The Effect of a Variable Anisotropic Continuum Source upon the Broad Emission Line Profiles and Responses

1996 ◽  
Vol 469 ◽  
pp. 113 ◽  
Author(s):  
Mike Goad ◽  
Ignaz Wanders
Keyword(s):  
Emission Line ◽  
Line Profiles ◽  
Continuum Source ◽  
Broad Emission ◽  
Broad Emission Line

scholarly journals The Effect of a Variable Anisotropic Continuum Source upon the Broad Emission-Line Profiles and Responses

1997 ◽  
Vol 159 ◽  
pp. 199-200
Author(s):  
Mike Goad ◽  
Ignaz Wanders
Keyword(s):  
Point Source ◽  
Emission Line ◽  
Response Function ◽  
Optical Monitoring ◽  
Line Profiles ◽  
Continuum Source ◽  
Gas Kinematics ◽  
Keplerian Orbits ◽  
Broad Emission ◽  
Broad Emission Line

Optical monitoring data over several years in combination with the reconstructed 1-d response function for C IV obtained from the 1993 HST monitoring campaign of NGC 5548, reveal that: (a) radial motion does not dominate the gas kinematics (Korista et al. 1995); (b) line-profile variations occur in fixed regions of velocity space, a core and two wing components, are stochastic in nature, and appear to be unrelated to reverberation effects (Wanders & Peterson 1996). Wanders et al. (1995) showed that these variations are broadly consistent with a spherical BLR geometry populated with optically thick clouds following randomly inclined circular Keplerian orbits, and illuminated by an anisotropically emitting point source of ionizing continuum radiation. Here we provide a brief description of this model and summarize its basic properties. A more thorough analysis is presented in Goad & Wanders (1996).

scholarly journals The Nature and Origin of Structure in Broad Emission Line Profiles

1997 ◽  
Vol 159 ◽  
pp. 193-194 ◽  
Author(s):  
C. Martin Gaskell ◽  
Stephanie A. Snedden
Keyword(s):  
Emission Line ◽  
The Other ◽  
Central Component ◽  
Balmer Line ◽  
Line Profiles ◽  
Broad Emission ◽  
Broad Emission Line

AbstractWe postulate that all structure in broad lines can be explained by a central component (at the systemic redshift) and the addition of two ‘displaced components’, one blueshifted and the other redshifted. We have been able to successfully classify all Balmer-line profiles on this basis. 3C 390.3-type objects are merely examples where the shifts of the displaced components are unusually large. We believe that the displaced peaks are less prominent in the UV lines because the higher ionization lines are broader.

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

2019 ◽  
Vol 629 ◽  
pp. A43 ◽  
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.

scholarly journals The Diversity of Broad Emission-Line Profiles

1997 ◽  
Vol 159 ◽  
pp. 197-198
Author(s):  
Giovanna M. Stirpe ◽  
Andrew Robinson ◽  
David J. Axon
Keyword(s):  
Simple Model ◽  
Emission Line ◽  
Power Law ◽  
Active Galaxies ◽  
Broad Line ◽  
Line Profiles ◽  
Broad Emission ◽  
Power Law Function ◽  
Broad Emission Line ◽  
Almost All

AbstractWe present preliminary results from a study of broad-line profiles in active galaxies. A simple model in which the emissivity is a broken power-law function of radius, and the BLR clouds emit anisotropically, yields very good fits to almost all the Ha profiles in our data base.

scholarly journals Long-term variability of the Broad Emission Line profiles in AGN

2009 ◽  
Vol 53 (7-10) ◽  
pp. 191-197 ◽  
Author(s):  
A.I. Shapovalova ◽  
L.Č. Popović ◽  
N.G. Bochkarev ◽  
A.N. Burenkov ◽  
V.H. Chavushyan ◽  
...  
Keyword(s):  
Emission Line ◽  
Line Profiles ◽  
Broad Emission ◽  
Broad Emission Line

scholarly journals 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?

2019 ◽  
Vol 487 (4) ◽  
pp. 5041-5061 ◽  
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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