Table 3: Table of emission lines used in this paper. Fluxes and EWs are as observed. Fluxes from the FORS spectrum are taken from Pian et al. (2006).
UVES spectrum
ID EW Flux
  (Å) ( $\times 10^{-17}$ erg s-1 cm-2)
$[O {\sc ii}]$ $\lambda $3727 1.59 $\pm$ 0.09 75.23 $\pm$ 3.42
$[O {\sc ii}]$ $\lambda $3729 2.62 $\pm$ 0.12 121.1 $\pm$ 4.0
$[Ne {\sc iii}]$ $\lambda $3869 0.75 $\pm$ 0.08 34.06 $\pm$ 3.51
$[Ne {\sc iii}]$ $\lambda $3969 0.26$\pm$ 0.06 11.80 $\pm$ 2.64
H$\beta$ $\lambda $4862 2.17 $\pm$ 0.06 92.92 $\pm$ 1.93
H$\gamma$ $\lambda $4341 0.90 $\pm$ 0.07 47.99 $\pm$ 3.46
H$\delta$ $\lambda $4102 0.61 $\pm$ 0.07 27.83 $\pm$ 3.04
H$\epsilon$ $\lambda $3971 0.29 $\pm$ 0.07 13.03 $\pm$ 3.02
H8 $\lambda $3889 0.27 $\pm$ 0.07 12.25 $\pm$ 2.90
H9 $\lambda $3835 0.18 $\pm$ 0.07 7.65 $\pm$ 2.92
$[O {\sc iii}]$ $\lambda $4960 2.88 $\pm$ 0.06 139.0 $\pm$ 2.08
$[O {\sc iii}]$ $\lambda $5008 8.34 $\pm$ 0.09 426.2 $\pm$ 2.48
$He {\sc i}$ $\lambda $5877 0.24 $\pm$ 0.04 9.55 $\pm$ 1.17
FORS spectrum
ID   Flux
    ( $\times 10^{-17}$ erg s-1 cm-2)
$[O {\sc ii}]$ $\lambda $3727, 3729   190 $\pm$ 50
(Doublet unresolved)    
$[Ne {\sc iii}]$ $\lambda $3869   31 $\pm$ 5
$[Ne {\sc iii}]$ $\lambda $3969   18 $\pm$ 3
H$\gamma$ $\lambda $4341   37 $\pm$ 6
$[O {\sc iii}]$ $\lambda $4364   21 $\pm$ 4
H$\beta$ $\lambda $4862   101 $\pm$ 4
$[O {\sc iii}]$ $\lambda $4960   150 $\pm$ 7
$[O {\sc iii}]$ $\lambda $5008   460 $\pm$ 10
$He {\sc i}$ $\lambda $5877   5.5 $\pm$ 1.0
H$\alpha$ $\lambda $6563   315 $\pm$ 25
$[N {\sc ii}]$ $\lambda $6584   19 $\pm$ 2
$[S {\sc ii}]$ $\lambda $6717   14 $\pm$ 2
$[S {\sc ii}]$ $\lambda $6731   14 $\pm$ 2


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