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Table 8

Absorption and emission lines of QSO J1408-0346 and the strong Mg ii absorber at z = 1.77425 towards it.

λobs λrest Species Redshift E Wresta
(Å) (Å) (Å)

3658 911.20 Ly-limit 3.01
 ≈ 4168.8  ≈ 1033 Ly β + O  vi  ≈ 3.04
4888 1215.80 Ly α 3.02
4992.72 1239.42 N  v 3.028
5621.30 2026.14 Zn ii 1.77425 <0.73
6208.75 1548.20 C iv 3.010
6210.62 1548.20 C iv 3.011
6219.37 1550.77 C iv 3.010
6220.87 1550.77 C iv 3.011
6229.35 1545.86 C  iv 3.030
6503.52 2344.21 Fe ii 1.77425 <0.49
6610.51 2382.77 Fe ii 1.77425 0.84 ± 0.15
7145.59 2586.65 Fe ii 1.77425 <0.54
7213.61 2600.17 Fe ii 1.77425 0.62 ± 0.19
 ≈ 7674.8  ≈ 1910 Si  ii , C  iii /Fe  ii 3.018
7756.18 2796.35 Mg ii 1.77425 1.24 ± 0.34b
7777.52 2803.53 Mg ii 1.77425 1.25 ± 0.19

Notes. Summary of the most important absorption and emission lines of the quasar and the strong Mg ii absorber at z = 1.77425. We show only those absorption lines that are redward of the quasar Lyα emission line. Emission lines are displayed in bold.

(a)

The restframe EWs (1σ errors) and the 3σ detection limits are measured assuming an aperture of 333   km   s-1, i.e. 2 × FWHM a Gaussian with Doppler parameter b = 100   km   s-1.

(b)

The EW of the lines of the Mg ii doublet are similar, indicating that the lines are saturated.

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