Rest-frame Optical Properties of High-Redshift Radio-Selected Broad Absorption Line Quasars

Details Rest-frame Optical Properties of High-Redshift Radio-Selected Broad Absorption Line Quasars Rest-frame Optical Properties of High-Redshift Radio-Selected Broad Absorption Line Quasars

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.4506r&link_type=abstract

American Astronomical Society, AAS Meeting #211, #45.06; Bulletin of the American Astronomical Society, Vol. 39, p.796

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Scientific paper

In order to further determine the nature of broad absorption line (BAL) quasars we observed near-infrared (rest frame optical) spectra of eight high redshift BAL quasars selected from the FIRST Bright Quasar Survey (FBQS).
All quasars including BALs seem to demonstrate a correlation of multiple optical properties, such as [O III] strength, Fe II strength, and H-alpha line width. This correlation suggests that there is some underlying physical driver behind these properties, though the nature of this driver is not yet clear. Low redshift, radio-quiet (RQ) BAL quasars are observed to be at one extreme of these properties, whereas high redshift, RQ BAL quasars are observed to be at one extreme for some but not all of these properties. Our sample of radio selected BAL quasars are also observed at the extreme of some properties such as Fe II and [O III] emission, but not others, such as H-alpha line width.
The predominant proposal for the physical driver behind these optical properties is accretion rate (L/Ledd). This explanation seems to work well for low redshift quasars, but seems to break down at higher redshift for which reason it was proposed that fuelling rate might actually be responsible. In order to directly test whether accretion rate might be driving the observed optical properties we made measurements of black hole mass and L/Ledd for the objects in our sample. We found that our measurements were consistent with similar quantities in high redshift RQ quasars.
This work was part of the Wyoming SURAP REU program funded by the NSF grant ASTR-0353760. We acknowledge support from the US National Science Foundation through grant AST 05-07781.

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