Table 2: Parameters of the strongest narrow absorption and emission lines in the RGS spectrum of NGC 7469 (significant at >99.99% confidence in Fig. 4). Columns 1 to 6: $\lambda_{\rm rest,~meas}$, the measured wavelength in the (cosmological) rest frame in Å (O I $_{\rm Gal}$ is measured in the rest frame of our Galaxy); the line identification; $\lambda_{\rm rest,~lab}$, the theoretical rest frame wavelength of the line; EW, the equivalent width of the line in mÅ (negative values correspond to emission lines); FWHM, the line FWHM in km s-1; $v_{\rm shift}$, the redshift or blueshift of the line in km s-1.
$\lambda_{\rm rest,~meas}$ Line $\lambda_{\rm rest,~lab}$ EW FWHM $v_{\rm shift}$
$\rm 24.73^{+0.02}_{-0.01}$ N VII Ly$\alpha $ 24.781 $\rm 25_{-8}^{+5}$ $\rm0^{+600}_{-0}$ $\rm -570 ^{+240}_{-120}$
$23.51 \pm 0.02$ O IGal 23.521 $\rm 29_{-8}^{+10}$ $\rm0^{+940}_{-0}$ $\rm -180^{+240}_{-230}$
$22.06 \pm 0.01$ O VII f 22.101 $-67 \pm 15$ $\rm 980^{+1070}_{-980}$ $-550 \pm 160$
$21.72 \pm 0.03$ O VII i+ra   $\rm -68_{-18}^{+16}$ $\rm 2710^{+1270}_{-790}$ -
$18.88 \pm 0.02$ O VIII Ly$\alpha $ 18.969 $24 \pm 7$ $1240 \pm 910$ $\rm -1370^{+320}_{-360}$
$17.55 \pm 0.03$ Fe XVIII 17.591 $-9 \pm 5$ $\rm 20^{+1440}_{-20}$ $\rm -770^{+340}_{-460}$
$15.97 \pm 0.01$ O VIII Ly$\beta$ 16.006 $\rm 30_{-5}^{+6}$ $960 \pm 770$ $-610 \pm$ 230
$14.17 \pm 0.01$ Fe XVIII 14.210 $\rm 23_{-4}^{+8}$ $\rm0^{+2400}_{-0}$ $\rm -760^{+170}_{-210}$
$13.431 \pm 0.007$ Fe XIX/Ne IX He$\alpha $ 13.462b $61 \pm 6$ $1710 \pm 330$ $-690 \pm 160$
$12.83 \pm 0.01$ Fe XX 12.832 $35 \pm 8$ $\rm 1680^{+930}_{-1240}$ $-160 \pm 310$
a No laboratory wavelength or blueshift are listed for this feature, since it is a blend of lines whose apparent average wavelength is heavily dependent upon the physical conditions and geometry of the emitting region.
b Appropriately weighted by the relative abundances of iron and neon as listed by Anders & Grevesse (1989).

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