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A. Sebrechts (CUA), F. Bruhweiler (CUA and GSFC/NASA), E. Verner (UDC/CUA/GSFC/NASA)
The QSO UV continuum is strongly affected by multitudinous weak, broadened Fe II lines producing an Fe II pseudo- continuum superposed upon the intrinsic continuum of the QSO. Several independent attempts have been made to estimate and subtract this somewhat uncertain Fe II contribution by the use of Fe II observational templates where the Fe II emission is measured in objects with recognizable and presumably easy to measure Fe II emission. The most popular object used to create Fe II observational templates is the narrow-lined Seyfert Galaxy, I Zw 1. For our presentation we summarize previous methods and our approach in measuring the Fe II flux in the UV. We make use of a sophisticated statistical equilibrium model (830 levels) for Fe II ion model and photoionization calculations in conjunction with HST/FOS data for I Zw 1. This represents a new approach at estimating the Fe II pseudo-continuum in QSOs. Our modeling also provides information about “spectral windows”, in which the QSO continuum is free from Fe II contamination.
AS and EV research and presentation at the AAS is supported by the National Science Foundation (Grant-NSF 0206150).
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Bulletin of the American Astronomical Society, 37 #4
© 2005. The American Astronomical Soceity.