Comparison of The UV and Optical Fe II Emission in Type 1 AGNs
  We present the kinematical properties of the UV and optical \FeII\ 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 \FeII\ emission
lines, indicating that both \FeII\ emission features arise from similar
distances in the broad line region (BLR). However, in detail we find differing
trends, depending on the width of \FeII. While the velocity shifts and
dispersions of the UV Fe II (\FeUV) and optical Fe II (\FeOPT) emission lines
are comparable to each other for AGNs with relatively narrow \FeOPT\ line
widths (i.e., FWHM < 3200 \kms; Group A), \FeOPT\ is broader than \FeUV\ for
AGNs 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 for
Group 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 whole
shows a large range of velocity shifts, suggesting complex nature of gas
kinematics.
