Geometry and kinematics in the central broad-line
 region  of a Seyfert 1 galaxy

Kollatschny, W.; Bischoff, K.

doi:10.1051/0004-6361:20020388

Cited by 30 publications

(40 citation statements)

References 20 publications

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“…It is intriguing that the very broad-line AGN 3C 390.3 shows the same pattern in the velocity-delay maps as the narrow-line AGN Mrk 110 (see Kollatschny & Bischoff 2002;Kollatschny 2003). The outer red and blue wings respond much faster to continuum variations than the central regions.…”

Section: D Ccf Of the Hβ Line Profilesmentioning

confidence: 85%

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Spectral optical monitoring of 3C 390.3 in 1995–2007

Popovic

Shapovalova

Ilić

et al. 2011

A&A

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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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Section: D Ccf Of the Hβ Line Profilesmentioning

confidence: 85%

“…We proceed in the same way as for the line-profile variations in Mrk 110 (Kollatschny & Bischoff 2002;Kollatschny 2003). Figure 14 shows the maximum response of the correlation functions of the Hβ line segment light curves with the continuum light curve, and Fig.…”

Section: D Ccf Of the Hβ Line Profilesmentioning

confidence: 99%

Spectral optical monitoring of 3C 390.3 in 1995–2007

Popovic

Shapovalova

Ilić

et al. 2011

A&A

Self Cite

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“…The line widths of Mrk 926 amount to 10 000 km s −1 (FWHM) compared to line widths of 2000 km s −1 only in Mrk 110 (Kollatschny et al 2001). It has been demonstrated that the narrow Balmer and helium emission lines in Mrk 110 originate in an accretion disk seen nearly face on (Kollatschny 2002(Kollatschny , 2003. The response of the very broad emission lines in Mrk 926 might be caused by an accretion disk seen nearly edge on relative to e.g.…”

Section: D Velocity Mapmentioning

confidence: 98%

“…We proceed in the same way as when we studied the line profile variations in Mrk 110 (Kollatschny & Bischoff 2002;Kollatschny 2003).…”

Section: -D Ccf Of the Hα And Hβ Line Profilesmentioning

confidence: 99%

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Line profile and continuum variability in the very broad-line Seyfert galaxy Mrk 926

Kollatschny

Zetzl

2010

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Aims. We present results of an intensive spectroscopic variability campaign of the very broad-line Seyfert 1 galaxy Mrk 926. Our aim is to investigate the broad-line region (BLR) by studying the intensity and line profile variations of this galaxy on short timescales. Methods. High signal-to-noise ratio (S/N) spectra were taken with the 9.2 m Hobby-Eberly Telescope (HET) in identical conditions during two observing campaigns in 2004 and 2005. After the spectral reduction and internal calibration we achieved a relative flux accuracy of better than 1%. Results. The rms profiles of the very broad Balmer lines have shapes that differ from their mean line profiles, consisting of two inner (v ±6000 km s −1 ) and two outer (v ±6000 km s −1 ) line components in addition to a central component (v ±600 km s −1 ). These outer and inner line segments varied with different amplitudes during our campaign. The radius of the BLR is very small with an upper limit of 2 light-days for the Hβ BLR size. We derived an upper limit to the central black hole mass of M = 11.2 × 10 7 M . The 2-D cross-correlation functions CCF(τ, v) of Hβ and Hα are flat within the error limits. The response of the Balmer line segments with respect to continuum variations is different in the outer and inner wings of Hα and Hβ. This double structure in the response curves -of two separate inner and outer components -has also been seen in the rms line profiles. We conclude that the outer and inner line segments originate in different regions and/or under different physical conditions.

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Active Galaxies in the UV

Kollatschny

Wang

Fundamental Questions in Astrophysics: Guidelines for Future UV Observatories

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In this article we present different aspects of AGN studies demonstrating the importance of the UV spectral range. Most important diagnostic lines for studying the general physical conditions as well as the metalicities in the central broad line region in AGN are emitted in the UV. The UV/FUV continuum in AGN excites not only the emission lines in the immediate surrounding but it is responsible for the ionization of the intergalactic medium in the early stages of the universe. Variability studies of the emission line profiles of AGN in the UV give us information on the structure and kinematics of the immediate surrounding of the central supermassive black hole as well as on its mass itself. 2 Wolfram Kollatschny, Wang Ting-GuiActive Galactic Nuclei (AGN) are the most luminous objects in the universe.Their luminosities, their spectral energy distribution from the radio to the γray range, as well as their emission line ratios cannot be generated by normal stars. Galaxies containing an active nucleus are called active galaxies. We divide the AGN in different subclasses such as Quasars, Seyfert galaxies and Liners.Many aspects of the generation of the energy in AGN are still unknown. Accretion of gas onto a central supermassive black hole (SMBH) is generally accepted to be the dominant physical process generating the enormous energies we are observing (Rees [Rees (1984)]). The accretion flow is the source of the non-thermal continuum emission in the UV, X-ray and optical. The spectral energy distribution (SED) of the non-thermal continuum emission in typical AGN has its maximum in the UV. The central continuum source ionizes the circumnuclear gas in the so called broad line region (BLR) and narrow line region (NLR). The majority of the most important emission lines are emitted in the UV spectral range.The overall continuum distribution as well as the UV spectral lines (narrow emission lines, broad emission lines, absorption lines) are tracers of the physical conditions of those regions where these emission lines originate.Active Galaxies in the UV 3

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Geometry and kinematics in the central broad-line region of a Seyfert 1 galaxy

Cited by 30 publications

References 20 publications

Spectral optical monitoring of 3C 390.3 in 1995–2007

Spectral optical monitoring of 3C 390.3 in 1995–2007

Line profile and continuum variability in the very broad-line Seyfert galaxy Mrk 926

Active Galaxies in the UV

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