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Article overview
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Comparison of The UV and Optical Fe II Emission in Type 1 AGNs | | Huynh Anh N. Le
; Jong-Hak Woo
; | | Date: |
10 Nov 2019 | | Abstract: | 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 ($40pm141$ kms and $182pm95$,
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. | | Source: | arXiv, 1911.3877 | | Services: | Forum | Review | PDF | Favorites | |
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