Exploring the link between C IV outflow kinematics and sublimation-temperature dust in quasars

Abstract Using data from SDSS, UKIDSS and WISE, we investigate the properties of the high-frequency cutoff to the infrared emission in ≃5000 carefully selected luminous (Lbol ∼ 1047) type 1 quasars. The strength of ≃2 μm emission, corresponding to emission from the hottest ($T>1200\rm \, K$) dust in the sublimation zone surrounding the central continuum source, is observed to correlate with the blueshift of the C iv λ1550 emission line. We therefore find that objects with stronger signatures of nuclear outflows tend to have a larger covering fraction of sublimation-temperature dust. When controlling for the observed outflow strength, the hot dust covering fraction does not vary significantly across our sample as a function of luminosity, black hole mass or Eddington fraction. The correlation between the hot dust and the C iv line blueshifts, together with the lack of correlation between the hot dust and other parameters, therefore provides evidence of a link between the properties of the broad emission line region and the infrared-emitting dusty regions in quasars.

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Constraining the geometry and kinematics of the quasar broad emission line region using gravitational microlensing

Astronomy and Astrophysics ◽

10.1051/0004-6361/201731087 ◽

2019 ◽

Vol 629 ◽

pp. A43 ◽

Cited By ~ 2

Author(s):

D. Hutsemékers ◽

L. Braibant ◽

D. Sluse ◽

R. Goosmann

Keyword(s):

Emission Line ◽

Line Profile ◽

Polar Wind ◽

Disk Model ◽

Continuum Source ◽

Broad Emission ◽

Gravitational Microlensing ◽

Line Region ◽

Broad Emission Line ◽

Single Epoch

The quadruply lensed quasar HE0435−1223 shows a clear microlensing effect that affects differently the blue and red wings of the Hα line profile in its image D. To interpret these observations, and constrain the broad emission line region (BLR) properties, the effect of gravitational microlensing on quasar broad emission line profiles and their underlying continuum has been simulated considering representative BLR models and microlensing magnification maps. The amplification and distortion of the Hα line profile, characterized by a set of four indices, can be reproduced by the simulations. Although the constraints on the BLR models set by the observed single-epoch microlensing signal are not very robust, we found that flattened geometries (Keplerian disk and equatorial wind) can more easily reproduce the observed line profile deformations than a biconical polar wind. With an additional independent constraint on the size of the continuum source, the Keplerian disk model of the Hα BLR is slightly favored.

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On the emergence of thousands of absorption lines in the quasar PG 1411+442: a clumpy high-column density outflow from the broad emission-line region?

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz1408 ◽

2019 ◽

Vol 487 (4) ◽

pp. 5041-5061 ◽

Cited By ~ 3

Author(s):

Fred Hamann ◽

Todd M Tripp ◽

David Rupke ◽

Sylvain Veilleux

Keyword(s):

Emission Line ◽

Galaxy Evolution ◽

Hubble Space Telescope ◽

Line System ◽

Continuum Source ◽

Broad Emission ◽

Line Region ◽

Balmer Lines ◽

Broad Emission Line ◽

Transient System

Abstract Quasar outflows are fundamental components of quasar environments that might play an important role in feedback to galaxy evolution. We report on the emergence of a remarkable new outflow absorption-line system in the quasar PG1411+442 (redshift ∼0.089) detected in the UV and visible with the Hubble Space Telescope Cosmic Origins Spectrograph and the Gemini Multi-Object Spectrograph, respectively. This new ‘transient’ system contains thousands of lines, including Fe ii and Fe ii∗ from excited states up to 3.89 eV, H i∗ Balmer lines, Na i D λλ5890, 5896, and the first detection of He i∗ λ5876 in a quasar. The transient absorber is spatially inhomogeneous and compact, with sizes ≲0.003 pc, based on covering fractions on the quasar continuum source ranging from ∼0.45 in strong UV lines to ∼0.04 in Na i D. cloudy photoionization simulations show that large total column densities log NH(cm−2) ≳ 23.4 and an intense radiation field ≲0.4 pc from the quasar are needed to produce the observed lines in thick zones of both fully ionized and partially ionized gas. The densities are conservatively log nH(cm−3) ≳ 7 based on Fe ii∗, H i∗, and He i∗ but they might reach log nH(cm−3) ≳ 10 based on Na i D. The transient lines appear at roughly the same velocity shift, v ∼ −1900 km s−1, as a ‘mini-BAL’ outflow detected previously, but with narrower Doppler widths, b ∼ 100 km s−1, and larger column densities in more compact outflow structures. We propose that the transient lines identify a clumpy outflow from the broad emission-line region that, at its current speed and location, is still gravitationally bound to the central black hole.

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The Kinematics of Quasar Broad Emission Line Regions Using a Disk-Wind Model

Publications of the Astronomical Society of Australia ◽

10.1017/pasa.2017.37 ◽

2017 ◽

Vol 34 ◽

Cited By ~ 5

Author(s):

Suk Yee Yong ◽

Rachel L. Webster ◽

Anthea L. King ◽

Nicholas F. Bate ◽

Matthew J. O’Dowd ◽

...

Keyword(s):

Emission Line ◽

Line Profile ◽

Inclination Angle ◽

Opening Angle ◽

Line Profiles ◽

Wind Model ◽

Disk Wind ◽

Reverberation Mapping ◽

Broad Emission ◽

Line Region

AbstractThe structure and kinematics of the broad line region in quasars are still unknown. One popular model is the disk-wind model that offers a geometric unification of a quasar based on the viewing angle. We construct a simple kinematical disk-wind model with a narrow outflowing wind angle. The model is combined with radiative transfer in the Sobolev, or high velocity, limit. We examine how angle of viewing affects the observed characteristics of the emission line. The line profiles were found to exhibit distinct properties depending on the orientation, wind opening angle, and region of the wind where the emission arises.At low inclination angle (close to face-on), we find that the shape of the emission line is asymmetric, narrow, and significantly blueshifted. As the inclination angle increases (close to edge-on), the line profile becomes more symmetric, broader, and less blueshifted. Additionally, lines that arise close to the base of the disk wind, near the accretion disk, tend to be broad and symmetric. Single-peaked line profiles are recovered for the intermediate and equatorial wind. The model is also able to reproduce a faster response in either the red or blue sides of the line profile, consistent with reverberation mapping studies.

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Near infrared hydrogen emission line ratios as diagnostics of the broad emission line region

Journal of Physics Conference Series ◽

10.1088/1742-6596/372/1/012069 ◽

2012 ◽

Vol 372 ◽

pp. 012069

Author(s):

Andrea J Ruff ◽

David J E Floyd ◽

Kirk T Korista ◽

Rachel L Webster ◽

Ryan L Porter ◽

...

Keyword(s):

Emission Line ◽

Near Infrared ◽

Hydrogen Emission ◽

Broad Emission ◽

Line Region ◽

Broad Emission Line ◽

Hydrogen Emission Line

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Velocity Diagnostics of the Broad Emission-Line Region of Active Galactic Nuclei

International Astronomical Union Colloquium ◽

10.1017/s0252921100039944 ◽

1997 ◽

Vol 159 ◽

pp. 175-178 ◽

Cited By ~ 1

Author(s):

Brian Espey

Keyword(s):

Emission Line ◽

Active Galactic Nuclei ◽

Galactic Nuclei ◽

Nuclear Region ◽

Driving Mechanisms ◽

Broad Emission ◽

Line Region ◽

Broad Emission Line ◽

Ongoing Project

AbstractWe present a brief review of emission-line velocity differences, and describe an ongoing project to determine the driving mechanisms responsible. We conclude with a brief outline of the use of velocity differences as probes of the conditions in the nuclear region of AGNs.

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Testing the relativistic Doppler boost hypothesis for supermassive binary black holes candidates via broad emission line profiles

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz3354 ◽

2019 ◽

Vol 491 (3) ◽

pp. 4023-4030 ◽

Cited By ~ 1

Author(s):

Zihao Song ◽

Junqiang Ge ◽

Youjun Lu ◽

Xiang Ji

Keyword(s):

Black Holes ◽

Emission Lines ◽

Binary Black Holes ◽

Broad Emission ◽

Line Region ◽

Two Samples ◽

Region Model ◽

Orbital Orientation ◽

The Continuum

ABSTRACT Optical periodicity QSOs found by transient surveys are suggested to be subparsec supermassive binary black holes (BBHs). An intriguing interpretation for the periodicity of some of those QSOs is that the continuum is radiated from the accretion disc associated with the BBH secondary component and modulated by the periodical rotation of the secondary via Doppler-boost effect. Close to edge-on orbital orientation can lead to more significant Doppler-boost effect and thus are preferred for these systems, which is distinct from those normal type-1 QSOs with more or less face-on orientations. Therefore, the profiles of broad lines emitted from these Doppler-modulated systems may be significantly different from other systems that are not Doppler modulated. We investigate the properties of the broad emission lines of optical-periodicity QSOs, including both a sample of QSOs that can be interpreted by the Doppler-modulated effects and a sample that cannot. We find that there is no obvious difference in the profiles and other properties of various (stacked) broad emission lines of these two samples, though a simple broad line region model would suggest significant differences. Our finding raises a challenge to the Doppler boost hypothesis for some of those BBHs candidates with optical periodicity.

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