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A Study of Time Variations of UV Continuum and Emission Lines in 3C390.3

Wei Zheng
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Abstract

Based on the IUE SWP spectra obtained between 1978 and 1994, the variations of the UV continuum and the Ly-alpha and C IV emission lines of the broad-line radio galaxy 3C390.3 are studied. The UV continuum between 1220 and 1990 A has varied considerably. In 1991 August, the flux at 1360 A reached a maximum level ~27 times as high as its minimum level. At 1850 A, the continuum varies by a factor of ~12. Significant variations are frequently observed in periods as short as one month. The total flux of Ly-alpha and C IV emission varies by a factor of ~5. Their profiles are fitted with one narrow component, unresolved at the instrumental resolution of FWHM ~2000 km/s, and three broad components (FWHM ~6000 km/s). The narrow component varies by a factor of ~2.5. The broad components on the blue and red wings of the Ly-alpha and C IV emission profile, which correspond to the double humps in the H-alpha and H-beta emission feature, display a close correlation to the varying continuum, with a time lag of ~45 days. The blue Ly-alpha component has been stronger than the red component except for several epochs in 1980 and 1991. The C IV/Ly-alpha flux ratio is ~0.4 for the narrow component. For the broad components, this ratio varies considerably around an average value of unity. In 1991 March, the blue Ly-alpha component was stronger than the red, while for C IV the red component was stronger. Such differential variations do not match the accretion disk characteristics. The findings suggest that the narrow- and broad-line region in 3C 390.3 may be associated with a radio jet.

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Wei Zheng. 1996-03-04. A Study of Time Variations of UV Continuum and Emission Lines in 3C390.3. https://doi.org/10.1086/117891

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