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Table 1

Emission line properties.

Line Fluxa Dust corrected fluxb FWHM c EW d z
Lyα 15.4 ± 1.0 e 240 ± 60 f 94 ± 20 e 3.2183f± 0.003
Lyα (blue) 5.1 ... ... ... 3.2126 ± 0.005
Lyα (red) 10.3 ... ... ... 3.2183 ± 0.003
N vλ1240 <0.16 <0.4 ... ... ...
C ivλ1550 <0.18 <0.4 ... ... ...
He iiλ1640g 0.6 ± 0.3 ... ... ...
O iii]λ1666g 0.5 ± 0.3 ... ... ...
C iii]λ1909 1.3 ± 0.3 400 ± 90 h 3.2127
[O ii]λ3727i 1.5 ± 1.5 ... <50 3.2126
Hβg 1.5 ± 0.8 ... 112 ± 60 3.2128 ± 0.005
[O iii]λ4959 5.4 ± 0.8 (7.4 ± 1.1) 155 ± 70 365 ± 70 3.2128 ± 0.0008
[O iii]λ5007 22.1 ± 0.8 147 ± 30 1103 ± 60 3.2126 ± 0.0006

Notes.

(a)

Observed emission line flux and error corrected for slit losses (50%) in units of 10-17 erg s-1 cm-2. In parenthesis, the [O iii]λ4959 flux adopting the theoretical ratio [ O iii ] λ5007 / [ O iii ] λ4959 = 3 (Storey & Zeippen 2000).

(b)

The emission line dust correction method is described in Appendix A.

(c)

FWHM (instrumental corrected) and error in units of km s-1.

(d)

Equivalent width and error in units of Å.

(e)

Sum of the two components.

(f)

Main component.

(g)

Marginal detections (Fig. 6): S/N(O iii ] λ1666) ~ 1.7, S/N(He iiλ1640) ~ 2, and S/N(Hβ) ~ 2.

(h)

FWHM is the contribution of the two blended components, 1907–1909 Å.

(i)

The error is large because the line is on the top of a sky line (Fig. 4).

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