Contribution of the disk emission to the broad emission lines   in
AGNs: Two-component model

Popović, L. Č.; Mediavilla, E.; Bon, E.; Ilić, D.

doi:10.1051/0004-6361:20034431

Cited by 113 publications

(182 citation statements)

References 44 publications

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“…11 (mean and rms profiles), the changes in the line profile also have double-peaked rms, which indicates that the changes in the blue wing are significantly (some) stronger, than in the red wing. One central peak in the rms profile may be caused by a central component in the BLR (Popović et al 2004;Bon et al 2006Bon et al , 2009. v) From the Lomb-Scargle periodogram method that we applied on the measured red-to-blue peak flux ratio (R = F(red)/F(blue)) of Hα and Hβ lines, we found possible periodical variations (signals) in this ratio.…”

Section: Resultsmentioning

confidence: 88%

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Spectral optical monitoring of a double-peaked emission line AGN Arp 102B

Shapovalova

Popovic

Burenkov

et al. 2013

A&A

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Context. We present results of long-term (1987-2010) optical spectral monitoring of the broad-line radio galaxy Arp 102B, a prototype of an active galactic nucleus with double-peaked broad emission lines that are commonly assumed to be emitted from an accretion disk. Aims. To explore the structure of the broad-line region (BLR), we analyze the light-curves of the broad Hα and Hβ lines and the continuum flux. We aim to estimate the dimensions of the broad-line emitting regions and the mass of the central black hole. Methods. We used the cross correlation function to find lags between the lines and continuum variations. We investigated the correlation between line and continuum fluxes in more detail and explored periodical variations of the red-to-blue line flux ratio using Lomb-Scargle periodograms. Results. The line and continuum light-curves show several flare-like events. The fluxes in lines and in the continuum show no significant change (around 20%) during the monitored period. We found a weak correlation between the line and continuum flux variation that may indicate that the line variation is weakly connected with the variation of the central photoionization source. In spite of this weak line-continuum correlation, we estimated a time lag for Hβ of about 20 days using various methods. The correlation between the Hβ and Hα flux variation is significantly higher than that between the lines and continuum. During the monitored period, the Hβ and Hα lines show double-peaked profiles, and we found an indication for a periodical oscillation in the red-to-blue flux ratio of the Hα line. The estimated mass of the central black hole is ∼1.1 × 10 8 M , which agrees with the mass estimated from the M-σ * relation.

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Section: Resultsmentioning

confidence: 88%

“…One central peak in the rms may be caused by a central component (see e.g. Popović et al 2004;Bon et al 2006Bon et al , 2009.…”

Section: Changes In the Broad-line Profilesmentioning

confidence: 99%

Spectral optical monitoring of a double-peaked emission line AGN Arp 102B

Shapovalova

Popovic

Burenkov

et al. 2013

A&A

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“…does not preclude the line from forming in a disk, provided that the emitting disk axis is seen at low inclination or that a part of the line core comes from a physically and kinematically different region (e.g., Popović et al 2004;Murray & Chiang 1997). The line core that partly arises from an extended emission region can especially account for the microlensing magnification dropping in the low-velocity part of both the CIV and Hα lines.…”

Section: Keplerian Diskmentioning

confidence: 99%

The different origins of high- and low-ionization broad emission lines revealed by gravitational microlensing in the Einstein cross

Braibant

Hutsemékers

Sluse

et al. 2016

A&A

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We investigate the kinematics and ionization structure of the broad emission line region of the gravitationally lensed quasar QSO2237+0305 (the Einstein cross) using differential microlensing in the high-and low-ionization broad emission lines. We combine visible and near-infrared spectra of the four images of the lensed quasar and detect a large-amplitude microlensing effect distorting the high-ionization CIV and low-ionization Hα line profiles in image A. While microlensing only magnifies the red wing of the Balmer line, it symmetrically magnifies the wings of the CIV emission line. Given that the same microlensing pattern magnifies both the high-and low-ionization broad emission line regions, these dissimilar distortions of the line profiles suggest that the high-and low-ionization regions are governed by different kinematics. Since this quasar is likely viewed at intermediate inclination, we argue that the differential magnification of the blue and red wings of Hα favors a flattened, virialized, low-ionization region whereas the symmetric microlensing effect measured in CIV can be reproduced by an emission line formed in a polar wind, without the need of fine-tuned caustic configurations.

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“…we have composite emission from the disk and an additional region (see e.g. Popović et al 2004;Ilić et al 2006;Bon et al 2009). Also, Arshakian et al (2010) considered that the BLR of 3C390.3 has a complex structure composed of two components: 1) BLR1 -the traditional BLR (accretion disk), 2) BLR2 -a sub-region (outflow) that surrounds the compact radio jet.…”

Section: Variability and The Blr Structure Of 3c 3903mentioning

confidence: 99%

“…The physics and geometry of the BLR are uncertain, and an investigation of the BEL shape variability in a long period is very useful for determining the BLR nature. The profiles of the BELs in AGN can indicate the geometry of emitting plasma in the BLR (see Sulentic et al 2000;Popović et al 2004;Gaskell 2009;Zamfir et al 2010, etc. ).…”

Section: Introductionmentioning

confidence: 99%

Spectral optical monitoring of 3C 390.3 in 1995–2007

Popovic

Shapovalova

Ilić

et al. 2011

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Context. We present a study of the variability of the broad emission-line parameters of 3C390.3, an active galaxy with the doublepeaked emission-line profiles. We give a detailed analysis of the variation in the broad Hα and Hβ emission-line profiles, the ratios, and the Balmer decrement of different line segments. Aims. We explore the disk structure with an investigation of the variability of the broad-line profiles. This is assumed to emit the broad double-peaked Hβ and Hα emission lines in the spectrum of 3C390.3. Methods. We divided the observed spectra into two periods (before and after the outburst in 2002) and separately analyzed the variation in these two periods. First we analyzed the spectral emission-line profiles of the Hα and Hβ lines and measured the peak positions. Then, we divided the lines into several segments and measured the line-segment fluxes. The Balmer decrement variation for the entire Hα and Hβ fluxes and for the line segments was investigated and discussed. Additionally, we modeled the variations in the line parameters with an accretion disk model and compared our modeled line parameter variations with observed ones. Results. We compared the variability in the observed line parameters with the disk model predictions and found that the variation in line profiles and in the line segments corresponds to the emission of a disk-like broad-line region (BLR). But there is probably another additional emission component that contributes to the Hα and Hβ line center. We found that the variation in the line profiles is caused by the variation in the parameters of the disk-like BLR, first of all in the inner (outer) radius, which can well explain the line parameters variations in Period I. The Balmer decrement across the line profile has a bell-like shape and is affected not only by physical processes in the disk, but also by different emitting disk dimension of the Hα and Hβ line. Conclusions. The geometry of the BLR of 3C390.3 seems to be very complex, and inflows/outflows may be present, but evidently the broad-line region with its disk-like geometry is the dominant emitter.

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Contribution of the disk emission to the broad emission lines in AGNs: Two-component model

Cited by 113 publications

References 44 publications

Spectral optical monitoring of a double-peaked emission line AGN Arp 102B

Spectral optical monitoring of a double-peaked emission line AGN Arp 102B

The different origins of high- and low-ionization broad emission lines revealed by gravitational microlensing in the Einstein cross

Spectral optical monitoring of 3C 390.3 in 1995–2007

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