Table 5: Intensities and full width at half maximum ( FWHM) of the main emission lines in the spectrum of LBQS 2212-1759; all intensities are in units of ${\rm 10^{-16}~erg~cm^{-2}~s^{-1}}$ and have been corrected for galactic extinction. Their uncertainties are typically 10%. The FWHM are expressed in ${\rm km~s^{-1}}$ and have an uncertainty of ${\rm \pm50~km~s^{-1}}$ .
Line ID Flux FWHM

H-Ly $_{\alpha}\lambda$ 1216 204 1610

NV $\lambda$ 1240 132 4780

SiIV $\lambda$ 1397 50 3600

CIV $\lambda$ 1549 33 2790

HeII $\lambda$ 1640 ${\leq}$ 4 -

NIII] $\lambda$ 1750 25 2780

CIII] $\lambda$ 1909 49 5150

MgII $\lambda$ 2798 41 2590

**Table 5:** Intensities and full width at half maximum ( *FWHM*) of the main emission lines in the spectrum of LBQS 2212-1759; all intensities are in units of ${\rm 10^{-16}~erg~cm^{-2}~s^{-1}}$ and have been corrected for galactic extinction. Their uncertainties are typically 10%. The *FWHM* are expressed in ${\rm km~s^{-1}}$ and have an uncertainty of ${\rm \pm50~km~s^{-1}}$ .
Line ID	Flux	FWHM
H-Ly $_{\alpha}\lambda$ 1216	204	1610
NV $\lambda$ 1240	132	4780
SiIV $\lambda$ 1397	50	3600
CIV $\lambda$ 1549	33	2790
HeII $\lambda$ 1640	${\leq}$ 4	-
NIII] $\lambda$ 1750	25	2780
CIII] $\lambda$ 1909	49	5150
MgII $\lambda$ 2798	41	2590

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