Correlations In Fe II(UV)/Mg II, Luminosity And Fe Abundance In Quasars At Z 3

Details Correlations In Fe II(UV)/Mg II, Luminosity And Fe Abundance In Quasars At Z 3 Correlations In Fe II(UV)/Mg II, Luminosity And Fe Abundance In Quasars At Z 3

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...21111806v&link_type=abstract

American Astronomical Society, AAS Meeting #211, #118.06; Bulletin of the American Astronomical Society, Vol. 39, p.947

Astronomy and Astrophysics

Astronomy

Scientific paper

The Fe enrichment relative to Mg is a potential probe of star formation activity and nucleosynthesis in the Early Universe. QSOs exhibit 2000-3000Å Fe II(UV) band and Mg II 2800 Å line emission at all redshifts with large scatter in Fe II(UV)/Mg II emission ratios. Our developed photoinization model for 14eV of Fe II atom indicates that 2000-3000Å region in QSOs can be covered by thousands of strong Fe II emission lines. While it also predicts that the Fe II (UV) emission and thus FeII(UV)/MgII ratios are sensitive to microturbulence, radiation field, hydrogen density and abundance, it allows to separate these effects using Fe II optical emission. We demonstrate the differences between the I Zw 1 Fe II and bright QSOs templates and discuss possible errors in Fe II(UV)/Mg II ratios measurements cause by use of the former. Our work provides evidence that the model approach is a better tool compared to templates.
We applied our model to IRTF/SpeX data of seven bright QSOs at 3.1We acknowledge the support of the National Science Foundation through grant AST-0607465 and our use of the IRTF/SpeX, which is operated by the University of Hawaii under Cooperative Agreement no. NCC 5-538 with the NASA.

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