Quasar emission lines as probes of orientation: implications for disc wind geometries and unification

Matthews, James H.; Knigge, Christian; Long, Knox S.

doi:10.1093/mnras/stx231

Cited by 15 publications

(12 citation statements)

References 135 publications

(188 reference statements)

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“…11 are extremely similar across the whole wavelength range. The composite spectra themselves are also very similar, apart from the presence of troughs in the BAL spectra, in agreement with Weymann et al (1991) and Matthews et al (2017). There are, however, subtle differences in some of the emission lines at certain areas in C iv-emission space which can only be seen when dividing the BAL spectra (reconstructions) by the non-BAL spectra (reconstructions) as shown in the bottom panel.…”

Section: IV and Other Uv Emission Linessupporting

confidence: 63%

BAL and non-BAL quasars: continuum, emission, and absorption properties establish a common parent sample

Rankine

Hewett

Banerji

et al. 2020

Monthly Notices of the Royal Astronomical Society

123

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Using a sample of 144 000 quasars from the Sloan Digital Sky Survey data release 14 we investigate the outflow properties, evident both in absorption and emission, of high-ionization Broad Absorption Line (BAL) and non-BAL quasars with redshifts 1.6 z ≤ 3.5 and luminosities 45.3 < log 10 (L bol ) < 48.2 erg s −1 . Key to the investigation is a continuum and emission-line reconstruction scheme, based on meanfield independent component analysis, that allows the kinematic properties of the C ivλ1550 emission line to be compared directly for both non-BAL and BAL quasars. C iv-emission blueshift and equivalent-width (EW) measurements are thus available for both populations. Comparisons of the emission-line and BAL-trough properties reveal strong systematic correlations between the emission and absorption properties. The dependence of quantitative outflow indicators on physical properties such as quasar luminosity and luminosity relative to Eddington-luminosity are also shown to be essentially identical for the BAL and non-BAL populations. There is an absence of BALs in quasars with the hardest spectral energy distributions (SEDs), revealed by the presence of strong He iiλ1640 emission, large C ivλ1550-emission EW and no measurable blueshift. In the remainder of the C iv-emission blueshift versus EW space, BAL and non-BAL quasars are present at all locations; for every BAL-quasar it is possible to identify non-BAL quasars with the same emission-line outflow properties and SED-hardness. The co-location of BAL and non-BAL quasars as a function of emission-line outflow and physical properties is the key result of our investigation, demonstrating that (high-ionization) BALs and non-BALs represent different views of the same underlying quasar population.

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Section: IV and Other Uv Emission Linessupporting

confidence: 63%

BAL and non-BAL quasars: continuum, emission, and absorption properties establish a common parent sample

Rankine

Hewett

Banerji

et al. 2020

Monthly Notices of the Royal Astronomical Society

123

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“…The velocity can be estimated from the width of the emission line: v f FWHM, 10 BLR =´( ) with f a geometrical factor accounting for projection effects (e.g., Decarli et al 2008;Grier et al 2013;Matthews et al 2017).…”

Section: Black Hole Massesmentioning

confidence: 99%

Physical Properties of 15 Quasars at z ≳ 6.5

Mazzucchelli

Bañados

Venemans

et al. 2017

ApJ

319

444

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Quasars are galaxies hosting accreting supermassive black holes; due to their brightness, they are unique probes of the early universe. To date, only a few quasars have been reported at (<800 Myr after the big bang). In this work, we present six additional quasars discovered using the Pan-STARRS1 survey. We use a sample of 15 quasars to perform a homogeneous and comprehensive analysis of this highest-redshift quasar population. We report four main results: (1) the majority of quasars show large blueshifts of the broad C iv λ1549 emission line compared to the systemic redshift of the quasars, with a median value ∼3× higher than a quasar sample at ; (2) we estimate the quasars’ black hole masses ( (0.3–5) × 109 M ⊙) via modeling of the Mg ii λ2798 emission line and rest-frame UV continuum and find that quasars at high redshift accrete their material (with ) at a rate comparable to a luminosity-matched sample at lower redshift, albeit with significant scatter (0.4 dex); (3) we recover no evolution of the Fe ii/Mg ii abundance ratio with cosmic time; and (4) we derive near-zone sizes and, together with measurements for quasars from recent work, confirm a shallow evolution of the decreasing quasar near-zone sizes with redshift. Finally, we present new millimeter observations of the [C ii] 158 μm emission line and underlying dust continuum from NOEMA for four quasars and provide new accurate redshifts and [C ii]/infrared luminosity estimates. The analysis presented here shows the large range of properties of the most distant quasars.

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“…Abbott and Lucy 1985;Lucy and Abbott 1993;Schaerer and Schmutz 1994;Schmutz 1997;Vink et al 1999Vink et al , 2000Sim 2004;Müller and Vink 2008;Muijres et al 2012b;Lucy 2012b;Noebauer and Sim 2015;Vink 2018), to determine synthetic light curves and spectra for SNe (see e.g. Mazzali and Lucy 1993;Lucy 1999a;Mazzali 2000;Lucy 2005;Kasen et al 2006;Sim 2007;Kromer and Sim 2009;Wollaeger et al 2013;Wollaeger and van Rossum 2014;Kerzendorf and Sim 2014;Bulla et al 2015;Magee et al 2018) or to treat RT in winds emanating from accretion discs of cataclysmic variables (Knigge et al 1995;Long and Knigge 2002;Noebauer et al 2010;Kusterer et al 2014;Matthews et al 2015) or active galactic nuclei (Sim 2005;Sim et al 2010Sim et al , 2012Higginbottom et al 2013;Matthews et al 2016Matthews et al , 2017Tomaru et al 2018). In applications such as these, our current implicit assumption, namely that RT occurs in static media or in environments with material velocities low enough to be safely ignored, can no longer be maintained.…”

Section: Mcrt: Application In Outflows and Explosionsmentioning

confidence: 99%

“…Lucy 1983;Abbott and Lucy 1985;Lucy and Perinotto 1987;Hillier 1991;Lucy and Abbott 1993;Schmutz 1997;Vink et al 1999;Harries 2000;Vink et al 2000;Sim 2004;Watanabe et al 2006;Lucy 2007;Müller and Vink 2008;Lucy 2010;Vink et al 2011;Lucy 2012a,b;Muijres et al 2012a,b;Šurlan et al 2012Müller and Vink 2014;Lucy 2015;Noebauer and Sim 2015;Vink 2018), mass outflows from disks (e.g. Knigge et al 1995;Knigge and Drew 1997;Long and Knigge 2002;Sim 2005;Sim et al 2005Sim et al , 2008Noebauer et al 2010;Sim et al 2010;Odaka et al 2011;Sim et al 2012;Higginbottom et al 2013;Kusterer et al 2014;Hagino et al 2015;Matthews et al 2015Matthews et al , 2016Matthews et al , 2017Tomaru et al 2018), or supernovae (e.g. Lucy 1987;Janka and Hillebrandt 1989;Mazzali and Lucy 1993;Lucy 1999b;…”

Section: Radiative Transfer Backgroundmentioning

confidence: 99%

Monte Carlo radiative transfer

Noebauer

Sim

2019

Living Rev Comput Astrophys

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The theory and numerical modelling of radiation processes and radiative transfer play a key role in astrophysics: they provide the link between the physical properties of an object and the radiation it emits. In the modern era of increasingly high-quality observational data and sophisticated physical theories, development and exploitation of a variety of approaches to the modelling of radiative transfer is needed. In this article, we focus on one remarkably versatile approach: Monte Carlo Radiative Transfer (MCRT). We describe the principles behind this approach, and highlight the relative ease with which they can (and have) been implemented for application to a range of astrophysical problems. All MCRT methods have in common a need to consider the adverse consequences of Monte Carlo (MC) noise in simulation results. We overview a range of methods used to suppress this noise and comment on their relative merits for a variety of applications. We conclude with a brief review of specific applications for which MCRT methods are currently popular and comment on the prospects for future developments.

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Quasar emission lines as probes of orientation: implications for disc wind geometries and unification

Cited by 15 publications

References 135 publications

BAL and non-BAL quasars: continuum, emission, and absorption properties establish a common parent sample

BAL and non-BAL quasars: continuum, emission, and absorption properties establish a common parent sample

Physical Properties of 15 Quasars at z ≳ 6.5

Monte Carlo radiative transfer

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