The present investigation is concerned with new calculations of Fe II line strengths, taking into account processes which were not considered previously. Attention is given to the theoretical aspects of the problem and ways to explain the energy output in the high energy transitions. A general method is presented for calculating the Fe II line intensities in a model designed to represent quasar photoionized clouds. It is shown that radiative excitation of Fe II, through continuum absorption, is important and can contribute up to about 20 percent of the observed flux in ultraviolet Fe II lines. Optical line strengths increase, and ultraviolet line strengths decrease as the optical depth in Fe II is increased.
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Netzer et al. (1983) studied this question.