Table 1.
Results of the multi-component line fitting.
| (1) | (2) | (3) | (4) | (5) | (6) | (7) | (8) |
|---|---|---|---|---|---|---|---|
| Line | λrest | Comp | FWHM | Central velocity | Flux (obs) | S/N (obs) | Flux (corr) |
| [Å] | [km/s] | [km/s] | [erg/s/cm2] | [erg/s/cm2] | |||
| Pβ | 12821.6 | 1 | 3000 ± 100 | 10 ± 100 | 7.2 ± 1.0 ⋅ 10−16 | 55.0 | 9.2 ± 1.3 ⋅ 10−16 |
| 2 | 11900 ± 700 | 10 ± 100 | 1.1 ± 0.4 ⋅ 10−15 | 44.4 | 1.5 ± 0.5 ⋅ 10−15 | ||
| Total | 3800 ± 100 | 1.9 ± 0.4 ⋅ 10−15 | 72.2 | 2.4 ± 0.5 ⋅ 10−15 | |||
| Hα | 6564.6 | 1 | 800 ± 100 | 10 ± 100 | 5.2 ± 0.6 ⋅ 10−16 | 16.9 | 1.0 ± 0.1 ⋅ 10−15 |
| 2 | 2000 ± 100 | 10 ± 100 | 1.0 ± 0.1 ⋅ 10−15 | 27.4 | 2.0 ± 0.3 ⋅ 10−15 | ||
| 3 | 4600 ± 100 | 10 ± 100 | 5.8 ± 0.3 ⋅ 10−15 | 141.7 | 1.1 ± 0.1 ⋅ 10−14 | ||
| 4 | 11100 ± 100 | 10 ± 100 | 6.6 ± 0.8 ⋅ 10−15 | 156.6 | 1.3 ± 0.2 ⋅ 10−14 | ||
| Total | 3700 ± 100 | 1.4 ± 0.1 ⋅ 10−14 | 342.3 | 2.8 ± 0.2 ⋅ 10−14 | |||
| Hβ | 4862.7 | 1 | 800 ± 100 | 10 ± 100 | 1.2 ± 0.4 ⋅ 10−16 | 16.5 | 3.0 ± 1.0 ⋅ 10−16 |
| 2 | 2100 ± 100 | 10 ± 100 | 4.0 ± 0.9 ⋅ 10−16 | 38.7 | 1.0 ± 0.2 ⋅ 10−15 | ||
| 3 | 9300 ± 200 | 420 ± 100 | 3.1 ± 0.5 ⋅ 10−15 | 71.2 | 7.9 ± 1.1 ⋅ 10−15 | ||
| Total | 4300 ± 100 | 3.7 ± 0.5 ⋅ 10−15 | 82.9 | 9.2 ± 1.2 ⋅ 10−15 | |||
| Mg II | 2796, 2803 | 1 | 2300 ± 1000 | 10 ± 250 | 9.7 ± 7.3 ⋅ 10−16 | 30.0 | 3.7 ± 2.8 ⋅ 10−15 |
| 2 | 5100 ± 1600 | 10 ± 410 | 1.6 ± 1.5 ⋅ 10−15 | 31.0 | 5.9 ± 5.6 ⋅ 10−15 | ||
| Total | 3100 ± 1200 | 2.5 ± 1.7 ⋅ 10−15 | 50.2 | 9.6 ± 6.2 ⋅ 10−15 | |||
Notes. The first two columns note which line was fit and the corresponding rest-frame wavelength λrest, while the third column corresponds to an individual component (1,2,3) or refers to the composite spectral model (“total”). The fourth column specifies the FWHM of any individual component, or of the summed spectral profile. The fifth column refers to the central velocity shift with respect to the rest frame wavelength of the line (assuming a redshift of 2.948), and the sixth to the integrated flux of the observed line without extinction correction. The seventh column specifies the S/N of the component or total line, using an rms-based noise estimate over ±2σ from the central wavelength (for the total profile, we used the Gaussian σ of the broadest component), without dust correction. The final column is the extinction-corrected flux, according to the Balmer decrement. In the case of Mg II, the quantities are averaged over the two doublet lines (which were tied to have the same flux). Fluxes for the optical and UV lines have been corrected for Galactic extinction as specified in the text.
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