman et al 2016Coatman et al , 2017Sulentic et al 2017;Marziani et al 2019).…”

Section: Introductionmentioning

confidence: 99%

“…They concluded that the line width of Mg II correlates well with that of Hβ from the SE spectroscopy, while the C IV line width is poorly correlated with the Mg II or Hβ line widths. Some other studies suggested that poor correlations between different line widths play more important roles than the continuum luminosities in the differences of virial BH mass estimates (Shen et al 2008;Denney 2012;Trakhtenbrot & Netzer 2012;Park et al 2013Park et al , 2017Runnoe et al 2013;Coatman et al 2017;Sulentic et al 2017;Mejía-Restrepo et al 2018;Marziani et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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C iv Emission-line Properties and Uncertainties in Black Hole Mass Estimates of z ∼ 3.5 Quasars

Zuo

Fan

et al. 2020

ApJ

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Using a high-luminosity (L bol ∼10 47.5-10 48.3 erg s −1), high-redshift (3.2<z<3.8) quasar sample of 19 quasars with optical and near-infrared spectroscopy, we investigate the reliability of the C IV-based black hole mass estimates (M BH). The median logarithm of the C IV-and Hβ-based M BH ratios is 0.110 dex, with a scatter of 0.647 dex. The C IV-to-Hβ BH mass differences are significantly correlated with the C IV FWHMs, blueshifts, and asymmetries. Corrections of the C IV FWHM using the blueshift and asymmetry reduce the scatter of the mass differences by ∼0.04-0.2 dex. Quasars in our sample accrete at the Eddington ratio R EDD >0.3 and cover a considerable range of blueshifts, with 18/19 of the quasars showing C IV blueshifts (with the median value of 1126 km s −1) and 14/19 of the quasars showing C IV blueshifts larger than 500 km s −1. It suggests that not all quasars with high Eddington ratios show large blueshifts. The Baldwin effect between the C IV rest-frame equivalent width (REW) and the continuum luminosity at 1350 Å is not seen, likely due to the limited luminosity range of our sample. We find a lack of flux in the red wing of the composite spectrum with larger C IV blueshift and detect a higher ratio of [O III] quasars with REW [O III] >5 Å in the subsample with lower C IV blueshift. It is more likely that they are caused by the combination of the Eddington ratio and the orientation effect.

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“…Fe Kα 6.4 keV X-ray Matt and Perola 1992;Campana and Stella 1995;Dovčiak et al 2004;Zoghbi et al 2012;Taylor and Reynolds 2018 Lyα 121.5 nm UV Ulrich et al 1993;Reichert et al 1994;O'Brien et al 1998;De Rosa et al 2015;Goad et al 2016;Lira et al 2018 C IV 155 nm UV Koratkar and Gaskell 1991;Vestergaard and Peterson 2006;Assef et al 2011;Mejía-Restrepo et al 2016Park et al 2017;Sun et al 2018;Hoormann et al 2019;Ge et al 2019 CIII] 190.9 nm UV Kong et al 2006;Trevese et al 2014;Mejía-Restrepo et al 2016;Lira et al 2018 Onken et al 2004;Graham et al 2011;Park et al 2012;Grier et al 2013;Bentz and Katz 2015;Grier et al 2017;Jiang et al 2016;Shapovalova et al 2008Shapovalova et al , 2010Shapovalova et al , 2017Du et al 2018;Huang et al 2019 Paα, β Brα, β 1282-4051 nm infrared Kim et al 2010Kim et al , 2015Landt et al 2013;Onori et al 2017;Ricci et al 2017 Figure 1. Scheme of the emitting gas motion in the SMBH vicinity (below) and expected broad line profile (up) with contributions of different emitting clouds (with...…”

Section: Spectral Rangementioning

confidence: 99%

Broad spectral lines in AGNs and supermassive black hole mass measurements

Popović

2020

Open Astronomy

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The mass measurement of supermassive black holes (SMBHs) is a very complex task. Between several methods for SMBH mass measurements, some of them use the spectral lines, which indicate the motion of the emitting/absorbing material around an SMBH. Mostly, there is an assumption of virialization of line emitting gas in the region which is close to the central SMBH. In this paper we will give an overview of methods for the SMBH mass measurements using broad emission spectral lines observed in Type 1 AGNs. First we give the basic idea to use the parameters of broad lines to SMBH mass measurements. After that we give an overview of broad lines from X-ray (Fe kα) to the IR (Pashen and Brecket lines) which have been used for SMBH mass estimates. Additionally, we describe and discuss a new method for SMBH mass measurements using the polarization in the broad lines emitted from Type 1 AGNs.

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Extending the Calibration of C iv-based Single-epoch Black Hole Mass Estimators for Active Galactic Nuclei*

Cited by 47 publications

References 98 publications

Using the Properties of Broad Absorption Line Quasars to Illuminate Quasar Structure

Using the Properties of Broad Absorption Line Quasars to Illuminate Quasar Structure

C iv Emission-line Properties and Uncertainties in Black Hole Mass Estimates of z ∼ 3.5 Quasars

Broad spectral lines in AGNs and supermassive black hole mass measurements

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