Steps toward Determination of the Size and Structure of the Broad‐Line Region in Active Galactic Nuclei. XIII. Ultraviolet Observations of the Broad‐Line Radio Galaxy 3C 390.3

As part of an extensive multi-wavelength monitoring campaign, theInternational Ultraviolet Explorer satellite was used to observe the broad-lineradio galaxy 3C 390.3 during the period 1994 December 31 to 1996 March 5.Spectra were obtained every 6-10 days. The UV continuum varied by a factor of 7through the campaign, while the broad emission-lines varied by factors of 2-5.Unlike previously monitored Seyfert 1 galaxies, in which the X-ray continuumgenerally varies with a larger amplitude than the UV, in 3C 390.3 the UVcontinuum light-curve is similar in both amplitude and shape to the X-raylight-curve observed by ROSAT. The UV broad emission-line variability lags thatof the UV continuum by 35-70 days for Ly-alpha and CIV 1549; values larger thanthose found for Seyfert 1 galaxies of comparable UV luminosity. These lags arealso larger than those found for the Balmer lines in 3C 390.3 over the sameperiod. The red and blue wings of CIV and Ly-alpha vary in phase, suggestingthat radial motion does not dominate the kinematics of the UV line-emittinggas. Comparison with archival data provides evidence for velocity-dependentchanges in the Ly-alpha and CIV line profiles, indicating evolution in thedetailed properties and/or distribution of the broad-line emitting gas.