Table 4
Comparison between observed extinction-corrected optical and UV line fluxes and models.
| Line | Obs. | Nebua | ℳ0a | ℳ4a |
|
|
||||
| H i 4861 Å | 1000 | 1000 | 1000 | 1000 |
| H i 6563 Å | 2860 | 2841 | 2858 | 2854 |
| He i 4471 Å | 21.4 | 36.6 | 36.9 | 35.2 |
| He i 6678 Å | 25.3 | 27.0 | 28.1 | 26.7 |
| He i 7065 Å | 24.4 | 23.9 | 22.4 | 21.8 |
| He ii 4686 Å | 36.8 | 36.8 | 38.8 | 35.6 |
| [N ii] 6548+84 Å | 9.2 | 9.2 | 7.8 | 7.3 |
| [O i] 6300+63 Å | 8.5 | 8.6 | 9.9 | 9.0 |
| [O ii] 3726+9 Å | 238 | 236.8 | 207 | 203 |
| [O ii] 7320+30 Å | 6.3: | 6.6 | 5.7 | 5.4 |
| [O iii] 4363 Å | 65.9 | 66.0 | 65.6 | 66.3 |
| [O iii] 5007+4959 Å | 2683 | 2679.4 | 2691 | 2653 |
| [Ne iii] 3869 Å+968 Å | 191 | 191.2 | 224 | 219.9 |
| [S ii] 6716 Å | 22.5 | 18.9 | 20.7 | 19.0 |
| [S ii] 6731 Å | 16.9 | 14.0 | 15.5 | 14.4 |
| [S ii] 6716/6731 | 1.33 | 1.35 | 1.33 | 1.32 |
| [S iii] 6312 Å | 6.7 | 6.4 | 7.6 | 7.2 |
| [S iii] 9069+532 Å | 114 | 113 | 129.4 | 122 |
| [Ar iii] 7136+751 Å | 23.5 | 23.4 | 20 | 18.6 |
| [Ar iv] 4740 Å | 4.5 | 7.2 | 9.5 | 9.5 |
| [Fe iii] 4658 Å | 4.5 | 4.5 | 4.8 | 4.5 |
| [Fe iii] 4986 Å | 7.4 | 6.7 | ... | ... |
|
|
||||
| C iii] 1909+07 Å | 467 | 465 | 430 | 411 |
| Si iii] 1882 Å | 164: | 207 | 225 | 209 |
| C iv 1549 Å | 512: | 393. | 413 | ... |
|
|
||||
| log L(Hβ) (erg s-1) | 39.43 | 39.43 | 39.36 | 39.43 |
Notes. Fluxes are scaled with Hβ = 1000. Observed values for the optical lines are from Izotov & Thuan (1999), Skillman & Kennicutt (1993), and P08. Kehrig et al. (2015) provide a new integrated He ii flux, but the observed He ii intensity to be modeled, based on an average of the relatively stable He ii/Hβ intensity ratio measured in different slit spectra of I Zw 18-NW, is not changed.
See Sect. 4.2.
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