Black Hole Masses and Enrichment of z ~ 6 SDSS Quasars*

TLDR: In this paper, the authors measured the Fe II/Mg II line ratio as an observational proxy for the Fe/α-element ratio and derived a ratio of 27 ± 08 for their sample, which is similar to that found for lower redshift quasars.

Abstract: We present sensitive near-infrared spectroscopic observations for a sample of five z ~ 6 quasars These quasars are among the most distant, currently known quasars in the universe The spectra have been obtained using ISAAC at the VLT and include the C IV, Mg II, and Fe II lines We measure the Fe II/Mg II line ratio, as an observational proxy for the Fe/α-element ratio We derive a ratio of 27 ± 08 for our sample, which is similar to that found for lower redshift quasars; ie, we provide additional evidence for the lack of evolution in the Fe II/Mg II line ratio of quasars up to the highest redshifts This result demonstrates that star formation must have commenced at z ≥ 8 in the quasar hosts The line widths of the Mg II and C IV lines give two estimates for the black hole masses A third estimate is given by assuming that the quasars emit at their Eddington luminosity The derived masses using these three methods agree well, implying that the quasars are not likely to be strongly lensed We derive central black hole masses of (03-52) × 109 M☉ We use the difference between the redshift of Mg II (a proxy for the systemic redshift of the quasar) and the onset of the Gunn-Peterson trough to derive the extent of the ionized Stromgren spheres around our target quasars The derived physical radii are about 5 Mpc Using a simple ionization model, the emission of the central quasars would need of order 106-108 yr to create these cavities As the e-folding timescale for the central accreting black hole is on the order of a few times 107 yr, it can grow by one e-folding or less within this time span