Comparison of The UV and Optical Fe II Emission in Type 1 AGNs
Abstract
We present the kinematical properties of the UV and optical \ emission gas based on the velocity shift and line width measurements of a sample of 223 Type 1 active galactic nuclei (AGNs) at 0.4 < z < 0.8. We find a strong correlation between the line widths of the UV and optical \ emission lines, indicating that both \ emission features arise from similar distances in the broad line region (BLR). However, in detail we find differing trends, depending on the width of . While the velocity shifts and dispersions of the UV Fe II () and optical Fe II () emission lines are comparable to each other for AGNs with relatively narrow \ line widths (i.e., FWHM < 3200 ; Group A), \ is broader than \ for AGNs with relatively broad \ (i.e., FWHM > 3200 ; Group B). \ emission lines are on average narrower than \ and \ for Group A, indicating the \ emission region is further out in the BLR, while for Group B AGNs \ is comparable to \ and broader than . While \ emission lines are on average redshifted (40141 \ and 18295, respectively for \ and ), indicating inflow, the sample as a whole shows a large range of velocity shifts, suggesting complex nature of gas kinematics.
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