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We present the kinematical properties of the UV and optical \FeII\ emissiongas based on the velocity shift and line width measurements of a sample of 223Type 1 active galactic nuclei (AGNs) at 0.4 $<$ z $<$ 0.8. We find a strongcorrelation between the line widths of the UV and optical \FeII\ emissionlines, indicating that both \FeII\ emission features arise from similardistances in the broad line region (BLR). However, in detail we find differingtrends, depending on the width of \FeII. While the velocity shifts anddispersions of the UV Fe II (\FeUV) and optical Fe II (\FeOPT) emission linesare comparable to each other for AGNs with relatively narrow \FeOPT\ linewidths (i.e., FWHM < 3200 \kms; Group A), \FeOPT\ is broader than \FeUV\ forAGNs with relatively broad \FeOPT\ (i.e., FWHM > 3200 \kms; Group B). \FeII\emission lines are on average narrower than \Hb\ and \MgII\ for Group A,indicating the \FeII\ emission region is further out in the BLR, while forGroup B AGNs \FeOPT\ is comparable to \Hb\ and broader than \MgII. While \FeII\emission lines are on average redshifted ($40\pm141$ \kms\ and $182\pm95$,respectively for \FeUV\ and \FeOPT), indicating inflow, the sample as a wholeshows a large range of velocity shifts, suggesting complex nature of gaskinematics.

Comparison of The UV and Optical Fe II Emission in Type 1 AGNs