Vertical broad-line region structure in nearby active galactic nuclei

Kollatschny, W.; Zetzl, M.

doi:10.1051/0004-6361/201321685

Cited by 44 publications

(50 citation statements)

References 64 publications

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“…12, in the case of the turbulent velocities ∼ 500 km s −1 we can reproduce well the line strength for a covering factor ∼ 0.2. Such a high turbulent velocity is consistent with the turbulent velocity of 400 km s −1 deduced for the Hβ line in NGC 5548 based on modeling the line shape (Kollatschny & Zetzl 2013).…”

Section: Local Conditions and The Covering Factor In The Blrsupporting

confidence: 88%

SALT long-slit spectroscopy of quasar HE 0435-4312: fast displacement of the Mg II emission line

Šredzińska

Hryniewicz

Krupa

et al. 2017

A&A

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Context. The Mg II emission line is visible in the optical band for intermediate redshift quasars (0.4 < z < 1.6) and it is thus an extremely important tool to measure the black hole mass and to understand the structure of the Broad Line Region. Aims. We aim to determine the substructure and the variability of the Mg II line with the aim to identify which part of the line comes from a medium in Keplerian motion. Methods. Using the Southern African Large Telescope (SALT) with the Robert Stobie Spectrograph (RSS) we performed ten spectroscopic observations of quasar HE 0435-4312 (z = 1.2231) over a period of three years (Dec 23/24, 2012 to Dec 7/8, 2015. Results. Both the Mg II line and the Fe II pseudo-continuum increase with time. We clearly detect the systematic shift of the Mg II line with respect to the Fe II over the years, corresponding to the acceleration of 104 ± 14 km s −1 year −1 in the quasar rest frame. The Mg II line shape is clearly non-Gaussian but single-component, and the increase in line equivalent width and line shift is not accompanied with significant evolution of the line shape. We analyse the conditions in the Mg II and Fe II formation region and we note that the very large difference in the covering factor and the turbulent velocity also support the conclusion that the two regions are spatially separated. Conclusions. The measured acceleration of the line systematic shift is too large to connect it with the orbital motion at a distance of the Broad Line Region (BLR) in this source. It may imply a precessing inner disk illuminating the BLR. Further monitoring is still needed to better constrain the variability mechanism.

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Section: Local Conditions and The Covering Factor In The Blrsupporting

confidence: 88%

SALT long-slit spectroscopy of quasar HE 0435-4312: fast displacement of the Mg II emission line

Šredzińska

Hryniewicz

Krupa

et al. 2017

A&A

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“…Inclination is also another uncertainty, as the BLR velocity field is not completely virialized, but contains a clear equatorial component (e.g. Collin et al 2006;Kollatschny & Zetzl 2013;Pancoast, Brewer & Treu 2014). Any equatorial component to the velocity field will be suppressed in low inclination (simple) NLS1s, so their masses will be systematically biased towards higher values compared to high inclination (complex) NLS1s.…”

Section: Discussionmentioning

confidence: 99%

Complex narrow-line Seyfert 1s: high spin or high inclination?

Gardner

Done

2015

Monthly Notices of the Royal Astronomical Society

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Complex narrow line Seyfert 1s (NLS1s), such as 1H0707-495, differ from simple NLS1s like PG1244+026 by showing stronger broad spectral features at Fe K and larger amplitude flux variability. These are correlated: the strongest Fe K features are seen during deep dips in the light curves of complex NLS1s. There are two competing explanations for these features, one where a compact X-ray source on the spin axis of a highly spinning black hole approaches the horizon and the consequent strong relativistic effects focus the intrinsic flux onto the inner edge of a thin disc, giving a dim, reflection dominated spectrum. The other is that the deep dips are caused by complex absorption by clumps close to the hard X-ray source. The reflection dominated model is able to reproduce the very short 30s soft lag from reverberation seen in the complex NLS1 1H0707-495. However, it does not explain the characteristic switch to hard lags on longer timescales. Instead, a full model of propagating fluctuations coupled to reverberation can explain the switch in the simple NLS1 PG1244+026 using a low spin black hole. However PG1244+026 has a longer reverberation lag of ∼ 200s.Here we extend the successful propagation-reverberation model for the simple NLS1 PG1244+026 to include the effect of absorption from clumps in a turbulent region above the disk. The resulting occultations of the inner accretion flow can introduce additional hard lags when relativistic effects are taken into account. This dilutes the soft lag from reverberation and shifts it to higher frequencies, making a smooth transition between the 200s lags seen in simple NLS1s to the 30s lags in complex NLS1s. These two classes of NLS1 could then be determined by inclination angle with respect to a clumpy, probably turbulent, failed wind structure on the disc.

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“…This region can depolarize the disc-like emission. The twocomponent BLR (disc covered by an outflowing region of randomly distributed clouds) seems to be a good approximation for nearby AGN (Kollatschny & Zetzl 2013), as well as for a number of single-peaked AGN (see in more details Bon et al 2009). …”

Section: Polarization -Connection Between Disc and Jetmentioning

confidence: 98%

Spectropolarimetric monitoring of active galaxy 3C 390.3 with 6-m telescope SAO RAS in the period 2009–2014

Afanasiev

Shapovalova

Borisov

2015

Monthly Notices of the Royal Astronomical Society

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Here we present the spectropolarimetric observations of the radio loud active galaxy 3C 390.3 in the period 2009-2014 (24 epochs). The galaxy has been observed with the 6-meter telescope of SAO RAS using the SCORPIO spectropolarimeter. We explore the variability and lags in the polarized light of the continuum and broad Hα line. We give the Stokes parameters Q, U , degree of linear polarization P and the position angle of the polarization plane, ϕ, for 24 epochs.We find a small lag (10-40 days) between the unpolarized and polarized continuum that is significantly smaller than the estimated lags for the unpolarized broad emission lines (lag(Hα)∼138-186 and lag(Hβ)∼60-79 days). This shows that the region of the variable polarized continuum is significantly smaller than the broad line region, indicating that a part of the polarized continuum is coming from the jet. The lag of the polarized light in the Hα line (89-156 days) indicates an additional component to the disc one that has an outflowing velocity of ∼-1200 km s −1 . This region seems to depolarize the polarized broad Hα line emitted from the disc and scattered in the inner part of the torus.

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Vertical broad-line region structure in nearby active galactic nuclei

Cited by 44 publications

References 64 publications

SALT long-slit spectroscopy of quasar HE 0435-4312: fast displacement of the Mg II emission line

SALT long-slit spectroscopy of quasar HE 0435-4312: fast displacement of the Mg II emission line

Complex narrow-line Seyfert 1s: high spin or high inclination?

Spectropolarimetric monitoring of active galaxy 3C 390.3 with 6-m telescope SAO RAS in the period 2009–2014

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