Table 3.
Properties of the UV–optical broad emission line components derived from the HST COS (top panel) and STIS (bottom) spectra.
| Component: |
Intermediate |
Broad |
Very broad |
||||
|---|---|---|---|---|---|---|---|
| Line | λ0 [Å] | FWHM | Flux | FWHM | Flux | FWHM | Flux |
| Lyα | 1216 | 1470 ± 20 | 258 ± 4 | 3600 ± 70 | 250 ± 7 | 8800 ± 100 | 200 ± 10 |
| N V(a) | 1239 | ⋯ | ⋯ | 3530 ± 70 | 37 ± 3 | ⋯ | ⋯ |
| Si II(b) | 1260 | ⋯ | ⋯ | 3800 ± 800 | < 20 | ⋯ | ⋯ |
| O I(b) | 1302 | ⋯ | ⋯ | 2390 ± 40 | 23.4 ± 0.8 | ⋯ | ⋯ |
| C II(b) | 1335 | 1800 ± 400 | 2 ± 1 | ⋯ | ⋯ | ⋯ | ⋯ |
| Si IV, OIV], SIV](b) | 1394 | ⋯ | ⋯ | 5800 ± 100 | 37 ± 1 | ⋯ | ⋯ |
| NIV] | 1486 | ⋯ | ⋯ | 2200 ± 100 | 4.0 ± 0.5 | ⋯ | ⋯ |
| C IV(c) | 1548 | 1760 ± 20 | 220 ± 40 | 6090 ± 80 | 218 ± 4 | 12 000 ± 200 | 112 ± 5 |
| He II, OIII](c) | 1640 | ⋯ | ⋯ | 3000 ± 100 | 52 ± 2 | ⋯ | ⋯ |
| SiIII], CIII](b)(e) | 1909 | ⋯ | ⋯ | 5400 ± 200 | 35 ± 3 | ⋯ | ⋯ |
| Mg II(d) | 2796 | ⋯ | ⋯ | 2810 ± 40 | 58 ± 2 | ⋯ | ⋯ |
| Hδ | 4102 | ⋯ | ⋯ | 3300 ± 100 | 6.1 ± 0.5 | ⋯ | ⋯ |
| Hγ | 4340 | ⋯ | ⋯ | 4600 ± 200 | 8.6 ± 0.8 | ⋯ | ⋯ |
| He II | 4686 | ⋯ | ⋯ | 5500 ± 200 | 10.3 ± 0.5 | ⋯ | ⋯ |
| Hβ | 4861 | 1710 ± 40 | 18.9 ± 0.7 | 4400 ± 100 | 16 ± 1 | ⋯ | ⋯ |
| He I | 5876 | 2100 ± 100 | 5.2 ± 0.3 | 3400 ± 700 | 2.0 ± 0.4 | ⋯ | ⋯ |
| Hα | 6563 | 1800 ± 40 | 98 ± 4 | 3300 ± 200 | 42 ± 8 | 7800 ± 400 | 29 ± 3 |
Notes. The FWHM is given in units of km s−1 and the flux in 10−14 erg s−1 cm−2, measured at Earth’s distance (154 Mpc). The flux is corrected for line absorption and Galactic dust extinction.
Doublet, intermediate components modelled separately, broad and very broad together as one Gaussian each.
Possible contribution from a feature from the Fe III UV34 multiplet, as explained in Leighly & Moore (2004).
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