Other
Scientific paper
Dec 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.4411b&link_type=abstract
American Astronomical Society, AAS Meeting #211, #44.11; Bulletin of the American Astronomical Society, Vol. 39, p.794
Other
Scientific paper
We use HST/FOS spectra of the narrow-lined BLR of the Seyfert 1 galaxy, I Zw 1, as a laboratory for modeling the UV Fe II 2100-3050 Å emission complex. We calculate a grid of Fe II emission spectra for range of physical conditions suitable for BLR clouds in AGNs. Predicted spectra, using CLOUDY and an 830-level model atom for Fe II with energies up to 14.06 eV, give a better fit to observed I Zw 1 Fe II emission than models with fewer levels. Our analysis indicates: 1) the deduced physical parameters in the BLR gas ( log nH /[cm-3] = 11.0; log(ΦH/[cm-2s-1] )=20.5; ξ /[km s-1] =20) ; 2) the observed UV Fe II emission must be corrected for an underlying Fe II pseudo-continuum; 3) Fe II emission peaks can be mis-identified as that of other ions in AGNs with narrow-lined BLRs resulting in possibly inaccurate physical parameters; 4) The shape of the 4200-4700 Å Fe II emission in QSOs is a relative indicator of contributing NLR and BLR Fe II emission. The Fe II 4200-4500 Å flux arises in NLR gas (ne ≤106 cm-3), while the 4500-4700 Å emission is almost exclusively from BLR clouds; 5) Predicted ratios of Lyα, C III], and Fe II emission relative to Mg II are in good agreement with extinction corrected observed values except for C IV 6) the sensitivity of Fe II emission to microturbulence makes the use of observed Fe II(UV)/Mg II flux ratio to infer Fe/Mg abundance ratios highly questionable. We are now extending our modeling to QSOs at higher redshift.
Bruhweiler Frederick C.
Verner Ekaterina
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