2014A&A...566A.106K


C.D.S. - SIMBAD4 rel 1.7 - 2019.08.19CEST10:53:09

2014A&A...566A.106K - Astronomy and Astrophysics, volume 566A, 106-106 (2014/6-1)

Broad-line region structure and kinematics in the radio galaxy 3C 120.

KOLLATSCHNY W., ULBRICH K., ZETZL M., KASPI S. and HAAS M.

Abstract (from CDS):

Broad emission lines originate in the surroundings of supermassive black holes in the centers of active galactic nuclei (AGN). These broad-line emitting regions are spatially unresolved even for the nearest AGN. The origin and geometry of broad-line region (BLR) gas and their connection with geometrically thin or thick accretion disks is of fundamental importance for the understanding of AGN activity. One method to investigate the extent, structure, and kinematics of the BLR is to study the continuum and line profile variability in AGN. We selected the radio-loud Seyfert 1 galaxy 3C120 as a target for this study. We took spectra with a high signal-to-noise ratio of 3C120 with the 9.2m Hobby-Eberly Telescope between Sept. 2008 and March 2009. In parallel, we photometrically monitored the continuum flux at the Wise observatory. We analyzed the continuum and line profile variations in detail (1D and 2D reverberation mapping) and modeled the geometry of the line-emitting regions based on the line profiles. We show that the BLR in 3C120 is stratified with respect to the distance of the line-emitting regions from the center with respect to the line widths (FWHM) of the rms profiles and with respect to the variability amplitude of the emission lines. The emission line wings of Hα and Hβ respond much faster than their central region. This is explained by accretion disk models. In addition, these lines show a stronger response in the red wings. However, the velocity-delay maps of the helium lines show a stronger response in the blue wing. Furthermore, the HeIIλ4686 line responds faster in the blue wing in contradiction to observations made one and a half years later when the galaxy was in a lower state. The faster response in the blue wing is an indication for central outflow motions when this galaxy was in a bright state during our observations. The vertical BLR structure in 3C 120 coincides with that of other AGN. We confirm the general trend: the emission lines of narrow line AGN originate at larger distances from the midplane than AGN with broader emission lines.

Abstract Copyright:

Journal keyword(s): galaxies: active - galaxies: Seyfert - galaxies: nuclei - galaxies: individual: 3C 120 - quasars: emission lines

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 Mrk 1501 Sy1 00 10 31.0058529490 +10 58 29.505989476   15.96 15.40 12.22   ~ 621 0
2 Mrk 1506 Sy1 04 33 11.0958197353 +05 21 15.617543663   15.72 15.05 10.08   ~ 1796 2
3 Mrk 110 Sy1 09 25 12.8479868736 +52 17 10.386808297   16.82 16.41     ~ 489 0
4 NGC 3227 GiP 10 23 30.57 +19 51 54.3   12.61 11.79     ~ 1488 2
5 Mrk 40 Sy1 11 25 36.1546693198 +54 22 57.128083405   17.06 16.47     ~ 204 0
6 NGC 3783 Sy1 11 39 01.7095761008 -37 44 19.008597647   12.46 13.43 11.33 12.1 ~ 1436 0
7 NGC 4151 Sy1 12 10 32.5771747733 +39 24 21.057727323   12.18 11.48     ~ 3287 2
8 NGC 4593 Sy1 12 39 39.4435521178 -05 20 39.035028119   13.95 13.15     ~ 907 0
9 NGC 5548 Sy1 14 17 59.5401093128 +25 08 12.600227883   14.35 13.73     ~ 2317 0
10 Mrk 817 Sy1 14 36 22.0820075123 +58 47 39.395406826   14.19 13.79     ~ 404 0
11 ICRF J184208.9+794617 Sy1 18 42 08.9910523393 +79 46 17.129210139   16.06 15.38     ~ 1177 0
12 Mrk 1513 Sy1 21 32 27.8163185343 +10 08 19.250705656   14.92 14.64     ~ 523 0
13 NGC 7469 Sy1 23 03 15.674 +08 52 25.28 12.60 13.00 12.34     ~ 1832 3
14 Mrk 926 Sy1 23 04 43.4773393553 -08 41 08.632325890   16.20 15.91 9.4   ~ 391 0

    Equat.    Gal    SGal    Ecl

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2019.08.19-10:53:09

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