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We aim to test the model proposed to explain the correlation between the fluxdensity at 15 GHz of a stationary component in the parsec-scale jet and theoptical continuum emission in the radio galaxy 3C~390.3. In the model, thedouble-peaked emission from 3C~390.3 is likely to be generated both near thedisk and in a rotating subrelativistic outflow surrounding the jet, due toionization of the outflow by the beamed continuum emission from the jet. Thisscenario is chosen since broad-emission lines are observed to vary followingchanges in the inner radio jet. For recent epochs we have imaged and modelledthe radio emission of the inner jet of 3C~390.3, which was observed with verylong baseline interferometry at 15 GHz, 22 GHz and 43 GHz, to image the innerpart of the parsec-scale jet, locate the exact region where the bulk of thecontinuum luminosity is generated and search for the mechanism that drives thedouble-peaked profile emission. We present the preliminary results of testingthe model using data from 11 years of active monitoring of 3C~390.3.

Radio-Optical Study of Double-Peaked AGNs. I. 3C 390.3