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 Å with a resolution of \sim 0.05 Å .
We see broad emission lines of C iii , N iii , O vi , and He ii as well as intrinsic absorption lines in the O vi \lambda \lambda 1032 , 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 \beta absorption is present .
The higher blueshift component is not quite saturated , and it has a total O vi column density of 8 \times 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 \sim 50 % of the continuum and broad-line emission .
It too has a column density of 8 \times 10 ^ { 14 } ~ { } cm ^ { -2 } , but this is less certain due to the high saturation .
We set an upper limit of < 1.5 \times 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-Newton grating 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 significant X-ray absorption is associated with it .