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A LINK BETWEEN VARIABLE OPTICAL CONTINUUM AND RADIO EMISSION OF A COMPACT JET IN THE RADIO-LOUD SEYFERT GALAXY 3C390.3
T.G. Arshakian1 , A.P. Lobanov1 , V.H. Chavushyan2 , A.I. Shap ovalova3 , J.A. Zensus 1 , N.G. Bo chkarev4 , A.N. Burenkov3
2

Max-Planck-Institut fur Radioastronomie, Auf dem Hugel 69, 53121 Bonn, Germany, Instituto Nacional de Astrofґ isica, Optica y Electrґ onica, Apartado Postal 51. C.P. 72000. Puebla, Pue., Mґ exico, 3 Sp ecial Astrophysical Observatory of RAS, Nizhnij Arkhyz, 369167, Russia, 4 Sternb erg Astronomical Institute, University of Moscow, Universitetskij Prosp ect 13, Moscow 119899, Russia tigar@mpifr-b onn.mpg.de

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We present an observational evidence for a relation b etween variability of radio emission of the compact jet, nucleus optical continuum emission and ejections of new jet comp onents in the radio galaxy 3C390.3. We combine results from the monitoring of 3C390.3 in the optical region (Shap ovalova 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 comp onents (C4-C8) and two stationary comp onents (D,S1). Prop er motions of the moving comp onents corresp ond to apparent velo cities from 0.8c to 1.5c. No significant correlation exists for the moving features b etween 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(S1-opt)0.4 year. Most probably the optical continuum is pro duced near the lo cation of radio emission of the S1 stationary comp onent. The lo calization 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 p c from the central engine. For the comp onents C4-C7, the ep o chs 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 comp onents are coupled with the long-term variability of optical continuum. We supp ose that the broad emission lines having a double-p eaked structure originate in two kinematically and physically different 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 (Shap ovalova 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 p c from the central engine. During the nucleus maximal brightness p erio ds 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 cross-correlation function describing the time-lag of broad line variations relatively to continuum on the base of the results of 3C390.3 optical monitoring in 1996-2000 (Shap ovalova et al. 2001).


Acknow ledgements. This work was supp orted by grants: CONACYT 39560F (Mexico), INTAS (N96-0328) and RFBR (00-02-16272; 03-02-17123 and 06-02-16843, Russia). References Shap ovalova et al.: A&A, 2001, 376, 775. Sergeev et al.: ApJ, 2002, 576, 660; Kellermann et al.: ApJ, 2004, 609, 539.