Table 1.
Properties of the emission lines of GS-14, derived from the VIMOS spectrum and fitting the lines with a Gaussian profile.
| Line | λ0 | FWHM | F |
|---|---|---|---|
| (Å) | (Å) | (erg s−1 cms−2) | |
| O VI1032 Å |
 |
 |
 |
| N V1240 Å |
 |
 |
 |
| C II*1335 Å |
 |
 |
 |
| N IV] 1483 Å |
 |
 |
7.3 ± 1.3 × 10−18 |
| N IV] 1486 Å |
 |
 |
1.9 ± 0.3 × 10−17 |
Notes. λ0 refers to the observed-frame centroid, FWHM is the full width at half maximum, and F is the line flux. For the N V emission line, the values refer to the fit obtained after the stellar component of the P Cygni profile was subtracted. The O VI line lies in the Lyman forest and its continuum is not detected. Its flux should therefore be considered a lower limit.
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