Abstract
We obtained far-ultraviolet spectra of the Seyfert 1 galaxy NGC 7469 using the Far Ultraviolet Spectroscopic Explorer on 1999 December 6. Our spectra cover the wavelength range 990-1187 A with a resolution of0:05 A. We see broad emission lines of Ciii ,N iii ,O vi ,a nd Heii as well as intrinsic absorption lines in the O vi1032; 1038 resonance doublet. The absorption arises in two distinct kinematic components at systemic velocities of 569 km s 1 and 1898 km s 1 . Both components are very highly ionized - no significant Ly absorption is present. The higher blueshift component is not quite saturated, and it has a total O vi column density of 8 10 14 cm 2 . It covers more than 90% of the continuum and broad- line emission. The lower blueshift component is heavily saturated and covers only 50% of the continuum and broad-line emission. It too has a column density of 8 10 14 cm 2 , but this is less certain due to the high saturation. We set an upper limit of<1:5 10 18 cm 2 on the O vi column density of this component. Its line depth is consistent with coverage of only the continuum, and thus this component may lie interior to the broad emission-line gas. The component at 569 km s 1 has a velocity comparable to the high-ionization X-ray absorption lines seen in the XMM-Newtongrating spectrum of NGC 7469, and photoionization models show that the observed column densities of O vi and H i are compatible with their formation in the same gas as that causing the X-ray absorption. The gas at 1898 km s 1 has lower ionization and column density, and no
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