Abstract
Abstract We present the kinematical properties of the UV and optical Fe ii 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 Fe ii emission lines, indicating that both Fe ii emission features arise from similar distances in the broad-line region (BLR). However, in detail we find differing trends, depending on the width of Fe ii. While the velocity shifts and dispersions of the UV Fe ii (Fe ii uv) and optical Fe ii (Fe ii opt) emission lines are comparable to each other for AGNs with relatively narrow Fe ii opt line widths (i.e., FWHM < 3200 km s−1; Group A), Fe ii opt is broader than Fe ii uv for AGNs with relatively broad Fe ii opt (i.e., FWHM > 3200 km s−1; Group B). Fe ii emission lines are on average narrower than Hβ and Mg ii for Group A, indicating the Fe ii emission region is further out in the BLR, while for Group B AGNs Fe ii opt is comparable to Hβ and broader than Mg ii. While Fe ii emission lines are on average redshifted (40 ± 141 km s−1 and 182 ± 95 respectively for Fe ii uv and Fe ii opt), indicating inflow, the sample as a whole shows a large range of velocity shifts, suggesting the complex nature of the gas kinematics.
Sign-in/Register to access full text options 
Talk to us
Join us for a 30 min session where you can share your feedback and ask us any queries you have
Schedule a callDisclaimer: All third-party content on this website/platform is and will remain the property of their respective owners and is provided on "as is" basis without any warranties, express or implied. Use of third-party content does not indicate any affiliation, sponsorship with or endorsement by them. Any references to third-party content is to identify the corresponding services and shall be considered fair use under The CopyrightLaw.
