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A LINK BETWEEN VARIABLE OPTICAL CONTINUUM
AND RADIO EMISSION OF A COMPACT JET IN THE
RADIOíLOUD SEYFERT GALAXY 3C390.3
T.G. Arshakian 1 , A.P. Lobanov 1 , V.H. Chavushyan 2 , A.I. Shapovalova 3 , J.A. Zensus 1 ,
N.G. Bochkarev 4 , A.N. Burenkov 3
1 MaxíPlanckíInstitut fur Radioastronomie, Auf dem Hugel 69, 53121 Bonn, Germany,
2 Instituto Nacional de AstrofÒÐsica, Optica y ElectrÒonica, Apartado Postal 51. C.P. 72000.
Puebla, Pue., MÒexico,
3 Special Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167, Russia,
4 Sternberg Astronomical Institute, University of Moscow, Universitetskij Prospect 13,
Moscow 119899, Russia
tigar@mpifríbonn.mpg.de
We present an observational evidence for a relation between variability of radio emission of
the compact jet, nucleus optical continuum emission and ejections of new jet components
in the radio galaxy 3C390.3. We combine results from the monitoring of 3C390.3 in the
optical region (Shapovalova et al. 2001; Sergeev at al. 2002) with ten very long baseline
interferometry (VLBI) observations of its radio emission at 15 GHz carried out from 1992
to 2002 using the VLBA (Kellermann et al. 2004). For ten VLBA images, we identified five
moving components (C4íC8) and two stationary components (D,S1). Proper motions of
the moving components correspond to apparent velocities from 0.8c to 1.5c. No significant
correlation exists for the moving features between optical continuum and radio emission.
However the variations of optical continuum are correlated with radio emission from a
stationary feature (S1) in the jet. The optical emission follows radio flares with the mean
delays t(S1íopt)#0.4 year. Most probably the optical continuum is produced near the
location of radio emission of the S1 stationary component. The localization of the source
of optical continuum with the innermost part of the jet near S1 implies that the broad
line emission originates in a conical region (dimension # 100 light days) at a distance of #
0.4 pc from the central engine. For the components C4íC7, the epochs t(S1) of separation
from the stationary feature S1 are coincident, within the errors, with maxima in optical
continuum. This suggests that radio ejection events of the jet components are coupled with
the longíterm variability of optical continuum.
We suppose that the broad emission lines having a doubleípeaked structure originate in
two kinematically and physically di#erent regions of 3C390.3:
1. BLR1 -- the traditional BLR (Accretion Disk (AD) and the surrounding gas). It is
at the distance # 30 light days from the nuclei (Shapovalova et al. 2001).
2. BLR2 -- in a subrelativistic outflow surrounding the jet in the cone within # 100
light days at a distance of # 0.4 pc from the central engine.
During the nucleus maximal brightness periods most of the continuum variable radiation
is emitted from the jet and ionizes the surrounding gas, creating a BLR2 that mainly
determines the broad line emission. During the brightness minima the jet contribution
to the ionizing continuum is decreasing and the main broad line emission comes from the
``classical'' BLR1 (AD), ionized by nuclei continuum related with the acctretion at BH.
Such a scenario explains two maxima (# 30d and #100d) found in the crossícorrelation
function describing the timeílag of broad line variations relatively to continuum on the base
of the results of 3C390.3 optical monitoring in 1996í2000 (Shapovalova et al. 2001).

Acknowledgements. This work was supported by grants: CONACYT 39560F (Mexico),
INTAS (N96í0328) and RFBR (00í02í16272; 03í02í17123 and 06í02í16843, Russia).
References
Shapovalova et al.: A&A, 2001, 376, 775.
Sergeev et al.: ApJ, 2002, 576, 660;
Kellermann et al.: ApJ, 2004, 609, 539.