Table 4: Photoionization models for the absorbers in NGC 7469.
U ${\rm log}~N_{{\rm tot}}$ N(H I) N(O  VI) N(O  VII) N(O  VIII) N(C IV) N(N V)
  $\rm ( cm^{-2} )$ $\rm ( cm^{-2} )$ $\rm ( cm^{-2} )$ $\rm ( cm^{-2} )$      
6.0$^{\rm a}$ 20.55 $1.1\times10^{14}$ $8.0\times10^{14}$ $7.3\times10^{16}$ $1.3\times10^{17}$ $1.1\times10^{12}$ $1.0\times10^{13}$
  Observed: $(8.0 \pm 4.2)\times10^{14}$ $(8.0 \pm 3.0) \times10^{14}$ $(3^{+5}_{-3})\times10^{16}$ $(2^{+2}_{-1})\times10^{17}$ ... ...
0.2$^{\rm b}$ 18.58 $6.9\times10^{13}$ $5.5\times10^{14}$ $8.2\times10^{14}$ $2.0\times10^{13}$ $2.4\times10^{13}$ $4.3\times10^{13}$
  Observed: $(2.1 \pm 4.8)\times10^{13}$ $(8.0 \pm 2.3) \times10^{14}$ $<3\times10^{16}$ $<3\times10^{16}$ ... ...
0.08$^{\rm c}$ 18.58 $2.0\times10^{14}$ $6.7\times10^{14}$ $8.7\times10^{14}$ $2.9\times10^{12}$ $5.7\times10^{13~\rm d}$ $7.2\times10^{14~\rm e}$
$^{\rm a}$ This model is our best match to Component #1.
$^{\rm b}$ This model is our best match to Component #2.
$^{\rm c}$ This model corresponds to Component #2 at the epoch of the 1996 FOS observations.
$^{{\rm d}}$ For a Doppler width of 100 km s-1, the blue line in the doublet would have an equivalent width of 0.20 Å.
$^{{\rm e}}$ For a Doppler width of 100 km s-1, the blue line in the doublet would have an equivalent width of 0.16 Å.

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