Abstract
In the Seyfert galaxy Fairall 9, low‐ionization lines (threshold energy between 1 and 3 Ry) appear to follow the UV bump and have a larger variation scale. The high‐ionization lines vary in step with the power‐law continuum. The results suggest that the variation amplitude of lines is inversely correlated to the ionization level. Our calculations suggest that the UV bump has a shape more complicated than a simple blackbody curve and has a quite steep drop around 30 eV. The degree of luminosity dependence of equivalent width of Lyα, C iii], Si iv, and C iv is inversely correlated with individual emission line’s ionization level. This offers a natural explanation as to why only the C iv equivalent width shows a significant luminosity dependence (the Baldwin effect).
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