Optical FeII emission and the BLR structure in QSOs

Details Optical FeII emission and the BLR structure in QSOs Optical FeII emission and the BLR structure in QSOs

Nov 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989esasp.296.1027o&link_type=abstract

In ESA, The 23rd ESLAB Symposium on Two Topics in X Ray Astronomy. Volume 2: AGN and the X Ray Background p 1027-1031 (SEE N90-2

Astronomy and Astrophysics

Astronomy

H Beta Line, Iron, Lyman Spectra, Quasars, Spectral Line Width, Accretion Disks, Emission Spectra, Light (Visible Radiation), Spectral Bands, X Ray Spectra

Scientific paper

The relation that objects with flat soft X-ray spectra have weak optical Fe II emission is not confirmed for a sample of 34 Quasi Stellar Objects (QSOs). Objects with strong optical Fe II emission have narrow H beta lines. This trend is much weaker with Ly alpha. These relations imply that the Fe II and H beta lines arise from gas in a different geometrical arrangement to that emitting Ly alpha, possibly in the form of an accretion disk. Models of the Broad Line Region (BLR) in QSO are considered.

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